Journal of Double Star Observations

of Double Star Observations Page Journal of Double Star Observations April 22, 2016 Astronomical Association of Queensland Program of Measurements of Seven Southern Multiple Stars Graeme Jenkinson Astronomical Association of Queensland Program of Measurement of Nine Neglected Southern Multiple Stars Graeme Jenkinson Results of 194 Double Stars Measurements from Astrometric CCD Observations at the Nikolaev Observatory (Ukraine) Daniil Bodryagin, Larisa Bondarchuk, and Nadiia Maigurova Jonckheere Double Star Photometry Part II: Delphinus Wilfried R.A. Knapp Double Star Measurements for December 2013 Frank Smith Photometry of Faint and Wide Doubles in Vulpecula Wilfried R.A. Knapp and Chris Thuemen Inside this issue: Jonckheere Double Star Photometry Part III: Lyra, Equuleus, and Eridanus Wilfried R.A. Knapp STT Doubles with Large ΔM Part IV: Ophiuchus and Hercules Wilfried R.A. Knapp and John Nanson Measurements with Reticle Micrometer Performed by a New Double Stars Observing Group from Poland Marcin Biskupski, Natalia Banacka, Justyna Cupryjak, Małgorzata Malinowska, Kamil Bujel, Zdzisław Kołtek, Jarosław Mazur, Marcin Muskała, Łukasz Płotkowski, Barłomiej Prowans, and Paweł Szkaplewicz CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs:The Autumn 2015 Observing Program at Brilliant Sky Observatory, Part 1 Richard W. Harshaw CCD Measurements of 8 Double Stars With Binary Nature: The Autumn 2015 Observing Program at Brilliant Sky Observatory, Part 2 Richard W. Harshaw CCD Measurements of 141 Proper Motion Stars: The Autumn 2015 Observing Program at the Brilliant Sky Observatory, Part 3 Richard W. Harshaw Measurements of Multi-star Systems LEO 5 and MKT 13 Faisal AlZaben, Allen Priest, Stephen Priest, Rex Qiu, Grady Boyce, and Pat Boyce GJ 282 AB (WDS 07400-0336 AB = BGH 3 AB) and GICLAS 112-29: A Very Wide System in Process of Dissociation F. M. Rica and R. Benavides Meeting Announcement: Opportunities for Student Astronomical Research in Southern California San Diego, California, June 12, 2016 414 Meeting Announcement: Small Telescope Research Communities of Practice American Astronomical Society s 228 th Meeting (Meeting in a Meeting Special Session), San Diego, CA, June 13/14 Meeting Announcement: Society for Astronomical Sciences 2016 Symposium Ontario California, June 16-18, 2016 417 308 313 320 327 338 347 351 361 374 376 388 394 400 406 415

Page 308 Astronomical Association of Queensland Program of Measurements of Seven Southern Multiple Stars Graeme Jenkinson Astronomical Association of Queensland. bluestars@iprimus.com.au Abstract: This paper pr esents the r esults of a mid-2014 program of the Astronomical Association of Queensland of photographic measurements of seven southern multiple stars. The images were obtained using a Meade DSI CCD camera in conjunction with an equatorially mounted 150mm F8 refractor. For each target pair, either a 2x or 5x barlow lens was used as required. Image processing was carried out using Losse s REDUC software. Introduction These latest results are part of an ongoing program commenced in 2008 by the Double Star Section of the Astronomical Association of Queensland. The target stars were selected from the Washington Double Star Catalog (WDSC) and were observed in Queensland from a latitude of approximately 27 S. Method Once obtained with the equipment described above, the images were analyzed using the astrometric double star program REDUC (Losse, 2008). Approximately 10 stacked images of each target were taken per night for seven nights and the results averaged to obtain measures of separation and position angle with sufficient confidence. Full details of the method are given in Napier- Munn and Jenkinson (2009). Some recent work on the errors inherent in the method is described in Napier- Munn and Jenkinson (2014). The images were obtained using a Meade DSI CCD camera in conjunction with an equatorially mounted 150mm F8 refractor. For each target pair, either a 2x or 5x barlow lens was used as required. As proficiency has grown in the use of this equipment with the 150mm refractor, close doubles with considerable magnitude difference between the components have been successfully measured. Results For all of the systems the WDSC information is first reproduced, showing the epoch 2000 position, magnitudes, separation, PA, and the last recorded measurement. The new measurements are then given in tabular form (Tables 2-8), including the mean and standard deviation and 95% confidence limits. Any uncertainties between the images and the last recorded measurements are discussed. Finally a conclusion is given as to whether any movement of the component stars has occurred in PA or separation, based on the P-value for the t-test comparing the new mean values with the cataloged value (P < 0.05 is considered as evidence of change). System Table 1. Summary of Measurements of Seven Multiple Stars Last listed measure New measure PA º Sep. " Epoch PA º Sep. " Epoch* Comment B2350 Libra 202.0 9.3 1999 203.70 9.34 2014.335 Slow movement HO554A-B Oph. 359.0 9.8 1904 355.89 9.59 2014.502 Definite change in PA HO554A-C Oph 350.0 35.3 1999 350.08 35.94 2014.502 Possible increase in sep. I 428 Circinus 315.0 11.0 2000 314.77 11.13 2014.330 No probable movement I 1282 Scorpius 248.0 12.1 1998 251.39 12.70 2014.461 Definite change in PA SEE114A-B Antlia 298.0 47.3 1999 298.57 52.58 2014.239 Changes since 1 st measure SEE234 Lupus 38.0 13.0 1999 37.04 13.33 2014.384 Little change * Epochs of new measures given in Besselian years as the average of the observations making up the measure.

Page 309 Measurements of Seven Southern Multiple Stars The mean 95% confidence intervals for the new measures were ± 0º.305 in PA and ± 0².082 in separation. The results are presented in Table 1. Acknowledgements This research has made use of the Washington Double Star Catalog maintained at the U.S. Naval Observatory. References Losse F., Reduc software, V4.5.1. http:// www.astrosurf.com/hfosaf/uk/tdownload.htm Napier-Munn, T. J. and Jenkinson, G. 2009, "Measurement of Some Neglected Southern Multiple Stars in Pavo", Webb Society Double Star Section Circular 17, 6-12. Napier-Munn, T.J. and Jenkinson, G., 2014, "Analysis of Errors in the Measurement of Double Stars Using Imaging and the Reduc Software", Journal of Double Star Observations, 10, 193-198. Argyle, Bob, 2004, Observing and Measuring Visual Double Stars, Springer Table 2. Measurements of B 2350 B2350 RA. 15 09.9 DEC. -23 59 Last Measure 1999 Libra MAG. 6.8 & 12.5 PA. 202.0 SEP. 9.3" Date No. images PA Sep" 19 Apr 2014 10 204.26 9.248 21 Apr 2014 10 203.13 9.352 23 Apr 2014 10 203.90 9.489 25 Apr 2014 10 203.80 9.376 03 May 2014 10 203.76 9.396 21 May 2014 10 203.75 9.340 24 May 2014 10 203.31 9.156 Mean 203.701 9.337 Standard dev. 0.376 0.107 95% CI +/- 0.347 0.099 P(t) movement 0.000 0.400 COMMENTS: Slow changes evident since the first measures in 1953 of 201 and 10.3" Table 3. Measurements of HO 554 AC HO554A-C RA. 17 01.2 DEC. -29.41 Last Measure 1999 Ophiuchus MAG. 9.13 & 11.59 PA. 350.0 SEP. 35.3" Date No. images PA Sep" 27 June 2014 10 350.26 35.960 29 June 2014 10 350.20 35.893 30 June 2014 10 349.87 35.880 2 July 2014 10 349.73 36.003 3 July 2014 10 350.17 35.925 5 July 2014 10 350.12 35.972 8 July 2014 10 350.21 35.940 Mean 350.080 35.939 Standard dev. 0.200 0.044 95% CI +/- 0.185 0.040 P(t) movement 0.000 0.000 COMMENTS: A small increase in separation may have occurred in the last 15 years.

Page 310 Measurements of Seven Southern Multiple Stars Table 4. Measurements of I 428 I 428 RA. 15 16.6 DEC. -60 54 Last Measure 2000 Circinus MAG. 5.8 & 11.6 PA. 315.0 SEP. 11.0" Date No. images PA Sep" 18 Apr 2014 10 314.63 11.194 19 Apr 2014 10 314.60 11.097 21 Apr 2014 10 314.80 11.143 23 Apr 2014 10 314.86 11.041 25 Apr 2014 10 314.93 11.121 01 May 2014 10 314.43 11.071 17 May 2014 10 315.13 11.262 Mean 314.769 11.133 Standard dev. 0.234 0.076 95% CI +/- 0.216 0.070 P(t) movement 0.000 0.004 COMMENTS: No probable movement in the last 14 years. Table 5. Measurements of I 1282 I 1282 RA. 16 02.7 DEC. -29 08 Last Measure 1998 Scorpius MAG. 6.03 & 13.0 PA. 248.0 SEP. 12.1" Date No. images PA Sep" 25 May 2014 10 251.51 12.966 18 June 2014 10 251.50 12.794 22 June 2014 10 251.35 12.592 25 June 2014 10 251.72 12.713 26 June 2014 10 251.82 12.728 27 June 2014 10 250.89 12.489 29 June 2014 10 250.96 12.611 Mean 251.393 12.699 Standard dev. 0.355 0.155 95% CI +/- 0.328 0.144 P(t) movement 0.000 0.000 COMMENTS: Definite movement in PA, small increase in separation possible.

Page 311 Measurements of Seven Southern Multiple Stars Table 6. Measurements of SEE 114 AB SEE114 A-B RA. 09 31.6 DEC. -35 43 Last Measure 1999 Antlia MAG. 6.0 & 12.8 PA. 298.0 SEP. 47.3" Date No. images PA Sep" 28 Feb 2014 10 298.67 52.616 7 Mar 2014 10 298.55 52.632 13 Mar 2014 10 298.51 52.682 29 Mar 2014 10 298.72 52.500 30 Mar 2014 10 298.52 52.610 31 Mar 2014 10 298.50 52.502 18 April 2014 10 298.51 52.543 Mean 298.569 52.584 Standard dev. 0.089 0.070 95% CI +/- 0.082 0.064 P(t) movement 0.000 0.000 COMMENTS: Considerable increase in separation since the first measure of 23.6" in 1897. Position angle has also increased from 283 at that time. Table 7. Measurements of SEE 234 SEE234 RA. 15 28.5 DEC. -51 36 Last Measure 1999 LUPUS MAG. 6.1 & 12.5 PA. 38.0 SEP. 13.0" Date No. images PA Sep" 25 Apr 2014 10 36.65 13.361 3 May 2014 10 37.90 13.319 21 May 2014 10 36.51 13.208 24 May 2014 10 36.87 13.463 25 May 2014 10 36.77 13.363 26 May 2014 10 37.55 13.251 7 June 2014 10 37.06 13.335 Mean 37.044 13.329 Standard deviation 0.506 0.083 95% CI +/- 0.468 0.076 P(t) movement 0.000 0.000 COMMENTS: Very slow changes since the first measure in 1897 of 31 and 14.0"

Page 312 Measurements of Seven Southern Multiple Stars Table 8. Measurements of HO 554 AB HO554A-B RA. 17 01.2 DEC. -29 41 Last Measure 1904 Ophiuchus MAG. 7.9 & 12.9 PA. 359.0 SEP. 9.8" Date No. images PA Sep" 27 June 2014 10 355.95 9.586 29 June 2014 10 356.39 9.545 30 June 2014 10 355.34 9.410 2 July 2014 10 355.43 9.648 3 July 2014 10 355.29 9.645 5 July 2014 10 356.67 9.634 8 July 2014 10 356.17 9.649 Mean 355.891 9.588 Standard deviation 0.550 0.088 95% CI +/- 0.509 0.081 P(t) movement 0.000 0.000 COMMENTS: Definite movement in PA and negligible change in separation in the last 110 years.

Page 313 Astronomical Association of Queensland Program of Measurement of Nine Neglected Southern Multiple Stars Graeme Jenkinson Astronomical Association of Queensland E-mail: bluestars@iprimus.com.au Abstract: Through the first half of 2015 measurements were completed for the following nine southern multiple stars as listed in the Washington Double Star Catalog. Using a 400mm F4.5 Newtonian reflector fitted with a Meade DSI 2 camera and software programme Astro- Planner V2.1 (Rodman) the obtained images were analyzed using Losse s REDUC software. Introduction These latest results are a continuation of the Astronomical Association of Queensland s program of measuring neglected southern multiple stars. Observed from an approximate latitude of 27 S, target stars were selected from the WDSC that met the criteria of a minimum of fifteen years since the last measure and preferably with very few previous observations. Method All images were obtained using a Meade DSI 2 CCD camera coupled to an equatorially mounted 400mm F4.5 Newtonian reflector. Separations and position angles were measured using the software program REDUC (Losse), which is specifically designed to measure double stars, using appropriate images of the target pairs together with images of calibration pairs of known separation and PA; Argyle s list of calibration pairs was used for this purpose (Argyle, 2004). For this optical/camera (Sony ICX429 752x582 pixel sensor) combination a FOV of approximately 0.2 was calculated using Argyle s list. The use of REDUC requires input of the image scale of the particular camera/scope combination. By using the same information from the calibration pairs, the image scale mean can be calculated over a number of nights. In this case 10 images themselves consisting of 10 stacked images per night over 7 nights provided the necessary information to calculate the mean. Using this optical assembly to image calibration pairs Beta Tucanae, Theta Serpens, and Omicron Capricorni, raw image scales varied from 0.940 to 0.978, with a mean figure of 0.96260" per pixel. This figure is then used in REDUC for all the target star reductions. The imaging and reduction methods were described in detail in Napier-Munn & Jenkinson 2009. In order to obtain statistically viable results, the DSI software is used to stack a minimum of 10 individual good quality images as they are acquired, to generate one image for measuring. About 10 such images are obtained per pair per night, plus 3 trailed images with the tracking switched off in order to calibrate the E-W axis in the images. The REDUC software is then used to generate a single average measure for the 10 images. This process is repeated on 6-7 separate nights, generating mean separations and position angles together with standard deviations from which a confidence interval for the measurement can be calculated and a decision made as to whether there has been a statistically significant change in PA or separation. Results The results are presented below, in order of increasing RA. For each system, the current WDSC information is first reproduced, including the epoch 2000 position, magnitudes (if known), PA, separation, and year of last measure. The new measures are then given

Page 314 Measurement of Nine Neglected Southern Multiple Stars in tabular form, including the date of measurement, mean, standard deviation, and 95% confidence limits (from the formula st / n, where t is the value of t for a 2-sided probability level (in this case = 0.05), s is the sample standard deviation, and n is the number of observations). An example of a relevant image used in the measures is included. A conclusion is then given as to whether the pair has moved or not. This is based on judicious interpretation of three criteria in terms of both PA and separation: 1. t-tests for a single sample mean comparing the new mean PA and separation values with the single values given in the WDSC; P 0.05 was taken as evidence of movement (that is, the new mean is significantly different to the single value reported in the WDSC, with 95% or more confidence). 2. Whether the last measure as recorded in the WDSC lies within the 95% confidence interval of our new measure (suggesting no movement) or not (suggesting movement). 3. The absolute size of the change; a statistically significant change that is very small is still very small and may not be of practical significance. Note that in a separate paper (Napier-Munn & Jenkinson 2014) we have shown that the uncertainty in PA increases with decrease in separation, and the uncertainty in separation increases with increase in separation, for reasons discussed in that paper. Uncertainty here is defined as the standard deviation of repeated measures. The mean 95% confidence intervals for the new measures were ± 0.589 in PA and ± 0.134" in separation. The results are given in Table 1. Details of each measure are given in Tables 2 through 10 with examples of the measured images. Acknowledgements This research has made use of the Washington Double Star Catalogue maintained at the U.S. Naval Observatory. References Losse F., Reduc software, V4.5.1. http:// www.astrosurf.com/hfosaf/uk/tdownload.htm Napier-Munn, T. J. and Jenkinson, G. 2009,"Measurement of Some Neglected Southern Multiple Stars in Pavo", Webb Society Double Star Section Circular 17, 6-12. Napier-Munn T.J. and Jenkinson, G. 2014, "Analysis of Errors in the Measurement of Double Stars Using Imaging and the Reduc Software", Journal of Double Star Observations, 10, 193-198. Argyle, Bob, 2004, Observing and Measuring Visual Double Stars, Springer Table 1. Summary of Measurements of Nine Multiple Stars. System Last listed measure New measure PA º Sep. " Epoch PA º Sep. " Epoch* Comment BU1419BC Puppis 300.0 7.8 1903 297.08 8.00 2015.083 Possible small PA change SEE98 Puppis 67.0 5.9 1928 66.35 5.08 2015.043 Little evident movement B2659 Pyxis 265.0 8.0 1932 172.79 18.61 2015.099 Large apparent movement B2263 Vela 315.0 7.0 1932 21.63 12.38 2015.099 Considerable movement CPO327 Centaurus 321.0 7.6 1930 324.34 6.55 2015.178 Movement RST3746AB Cen 317.0 16.0 1944 325.97 14.81 2015.178 Clear movement ARA1790 Corvus 184.0 11.3 1922 151.60 47.63 2015.303 Questionable Sep. change RSS370 Lupus 148.0 7.2 1976 149.64 7.52 2015.308 Possible small PA RSS386 TrA 270.0 10.3 1974 14.63 10.31 2015.308 Questionable PA change * Epochs of new measures given in Besselian years as the average of the observations making up the measure.

Page 315 Measurement of Nine Neglected Southern Multiple Stars Table 2. Measurements of BU 1419 BC. RA. 08 08.5 DEC. -19 52 Last Measure 1903 BU1419BC MAG. 7.55 & Puppis PA. 300.0 SEP. 7.8" 13.0 Date No. images PA Sep" 16 January 2015 11 298.440 8.034 17 January 2015 10 297.130 8.113 30 January 2015 10 295.310 7.915 31 January 2015 9 298.250 7.777 6 February 2015 11 296.550 8.125 14 February 2015 10 297.380 8.131 15 February 2015 10 296.520 7.924 Mean 297.083 8.003 Standard dev. 1.083 0.135 95% CI +/- 1.002 0.125 P(t) movement 0.000 0.007 COMMENTS: Possible slight movement in PA over the last 112 years. Table 3. Measurements of HO 554 AC. SEE98 RA. 08 14.9 DEC. -35 41 Last Measure 1928 Puppis MAG. 6.7 & 12.7 PA. 67 SEP. 5.9" Date No. images PA Sep" 6 January 2015 10 66.540 5.125 7 January 2015 10 66.380 5.134 8 January 2015 10 67.220 5.275 16 January 2015 10 66.750 5.612 17 January 2015 10 65.690 4.835 30 January2015 10 65.620 4.789 31 January 2015 10 66.220 4.787 Mean 66.346 5.080 Standard dev. 0.569 0.305 95% CI +/- 0.526 0.282 P(t) movement 0.000 0.000 COMMENTS:Little movement evident since 1929.

Page 316 Measurement of Nine Neglected Southern Multiple Stars Table 4. Measurements of B 2659. RA. 08 29.5 DEC. -18 45 Last Measure 1932 B2659 MAG. 7.7 & Pyxis PA. 265.0 SEP. 8.0" 13.2 Date No. images PA Sep" 17 January 2015 10 172.440 18.464 30 January 2015 10 172.940 18.639 31 January 2015 11 172.270 18.564 6 February 2015 10 173.220 18.625 14 February 2015 10 172.700 18.746 23 February 2015 10 173.020 18.607 24 February 2015 10 172.910 18.612 Mean 172.786 18.608 Standard dev. 0.336 0.085 95% CI +/- 0.310 0.078 P(t) movement 0.000 0.000 COMMENTS: Large apparent movement in both axes since the only previous measurement in 1932 warrants further investigation. B2263 Vela Table 5. Measurements of B 2263. RA. 11 03.2 DEC. -51 00 Last Measure 1932 MAG. 7.8 & 13.0 PA. 315.0 SEP. 7.0" Date No. images PA Sep" 17 January 2015 10 21.660 12.232 30 January 2015 10 21.870 12.184 6 February 2015 10 21.000 12.407 14 February 2015 10 21.040 12.346 21 February 2015 10 23.330 12.143 23 February 2015 10 22.330 12.594 24 February 2015 9 21.880 12.497 Mean 21.630 12.377 Standard dev. 0.521 0.156 95% CI +/- 0.547 0.164 P(t) movement 0.000 0.000 COMMENTS: Poor seeing on 21 February 2015 results deleted from calculation of mean. Considerable movement apparent since the only previous measure in 1932.

Page 317 Measurement of Nine Neglected Southern Multiple Stars Table 6. Measurements of CPO 327. CPO327 RA. 11 31.1 DEC. -43 33 Last Measure 1930 Centaurus MAG. 8.0 & 12.8 PA. 321.0 SEP. 7.6" Date No. images PA Sep" 21 February 2015 10 324.540 6.245 27 February 2015 10 325.720 6.348 7 March 2015 10 322.320 6.667 12 March 2015 10 323.680 6.532 14 March 2015 10 323.980 6.538 17 March 2015 10 325.640 6.710 19 March 2015 10 324.500 6.796 Mean 324.340 6.548 Standard dev. 1.177 0.198 95% CI +/- 1.088 0.183 P(t) movement 0.000 0.000 COMMENTS: Increase in PA and decrease in separation appear consistent with the two previous measures in 1902 and 1930. Table 7. Measurements of RST 3746 AB. RST3746AB RA. 11 35.8 DEC. -63 01 Last Measure 1944 CENTAURUS MAG. 3.12 & 11.5 PA. 317.0 SEP. 16.0" Date No. images PA Sep" 21 February 2015 10 326.260 14.684 27 February 2015 10 326.310 14.882 7 March 2015 10 325.880 14.774 12 March 2015 10 325.650 14.998 13 March 2015 10 326.020 14.510 14 March 2015 10 325.830 15.163 17 March 2015 10 325.830 14.640 Mean 325.969 14.807 Standard dev. 0.242 0.224 95% CI +/- 0.224 0.207 P(t) movement 0.000 0.063 COMMENTS: Changes in PA & separation consistent with two previous measures in 1937 & 1944.

Page 318 Measurement of Nine Neglected Southern Multiple Stars Table 8. Measurements of ARA 1790. ARA 1790 RA. 12 06.2 DEC. -22 47 Last Measure 1922 Corvus MAG. 8.8 & 11.1 PA. 184.0 SEP. 11.3" Date No. images PA Sep" 16 April 2015 10 151.660 47.566 17 April 2015 10 151.720 47.724 22 April 2015 10 151.680 47.550 24 April 2015 10 151.680 47.479 26 April 2015 10 151.150 47.511 28 April 2015 10 151.510 47.773 29 April 2015 10 151.790 47.781 Mean 151.599 47.626 Standard dev. 0.215 0.129 95% CI +/- 0.199 0.119 P(t) movement 0.000 0.000 COMMENTS:Large increase in separation over 93 years. Change in PA relative to separation change seems viable. Table 9. Measurements of RSS 370. RSS 370 RA. 15 17.0 DEC. -39 57 Last Measure 1976 Lupus MAG. 8.64 & -- PA. 148.0 SEP. 7.2" Date No. images PA Sep" 14 April 2015 11 150.100 7.498 17 April 2015 10 150.230 7.520 18 April 2015 10 149.740 7.559 24 April 2015 10 151.040 7.587 26 April 2015 10 149.240 7.504 04 May 2015 10 148.840 7.615 05 May 2015 10 148.290 7.394 Mean 149.640 7.525 Standard dev. 0.927 0.072 95% CI +/- 0.857 0.067 P(t) movement 0.003 0.000 COMMENTS: Possible small increase in PA since the only previous measure in 1976.

Page 319 Measurement of Nine Neglected Southern Multiple Stars Table 10. Measurements of RSS 386. RSS 386 RA. 15 48.6 DEC. -65 14 Last Measure 1974 Triangulum Aust. MAG. 8.6 & 12.0 PA. 270 SEP. 10.3" Date No. images PA Sep" 16 April 2015 10 14.460 10.246 17 April 2015 10 14.330 10.388 18 April 2015 10 13.590 10.285 24 April 2015 10 15.140 10.159 04 May 2015 10 14.870 10.378 05 May 2015 10 15.400 10.319 08 May 2015 10 14.610 10.364 Mean 14.629 10.306 Standard dev. 0.593 0.083 95% CI +/- 0.549 0.077 P(t) movement 0.000 0.864 COMMENTS: No change in separation makes large change in PA questionable over the last 41 years.

Page 320 Results of 194 Double Stars Measurements from Astrometric CCD Observations at the Nikolaev Observatory (Ukraine) Daniil Bodryagin, Larisa Bondarchuk, and Nadiia Maigurova Research Institute "Nikolaev Astronomical Observatory", Nikolaev, Ukraine daniilmaomail@gmail.com Abstract: This paper presents the results of double stars measurements from CCD observations at the 50-cm telescope of the Nikolaev Observatory. The accurate positions at current epoch and proper motions were obtained for 194 WDS pairs. The position angles and separations were measured using REDUC software. The measures standard errors were 0.05" for separations and 0.2 for position angles. Instruments These observations were carried out in Nikolaev Astronomical Observatory subordinated to Ministry of Education and Science of Ukraine. The observatory is located at an altitude of 52 m above sea level, the geographic coordinates are longitude 31 o 58 E, and latitude 46 o 58 N [1]. The observations were made at the mobile multi-channel automatic telescope (Mobitel, Figure 1), which was created in the RI NAO. The main telescope is a Maksutov telescope (D = 500 mm, F = 3000 mm), that is equipped with an Alta U9000 CCD camera from Apogee Imaging Systems. The CCD has a sensor array of 3056 by 3056 pixels, and each pixel is 12 microns square which allows us to obtain imaging with scale 0.83"/pixel and FOV = 42.6 42.6 in drift scan mode. That system enables us to obtain a sufficient number of reference stars for astrometric reduction in the UCAC4 catalog. For most stars the mean FWHM is less than 3". Program and Processing For the observational program, we selected WDS catalog [2] objects which are most appropriate to be observed by our telescope in the expected time frame (the full time of exposure is 85 s at the equator). For the main selection criteria we used a magnitude limit of 17 and a separation bigger than two FWHM. We also measured other WDS doubles from the observation volume, which appeared in the imaged field. All raw frames were processed using Astrometrica Figure 1: The mobile multi-channel automatic telescope (Mobitel) [3] software. The star positions were obtained using reference stars from UCAC4 catalog [4]. Equatorial coordinates were calculated for all objects in the field of view. The mean number of observations per star was about 8. The coordinates in right ascension and declination at mean observational epoch were averaged. Then we cross-matched our positional data with WDS catalog and other astronomical catalogs for calculating the primary and secondary components proper motions and

Page 321 Results of 194 Double Stars Measurements from Astrometric CCD Observations at the Nikolaev... selecting all WDS doubles which appeared in the imaged field. Measurement The measurements of doubles were made with RE- DUC software [5]. For calibration, we used previously determined exact values of orientation angle and image inclination regarding the celestial equator from astrometric reductions. Position angle (Theta), separation (Rho), and their standard deviations were measured for each WDS double. The relationship between the standard error of the positional angle and separation measurements versus the separation are shown in Figure 2. Summary of the measurements is presented in Table 1. The table data set also includes estimation of magnitude difference between components made by REDUC software, date of observation, and number of observations for each WDS object. References 1. http://www.mao.nikolaev.ua/ 2. Mason B.D. et al: 2001, Astron. J., 122, 3466 3. http://www.astrometrica.at/ 4. Zacharias N. et al: 2013, Astron. J., 145, 44Z 5. http://www.astrosurf.com/hfosaf/index.htm Figure 2. Standard errors in positional angle (left) and separation vs separation.

Page 322 Results of 194 Double Stars Measurements from Astrometric CCD Observations at the Nikolaev... Table 1. Results of measurements of the 194 doubles stars using REDUC software. WDS no mag * Theta Std_Theta Rho Std_Rho Y M D N 00109+1705 5.82 98.1 1.5 13.46 0.27 2014 9 15 5 00146+2508 0.17 229.3 0.7 8.04 0.21 2014 10 11 9 00152+2454 1.38 159.6 0.2 31.27 0.15 2014 10 11 10 00197+1951 0.18 262.5 0.2 52.83 0.07 2014 10 9 10 00320+2509 1.32 228.9 0.2 38.10 0.12 2014 10 12 10 00374-0714 2.11 50.3 0.4 35.75 0.19 2014 10 11 9 00509+1215 2.82 95.6 1.1 24.36 0.43 2014 10 9 5 00541+1247 0.39 251.5 0.3 14.55 0.15 2014 10 1 10 00599+1400 2.54 158.5 0.2 45.74 0.21 2014 10 12 10 01116+0446 0.55 357.69 0.03 163.16 0.17 2014 10 6 8 01242+1254 0.03 217.1 0.1 28.58 0.30 2014 10 19 10 01493+1808 2.45 24.0 0.8 21.09 0.12 2014 10 14 10 01496+1741 4.17 343.9 0.2 24.30 0.13 2014 10 14 4 01598+1543 0.79 327.1 0.2 75.65 0.17 2014 10 19 10 02154+1126 0.98 162.7 0.3 43.19 0.31 2014 10 19 10 02476+1706 0.36 329.1 0.6 26.20 0.21 2014 10 19 10 02595+2440 0.59 210.5 0.4 13.73 0.12 2014 9 17 10 03134-0852 3.69 150.7 1.4 33.08 1.24 2014 10 19 10 03214+0803 1.01 84.5 1.2 4.31 1.23 2014 9 17 10 03216+0821 2.8 248.8 0.6 17.19 0.14 2014 9 17 10 03299+2417 3.48 13.5 0.2 26.17 0.37 2014 10 19 9 03308+2511 2.15 309.6 0.2 17.08 0.07 2014 9 19 5 03311+2437 1.55 50.5 0.1 14.47 0.08 2014 9 19 6 03308+2451 0.28 96.4 0.4 14.14 0.06 2014 9 19 5 03426+2430 0.59 344.5 2.2 3.54 0.71 2014 9 17 10 03435+2424 3.04 270.0 0.2 56.12 0.13 2014 9 17 10 03572-0706 2.13 104.4 0.2 65.73 0.06 2014 9 19 3 04026+1230 1.43 122.4 0.2 52.18 0.20 2014 9 14 7 04029+1228 1.25 339.7 0.2 39.78 0.18 2014 9 14 7 09225-0454 2.17 238.1 2.3 8.06 0.19 2014 3 18 10 09228-0516 3.37 309.9 0.3 33.64 0.22 2014 3 18 10 13040+2249 0.12 196.0 0.2 53.50 0.22 2014 3 21 9 13334+0636 1.92 78.2 0.1 165.13 0.22 2014 3 21 10 14491+0720 2.83 42.3 0.3 28.37 0.07 2013 4 29 10 16144+2740 0.04 39.7 0.2 38.08 0.03 2013 4 29 10 16244+3250 1.38 287.4 1.0 10.09 0.17 2013 5 25 10 16255+1944 0.14 339.8 0.5 7.87 0.09 2013 6 11 10 17018+1746 0.24 106.8 0.1 117.23 0.08 2013 5 27 10 17037+1336 0.0 116.55 0.01 304.94 0.03 2014 3 31 10 17126+1609 0.48 200.2 2.8 7.45 0.24 2013 6 19 10 17427+2459 0.08 123.9 1.5 6.44 0.12 2013 5 20 10 17512+2946 0.67 146.9 0.8 7.61 0.20 2013 7 11 10 17599+0435 0.41 359.7 0.2 26.98 0.11 2014 7 26 10 Table 1 continues on next page.

Page 323 Results of 194 Double Stars Measurements from Astrometric CCD Observations at the Nikolaev... Table 1 (continued). Results of measurements of the 194 doubles stars using REDUC software. WDS no mag * Theta Std_Theta Rho Std_Rho Y M D N 18048+1253 0.56 277.1 0.4 18.62 0.13 2014 7 26 10 18057+1253 0.88 271.5 0.6 10.95 0.09 2014 7 26 10 18328+0633 1.05 58.3 0.6 12.16 0.09 2013 6 11 10 18331+0649 0.24 342.7 1.0 7.76 0.06 2013 6 11 10 18490+2405 0.81 273.4 1.0 9.58 0.15 2013 6 11 10 18491+2405 1.31 255.6 1.0 8.76 0.19 2013 6 11 10 18493+2411 0.9 106.5 1.3 7.47 0.26 2013 6 11 10 18499+2403 0.26 176.0 0.3 15.46 0.11 2013 6 11 9 18502+2414 0.88 169.5 0.5 8.90 0.11 2013 6 11 10 19328+1219 0.62 31.4 0.2 41.92 0.11 2013 7 9 10 19329+1223 1.54 148.7 0.1 112.96 0.14 2013 7 9 10 19332+1241 0.93 58.60 0.03 293.43 0.09 2013 7 9 10 19333+1248 0.49 193.9 0.1 37.64 0.05 2013 7 9 10 19338+1247 0.38 4.90 0.04 87.30 0.11 2013 7 9 5 19461+0131 0.51 257.1 0.4 10.38 0.07 2013 7 9 10 19503+1148 1.19 68.3 0.1 73.84 0.17 2013 6 11 10 19511+1140 1.34 237.84 0.04 140.99 0.12 2013 6 11 10 19568+2516 1.94 322.3 0.3 10.84 0.13 2013 6 19 6 20029+1328 0.36 56.56 0.02 80.40 0.14 2013 6 19 3 20030+1328 0.48 169.7 0.2 56.61 0.16 2013 6 19 3 20033+1354 0.82 40.31 0.05 47.94 0.08 2013 6 19 3 20033+1347 2.02 140.85 0.03 117.17 0.05 2013 6 19 3 20221+0331 2.56 217.4 0.5 20.51 0.13 2013 6 11 10 20253+0355 1.51 87.0 0.3 20.53 0.08 2013 6 11 10 20305+2411 0.45 220.0 0.2 20.56 0.10 2013 6 11 10 20305+2358 1.31 140.9 0.4 19.05 0.07 2013 6 11 10 20306+2417 0.79 228.9 0.3 17.91 0.13 2013 6 11 10 20306+2406 0.16 59.3 0.1 16.16 0.12 2013 6 11 10 20308+2416 0.27 248.5 0.3 22.51 0.14 2013 6 11 10 20308+2404 1.26 227.0 0.9 8.33 0.29 2013 6 11 10 20311+2429 0.15 281.8 0.4 13.17 0.11 2013 6 11 10 20313+2406 0.97 245.3 0.3 11.81 0.11 2013 6 11 6 20359+2331 0.87 292.8 0.4 17.90 0.10 2014 9 19 8 20359+2327 1.07 152.1 0.6 18.42 0.11 2014 9 19 8 20365+2334 2.35 56.6 0.2 18.28 0.10 2014 9 19 8 20365+2327 1.04 226.6 0.3 17.10 0.08 2014 9 19 8 20366+2342 0.25 22.5 0.8 6.75 0.20 2014 9 19 8 20367+2328 1.6 24.9 0.3 19.9 0.08 2014 9 19 8 20367+2327 0.61 300.7 0.6 8.23 0.20 2014 9 19 8 20367+2319 1.12 240.6 2.7 5.27 0.24 2014 9 19 9 20367+2316 2.48 331.8 0.8 7.87 0.09 2014 9 19 9 20368+2324 1.02 76.3 0.4 15.01 0.12 2014 9 19 9 20369+2330 0.93 326.3 0.3 17.29 0.16 2014 9 19 8 20369+2325 1.69 268.2 0.5 17.94 0.12 2014 9 19 9 20363+2321 0.82 134.1 0.3 21.57 0.19 2014 9 19 9 Table 1 continues on next page.

Page 324 Results of 194 Double Stars Measurements from Astrometric CCD Observations at the Nikolaev... Table 1 (continued). Results of measurements of the 194 doubles stars using REDUC software. WDS no mag * Theta Std_Theta Rho Std_Rho Y M D N 20397+1415 0.97 147.1 0.3 32.54 0.13 2013 6 11 10 20397+1406 1.57 285.6 1.8 6.46 0.58 2013 6 11 10 20401+2509 2.07 288.9 0.4 10.36 0.11 2014 8 30 10 20401+2458 0.34 24.1 1.1 16.11 0.30 2014 8 30 9 20401+2450 0.4 34.5 1.6 5.63 0.22 2014 8 30 10 20412+2448 1.54 139.2 0.2 15.47 0.13 2014 8 30 10 20415+2459 1.42 197.7 0.6 8.83 0.10 2014 8 30 10 20417+2449 0.72 35.7 0.7 8.40 0.10 2014 8 30 9 20417+2437 2.99 94.1 0.6 8.37 0.10 2014 8 30 8 20401+2516 0.51 339.6 0.3 21.87 0.13 2014 9 17 10 20401+2513 1.1 296.1 0.2 18.58 0.05 2014 9 17 10 20408+2521 1.54 232.6 0.4 16.89 0.13 2014 9 17 10 20408+2505 3.2 302.7 0.3 18.68 0.06 2014 9 17 10 20413+2513 2.06 244.9 0.5 13.26 0.13 2014 9 17 10 20478+1109 0.64 58.3 0.2 48.63 0.09 2013 8 8 10 20487+2517 1.31 78.3 0.7 14.63 0.13 2014 8 20 10 20491+2509 0.09 101.1 0.6 8.81 0.18 2014 8 20 10 20492+2504 0.78 68.2 1.5 3.93 0.08 2014 8 20 10 20492+2510 1.2 355.6 1.8 5.98 0.10 2014 8 20 10 20495+2516 1.38 80.2 1.0 8.58 0.09 2014 8 20 10 20497+2507 1.42 276.1 0.8 9.61 0.16 2014 8 20 10 20497+2526 0.1 336.3 0.3 14.64 0.10 2014 8 20 10 20499+2454 0.41 53.8 0.7 9.69 0.14 2014 8 20 10 20499+2456 1.04 235.2 1.1 8.27 0.22 2014 8 20 10 20499+2508 0.22 341.7 1.5 4.55 0.16 2014 8 20 10 20499+2510 1.49 19.5 0.2 12.23 0.14 2014 8 20 10 20500+2508 0.89 253.9 0.7 12.48 0.19 2014 8 20 10 20501+2512 3.11 341.6 0.5 16.14 0.13 2014 8 20 10 20503+2507 2.78 83.9 0.4 10.72 0.10 2014 8 20 10 20543+2441 0.99 201.8 0.7 9.14 0.14 2014 9 2 11 20573+1434 0.68 60.9 0.2 72.94 0.12 2014 9 19 9 20580+1426 0.58 339.3 0.2 14.31 0.12 2014 9 19 10 21017+2516 0.59 167.3 0.8 6.79 0.07 2014 9 17 10 21024+2518 0.54 124.5 0.3 21.44 0.09 2014 9 17 10 21026+2515 0.47 353.4 0.4 16.86 0.15 2014 9 17 10 21027+2508 0.58 25.4 0.6 10.04 0.12 2014 9 17 10 21020+2515 0.83 312.0 0.2 18.30 0.12 2014 9 17 10 21057+2412 0.17 245.9 0.1 16.03 0.27 2014 8 30 3 21060+1443 0.34 137.3 0.1 68.31 0.08 2013 11 1 8 21060+2406 3.08 188.2 0.6 11.00 0.08 2014 8 30 10 21062+2346 0.51 76.4 0.4 15.19 0.09 2014 8 30 10 21065+2332 0.02 190.3 2.3 4.89 0.46 2014 8 30 10 21066+2347 2.17 223.1 0.4 20.09 0.09 2014 8 30 10 21068+2400 0.08 169.0 0.7 12.25 0.14 2014 8 30 10 21069+0458 4.61 271.4 0.1 53.01 0.08 2013 8 8 10 Table 1 continues on next page.

Page 325 Results of 194 Double Stars Measurements from Astrometric CCD Observations at the Nikolaev... Table 1 (continued). Results of measurements of the 194 doubles stars using REDUC software. WDS no mag * Theta Std_Theta Rho Std_Rho Y M D N 21070+1500 0.42 317.4 0.1 38.13 0.08 2013 11 1 8 21071+2332 0.29 86.1 0.4 11.48 0.08 2014 8 30 10 21101+2516 1.77 249.9 0.5 12.14 0.10 2014 8 20 10 21104+2512 0.75 247.0 1.7 5.38 0.09 2014 8 20 10 21105+2452 1.0 190.8 1.4 6.17 0.17 2014 8 20 10 21107+2512 0.36 138.9 0.5 13.93 0.14 2014 8 20 10 21108+2445 2.44 58.7 0.4 14.52 0.10 2014 8 20 10 21108+2452 0.63 145.0 1.0 8.11 0.08 2014 8 20 10 21110+2448 0.59 84.5 0.8 11.83 0.10 2014 8 20 10 21110+2519 2.13 194.0 0.3 13.83 0.06 2014 8 20 10 21185+2454 1.99 31.9 0.8 9.13 0.12 2014 8 28 10 21189+2504 1.24 166.3 0.2 16.87 0.11 2014 8 28 10 21194+2513 0.12 53.7 0.6 9.87 0.11 2014 8 28 9 21198+2435 0.81 85.2 1.2 5.85 0.32 2014 8 28 6 21200+2440 1.04 267.3 0.6 11.44 0.09 2014 8 28 9 21223+1111 0.9 191.1 1.3 4.16 0.25 2014 10 12 9 21227+1101 1.45 336.1 0.1 96.62 0.14 2014 10 12 10 21229+2346 0.09 192.2 0.4 13.84 0.13 2014 9 17 10 21240+2352 0.61 240.7 1.2 7.16 0.19 2014 9 17 10 21233+2401 1.02 49.3 0.5 12.71 0.08 2014 9 17 10 21282+1519 2.32 174.2 0.6 11.11 0.18 2013 8 8 10 21314+2451 2.68 127.0 0.4 17.23 0.12 2014 8 10 8 21315+2503 1.25 18.4 1.1 8.83 0.09 2014 8 20 10 21326+2522 1.11 66.4 0.2 36.63 0.11 2014 8 20 10 21329+2509 2.35 192.0 0.6 14.57 0.08 2014 8 20 10 21447+2402 1.99 298.4 0.8 7.06 0.10 2014 9 17 6 21462+2353 ** 0.23 128.6 0.8 8.13 0.19 2014 9 17 6 21462+2353 ** 0.99 212.2 0.5 19.65 0.11 2014 9 17 6 21455+2349 0.11 39.4 0.3 12.76 0.07 2014 9 17 10 21449+1040 0.22 55.0 0.9 7.89 0.09 2014 8 30 9 21528+2458 0.09 178.3 0.7 10.38 0.16 2014 8 20 10 21529+2525 0.03 11.9 0.3 23.47 0.14 2014 8 20 10 21534+2447 1.26 100.1 0.3 9.91 0.12 2014 8 20 10 21536+2516 1.57 322.9 0.3 18.07 0.17 2014 8 20 10 21539+2446 1.17 359.9 0.5 15.52 0.15 2014 8 20 10 21545+1615 1.49 20.2 1.1 8.44 0.11 2013 8 8 9 22010+2439 2.14 19.9 0.6 14.15 0.05 2014 8 28 10 22010+2453 0.09 178.8 0.5 12.25 0.14 2014 8 28 10 22016+2421 0.59 135.9 0.9 7.78 0.12 2014 8 28 10 22017+2446 0.85 78.0 0.5 13.82 0.11 2014 8 28 10 22021+2422 0.64 255.5 1.3 4.82 0.42 2014 8 28 10 22024+2420 0.7 65.0 0.5 7.40 0.10 2014 8 28 9 22138+2408 2.03 248.3 0.5 14.51 0.17 2014 8 20 10 22146+2342 0.2 28.5 0.4 16.94 0.08 2014 8 20 10 22312+0253 1.24 168.0 0.2 20.44 0.10 2014 8 30 10 Table 1 concludes on next page.

Page 326 Results of 194 Double Stars Measurements from Astrometric CCD Observations at the Nikolaev... Table 1 (conclusion). Results of measurements of the 194 doubles stars using REDUC software. WDS no mag * Theta Std_Theta Rho Std_Rho Y M D N 22335+1519 0.48 263.0 1.2 42.30 0.24 2014 10 19 10 22351+0346 2.1 289.31 0.04 369.81 0.13 2014 8 20 9 22428+2947 1.06 276.6 0.3 25.45 0.12 2014 8 28 10 22429+2958 0.79 52.4 0.3 28.49 0.12 2014 8 28 10 22430+2944 0.43 124.3 0.5 13.63 0.13 2014 8 28 10 22432+2941 0.63 283.9 0.5 18.06 0.11 2014 8 28 10 22439+2938 0.07 227.7 0.7 9.12 0.13 2014 8 28 10 22441+2940 1.46 149.9 0.2 23.85 0.10 2014 8 28 10 22443+2957 0.27 218.5 0.2 24.58 0.10 2014 8 28 10 22481+2444 0.74 38.9 0.1 41.25 0.15 2014 9 17 6 22482+2434 0.08 195.7 0.4 11.84 0.08 2014 9 17 10 22578+1833 0.62 80.8 0.5 16.85 0.08 2014 10 14 8 22574+1827 0.11 183.9 0.1 111.56 0.09 2014 10 14 9 23232-0839 2.02 94.4 0.7 157.30 0.13 2014 10 19 10 23527-0328 3.47 1.6 0.7 6.04 0.62 2014 10 14 4 23523-0341 1.9 178.6 0.1 277.12 0.10 2014 10 14 10 23533+0208 0.23 1.2 0.8 15.64 0.19 2013 11 1 4 Notes: * all observations were obtained with filter close to R c band; ** this star is triple and has two records in WDS; we measured both in the same order as in the catalog.

Page 327 Jonckheere Double Star Photometry Part II: Delphinus Wilfried R.A. Knapp Amateur visual double star astronomer Vienna, Austria wilfried.knapp@gmail.com Abstract: If any double star discoverer is in urgent need of photometry then it is Jonckheere. There are over 3000 Jonckheere objects listed in the WDS catalog and a good part of them have magnitudes which are obviously far too bright. To keep the workload manageable only one image per object is taken and photometry is done with a software allowing a simple point and click procedure even a single measurement is better than the currently usually given estimation Introduction As follow up to the first report on J-objects in Cygnus (Knapp; Nanson 2016) I selected for this report all J-objects in Delphinus (Del) (plus ROE14AB in combination with J563BC) given in Table 1 with all values based on WDS data as of April 2015. Photometry For each of the listed J-objects one single image was taken (in Bessel epoch 2015.683) with itelescope it24 with 3 second exposure time. The imaging sessions were not straight forward as in previous sessions in Cygnus, mostly due to uncooperative weather conditions. So, for several objects repeated imaging sessions were required and in a few cases I had to resort to another telescope location. In these cases, the different Bessel epochs and different scopes are indicated in the notes column. In all cases the initial plate solving was done by AAVSO VPhot and in the few cases with negative VPhot result, but positive with MaxIm PinPoint. Each image was then once more plate solved with Astrometrica, using the UCAC4 catalog with reference stars in the Vmag range of 10.5 to 14.5 giving not only RA/Dec coordinates but also photometry results for all reference stars used including an average dvmag error. The J-objects were then located in the center of the image with a few exceptions, indicating that the given RA/Dec coordinates are usually correct with the exceptions suggesting position problems. Photometry was then done using the Astrometrica procedure with point and click at the components delivering Vmag measurements based on all reference stars used for plate solving. The only changing parameter was the aperture radius used for photometry aiming to keep it equal or at least near 1.5x FWHM. In cases with smaller separation the star disks touched or overlapped but, nevertheless individual photometry could be done though less reliable than with clearly separated disks. Several cases allowed only the measurement of the combined magnitude, but even in these cases it is possible to make a well-founded estimate for the components based on the initial observed m between the components based on the formula m combined according to Greaney 2012. Summary Table 2 shows, with few exceptions, quite large differences for the magnitudes compared with the WDS data, often even in cases where double digit values suggest recent precise measurements. A few cases suggest errors in position, separation, and position angle, Several times the images suggest the nonexistence of the objects in question. References 10 m 2.5log 2.521 2.521 m 1` 2 Buchheim, Robert, 2008, "CCD Double-Star Measurements at Altimira Observatory in 2007", Journal of Double Star Observations, 4, 27-31.

Page 328 Jonckheere Double Star Photometry Part II: Delphinus Greaney, Michael, 2012, "Some Useful Formulae" in R.W. Argyle, Observing and Measuring Visual Double Stars, 2nd Edition 2012, Chapter 25, Page 359, Springer. Knapp, Wilfried and Nanson, John, 2016, "Jonckheere Double Star Photometry Part I: Cyg", JDSO, 12, 168-179. Acknowledgements The following tools and resources have been used for this research: AAVSO APASS (via the UCAC4 catalog) AAVSO VPhot Aladin Sky Atlas v8.0 Astrometrica v4.8.2.405 AstroPlanner v2.2 itelescope it24 & it27 MaxIm DL6 v6.08 SIMBAD, VizieR Table 1: WDS April 2015 values for the Jonckheere objects in Del sorted by designation number WDS ID Name C RA Dec Sep M1 M2 PA WDS20329+1142 J1 AB 20:32:52.760 +11:44:37.200 2.0 10.04 10.57 57 WDS20316+1150 J3 AB 20:31:33.391 +11:50:24.800 2.0 10.00 10.00 129 WDS20157+1003 J135 AB 20:15:43.430 +10:02:08.901 3.6 11.42 11.58 322 WDS20345+1138 J142 AB 20:34:25.910 +11:37:17.500 6.5 10.35 12.50 241 WDS20403+0349 J156 AB 20:40:20.583 +03:50:04.000 2.3 10.95 11.64 21 WDS20559+0835 J157 AB 20:55:51.537 +08:34:17.901 3.8 11.32 10.93 172 WDS20409+1738 J191 AB 20:40:52.162 +17:37:59.203 1.2 9.30 9.60 141 WDS20416+1058 J192 AB 20:42:36.580 +11:00:55.100 5.5 9.40 13.10 133 WDS20420+1821 J193 AB 20:42:02.550 +18:21:02.302 5.3 9.11 12.10 83 WDS20494+1124 J194 AB 20:49:23.528 +11:24:09.601 0.6 10.32 9.97 155 WDS20494+1124 J194 AB,C 20:49:23.528 +11:24:09.601 11.2 10.32 13.94 33 WDS20509+1907 J195 AB 20:50:53.568 +19:06:42.697 3.4 11.40 11.40 26 WDS21033+1655 J284 AB 21:03:12.192 +16:53:25.900 2.8 9.50 11.10 235 WDS20298+1712 J510 AB 20:29:45.690 +17:11:55.697 3.5 9.91 13.70 242 WDS20181+1555 J553 AB 20:18:06.692 +15:54:09.498 3.6 9.40 10.50 21 WDS20271+0948 J559 AB 20:27:06.862 +09:48:52.100 2.0 11.65 11.45 279 WDS20311+1248 J562 AB 20:31:07.271 +12:46:52.799 2.2 10.80 11.70 145 WDS20311+1648 ROE14 AB 20:31:03.178 +16:48:41.299 7.1 11.00 12.00 213 WDS20311+1648 J563 BC 20:31:02.691 +16:48:40.399 5.0 12.00 12.30 213 WDS20351+1533 J566 AB 20:35:09.952 +15:32:10.099 4.2 10.90 12.20 120 WDS20527+0527 J572 AB 20:52:39.400 +05:26:20.900 3.4 10.20 11.30 138 WDS20534+1921 J573 AB 20:53:18.532 +19:22:30.199 3.9 11.30 11.70 187 WDS20151+1143 J604 AB 20:15:05.438 +11:42:41.500 0.7 10.23 10.44 235 WDS20527+1726 J605 AC 20:52:44.069 +17:26:12.700 38.2 11.55 12.16 161 WDS20527+1726 J605 AB 20:52:44.069 +17:26:12.700 1.7 11.40 11.90 241 WDS20571+1801 J607 AB 20:57:05.297 +18:00:59.903 3.1 10.80 12.40 305 WDS20348+1857 J790 AB 20:34:54.001 +18:56:42.397 2.3 9.50 10.00 88 WDS21056+1749 J797 AB 21:05:37.301 +17:49:46.503 3.4 12.30 13.80 214 WDS20198+1203 J837 AB 20:19:52.010 +12:03:10.400 2.0 11.10 11.70 297 WDS20210+1028 J838 AB 20:21:00.667 +10:28:20.999 6.5 11.52 12.00 118 Table 1 continues on next page.

Page 329 Jonckheere Double Star Photometry Part II: Delphinus Table 1 (continued): WDS April 2015 values for the Jonckheere objects in Del sorted by designation number WDS ID Name C RA Dec Sep M1 M2 PA WDS20235+1811 J839 AB 20:23:35.739 +18:10:40.901 1.9 11.50 11.70 350 WDS20249+1124 J840 AB 20:24:46.958 +11:23:38.599 3.8 9.50 10.50 51 WDS20249+1309 J841 AB 20:24:56.070 +13:08:58.000 0.2 10.50 11.50 274 WDS20249+1309 J841 AB.C 20:24:56.070 +13:08:58.000 8.4 10.10 10.50 82 WDS20250+1451 J842 AB 20:24:57.972 +14:51:16.501 4.2 10.04 12.10 179 WDS20314+2054 J844 AB 20:30:50.688 +20:53:41.603 4.1 12.20 12.80 118 WDS20434+1712 J845 AB 20:43:21.981 +17:12:28.499 4.0 11.99 12.20 224 WDS20541+1402 J846 AB 20:54:07.202 +14:02:13.000 3.3 10.80 11.14 157 WDS20396+1310 J912 AB 20:39:39.021 +13:09:45.400 1.8 10.00 10.00 125 WDS20385+1118 J1073 AB 20:38:25.577 +11:16:24.701 5.3 9.70 14.00 113 WDS20209+1332 J1173 AB 20:20:50.478 +13:31:04.600 3.7 10.41 13.70 83 WDS20157+0957 J1234 AB 20:15:42.778 +09:56:37.900 4.4 12.51 15.00 43 WDS20280+1244 J1241 AB 20:28:00.112 +12:44:08.100 1.1 10.33 12.30 168 WDS20386+1120 J1242 AB 20:38:30.871 +11:18:39.201 5.1 9.60 11.00 204 WDS20298+1154 J1243 AB 20:30:22.240 +11:54:28.999 3.2 10.80 10.80 121 WDS20146+1116 J1296 AB 20:14:28.497 +11:17:34.602 3.3 11.90 12.40 236 WDS20276+0745 J1297 AB 20:27:33.147 +07:44:07.799 1.2 11.23 11.27 14 WDS20554+0836 J1318 AB 20:55:23.570 +08:35:38.200 0.8 10.30 10.77 142 WDS20247+0302 J1342 AB 20:24:44.823 +03:05:03.200 2.7 9.40 11.50 307 WDS20270+1008 J1343 AB 20:27:01.891 +10:11:16.301 2.4 9.60 10.00 54 WDS20348+1121 J1344 AB 20:34:45.562 +11:20:14.199 2.3 9.10 11.50 103 WDS20438+1440 J1345 AB 20:43:47.751 +14:39:14.501 3.7 9.60 10.50 280 WDS20560+0837 J1346 AB 20:56:00.223 +08:35:46.100 2.4 13.20 13.20 327 WDS20260+1212 J1704 AB 20:26:02.949 +12:11:07.001 6.0 10.16 10.80 202 WDS20586+0723 J1715 AB 20:58:36.422 +07:23:15.399 5.2 11.61 13.00 125 WDS20593+1744 J1716 AB 20:59:15.210 +17:43:17.099 6.4 10.00 11.00 224 WDS20169+1303 J1879 AB 20:16:56.723 +13:02:42.601 10.9 11.83 11.95 233 WDS20169+1303 J1879 AC 20:16:56.723 +13:02:42.601 13.7 11.83 14.40 272 WDS20172+1304 J1880 AB 20:17:08.121 +13:04:32.001 13.5 11.23 13.30 246 WDS20303+0917 J1883 AB 20:30:08.851 +09:20:52.201 6.4 11.53 12.00 115 WDS20315+1448 J1884 AB 20:31:23.290 +14:50:01.400 8.6 9.80 9.80 131 WDS20315+1446 J1885 AB 20:31:24.148 +14:47:04.200 11.9 12.00 12.00 353 WDS20351+1413 J1887 AB 20:35:04.623 +14:13:40.799 5.5 11.68 11.70 280 WDS20439+1255 J1888 AB 20:43:49.688 +12:53:40.501 9.8 9.70 12.50 159 WDS20441+1258 J1889 AB 20:44:04.073 +12:31:48.799 4.8 14.30 14.30 15 WDS20485+1448 J1890 AB 20:48:29.901 +14:50:57.100 6.8 11.20 11.50 140 WDS20360+0411 J2192 AB 20:36:31.120 +04:15:22.100 4.9 9.90 12.50 17 WDS20305+1829 J2313 AB 20:30:30.178 +18:29:07.801 6.0 9.50 11.90 133 WDS20327+0453 J2314 AB 20:32:40.229 +04:52:49.300 4.9 10.60 11.60 70 WDS20327+0453 J2314 AC 20:32:40.229 +04:52:49.300 17.6 10.60 14.00 154 WDS20415+1611 J2319 AB 20:41:16.627 +16:12:44.999 7.0 9.80 12.00 188 WDS20488+0512 J2321 AB 20:48:50.727 +05:11:58.101 6.6 9.61 10.80 151 WDS20518+1736 J2325 AB 20:51:50.799 +17:36:17.401 5.3 11.60 13.70 260 WDS20230+0929 J2572 AB 20:23:08.260 +09:28:43.700 4.1 9.80 13.20 281 WDS20321+0330 J2573 AB 20:32:27.519 +03:29:17.300 4.0 12.50 12.80 150 Table 1 concludes on next page.

Page 330 Jonckheere Double Star Photometry Part II: Delphinus Table 1 (conclusion): WDS April 2015 values for the Jonckheere objects in Del sorted by designation number WDS ID Name C RA Dec Sep M1 M2 PA WDS20418+1404 J2575 AB 20:41:55.059 +14:05:23.400 0.7 9.70 13.00 311 WDS20393+1101 J2603 AB 20:39:18.160 +10:59:36.201 1.8 11.39 13.40 354 WDS20398+1927 J2604 AB 20:39:44.109 +19:26:07.502 2.0 12.12 12.10 142 WDS21058+1939 J2702 AB 21:05:43.851 +19:40:09.899 5.4 11.20 11.60 178 WDS20152+1357 J3066 AB 20:15:23.751 +14:00:30.401 4.5 11.00 11.50 334 WDS20152+1357 J3066 AC 20:15:23.751 +14:00:30.401 9.1 11.00 15.00 215 WDS20227+1345 J3079 AB 20:22:29.808 +13:45:35.300 7.6 12.90 13.30 139 WDS20227+2023 J3080 AB 20:22:46.940 +20:22:23.401 7.4 12.00 13.00 292 WDS20228+2023 J3081 AB 20:22:51.403 +20:22:15.999 6.3 10.00 11.00 0 WDS20229+1346 J3082 AB 20:23:07.148 +13:47:43.401 6.1 14.20 15.80 19 WDS20259+0902 J3084 AB 20:25:53.487 +09:02:12.701 5.8 12.03 12.90 88 WDS20263+1445 J3085 AB 20:26:15.488 +14:45:35.201 6.1 9.80 9.80 204 WDS20275+1514 J3087 AB 20:27:27.633 +15:13:46.000 5.6 10.50 11.60 328 WDS20293+1029 J3088 AB 20:29:20.690 +10:27:58.399 7.4 10.50 11.30 80 WDS20295+1033 J3089 AB 20:29:21.321 +10:31:41.301 4.6 11.60 12.30 316 WDS20314+2049 J3091 AB 20:31:34.228 +20:51:20.402 5.7 11.20 11.50 116 WDS20326+1024 J3092 AB 20:32:36.301 +10:23:49.902 5.3 12.10 12.60 335 WDS20334+1359 J3093 AB 20:33:25.012 +13:58:46.299 4.2 12.80 12.80 43 WDS20339+1915 J3094 AB 20:33:54.002 +19:14:56.299 7.4 11.10 14.80 22 WDS20363+1636 J3095 AB 20:36:07.760 +16:35:11.002 5.3 12.40 12.40 179 WDS20365+2044 J3096 AB 20:36:33.647 +20:43:53.100 21.9 10.50 12.60 2 WDS20365+2044 J3096 BC 20:36:33.880 +20:44:20.902 8.3 12.60 13.10 9 WDS20370+1420 J3098 AB 20:36:59.822 +14:21:15.300 4.9 12.60 13.10 303 WDS20378+1936 J3099 AB 20:37:26.869 +19:38:08.898 5.5 12.50 12.70 147 WDS20385+1848 J3102 AB 20:38:44.027 +18:49:32.097 6.2 11.60 12.10 97 WDS20393+2003 J3103 AB 20:39:30.499 +20:03:30.903 5.7 12.05 12.42 224 WDS20397+1406 J3104 AB 20:39:44.061 +14:06:00.698 6.3 9.90 11.20 286 WDS20416+1738 J3107 AB 20:41:23.013 +17:39:12.502 5.9 11.70 11.70 120 WDS20436+1537 J3108 AB 20:43:43.041 +15:38:59.501 6.2 11.00 12.50 197 WDS20433+1728 J3109 AB 20:43:20.107 +17:27:50.203 7.9 12.50 13.10 245 WDS20466+1532 J3110 AB 20:46:29.353 +15:31:51.501 6.7 11.20 11.50 222 WDS20509+1517 J3113 AB 20:51:01.663 +15:19:44.999 4.8 11.50 11.50 112 WDS20513+1647 J3115 AB 20:51:14.387 +16:46:12.798 7.2 12.16 15.20 318 WDS20522+1656 J3116 AB 20:52:09.600 +16:56:13.002 73.3 8.77 12.88 39 WDS20522+1656 J3116 BC 20:52:12.841 +16:57:09.897 5.9 13.30 14.80 139 WDS20585+1607 J3118 AB 20:58:30.880 +16:06:43.899 5.8 9.40 11.20 74 WDS21081+1857 J3125 AB 21:08:17.131 +18:57:53.801 4.7 12.40 13.60 258 WDS20285+0443 J3220 AB 20:28:18.933 +04:41:49.300 3.9 10.75 12.50 181 WDS20314+0701 J3221 AB 20:31:15.792 +06:59:14.300 3.8 10.00 11.60 166 WDS20487+0706 J3223 AB 20:48:44.561 +07:05:43.700 3.5 10.69 11.40 310 WDS20311+1247 J3244 AB 20:31:07.999 +12:45:59.000 4.6 11.38 12.90 160 WDS20519+1203 J3245 AB 20:51:51.877 +12:01:57.598 3.8 11.80 12.60 249 WDS20289+1022 J3263 AB 20:28:49.413 +10:23:15.099 7.1 11.30 12.10 55 WDS20292+1019 J3264 AB 20:29:10.829 +10:19:27.699 6.3 11.64 12.30 358 WDS20502+1246 J3277 AB 20:50:05.372 +12:42:41.500 4.1 10.70 12.50 327 WDS20555+1730 J3328 AB 20:55:28.239 +17:29:14.997 3.9 11.99 14.70 122

Page 331 Jonckheere Double Star Photometry Part II: Delphinus Table 2. Bessel epoch 2015.683 (exceptions see notes column) photometry results for the J objects in Del. M1 WDS and M2 WDS are the WDS catalog values. M1 new stands for measured M1, dm1 stands for delta between M1 WDS and M1 new. M2 new stands for measured M2, dm2 stands for delta M1 WDS and M1 new. Err M1 stands for the estimated error range calculated from the average delta Vmag over all reference stars used in the image and the SNR value of the star with the formula 2 2 dv (2.5log (1 1/ SNR)). WDS ID Name M1 WDS M1 new dm1 Err M1 M2 WDS M2 new dm2 Err M2 Notes 20329+1142 J1 AB 10.04 9.650 0.39 0.070 10.57 10.180 0.39 0.070 Overlapping star disks - no separate photometry possible. Combined magnitude 9.118 with SNR 238.97 gives estimated M1 new and M2 new values not confirming the current, seemingly a bit too faint, WDS values 20316+1150 J3 AB 10.00 11.946-1.95 0.074 10.00 12.127-2.13 0.074 Touching/overlapping star disks 20157+1003 J135 AB 11.42 11.216 0.20 0.102 11.58 11.455 0.13 0.103 Touching star disks 20345+1138 J142 AB 10.35 10.285 0.06 0.080 12.50 12.523-0.02 0.084 20403+0349 J156 AB 10.95 10.698 0.25 0.081 11.64 11.083 0.56 0.081 Touching/overlapping star disks 20559+0835 J157 AB 11.32 11.484-0.16 0.083 10.93 11.130-0.20 0.082 Touching star disks 20409+1738 J191 AB 9.30 10.880-1.58 0.140 9.60 11.180-1.58 0.140 Overlapping star disks - no separate photometry possible. Combined magnitude 10.268 with SNR 119.36 gives estimated M1 new and M2 new values suggesting much fainter magnitudes than currently WDS listed 20416+1058 J192 AB 9.40 11.381-1.98 0.081 13.10 14.559-1.46 0.158 Very low SNR <10 for B. 20420+1821 J193 AB 9.11 8.976 0.13 0.080 12.10 11.675 0.42 0.083 20494+1124 J194 AB 10.32 10.270 0.05 0.090 9.97 9.920 0.05 0.090 Overlapping star disks - no separate photometry possible. Combined magnitude 9.325 with SNR 131.09 gives estimated M1 new and M2 new values confirming rather well the current WDS values 20494+1124 J194 AB. C mag 10 10.32 9.325 1.00 0.090 13.94 14.005-0.07 0.126 WDS gives here obviously M1 for A and not AB combined. WDS value for C well confirmed 20509+1907 J195 AB 11.40 12.365-0.97 0.114 11.40 12.385-0.98 0.115 21033+1655 J284 AB 9.50 11.236-1.74 0.101 11.10 12.518-1.42 0.107 Touching star disks 20298+1712 J510 AB 9.91 9.829 0.08 0.090 13.70 13.052 0.65 0.106 20181+1555 J553 AB 9.40 10.641-1.24 0.080 10.50 11.897-1.40 0.082 20271+0948 J559 AB 11.65 11.350 0.30 0.088 11.45 11.248 0.20 0.089 Overlapping/Touching star disks 20311+1248 J562 AB 10.80 10.104 0.70 0.132 11.70 10.654 1.05 0.139 Overlapping star disks 20311+1648 ROE14 AB 11.00 11.457-0.46 0.091 12.00 12.630-0.63 0.094 ROE14 AB as "bonus" 20311+1648 J563 BC 12.00 12.630-0.63 0.094 12.30 13.193-0.89 0.097 20351+1533 J566 AB 10.90 10.126 0.77 0.130 12.20 11.252 0.95 0.131 20527+0527 J572 AB 10.20 9.927 0.27 0.120 11.30 11.446-0.15 0.126 Touching star disks 20534+1921 J573 AB 11.30 11.766-0.47 0.081 11.70 12.925-1.23 0.086 Table 2 continues on next page.

Page 332 Jonckheere Double Star Photometry Part II: Delphinus Table 2 (continued). Bessel epoch 2015.683 (exceptions see notes column) photometry results for the J objects in Del.... WDS ID Name M1 WDS M1 new dm1 Err M1 M2 WDS M2 new dm2 Err M2 Notes 20151+1143 J604 AB 10.23 10.210 0.02 0.080 10.44 10.420 0.02 0.080 Overlapping star disks - no separate photometry possible. Combined magnitude 9.552 with SNR 210.02 gives estimated M1 new and M2 new values confirming rather well the current WDS values 20527+1726 J605 AC 11.55 11.665-0.11 0.111 12.16 12.160-0.112 WDS values for A with 11.4 and 11.55 not consistent 20527+1726 J605 AB 11.40 11.665-0.26 0.111 11.90 11.982-0.08 0.112 Overlapping star disks 20571+1801 J607 AB 10.80 10.714 0.09 0.130 12.40 12.440-0.04 0.136 Touching star disks 20348+1857 J790 AB 9.50 11.554-2.05 0.091 10.00 12.080-2.08 0.092 Touching star disks 21056+1749 J797 AB 12.30 12.053 0.25 0.101 13.80 13.259 0.54 0.106 20198+1203 J837 AB 11.10 10.848 0.25 0.100 11.70 11.905-0.21 0.102 Overlapping/Touching star disks 20210+1028 J838 AB 11.52 12.543-1.02 0.093 12.00 12.579-0.58 0.093 20235+1811 J839 AB 11.50 11.138 0.36 0.121 11.70 11.156 0.54 0.121 Overlapping/Touching star disks 20249+1124 J840 AB 9.50 11.314-1.81 0.081 10.50 12.835-2.34 0.085 20249+1309 J841 AB 10.50 10.400 0.10 0.100 11.50 11.400 0.10 0.100 Overlapping star disks - no separate photometry possible. Combined magnitude 10.045 with SNR 174.65 gives estimated M1 new and M2 new values confirming rather well the current WDS values 20249+1309 J841 AB.C 10.10 10.045 0.05 0.100 10.50 10.664-0.16 0.100 20250+1451 J842 AB 10.04 9.926 0.11 0.090 12.10 11.713 0.39 0.092 20314+2054 J844 AB 12.20 11.863 0.34 0.141 12.80 12.825-0.02 0.146 20434+1712 J845 AB 11.99 12.658-0.67 0.094 12.20 13.137-0.94 0.100 20541+1402 J846 AB 10.80 10.622 0.18 0.071 11.14 11.060 0.08 0.071 20396+1310 J912 AB 10.00 12.618-2.62 0.096 10.00 12.701-2.70 0.097 Touching star disks 20385+1118 J1073 AB 9.70 11.492-1.79 0.081 14.00 14.170-0.17 0.108 Low SNR <20 for B 20209+1332 J1173 AB 10.41 10.551-0.14 0.071 13.70 12.164 1.54 0.079 Touching star disks 20157+0957 J1234 AB 12.51 11.892 0.62 0.095 15.00 13.392 1.61 0.137 Very low SNR <10 for B 20280+1244 J1241 AB 10.33 10.090 0.24 0.110 12.30 12.060 0.24 0.110 Overlapping star disks - no separate photometry possible. Combined magnitude 9.925 with SNR 102.93 gives estimated M1 new and M2 new values confirming rather the current WDS values 20386+1120 J1242 AB 9.60 11.546-1.95 0.113 11.00 12.538-1.54 0.121 20298+1154 J1243 AB 10.80 12.608-1.81 0.102 10.80 12.628-1.83 0.102 it27. Bessel epoch 2015.799 20146+1116 J1296 AB 11.90 12.619-0.72 0.102 12.40 13.408-1.01 0.106 it27. Bessel epoch 2015.799 Table 2 continues on next page.

Page 333 Jonckheere Double Star Photometry Part II: Delphinus Table 2 (continued). Bessel epoch 2015.683 (exceptions see notes column) photometry results for the J objects in Del.... WDS ID Name M1 WDS M1 new dm1 Err M1 M2 WDS M2 new dm2 Err M2 Notes 20276+0745 J1297 AB 11.23 11.180 0.05 0.111 11.27 11.220 0.05 0.111 Overlapping star disks - no separate photometry possible. Combined magnitude 10.448 with SNR 95.51 gives estimated M1 new and M2 new values confirming rather well the current WDS values 20554+0836 J1318 AB 10.30 10.270 0.03 0.140 10.77 10.740 0.03 0.140 Overlapping star disks - no separate photometry possible. Combined magnitude 11.425 with SNR 44.81 gives estimated M1 new and M2 new values confirming rather well the current WDS values 20247+0302 J1342 AB 9.40 12.090-2.69 0.076 11.50 12.801-1.30 0.072 Overlapping/Touching star disks 20270+1008 J1343 AB 9.60 11.889-2.29 0.121 10.00 12.039-2.04 0.121 Overlapping/Touching star disks. Bessel epoch 2015.713 20348+1121 J1344 AB 9.10 10.646-1.55 0.070 11.50 10.878 0.62 0.071 Overlapping/Touching star disks. Bessel epoch 2015.713 20438+1440 J1345 AB 9.60 11.712-2.11 0.143 10.50 12.682-2.18 0.151 Low SNR <20 for B 20560+0837 J1346 AB 13.20 12.477 0.72 0.102 13.20 12.524 0.68 0.102 it27. Touching star disks. Bessel epoch 2015.801 20260+1212 J1704 AB 10.16 10.320-0.16 0.190 10.80 11.324-0.52 0.191 Bessel epoch 2015.809 20586+0723 J1715 AB 11.61 12.232-0.62 0.084 13.00 13.748-0.75 0.124 Low SNR <20 for B 20593+1744 J1716 AB 10.00 11.781-1.78 0.112 11.00 13.071-2.07 0.122 20169+1303 J1879 AB 11.83 11.972-0.14 0.095 11.95 12.811-0.86 0.110 Low SNR <20 for B. Bessel epoch 2015.809 20169+1303 J1879 AC 11.83 11.972-0.14 0.095 14.40 13.959 0.44 0.165 Very low SNR <10 for B. Bessel epoch 2015.809 20172+1304 J1880 AB 11.23 11.113 0.12 0.101 13.30 12.910 0.39 0.110 20303+0917 J1883 AB 11.53 11.665-0.14 0.102 12.00 12.250-0.25 0.103 20315+1448 J1884 AB 9.80 11.782-1.98 0.152 9.80 12.355-2.56 0.154 20315+1446 J1885 AB 12.00 13.283-1.28 0.128 12.00 13.693-1.69 0.136 Low SNR <20 for B 20351+1413 J1887 AB 11.68 11.934-0.25 0.135 11.70 12.319-0.62 0.139 20439+1255 J1888 AB 9.70 12.023-2.32 0.092 12.50 13.897-1.40 0.107 Low SNR <10 for B. Bessel epoch 2015.809 20441+1258 J1889 AB 14.30 14.386-0.09 0.106 14.30 15.405-1.11 0.198 Low SNR <20 for A and very low SNR <10 for B. Bessel epoch 2015.809 20485+1448 J1890 AB 11.20 11.670-0.47 0.182 11.50 12.056-0.56 0.183 20360+0411 J2192 AB 9.90 11.440-1.54 0.051 12.50 12.882-0.38 0.054 Bessel epoch 2015.713 20305+1829 J2313 AB 9.50 11.542-2.04 0.122 11.90 13.209-1.31 0.132 Low SNR <20 for B 20327+0453 J2314 AB 10.60 12.475-1.88 0.113 11.60 12.800-1.20 0.119 Low SNR <20 for B 20327+0453 J2314 AC 10.60 12.475-1.88 0.052 14.00 No resolution, C fainter than 14mag 20415+1611 J2319 AB 9.80 12.035-2.24 0.102 12.00 13.711-1.71 0.122 20488+0512 J2321 AB 9.61 9.700-0.09 0.091 10.80 12.402-1.60 0.097 Table 2 continues on next page.

Page 334 Jonckheere Double Star Photometry Part II: Delphinus Table 2 (continued). Bessel epoch 2015.683 (exceptions see notes column) photometry results for the J objects in Del.... WDS ID Name M1 WDS M1 new dm1 Err M1 M2 WDS M2 new dm2 Err M2 Notes 20518+1736 J2325 AB 11.60 11.777-0.18 0.142 13.70 13.254 0.45 0.151 Low SNR <20 for B. Similar pair UCAC4-538 -140054/UCAC4-538- 140056 nearby 20230+0929 J2572 AB 9.80 12.206-2.41 0.172 13.20 14.208-1.01 0.213 Very low SNR<10 for B. Image quality questionable 20321+0330 J2573 AB 12.50 12.945-0.45 0.102 12.80 13.323-0.52 0.117 Low SNR<20 for B 20418+1404 J2575 AB 9.70 13.00 Overlapping star disks - no separate photometry possible. Combined magnitude 11.768 with SNR 58.88 - questionable object, Bogus assumed. If double at all than A could be not brighter than 11.8mag 20393+1101 J2603 AB 11.39 13.40 Overlapping star disks - no trace of a secondary, no separate photometry possible. Combined magnitude 11.376 with SNR 52.42 - questionable object, potential bogus 20398+1927 J2604 AB 12.12 12.10 Overlapping star disks - no trace of a secondary, no separate photometry possible. Combined magnitude 12.338 with SNR 21.91 - questionable object, potential bogus 21058+1939 J2702 AB 11.20 11.038 0.16 0.081 11.60 11.268 0.33 0.082 20152+1357 J3066 AB 11.00 12.789-1.79 0.106 11.50 13.641-2.14 0.113 20152+1357 J3066 AC 11.00 12.789-1.79 0.106 15.00 15.834-0.83 0.345 Very low SNR<5 for C 20227+1345 J3079 AB 12.90 12.645 0.26 0.063 13.30 13.366-0.07 0.067 Bessel epoch 2015.702 20227+2023 J3080 AB 12.00 12.058-0.06 0.221 13.00 12.732 0.27 0.221 Large dvmag 0.22. Bessel epoch 2015.702 20228+2023 J3081 AB 10.00 12.111-2.11 0.171 11.00 12.741-1.74 0.172 Large dvmag 0.17. Bessel epoch 2015.702 20229+1346 J3082 AB 14.20 15.80 Most probably position error. Only very faint single star with 14.634mag and SNR 14.01 in the given position. But nearby UCAC4-519-126369 20:23:07.099 +13:47:41.640 +14.264Vmag with companion UCAC4-519- 126370 15.616mag model fit, no Vmag. Bessel epoch 2015.702 20259+0902 J3084 AB 12.03 13.208-1.18 0.114 12.90 14.052-1.15 0.127 Low SNR<20 for B. Bessel epoch 2015.702 20263+1445 J3085 AB 9.80 11.608-1.81 0.081 9.80 12.258-2.46 0.082 Bessel epoch 2015.702 Table 2 continues on next page.

Page 335 Jonckheere Double Star Photometry Part II: Delphinus Table 2 (continued). Bessel epoch 2015.683 (exceptions see notes column) photometry results for the J objects in Del.... WDS ID Name M1 WDS M1 new dm1 Err M1 M2 WDS M2 new dm2 Err M2 Notes 20275+1514 J3087 AB 10.50 11.928-1.43 0.241 11.60 13.040-1.44 0.245 Large dvmag 0.24. Bessel epoch 2015.702 20293+1029 J3088 AB 10.50 12.865-2.37 0.181 11.30 13.033-1.73 0.184 Low SNR<20 for A and B. Bessel epoch 2015.702 20295+1033 J3089 AB 11.60 12.441-0.84 0.222 12.30 14.097-1.80 0.341 Low SNR<20 for A and very low SNR<5 for B. Bessel epoch 2015.702 20314+2049 J3091 AB 11.20 13.367-2.17 0.226 11.50 13.407-1.91 0.225 Bessel epoch 2015.702 20326+1024 J3092 AB 12.10 12.60 No resolution, no photometry possible. Both components probably much fainter than WDS value. UCAC4-502- 130763 13.156fmag, UCAC4-502-130762 13.652fmag. Given Vmag 12.705 for A seems questionable, especially as the same value is given for B and similar bright stars nearby are listed with 13.764 Vmag. Bessel epoch 2015.702 20334+1359 J3093 AB 12.80 12.80 No resolution, no photometry possible. Both components probably much fainter than WDS value. UCAC4-520- 130741 13.538fmag, 4UCAC4-520-130739 13.176fmag. Vmag 12.79mag for A seems questionable, especially as similar bright stars nearby are listed with 14.240Vmag. Bessel epoch 2015.702 20339+1915 J3094 AB 11.10 10.456 0.64 0.272 14.80 Companion too faint for resolution, thus rather confirming WDS value. Image quality questionable. Bessel epoch 2015.702 20363+1636 J3095 AB 12.40 12.462-0.06 0.280 12.40 12.766-0.37 0.286 Low SNR<20 for A and B, image quality questionable. Bessel epoch 2015.702 20365+2044 J3096 AB 10.50 10.676-0.18 0.171 12.60 12.825-0.23 0.192 Low SNR<20 for B. Bessel epoch 2015.702 20365+2044 J3096 BC 12.60 12.825-0.23 0.192 13.10 Low SNR<20 for B, no resolution for C, thus probably much fainter than 13.1mag. Questionable image quality. Bessel epoch 2015.702 20370+1420 J3098 AB 12.60 13.506-0.91 0.159 13.10 13.529-0.43 0.154 Low SNR<20 for A and B. Bessel epoch 2015.702 Table 2 concludes on next page.

Page 336 Jonckheere Double Star Photometry Part II: Delphinus Table 2 (conclusion). Bessel epoch 2015.683 (exceptions see notes column) photometry results for the J objects in Del.... WDS ID Name M1 WDS M1 new dm1 Err M1 M2 WDS M2 new dm2 Err M2 Notes 20378+1936 J3099 AB 12.50 13.012-0.51 0.116 12.70 13.558-0.86 0.121 Bessel epoch 2015.702 20385+1848 J3102 AB 11.60 11.678-0.08 0.171 12.10 12.845-0.75 0.173 Bessel epoch 2015.702 20393+2003 J3103 AB 12.05 10.494 1.56 0.170 12.42 12.618-0.20 0.174 Bessel epoch 2015.702 20397+1406 J3104 AB 9.90 11.717-1.82 0.111 11.20 13.103-1.90 0.115 Bessel epoch 2015.702 20416+1738 J3107 AB 11.70 13.205-1.51 0.132 11.70 13.295-1.60 0.130 Bessel epoch 2015.702 20436+1537 J3108 AB 11.00 11.214-0.21 0.101 12.50 12.133 0.37 0.102 Bessel epoch 2015.702 20433+1728 J3109 AB 12.50 12.577-0.08 0.134 13.10 12.659 0.44 0.135 Bessel epoch 2015.702 20466+1532 J3110 AB 11.20 11.105 0.09 0.111 11.50 11.751-0.25 0.112 Bessel epoch 2015.702 20509+1517 J3113 AB 11.50 12.829-1.33 0.107 11.50 12.880-1.38 0.106 Bessel epoch 2015.702 20513+1647 J3115 AB 12.16 11.714 0.45 0.104 15.20 13.673 1.53 0.128 Low SNR<20 for B. Bessel epoch 2015.702 20522+1656 J3116 AB 8.77 8.687 0.08 0.080 12.88 13.155-0.27 0.115 A too bright for reliable photometry, low SNR<20 for B. Bessel epoch 2015.702 20522+1656 J3116 BC 13.30 13.155 0.15 0.115 14.80 C too faint to be resolved, inconsistent WDS data for B (12.88 vs 13.3mag). Bessel epoch 2015.702 20585+1607 J3118 AB 9.40 9.607-0.21 0.110 11.20 11.978-0.78 0.113 Bessel epoch 2015.702 21081+1857 J3125 AB 12.40 12.490-0.09 0.119 13.60 13.588 0.01 0.137 Low SNR<20 for B. Bessel epoch 2015.702 20285+0443 J3220 AB 10.75 10.811-0.06 0.102 12.50 11.972 0.53 0.111 Bessel epoch 2015.702 20314+0701 J3221 AB 10.00 11.543-1.54 0.148 11.60 12.733-1.13 0.183 Very low SNR <10 for B. Bessel epoch 2015.702 20487+0706 J3223 AB 10.69 10.538 0.162 0.112 11.40 No resolution, not even an elongation. Probably WDS catalog mismatch. Bessel epoch 2015.828 20311+1247 J3244 AB 11.38 12.847-1.47 0.105 12.90 15.732-2.83 0.305 Very low SNR <10 for B. Same image as for J562. Bessel epoch 2015.702 20519+1203 J3245 AB 11.80 12.835-1.04 0.131 12.60 13.222-0.62 0.139 Low SNR<20 for A and B. Bessel epoch 2015.828 20289+1022 J3263 AB 11.30 12.489-1.19 0.141 12.10 13.801-1.70 0.183 Low SNR<20 for A and very low SNR<10 B. Bessel epoch 2015.828 20292+1019 J3264 AB 11.64 12.900-1.26 0.128 12.30 14.295-2.00 0.185 Very low SNR <10 for B. Bessel epoch 2015.828 20502+1246 J3277 AB 10.70 11.562-0.86 0.134 12.50 13.469-0.97 0.249 Very low SNR <10 for B. Bessel epoch 2015.828 20555+1730 J3328 AB 11.99 11.740 0.25 0.133 14.70 13.037 1.66 0.181 Low SNR<20 for A and very low SNR<10 B. Bessel epoch 2015.831 Table 2 notes on next page.

Page 337 Jonckheere Double Star Photometry Part II: Delphinus Notes regarding the notes column: it27 indicates the use of telescope it27 instead of it24. Bessel epoch indicates an epoch given different from 2015.683. Touching star disks indicates that the rims of the star disks are touching and that the measurement results might be a bit less precise than with clearly separated star disks. Overlapping/Touching star disks indicates that the star disks overlap to the degree of an elongation and that the measurement results is probably less precise than with clearly separated star disks. Overlapping star disks indicates star disk overlap to the degree that photometry for the separated components was no longer possible and that it was necessary to resort to the measurement of the combined magnitude. Low SNR <20 indicates that the measurement result might be a bit less precise than desired due to a low SNR value but this is already included in the calculation of the error range estimation. Very low SNR <10 indicates that the measurement result is probably a bit less precise than desired due to a very low SNR value but this is already included in the calculation of the error range estimation. Image quality questionable indicates a rather large average magnitude error for the reference stars used for plate solving either due to not this perfect weather conditions during imaging or may be erroneous Vmag values for the stars used for plate solving. But this is already included in the calculation of the error range estimation. too bright for reliable photometry indicates a star far brighter than the for plate solving used range 10.5 to 14.5mag despite this most such cases showed a reasonable measurement result anyway In case of J3223 separation is calculated based on the RA/Dec coordinates of the components. This is done using the formulae provided by Buchheim, 2008. Specifications of the used telescopes: it24: 610.mm CDK with 3962 mm focal length. Resolution 0.625 arcsec/pixel. V-filter. No transformation coefficients available. Located in Auberry, California. Elevation 1405 m. it27: 700.mm CDK with 4531.mm focal length. CCD: FLI PL09000. Resolution 0.53 arcsec/pixel. V-filter. No B-V transformation coefficients available. Located in Siding Spring, Australia. Elevation 1122 m.

Page 338 Double Star Measurements for December 2013 Frank Smith 20 Coburn Way Jaffrey, NH 03452 fhasmith@frankandluann.net Abstract: I report 288 measurements of binary systems from 2013.911. The observations were conducted with the T24 robotic telescope located at the itelescope Observatory, Auberry CA, USA (http:// www.itelescope.net/). Discussion includes notes on a number of the observed doubles. Several new components of existing binaries were discovered. One new multiple star system is described. Information about instrumentation and methodology and results is included. Introduction and Instrumentation I have been imaging double stars for a number of years using the equipment at itelescopes. This series of measurements of visual doubles used the T21 telescope at the itelescopes Observatory. The instrument is a Planewave 24inch (0.61m) Dall- Kirkham Astrograph with a focal length of approximately 3962 mm. The CCD camera is a FLI-PL0900 with 12um square pixels. The field of view is 31.8 X 31.8 arc-mins. The resolution is 0.62 arc-sec/pixel.the OTA is mounted on a Planewave Ascension 200HR. The instrument is capable of quickly and accurately slewing to a selected double star. The system takes about one minute to take short exposure and save the resulting image in a FITS format. Taking 5 to 6 exposures per double star allows 6 doubles to be imaged per hour. To maximize telescope time, the FITS images are stored on the itelescopes server and are retrieved later to be analyzed by suitable software (in my case MPO Canopus). Methods Imaging was done by entering the coordinates of the double into the robotic telescope s web interface. A test exposure was done and checked for centering and proper exposure. If all was well an exposure run of 5 to 7 images through a clear filter was done for each pair. Exposures typically ran about 10-15 seconds for 10-13 magnitude doubles. After the observing session was completed, the images were retrieved from an ftp site provided by the itelescope observatory. Some doubles appeared on more than one image and were measured more than 5 times. Each image in the exposure sequence was examined and any trailed or sub-par images were discarded. MPO Canopus was used to reduce the images (Warner, 2006). Any image that the software could not reach a plate solution was also discarded. Canopus produces an astronomic solution to the image based on the UCAC3 catalog (Zacharias et all.2010). The software measures double stars using a subroutine built into Canopus. It also produces a great amount of information about the astrometric solution. All images were copied to archival CD-ROM material and are available by request from the author. Each starting and ending image was blinked just in case. Results Table 1 shows the results for the 288 doubles measured. Discussion POU1903. I report a new C component. See Notes following Table 1. POU1912. I report a new C component. See Notes following Table 1. I report that components of POU894, POU1470, POU1889, and POU 1920 have close doubles as one of their components. In each case, I measured to the

Page 339 Double Star Measurements for December 2013 References itelecopes. http://www.itelescope.net/ Mason, B.D., 2006 Requesting double star data from the US Naval Observatory. JDSO. 2, 21-35. UCAC3 Catalog (Zacharias, et al. 2010). UCAC4 Catalog (Zacharias, et al. 2012). Warner, Brian 2006. MPO Canopus, http:// www.minorplanetobserver.com/mposoftware/ MPOCanopus.htm. Figure 1. CCD image showing SLE766 and new doubles Table 1 starts on next page. brighter of the two new components, which will be a little different than previous measures. New System I am aware that WDS does not need any more doubles, but I could not resist measuring a striking quadruple star located near SLE 766. As usual, Dr. Mason and Dr. Hartkopf have the final say in determining if the measure warrants inclusion in the WDS catalog. See image of this system in Figure 1. A star is UCAC4 503-030116. Position 06:42:25.0975+10:26:56.715. APASS V mag 10.382. proper motion PA 8.4 DEC -17.2. B Star is UCAC4 503-030113. 2MASS J mag 11.215. proper motion PA -1.8 DEC -42.4. C star is UCAC4 503-030109. 2MASS J mag 11.332. C is also URAT1 503-6011053 proper motion PA 0.9 DEC -2.4. D star is UCAC4 503-030108. 2MASS J mag 11.633. proper motion: PA 6.4 DEC -46.7. The B and D components have similar proper motions and could be a CPM pair. Acknowledgements Thank you to Dr. Mason and Dr. Hartkopf for being willing to work with amateurs and for answering data requests. Thank you also to my sister Gail Smith who proofread this article. This article made use of the Washington Double Star Catalog maintained by the U.S. Naval Observatory. This research made use of the VizierR Catalog Access Tool, CDS, Strasbourg, France. The original description of the Vizier service was published in A&AS 143,2.

Page 340 Double Star Measurements for December 2013 Table 1. Reported Measurements from December 2013 WDS ID Discoverer RA DEC PA SEP Epoch No. PAsd SEPsd Notes 06036+2427 POU862 AB 0604.5 2427 168.6 9.62 2013.911 5 0.10 0.054 06036+2427 POU 863 AC 0604.5 2427 106.3 9.08 2013.911 5 0.28 0.107 06043+2439 POU 882 0604.5 2445 34.2 12.81 2013.911 7 1.00 0.707 06038+2416 POU 867 0604.7 2416 48.6 8.25 2013.911 5 0.74 0.088 06039+2418 POU 868 0604.8 2418 252.6 14.68 2013.911 5 0.32 0.085 06040+2425 POU 871 0604.9 2425 121.2 9.87 2013.911 5 0.31 0.065 06042+2424 POU 881 0605.1 2424 116.7 11.09 2013.911 5 0.29 0.073 06043+2422 POU 883 0605.2 2422 193.7 9.40 2013.911 5 0.34 0.021 06046+2438 POU 894 0605.5 2437 1.4 12.70 2013.911 5 0.07 0.036 1 06046+3644 ALI 315 0605.5 3643 262.2 11.12 2013.911 5 0.07 0.085 06048+2411 POU 898 0605.7 2411 358.7 11.69 2013.911 5 0.40 0.039 06048+2408 POU 900 0605.7 2408 222.0 8.54 2013.911 5 0.83 0.144 06048+2413 POU 897 0605.7 2412 327.6 13.56 2013.911 5 0.41 0.095 06048+2410 POU 899 0605.7 2409 302.6 8.68 2013.911 5 0.27 0.164 06050+2446 POU 903 0605.8 2446 110.0 13.88 2013.911 5 0.34 0.041 06052+2443 POU 908 0606.0 2411 72.5 8.18 2013.911 5 0.73 0.075 06052+2443 POU 910 0606.1 2442 27.5 14.62 2013.911 5 0.69 0.083 2 06053+2416 POU 914 0606.2 2416 228.8 14.88 2013.911 5 0.04 0.028 06055+1336 SLE 832 0606.2 1336 64.5 10.96 2013.911 5 0.89 0.099 06055+2439 POU 916 0606.4 2439 283.3 12.30 2013.911 5 0.11 0.020 06058+1326 SLE 833 AB 0606.6 1326 343.5 38.56 2013.911 5 0.28 0.066 06058+1326 SLE 833 AC 0606.6 1326 345.2 32.28 2013.911 5 0.20 0.248 06059+3632 ALI 316 0606.8 3632 243.9 13.71 2013.911 5 0.37 0.040 06277+2249 BTG 10 0628.7 2251 310.4 35.32 2013.911 2 0.12 0.105 06277+2249 BTG 10 AC 0628.7 2251 310.8 35.36 2013.911 3 0.18 0.137 06277+2249 J 1092 AB 0628.7 2251 226.5 6.28 2013.911 5 0.43 0.277 06280+2332 POU 1338 0628.8 2331 149.9 18.74 2013.911 5 0.21 0.074 06281+2320 POU 1340 0628.9 2320 11.2 16.07 2013.911 5 0.26 0.065 06283+2325 POU 1343 0629.1 2325 166.8 7.50 2013.911 5 0.29 0.175 06285+2307 POU 1345 0629.3 2307 180.8 16.63 2013.911 5 0.22 0.090 06288+2313 POU 1347 0629.6 2311 80.5 14.59 2013.911 5 0.07 0.075 06289+2322 POU 1350 0629.7 2321 157.2 15.78 2013.911 5 0.17 0.075 06291+2322 POU 1355-2 0629.9 2326 141.7 8.83 2013.911 5 0.50 0.076 3 06294+2311 POU 1360 0630.2 2311 41.5 15.41 2013.911 5 0.23 0.083 06293+2308 POU 1358 0630.2 2308 162.6 8.34 2013.911 5 0.38 0.078 06342+2257 POU 1463 0635.0 2257 223.1 21.85 2013.911 6 0.09 0.089 06342+2305 POU 1465 0635.0 2305 53.9 18.24 2013.911 6 0.10 0.092 06343+2311 POU 1470 0635.2 2310 268.9 14.76 2013.911 6 0.11 0.083 4 06344+2408 POU 1478 0635.2 2308 56.8 15.10 2013.911 6 0.34 0.087 06344+2314 POU 1476 0635.2 2314 80.1 15.48 2013.911 6 0.25 0.069 06345+2322 POU 1481 0635.3 2321 302.5 7.58 2013.911 6 0.38 0.325 06346+2318 POU 1489 0635.4 2318 169.1 12.35 2013.911 6 0.25 0.074 06347+2310 POU 1492 0635.5 2310 315.9 15.07 2013.911 6 0.14 0.037 06350+2302 POU 1508 AB 0635.8 2302 62.6 10.72 2013.911 6 0.43 0.088 Table 1 continues on next page.

Page 341 Double Star Measurements for December 2013 Table 1 (continued). Reported Measurements from December 2013 WDS ID Discoverer RA DEC PA SEP Epoch No. PAsd SEPsd Notes 06350+2302 POU 1509 AC 0635.8 2302 221.8 14.65 2013.911 6 0.26 0.069 06351+2258 POU 1523 0635.9 2257 283.8 16.64 2013.911 6 0.21 0.051 06353+2252 POU 1528 0636.1 2252 294.6 8.80 2013.911 6 0.03 0.036 06353+2258 POU 1530 0636.1 2257 42.3 14.76 2013.911 5 0.28 0.072 06356+2253 POU 1542 0636.4 2252 191.7 10.97 2013.911 5 0.38 0.019 06356+2319 POU 1546 0636.5 2319 243.1 9.47 2013.911 6 0.74 0.088 06357+2305 POU 1548 0636.5 2305 14.8 12.23 2013.911 6 0.41 0.074 06357+2258 POU 1556 AB 0636.6 2257 131.0 11.54 2013.911 5 0.17 0.034 06357+2258 POU 1557 AC 0636.6 2257 155.6 22.04 2013.911 5 0.19 0.065 06258+2259 POU 1563 0636.6 2259 233.1 11.35 2013.911 6 0.42 0.059 06358+2255 POU1564 0636.6 2254 298.5 14.13 2013.911 6 0.29 0.158 5 06359+2257 POU 1568 0636.7 2256 94.7 13.38 2013.911 6 0.11 0.058 06359+2306 POU 1573 0636.7 2305 300.2 8.76 2013.911 6 0.64 0.084 06361+2257 POU 1579 0636.9 2256 47.1 11.64 2013.911 6 0.47 0.091 06363+2300 POU 1592 0637.1 2300 146.0 16.94 2013.911 6 0.35 0.117 06364+2257 POU 1598 0637.2 2256 35.8 11.37 2013.911 6 0.35 0.057 06370+2320 POU 1640 0637.8 2319 144.0 15.65 2013.911 6 0.12 0.064 06371+2342 POU 1644 0637.9 2341 141.1 13.48 2013.911 7 0.08 0.052 06370+2329 POU 1645 0637.9 2328 331.8 9.36 2013.911 6 0.30 0.036 06371+2329 POU 1652 0638.0 2328 121.6 10.73 2013.911 6 0.26 0.056 06371+2328 POU 1648 0638.0 2327 58.1 6.00 2013.911 6 0.90 0.216 06372+2424 POU 1653 0638.1 2424 0.3 12.62 2013.911 5 0.12 0.043 6 06372+2426 POU 1654 0638.1 2425 129.8 13.09 2013.911 5 0.08 0.054 06373+2429 POU 1655 0638.2 2428 136.9 12.49 2013.911 5 0.13 0.022 06373+2430 POU 1657 0638.2 2430 263.4 12.19 2013.911 5 0.28 0.063 06373+2326 POU 1660 0638.2 2325 230.6 15.19 2013.911 6 0.12 0.034 06374+2325 POU 1666 0638.2 2324 27.0 7.07 2013.911 6 0.21 0.129 06375+2321 POU 1671 0638.3 2321 234.7 17.27 2013.911 6 0.11 0.016 06374+2443 POU 1662 0638.3 2442 234.5 13.89 2013.911 5 0.19 0.031 06375+2347 POU 1672 0638.4 2346 197.2 10.47 2013.911 6 0.31 0.055 06376+2337 POU 1679 0638.4 2336 216.0 14.06 2013.911 6 0.16 0.021 06375+2411 POU 1676 0638.4 2410 249.7 9.42 2013.911 11 0.21 0.032 06376+2429 POU 1681 AB 0638.5 2428 211.8 7.93 2013.911 5 0.23 0.123 06376+2429 POU 1682 AC 0638.5 2428 29.5 12.05 2013.911 5 0.21 0.021 06377+2353 POU 1688 AB 0638.6 2352 32.9 18.80 2013.911 6 0.12 0.018 06377+2353 POU 1689 AC 0638.6 2352 208.4 9.70 2013.911 6 0.21 0.075 06377+2353 POU 1690 AD 0638.6 2352 132.8 11.72 2013.911 6 0.07 0.062 06377+2439 POU 1691 0638.6 2438 133.1 11.34 2013.911 5 0.38 0.076 06377+2441 POU 1686 0638.6 2440 127.2 18.21 2013.911 5 0.17 0.039 06377+2421 POU 1692 0638.6 2420 77.6 9.85 2013.911 5 0.34 0.039 06379+2336 POU 1700 AB 0638.7 2335 33.5 22.56 2013.911 5 0.73 0.119 06378+2322 POU 1697 0638.7 2321 225.9 13.53 2013.911 6 0.16 0.049 06379+2413 POU 1701 0638.8 2412 252.6 12.63 2013.911 6 0.33 0.048 06381+2344 POU 1708 0638.9 2343 257.6 11.02 2013.911 6 0.24 0.030 06380+2425 POU 1707 0638.9 2425 327.7 17.64 2013.911 5 0.10 0.021 06382+2334 POU 1717 0639.0 2333 226.5 10.87 2013.911 6 0.35 0.032 06383+2323 POU1715 0639.0 2322 35.4 13.61 2013.911 6 0.24 0.036 06383+2410 POU 1716 0639.1 2409 247.6 8.51 2013.911 11 0.08 0.086 06382+2425 POU 1718 0639.2 2422 57.8 11.56 2013.911 5 0.19 0.057 06385+2329 POU1725 0639.3 2328 266.4 8.98 2013.911 6 0.17 0.049 06385+2337 POU 1724 0639.3 2336 1.6 11.54 2013.911 6 0.09 0.028 06386+2321 POU1726 0639.4 2320 3.5 9.46 2013.911 6 0.62 0.079 06386+2427 POU 1729 0639.4 2426 179.7 11.34 2013.911 5 0.11 0.043 06387+2344 POU 1734 0639.5 2343 296.5 13.18 2013.911 11 0.18 0.061 Table 1 continues on next page.

Page 342 Double Star Measurements for December 2013 Table 1 (continued). Reported Measurements from December 2013 WDS ID Discoverer RA DEC PA SEP Epoch No. PAsd SEPsd Notes 063872317 POU 1735 0639.5 2316 66.3 15.66 2013.911 6 0.16 0.031 06386+2426 POU 1730 0639.5 2425 32.1 13.13 2013.911 5 0.17 0.023 06387+2356 POU 1731 0639.5 2355 27.2 13.35 2013.911 6 0.13 0.048 06388+2304 POU 1740 0639.6 2303 185.1 7.52 2013.911 5 0.44 0.082 06388+2301 POU 1737 0639.6 2300 223.7 6.52 2013.911 5 0.23 0.090 06388+2350 POU 1739 0639.6 2349 216.2 9.03 2013.911 6 0.20 0.036 06389+2359 POU 1741-1 0639.7 2358 97.6 12.62 2013.911 6 0.37 0.047 7 06389+2359 POU 1741-2 0639.8 2358 108.8 11.93 2013.911 6 0.92 0.095 7 06389+2341 POU 1744 0639.7 2340 112.8 12.17 2013.911 11 0.51 0.031 06390+2446 POU 1746 0639.8 2445 33.9 9.17 2013.911 5 0.17 0.099 06389+2444 POU 1742 0639.8 2443 100.6 17.22 2013.911 5 0.15 0.025 06389+2448 POU 1743 0639.8 2447 109.8 17.28 2013.911 5 0.19 0.028 06390+2410 POU 1749 0639.8 2409 197.9 10.77 2013.911 11 0.30 0.098 06391+2405 POU 1757 AB 0639.9 2403 129.0 11.49 2013.911 11 0.19 0.039 06391+2405 POU 1758 AC 0639.9 2403 53.8 16.94 2013.911 11 0.17 0.043 06390+2453 POU 1750 0639.9 2452 298.7 12.20 2013.911 5 0.31 0.063 06392+2314 POU 1761 0640.0 2313 156.1 15.50 2013.911 6 0.13 0.023 06393+0357 BAL 2679 0640.0 0355 186.0 11.00 2013.911 5 0.03 0.051 06392+2307 POU 1765 0640.0 2306 293.3 7.95 2013.911 5 0.28 0.159 06393+2307 POU 1768 AB 0640.1 2306 331.0 9.39 2013.911 5 0.28 0.022 06393+2307 POU 1769 AC 0640.1 2306 62.9 15.98 2013.911 5 0.16 0.022 06392+2452 POU 1762 0640.1 2451 145.3 10.67 2013.911 5 0.31 0.054 06393+2340 POU 1767 0640.1 2338 277.2 14.60 2013.911 5 0.20 0.054 06394+2421 POU 1773 0640.2 2419 297.5 16.47 2013.911 6 0.29 0.068 06393+2409 POU 1771 0640.2 2408 261.1 14.92 2013.911 16 0.31 0.057 06394+2335 POU 1772 0640.2 2333 242.1 13.95 2013.911 5 0.21 0.042 06394+2318 POU 1774 0640.2 2317 218.4 11.08 2013.911 6 0.19 0.038 06396+0417 BAL 2681 0640.3 0416 295.4 11.07 2013.911 5 0.19 0.026 06403+2320 POU1825 0640.3 2326 31.7 16.21 2013.911 5 0.08 0.025 06395+2436 TOK 19 0640.4 2435 248.5 31.38 2013.911 3 0.27 0.110 06396+2333 POU 1779 AB 0640.4 2332 340.6 5.86 2013.911 5 0.18 0.359 06396+2333 POU 1780 AC 0640.4 2332 352.8 13.63 2013.911 5 0.26 0.118 06397+0410 BAL 2683 0640.4 0409 302.5 9.01 2013.911 5 0.13 0.053 06396+2338 POU 1781 0640.4 2337 256.7 11.88 2013.911 5 0.16 0.023 06395+2355 POU 1777 0640.4 2354 134.9 7.35 2013.911 5 0.64 0.133 06396+2340 POU 1782 0640.4 2339 13.5 13.88 2013.911 5 0.19 0.049 06397+0334 HJ 2329 0640.5 0333 87.2 17.37 2013.911 5 0.02 0.031 06397+2305 POU 1786 0640.5 2304 355.2 8.09 2013.911 5 0.61 0.104 06397+2321 POU 1788 0640.5 2321 259.6 10.90 2013.911 5 0.26 0.061 06396+2356 POU 1785 0640.5 2355 83.4 14.88 2013.911 5 0.51 0.065 06397+2323 POU 1789 0640.6 2322 56.4 9.75 2013.911 5 0.10 0.064 06397+2442 POU 1787 0640.6 2441 234.0 10.59 2013.911 10 0.23 0.054 06398+2259 POU 1791 0640.6 2257 141.2 8.07 2013.911 5 0.15 0.048 06398+0839 SLE 557 0640.6 0839 168.6 11.01 2013.911 5 0.21 0.062 06398+2439 POU 1790 0640.7 2438 72.1 12.64 2013.911 10 0.24 0.033 06398+2432 POU 1792 0640.7 2431 4.3 13.83 2013.911 5 0.20 0.028 06398+2434 POU 1794 0640.7 2432 15.0 10.94 2013.911 5 0.35 0.076 06399+2313 POU 1795 0640.7 2312 135.1 8.16 2013.911 5 0.32 0.019 06400+2317 POU 1799 0640.8 2316 304.3 11.36 2013.911 5 0.24 0.116 06400+2313 POU 1800 0640.8 2311 220.8 10.81 2013.911 5 0.43 0.038 06399+2431 POU 1796 0640.8 2429 301.1 15.08 2013.911 5 0.38 0.046 06403+2320 POU 1825 0640.8 2325 31.7 16.21 2013.911 5 0.08 0.025 06401+2410 POU 1806 AB 0640.9 2408 166.1 8.87 2013.911 5 0.43 0.043 06401+2410 POU 1807 AC 0640.9 2408 271.6 11.43 2013.911 5 0.25 0.124 Table 1 continues on next page.

Page 343 Double Star Measurements for December 2013 Table 1 (continued). Reported Measurements from December 2013 WDS ID Discoverer RA DEC PA SEP Epoch No. PAsd SEPsd Notes 06400+2414 POU 1802 AC 0640.9 2412 162.4 7.17 2013.911 5 0.56 0.152 06400+2343 POU 1803 0640.9 2342 244.3 11.95 2013.911 5 0.20 0.036 06401+2342 POU 1805 0640.9 2341 40.3 10.48 2013.911 10 0.32 0.077 06400+2404 POU 1804 0640.9 2403 344.0 7.49 2013.911 10 1.26 0.083 06401+2309 POU 1808 0640.9 2308 15.4 8.19 2013.911 5 0.31 0.053 06403+0332 HJ 2331 AB 0641.0 0332 293.5 26.92 2013.911 5 0.15 0.087 06403+0332 HJ 2331 AC 0641.0 0332 50.8 25.46 2013.911 5 0.15 0.031 06402+2332 POU 1813 0641.0 2331 322.0 13.91 2013.911 9 0.29 0.091 06402+2331 POU 1810 0641.0 2330 334.6 9.22 2013.911 10 0.19 0.046 06402+2304 POU 1811 0641.0 2303 110.7 9.15 2013.911 5 0.29 0.051 06402+2423 POU 1814 AB 0641.1 2422 17.6 7.09 2013.911 4 0.47 0.413 06402+2423 POU 1815 AC 0641.1 2422 55.9 13.27 2013.911 5 0.33 0.143 06403+2431 POU 1822 AC 0641.1 2430 55.8 13.22 2013.911 5 0.30 0.059 06404+0344 BAL 2184 0641.1 0343 204.8 16.65 2013.911 5 0.06 0.036 06402+2404 POU 1816 0641.1 2403 220.4 10.96 2013.911 10 0.30 0.040 06402+2431 POU 1812 0641.1 2430 151.7 10.60 2013.911 5 0.24 0.032 06402+2422 POU 1817 0641.1 2421 168.0 7.93 2013.911 7 0.29 0.094 06404+2301 POU 1831 AB 0641.2 2300 152.1 11.26 2013.911 5 0.23 0.028 06404+2301 POU 1832 AC 0641.2 2300 263.2 8.10 2013.911 5 0.49 0.092 06404+2331 POU 1826 AB 0641.2 2330 77.6 17.78 2013.911 11 0.30 0.058 06404+2331 POU 1827 AC 0641.2 2330 197.8 15.62 2013.911 11 0.44 0.072 06403+2428 POU 1820 0641.2 2427 1.5 10.40 2013.911 5 0.52 0.094 06405+2302 POU 1830 0641.2 2301 74.0 13.08 2013.911 5 0.35 0.102 06403+2421 POU 1824 0641.2 2420 323.2 16.62 2013.911 5 0.25 0.049 06406+0402 BAL 2687 0641.3 0402 164.3 18.08 2013.911 5 0.11 0.037 06404+2307 POU 1836 0641.3 2305 280.7 11.95 2013.911 5 0.14 0.093 06405+2438 POU 1837 AB 0641.4 2437 130.1 12.49 2013.911 5 0.22 0.038 06405+2438 POU 1838 AC 0641.4 2437 171.5 21.29 2013.911 5 0.10 0.057 06405+2424 POU 1834 0641.4 2422 200.1 12.57 2013.911 5 0.19 0.037 06405+2349 POU 1835 0641.4 2348 138.7 15.84 2013.911 10 0.17 0.039 06405+2413 POU 1839 0641.4 2412 280.9 12.22 2013.911 5 0.41 0.077 06405+2354 POU 1840 0641.4 2353 289.8 5.51 2013.911 9 0.74 0.521 06406+2411 POU 1841 0641.4 2410 8.6 6.66 2013.911 5 0.65 0.213 06406+2402 POU 1842 0641.4 2400 296.5 5.27 2013.911 9 0.59 0.298 06407+2315 POU 1847 0641.5 2313 335.7 11.19 2013.911 5 0.27 0.037 06406+2319 POU 1844 0641.5 2320 256.2 18.89 2013.911 5 0.10 0.040 06408+2357 POU 1848 AB 0641.6 2355 183.7 11.46 2013.911 9 0.25 0.034 06408+2357 POU 1849 AC 0641.6 2355 112.2 17.43 2013.911 9 0.17 0.072 06408+2424 POU 1851 0641.7 2423 233.5 11.90 2013.911 6 0.19 0.055 06409+2328 POU 1853 0641.7 2326 122.3 12.95 2013.911 5 0.19 0.028 06410+2418 POU 1854 0641.8 2418 204.2 8.28 2013.911 5 0.29 0.055 06411+2355 POU 1855 0641.9 2348 206.0 15.53 2013.911 10 0.21 0.046 06411+2415 POU 1856 0641.9 2414 313.9 12.73 2013.911 10 0.58 0.111 06411+2347 POU 1857 0641.9 2346 321.5 10.69 2013.911 10 0.20 0.087 06463+2425 POU 2002 0641.9 2449 273.5 7.89 2013.911 5 0.64 0.049 06411+2425 POU 1863 AC 0642.0 2425 229.4 11.55 2013.911 5 0.22 0.093 06412+2412 POU 1864 0642.0 2411 17.3 16.54 2013.911 5 0.21 0.051 06411+2416 POU 1861 0642.0 2415 224.5 10.00 2013.911 5 0.58 0.160 06411+2427 POU 1858 0642.0 2427 279.0 10.95 2013.911 5 0.40 0.068 06411+2354 POU 1859 0642.0 2354 111.1 10.96 2013.911 9 0.45 0.104 06411+2340 POU 1860 0642.0 2339 325.4 9.99 2013.911 10 0.21 0.049 06412+2356 POU 1867 AB 0642.1 2356 211.2 11.68 2013.911 10 0.36 0.059 06412+2356 POU 1868 AC 0642.1 2356 232.4 20.53 2013.911 10 0.11 0.060 06412+2454 POU 1865 0642.1 2449 171.0 14.11 2013.911 5 0.24 0.012 Table 1 continues on next page.

Page 344 Double Star Measurements for December 2013 Table 1 (continued). Reported Measurements from December 2013 WDS ID Discoverer RA DEC PA SEP Epoch No. PAsd SEPsd Notes 06412+2418 POU 1869 0642.1 2418 126.1 7.50 2013.911 5 1.13 0.096 06413+2412 POU 1870 0642.1 2412 111.4 12.00 2013.911 5 0.43 0.112 06465+2359 POU 2004 0642.1 2423 29.8 7.26 2013.911 5 0.69 0.046 06413+2408 POU 1873 0642.2 2408 160.1 15.94 2013.911 5 0.14 0.023 06413+2439 POU 1875 0642.2 2439 292.0 8.79 2013.911 5 0.19 0.034 06417+2359 POU 1894 0642.2 2358 221.9 10.96 2013.911 9 0.25 0.064 06466+2423 POU 2005 0642.2 2447 43.4 13.85 2013.911 5 0.52 0.044 06466+2431 POU 2006 0642.2 2455 335.1 5.35 2013.911 5 0.46 0.310 06414+2336 POU 1883 AB 0642.3 2335 25.7 17.31 2013.911 5 0.33 0.062 06414+2453 POU 1877 0642.3 2452 259.4 15.72 2013.911 5 0.22 0.069 06414+2337 POU 1881 0642.3 2336 328.2 12.24 2013.911 5 0.32 0.043 06415+2434 POU 1885 0642.3 2434 137.4 10.40 2013.911 5 0.37 0.069 06414+2415 POU 1882 0642.3 2450 48.3 11.99 2013.911 5 0.31 0.038 13 06415+2314 POU 1886 0642.3 2341 109.3 9.94 2013.911 5 0.16 0.050 06415+2421 POU 1889 0642.4 2420 140.3 15.86 2013.911 5 0.61 0.150 8 06415+2315 POU 1890 0642.4 2350 22.4 14.34 2013.911 5 0.28 0.031 06417+2411 POU 1893 0642.5 2411 67.3 10.60 2013.911 5 0.31 0.112 06417+2327 POU 1895 0642.6 2327 336.5 6.52 2013.911 5 0.80 0.315 06470+2405 POU 2010 0642.6 2429 264.7 12.44 2013.911 6 0.34 0.077 06418+2412 POU 1896 0642.6 2412 221.9 10.37 2013.911 5 0.41 0.051 06419+2406 POU 1903 AB 0642.7 2406 98.9 14.89 2013.911 5 0.28 0.035 9 06419+2406 POU 1903 AC 0642.7 2406 127.0 14.18 2013.911 5 0.11 0.033 9 06419+2444 POU 1902 0642.7 2443 132.3 11.67 2013.911 5 0.40 0.070 11 06418+2436 POU 1901 0642.7 2436 128.9 15.57 2013.911 5 0.13 0.039 12 06419+2416 POU 1905 0642.8 2415 30.7 13.07 2013.911 5 0.13 0.032 06419+2437 POU 1906 0642.8 2436 332.9 16.57 2013.911 5 0.26 0.095 06419+2438 POU 1907 0642.8 2438 47.5 18.74 2013.911 5 0.05 0.024 06742+2409 POU 2012 0642.8 2433 266.5 9.78 2013.911 5 0.13 0.009 06420+2402 POU 1908 0642.8 2401 262.1 14.80 2013.911 5 0.20 0.047 06421+2400 POU 1911 0642.9 2400 272.9 15.26 2013.911 5 0.22 0.029 06421+2329 POU 1915 0642.9 2329 140.2 6.33 2013.911 5 0.65 0.121 06421+2359 POU 1910 0642.9 2359 66.6 5.70 2013.911 5 0.23 0.201 06421+2441 POU 1912 BC 0643.0 2440 141.3 8.63 2013.911 5 0.03 0.015 10 06421+2441 POU 1912 AB 0643.0 2441 202.8 15.75 2013.911 5 0.19 0.019 10 06421+2441 POU 1912 AC 0643.0 2441 182.0 21.27 2013.911 5 0.17 0.033 10 06421+2420 POU 1913 0643.0 2420 208.0 16.66 2013.911 5 0.19 0.038 06422+2431 POU 1916 0643.0 2430 94.9 12.25 2013.911 5 0.38 0.061 06474+2413 POU 2013 0643.0 2437 350.3 11.02 2013.911 5 0.30 0.038 06421+2437 POU 1914 0643.0 2437 258.5 10.97 2013.911 5 0.08 0.014 06422+2448 POU 1917 0643.1 2448 225.0 12.33 2013.911 5 0.24 0.068 06423+2412 POU 1918 0643.1 2412 357.8 10.36 2013.911 5 0.39 0.064 06423+2355 POU 1919 0643.1 2355 229.8 6.86 2013.911 5 0.38 0.200 NEW AB 0643.2 1026 235.6 6.93 2013.911 5 0.55 0.157 14 NEW AC 0643.2 1026 278.1 12.40 2013.911 5 0.08 0.027 14 NEW AD 0643.2 1026 233.4 15.30 2013.911 5 0.18 0.036 14 06424+2423 POU 1921 0643.2 2422 107.7 10.76 2013.911 5 0.09 0.070 06424+2448 POU 1920 0643.2 2448 350.7 15.02 2013.911 5 0.11 0.080 11 06422+2431 POU 2016 0643.2 2425 333.1 11.11 2013.911 5 0.50 0.044 06424+2413 POU 1923 0643.3 2413 127.9 13.41 2013.911 6 0.13 0.018 06477+2357 POU 2018 0643.3 2421 211.2 11.39 2013.911 5 0.38 0.077 06478+2408 POU 2022 0643.4 2432 73.1 10.74 2013.911 5 0.06 0.016 06426+1034 SLE 766 0643.4 1033 192.6 11.04 2013.911 5 0.24 0.053 06478+2406 POU 2024 0643.4 2430 126.0 11.34 2013.911 5 0.23 0.026 06478+2427 POU 2021 0643.4 2451 32.4 10.90 2013.911 5 0.27 0.063 Table 1 continues on next page.

Page 345 Double Star Measurements for December 2013 Table 1 (conclusion). Reported Measurements from December 2013 WDS ID Discoverer RA DEC PA SEP Epoch No. PAsd SEPsd Notes 06425+2438 POU 1925 0643.4 2437 152.0 17.66 2013.911 5 0.18 0.051 06428+2436 POU 1933 0643.5 2436 129.9 16.47 2013.911 5 0.32 0.071 06428+2427 POU 1930 0643.6 2426 222.8 13.61 2013.911 5 0.09 0.024 06481+2401 POU 2025 0643.7 2425 191.7 8.67 2013.911 5 0.50 0.054 06430+1020 SLE 767 0643.7 1019 61.5 19.41 2013.911 5 0.25 0.067 06429+2422 POU 1934 0643.7 2421 309.1 16.96 2013.911 5 0.15 0.079 06430+2436 POU 1938 0643.8 2435 107.2 11.19 2013.911 5 0.05 0.008 063431+2425 POU 1940 0643.9 2424 60.8 16.88 2013.911 5 0.14 0.022 06483+2405 POU 2027 0643.9 2429 227.6 14.92 2013.911 5 0.33 0.039 06430+2442 POU 1939 0643.9 2441 78.0 8.44 2013.911 5 0.30 0.062 06432+2430 POU 1948 0644.1 2430 27.3 16.17 2013.911 5 0.23 0.057 06434+2419 POU 1952 0644.2 2419 281.9 14.49 2013.911 5 0.30 0.098 06487+2359 POU 2032 0644.2 2424 194.9 8.38 2013.911 5 0.71 0.127 06433+2432 POU 1950 0644.2 2432 330.4 8.07 2013.911 5 0.36 0.028 06487+2403 POU 2033 0644.3 2427 167.3 13.89 2013.911 5 0.11 0.046 06435+2439 POU 1955 0644.3 2437 129.2 13.26 2013.911 5 0.14 0.039 06434+2418 POU 1953 0644.3 2418 76.4 9.21 2013.911 5 0.50 0.027 06436+2421 POU 1956 0644.4 2419 288.4 16.28 2013.911 5 0.04 0.007 06451+0251 BAL 1715 0645.8 0250 310.1 17.85 2013.911 5 0.27 0.080 06452+0306 BAL 2191 0645.9 0306 120.4 11.03 2013.911 5 0.22 0.048 06462+0256 BAL 2193 0647.1 0310 184.3 7.68 2013.911 6 0.36 0.118 06463+0247 BAL 1721 0647.1 0246 71.2 12.31 2013.911 5 0.15 0.090 06472+2346 POU 2011 0648.0 2344 208.6 7.87 2013.911 5 0.58 0.045 06481+2337 POU 2026 0648.9 2337 356.2 9.63 2013.911 5 0.48 0.037 06483+2337 POU 2029 0649.2 2337 91.6 12.99 2013.911 5 0.03 0.096 06490+2345 POU 2035 0649.8 2344 110.4 12.41 2013.911 5 0.16 0.095 Notes: 1. POU894. "A" star is a close binary, see Figure 2. 2. POU610. "B" star faint. 3UCAC 23005118 has a listed V mag of 15.903. 3. POU 1355. I'm measuring 3UCAC 227-059131 06:29:05.68 +23:26:25.3 Mag 14.9 as the "A" star and 3UCAC 227-059127 06:29:06.09+23:26:18.7 Mag 14.74 as the "B" star. 4. POU1470. "B" star is a close double. See image. I'm measuring to the brighter component 3UCAC 227-062476 Mag 12.59. The other star is 3UCAC 227-062480. See Figure 3. 5. POU1546. I'm measuring 3UCAC 226-064744 06:46.76.7+22:55:06.7 Mag 14.6 as the "A"star. "B" is 3UCAC 226-064729 06:35:45.86+22:55:13.3 Mag 15.2 is the "B" star. 6. POU1653."A" star is much fainter in my CCD image. "A" 3UCAC 229-069631 V mag 14.365, "B" 3UCAC 229-069633 V mag 13.37. 7. POU1741.There are two pairs available. One matches the 1906 measure and one matches 1998 measure. POU1741-1. Measuring 3UCAC 228-068389 V mag 15.04 and 3UCAC 228-068382 V mag 14.81. POU1741-2. Measuring: star at 06:38:57.47+23:58:36.3 mag 17.37, 06:38:58.32+23:58:32.6 mag 16.41 8. POU1889. 'B" star is a close double. See Figure 4. 9. POU1903. New "C" star. See Figure 5. "C" is UCAC-4 4UC571-033128. "A" and "B" stars have large and similar proper motions. Probable CPM pair. Figure 2. POU894. "A" is a close double Figure 3. POU1470. "B" star is a close double

Page 346 Double Star Measurements for December 2013 Illustration 4: POU1889 showing "B" star as a close double. Figure 5. POU1903 showing "B" and "C" components. 10. POU1912. Measuring new "C" star. See Figure 6. "C" is 3UCAC 230-070508 Mag 15.73. 11. POU1920. "A" star is a close double. See Figure 7. 12. POU1901. I'm measuring 3UCAC 230-070377 and 3UCAC 230-070384. "A" star is at 06:41:52.31+24:44:02.5 13. POU1882. Position seems wrong. I'm measuring 3UCAC 230-070172 and 3UCAC 230-070181. "A" is at 06:41:29.46+24:51:14.8. 14. New quadruple star. See "Discussion". Figure 6. POU1912 showing new "C" component. Figure 7. POU1920. Measuring to brighter companion.

Page 347 Photometry of Faint and Wide Doubles in Vulpecula Wilfried R.A. Knapp Vienna, Austria wilfried.knapp@gmail.com Chris Thuemen Double Star Imaging Project Pembroke, Ontario, Canada thuemen_cm@yahoo.ca Abstract: Images of several double stars in Vulpecula published on the Double Star Imaging Project Yahoo Group page suggest magnitude issues compared with the corresponding WDS catalog data per April 2015. Taking additional images with V-filter enabled photometry for these pairs, providing confirming results. Introduction This paper identifies double star systems in Vulpecula that appear to have visual magnitudes that are in conflict with the data as published in the WDS. During the course of a long term project to image double stars accessible to backyard telescopes while employing a consistent imaging regime, from one location, the sheer volume of images has allowed the authors to identify with some certainty double star systems having component magnitudes that are clearly in conflict with the published data. After visually identifying these suspect systems, the authors consult the University of Strasburg s website, VizieR, to access the online digital sky survey catalogues to confirm the visual observations. The preliminary findings are listed below: J 1303 - WDS mags. 9.8, 10.3. UCAC4 fmags 12.350 and 12.578; Vmag for A 12.086 but no value for "B". J 1303 actually belongs to Sagitta and somehow slipped into this list but we decided to keep it here to make use of the already existing photometry result. The image clearly shows, with the benefit of 4 additional field stars, that the WDS data is suspect (see Figure 1) AG 247 WDS mags. 9.02, 12. UCAC4 provides fmags for A & B of 8.965 and 13.121.Vmag for A only, 9.015. During our imaging run in Vulpecula, it became apparent, given the better seeing and transparency, our imaging setup was able to record Figure 1: J 1303 deeper, at least an additional magnitude, to reach beyond 12.5. In spite of this, our image contained only the smallest hint of the companion. We estimate B to be approaching magnitude 13. See Figure 2. HJ 1504 Chris Thuemen found what appeared to be clerical errors in the WDS data per April 2015 position angles or magnitudes had been interchanged A for B and B for A, and sent Brian Ma-

Page 348 Photometry of Faint and Wide Doubles in Vulpecula Figure 2. Image of AG 247 Figure 3. Star map of A 264 based on WDS coordinates. son/usno an email to confirm this in the latter part of August 2015. This led to a change in the WDS data accordingly, including changes in the estimated magnitudes for A, B, C to 7.1, 12.4, and 11.3. A 264AB WDS mags. of 8.20 and 13.00. There is conflicting data in the UCAC4 and NOMAD1 surveys. The image clearly shows something at the approximate location of the B component which tells us it has to be brighter than mag 13 with an estimation around 12.0. A careful review of the WDS records indicates there is is a second component, the C from MAD 7AC that is likely contributing to the unexpected brightness at the B component location. A 264 is actually a multiple with six components including HDS 2720 Aa,Ab indicating A to be a close double itself. MAD 7 contains two entries in the WDS, MAD 7AC and BC. A star map (see Figure 3) based on the WDS data shows inconsistent positions for B and C. Using the WDS given positions for A and B for calculating separation and position angle with the formulae provided by Buchheim 2008 we get 3.1 and 285 PA means somewhat off from the listed values and for this reason we included MAD7 in our list. Also the coordinates for HDS2720 are somewhat questionable if A264A is a close double then HDS2720Aa cannot have identical coordinates. HO 445 with WDS M1 9.8 and M2 10.9. The image is suggesting that the companion is dimmer than the WDS data. We estimate a magnitude in the order of 11.5 DAM 373 was added to the list because it is in the same field of view as A 264 and WDS mags with single digit precision suggested estimation instead of measurement. The WDS data indicates a DM of 2.2 but our image is suggesting the difference to be negligible. STF 2523CD a.k.a. KRU 8 WDS mags of C and D are 7.10 & 14.20. The DSS2.F.POSSII image from Aladin very nicely shows the D component as a real bump on the southeast quadrant of the primary C component. This is consistent with our new image in that the D component is quite obvious and clearly separated from the primary. Component D is brighter than the mag. 12.804 (UCAC 4 # 556-091331) south southwest of the C star. We found no mag value for D from either UCAC4 or NOMAD1 data but we estimate the D component magnitude at ~11.9. A summary of the WDS April 2015 data is given in Table 1. To investigate further our initial findings, we concluded that the best approach would be to obtain new images suitable for photometry. These images were taken with an online 610mm f/6.5 CDK telescope having a resolution of 0.625 arcseconds per pixel and equipped with a V-filter, located in Auberry, California. Initial plate solving and stacking of 5 images each was done with AAVSO VPhot and plate solving of the stacked image was then repeated with Astrometrica with UCAC4 as reference star catalog. Photometry was completed with Astrometrica based on all plate solving using reference star Vmags. Only reference stars with magnitude between 10.5 and 14.5 were used because of the higher precision in this magnitude range, thus results for stars significantly brighter are less reliable than

Page 349 Photometry of Faint and Wide Doubles in Vulpecula ID Name RA Dec Sep PA M1 M2 WDS19157+1654 J 1303 AB Sge 19:15:42.819 +16:54:02.601 4.7 198 9.80 10.30 WDS20089+2520 AG 247 AB Vul 20:08:54.732 +25:20:12.403 39.0 30 9.02 12.00 WDS20225+2618 HJ 1504 AC Vul 20:22:32.589 +26:17:53.103 52.0 228 7.16 11.20 WDS19127+2435 A 264 AB Vul 19:12:42.437 +24:34:36.299 3.2 288 8.20 13.00 WDS19127+2435 A 264 DE Vul 19:12:44.250 +24:34:24.798 5.0 119 15.00 15.50 WDS19127+2435 A 264 AD Vul 19:12:42.437 +24:34:36.299 27.3 115 8.23 15.00 WDS19127+2435 MAD 7 AC Vul 19:12:42.437 +24:34:36.299 1.9 340 8.20 12.80 WDS19127+2435 MAD 7 BC Vul 19:12:42.218 +24:34:37.103 2.3 72 13.00 12.80 WDS19124+2435 HO 445 AB Vul 19:12:27.022 +24:35:29.102 5.4 243 9.80 10.90 WDS19126+2433 DAM 373 AB Vul 19:12:38.270 +24:32:37.297 8.7 123 12.00 14.20 WDS19268+2110 Table 1: WDS 2015 April values for the objectsfurther Research STF 2523 KRU 8 CD Vul 19:26:58.870 +21:06:22.997 10.5 138 7.10 14.20 Table 2: Photometry and measurement results based on itelescope it24 images used with AAVSO VPhot ID Name M1+ Err1 M2+ Err2 Date Notes WDS19157+1654 J 1303 AB 12.677 0.07 13.042 0.07 2015.762 WDS20089+2520 AG 247 AB 9.987 0.06 12.942 0.06 2015.678 1 WDS20225+2618 HJ 1504 AB 6.981 0.08 12.304 0.08 2015.678 1 WDS20225+2618 HJ 1504 AC 6.981 0.08 11.218 0.08 2015.678 1 WDS19127+2435 A 264 AB 8.189 0.13 11.941 0.13 2015.678 1 WDS19127+2435 A 264 DE 15.021 0.22 15.423 0.30 2015.678 2 WDS19127+2435 A 264 AD 8.189 0.13 15.021 0.22 2015.678 3 WDS19127+2435 MAD 7 AC 8.189 0.13 - - 2015.678 4 WDS19127+2435 MAD 7 BC 11.941 0.13 - - 2015.678 5 WDS19124+2435 HO 445 AB 10.191 0.16 11.614 0.16 2015.678 1 WDS19126+2433 DAM 373 AB 13.918 0.15 14.480 0.17 2015.672 2 WDS19268+2110 STF2523 KRU 8 CD 6.402 0.17 12.818 0.18 2015.678 1 Notes: 1. A too bright for reliable photometry as the used UCAC4 reference stars were in the 12mag range 2. Very low SNR 3. A too bright for reliable photometry as the used UCAC4 reference stars were in the 12mag range. WDS mag for A not consistent (8.20 vs 8.23) 4. A too bright for reliable photometry as the used UCAC4 reference stars were in the 12mag range. No resolution for C, too close to the bright A component. Position C inconsistent from A and B 5. No resolution for C, too close to the bright A component. Position for MAD 7 B not consistent with A264 B

Page 350 Photometry of Faint and Wide Doubles in Vulpecula Table 3: Summary of results compared to WDS per April 2015. With a few exception WDS data changes are suggested ID Name Notes WDS19157+1654 J 1303 AB The components are about 3 mag fainter than listed but delta_m remained similar to Jonckheere s estimation WDS20089+2520 AG 247 AB B is about 1 mag fainter than listed WDS20225+2618 HJ 1504 AB WDS20225+2618 HJ 1504 AC WDS19127+2435 A 264 AB As already mentioned in the introduction the mag data for B was changed meanwhile to 12.4 quite close to the new measurement result of 12.304 As already mentioned in the introduction the mag data for C was changed meanwhile to 11.3 quite close to the new measurement result of 11.218 B as suspected is more than 1 mag. brighter than listed. Astrometry results based on Astrometrica: 19:12:42.517/+ 24:34:36.22 for A and 19:12:42.284/+ 24:34:37.18 for B with average error 0.15/0.13 giving 3.320 +/-0.198 separation and 286.806 +/-3.421 PA rather confirm the current WDS Sep/PA data within the given error range. Latest GAIA measurements with 19:12:42.448/+ 24:34:36.318 for A and 19:12:42.231/+ 24:34:37.117 for B would give 3.066 separation and 285.123 PA WDS19127+2435 A 264 DE WDS mag for E 15.5 quite confirmed with 15.423 WDS19127+2435 A 264 AD WDS mag for D 15 quite confirmed with 15.041 WDS19127+2435 MAD 7 AC WDS19127+2435 MAD 7 BC Position C could not be verified A too bright and C too close to be separated Position for B measured with RA 19:12:42.284 with an average error of 0.15 and Dec +24:34:37.18 with an average error of 0.13. With the given error range of our tools we cannot decide if the A 264 or the MAD 7 data should be corrected, it is only clear that the current data does not match. Probably it would be best to accept the latest precise measurements from GAIA WDS19124+2435 HO 445 AB Both components fainter than listed, especially B WDS19126+2433 DAM 373 AB Both components fainter than listed, especially A WDS19268+2110 KRU 8 CD D is about 1.5mag brighter than WDS listed (Continued from page 348) the results for star in the indicated magnitude range. The new values are included in Table 2. M+ is new measurement, Err is the error estimation calculated as mag 2 2.5log 10(1 1/ ) 2 Err dv SNR where SNR = Signal to noise ratio, dvmag = average Vmag error over all used reference stars (SNR and dvmag not listed due to space restrictions). Number of observations is 5 for all objects. Date given is the Bessel epoch of the observation. Summary With few exceptions the photometry results confirmed the image based first impressions at least to some degree. In the Table 3 we give a summary per object. References Buchheim, Robert 2008, CCD Double-Star Measurements at Altimira Observatory in 2007, Journal of Double Star Observations, Vol. 4 No. 1 Page 28 Acknowledgements The following tools and resources have been used for this research: Washington Double Star Catalog itelescope AAVSO VPhot AAVSO APASS UCAC4 catalog via the University of Heidelberg website Aladin Sky Atlas CDS, SIMBAD, VizieR, UCAC4, Nomad, URAT1, GAIA 2MASS All Sky Catalog AstroPlanner Astrometrica

Page 351 Jonckheere Double Star Photometry Part III: Lyra, Equuleus, and Eridanus Wilfried R.A. Knapp Vienna, Austria wilfried.knapp@gmail.com Abstract: If any double star discoverer is in urgent need of photometry then it is Jonckheere. There are over 3000 Jonckheere objects listed in the WDS catalog and a good part of them have magnitudes which are obviously far too bright. To keep the workload manageable only one image per object is taken and photometry is done with a software allowing a simple point and click procedure even a single measurement is better than the currently usually given estimation. 1. Introduction As follow up to the first two reports on J-objects in Cygnus (Knapp; Nanson 2016) and Delphinus (Knapp 2016) I selected for this report all J-objects in Lyra (Lyr), Equuleus (Equ), and Eridanus (Eri) given in the Tables 1 to 3 with all values based on WDS data as of April 2015. 2. Measurements 2.1 Photometry for the J-objects in Lyra For each of the listed J-objects one single image was taken (in Bessel epoch 2015.713) with itelescope it24 with 3 second exposure time. The initial plate solving was done by AAVSO VPhot and in the few cases with negative VPhot result again but positive with MaxIm DL6/PinPoint. Each image was then once more plate solved with Astrometrica using the UCAC4 catalog with reference stars in the Vmag range of 10.5 to 14.5 giving not only RA/Dec coordinates but also photometry results for all reference stars used including an average dvmag error. The J-objects were then located in the center of the image (worked fine with few exceptions indicating that the given RA/Dec coordinates are usually correct with the exceptions suggesting position problems) and photometry was then done using the Astrometrica procedure with point and click at the components delivering Vmag measurements based on all reference stars used for plate solving. The only changing parameter was the aperture radius used for photometry aiming to keep it equal or at least near 1.5x FWHM. In cases with smaller separation the star disks touched or overlapped but allowed nevertheless individual photometry even if less reliable than with clear separated disks. J110 allowed only the measurement of the combined magnitude but even in this case it is then possible to make a well-founded estimation for the components based on the initial observed m between the components based on the formula m combined 10 m 2.5log 2.521 2.521 m 1` 2 according to Greaney 2012. Measurements of the J-objects in Lyra are given in Table 4. 2.2 Photometry and Astrometry for the J-objects in Equ Beginning with the J-objects in Equ, I decided to provide photometric results and astrometric measurements in the form of RA/Dec coordinates resulting from plate solving as well as separation and position angle calculated based on the RA/Dec coordinates of the components. This is done by using the spherical trigonometry formulas provided by Buchheim 2008. Measurements of the J-objects in Equ are given in Table 5. 2.3 Photometry and Astrometry for the J-objects in Eri In Table 6, I again report photometric results and astrometric measurements in the form of RA/Dec coordinates resulting from plate solving as well as separation and position angle calculated based on the RA/Dec coordinates of the components. This is done by using the spherical trigonometry formulas provided by Buchheim 2008. Table 6 gives the measurements of the J-objects in Eri. (Continued on page 360)

Page 352 Jonckheere Double Star Photometry Part III: Lyra, Equuleus, and Eridanus Table 1: WDS April 2015 values for the Jonckheere objects in Lyra sorted by designation number WDS ID Name RA Dec Sep M1 M2 PA 18511+3524 J110 AB 18:51:06.099 +35:24:14.095 2.0 10.47 11.81 174 19018+3337 J112 AB 19:01:48.373 +33:37:16.501 25.4 6.39 13.30 178 18497+3223 J131 AB 18:49:41.470 +32:23:14.701 2.7 10.77 13.00 179 18386+2937 J525 AB 18:38:31.427 +29:37:06.997 3.1 9.20 9.40 69 18225+3130 J760 AB 18:22:28.757 +31:30:17.400 2.4 9.50 13.00 212 18274+3137 J761 AB 18:27:19.009 +31:36:35.803 3.7 9.60 11.20 180 18300+4033 J762 AB 18:30:01.387 +40:34:18.206 3.9 10.00 12.50 249 18301+4325 J763 AB 18:30:09.647 +43:26:30.106 1.8 9.70 9.70 309 18349+4053 J764 AB 18:34:53.410 +40:54:10.099 2.8 12.56 13.70 201 18494+3324 J765 AB 18:49:11.951 +33:25:51.105 2.3 12.30 12.50 333 19030+3729 J766 AB 19:02:56.942 +37:27:53.300 3.0 10.80 11.40 2 19030+3729 J766 AC 19:02:56.942 +37:27:53.300 16.7 10.80 12.10 176 19064+3750 J767 AB 19:06:29.987 +37:49:27.503 3.0 10.51 12.00 1 19064+3750 J767 AC 19:06:29.987 +37:49:27.503 7.9 10.51 13.00 181 19131+2946 J768 AB 19:13:05.571 +29:46:56.798 2.9 10.50 12.20 350 19203+2914 J769 AB 19:20:15.527 +29:12:01.500 3.7 9.70 9.90 207 19031+2757 J811 AB 19:03:08.340 +27:56:44.903 2.6 11.90 12.40 248 18381+3000 J1138 AB 18:38:00.693 +30:00:38.802 2.7 9.80 9.80 300 19075+2728 J1205 AB 19:07:25.667 +27:28:39.202 3.5 10.00 10.20 317 19117+2712 J1206 AB 19:11:37.632 +27:12:44.703 3.0 11.94 12.20 332 18491+2834 J1208 AB 18:49:09.932 +28:34:17.499 5.0 9.50 10.00 333 19045+3406 J1209 AB 19:04:25.079 +34:06:19.893 4.6 9.50 10.00 155 19115+2953 J1263 AB 19:11:31.418 +29:53:24.602 31.1 7.62 13.00 255 19115+2953 J1263 BC 19:11:28.699 +29:53:10.203 8.0 13.00 14.10 42 19047+2850 J2941 AB 19:04:46.441 +28:51:04.499 8.6 10.80 12.50 234 19056+2848 J2942 AB 19:05:40.549 +28:49:42.802 6.8 11.80 13.00 60 19079+3043 J2945 AC 19:07:48.567 +30:43:36.202 9.8 10.81 14.10 192 19068+3815 J3213 AB 19:06:51.500 +38:15:42.105 2.5 9.70 9.70 201 19145+2945 J3313 AB 19:14:31.738 +29:45:13.898 10.7 8.94 14.00 32

Page 353 Jonckheere Double Star Photometry Part III: Lyra, Equuleus, and Eridanus Table 2: WDS April 2015 values for the Jonckheere objects in Equuleus sorted by designation number WDS ID Name RA Dec Sep M1 M2 PA 21021+1016 J158 AB 21:02:08.863 +10:17:33.400 5.0 10.93 13.10 166 21086+0938 J159 AB 21:08:35.231 +09:37:46.301 4.0 10.30 11.30 247 21225+1057 J161 AB 21:22:28.071 +10:57:18.401 2.0 10.45 10.66 299 21124+0745 J576 AB 21:12:25.450 +07:45:06.101 2.3 10.10 10.60 236 20595+1113 J608 AB 20:59:27.721 +11:13:22.301 5.0 11.20 13.50 105 21091+0429 J848 AB 21:09:07.730 +04:28:57.100 2.6 10.23 13.00 145 20592+1129 J913 AB 20:59:09.882 +11:28:41.001 2.9 9.20 10.90 120 21242+0248 J914 AB 21:24:11.060 +02:46:59.600 1.9 11.11 11.11 0 21256+0248 J1039 AB 21:25:37.509 +02:47:43.900 4.3 9.60 10.50 332 21224+0953 J1356 AB 21:22:26.478 +09:52:36.200 7.7 12.00 12.40 178 21192+0339 J1721 AB 21:19:20.568 +03:40:56.800 3.8 11.10 13.80 275 21066+1137 J1781 AB 21:06:38.907 +11:36:55.802 7.8 9.40 11.00 117 21197+0537 J2341 AB 21:19:43.111 +05:37:11.900 7.3 11.90 11.90 349 21071+1042 J2576 AB 21:06:55.702 +10:29:50.099 6.1 12.00 13.00 59 21222+1114 J2605 AB 21:22:21.451 +11:13:50.800 1.9 11.55 13.30 222 Table 3: WDS April 2015 values for the Jonckheere objects in Eridanus sorted by designation number WDS ID Name RA Dec Sep M1 M2 PA 04531-1039 J318 AB 04:53:10.249-10:39:16.900 4.8 12.44 12.60 286 05043-0514 J319 AB 05:04:21.341-05:12:59.700 3.3 11.05 12.10 233 04234-0634 J708 AB 04:23:23.471-06:34:15.400 2.2 10.84 11.13 282 04297-0335 J709 AB 04:29:42.339-03:34:40.600 1.2 10.72 10.86 87 04383-0243 J710 AB 04:38:19.390-02:42:55.900 3.2 10.50 11.70 315 04584-0908 J1003 AB 04:58:26.311-09:06:00.101 5.4 11.36 13.60 238 05088-0830 J1004 AB 05:08:49.960-08:30:58.801 3.3 12.52 12.50 322 04302-0337 J1087 AB 04:30:12.760-03:37:12.900 2.6 11.06 15.10 13 02475-0601 J1245 AB 02:47:29.960-06:00:51.801 2.3 11.00 11.04 12 02501-0616 J1453 AB 02:50:07.000-06:16:11.900 9.2 11.10 10.70 201 02501-0616 J1453 AC 02:50:07.000-06:16:11.900 38.5 11.13 13.00 69 03032-0215 J1455 AB 03:03:07.460-02:14:53.700 6.2 11.50 11.80 61 03175-1222 J1456 AB 03:17:30.390-12:22:51.801 3.6 11.06 11.16 319 03361-0320 J1457 AB 03:36:04.420-03:20:05.800 2.9 10.34 10.84 216 04220-0626 J1459 AB 04:21:59.820-06:25:33.901 3.0 11.03 11.10 241

Page 354 Jonckheere Double Star Photometry Part III: Lyra, Equuleus, and Eridanus Table 4. Bessel epoch 2015.713 photometry results for the J objects in Lyr. M1 WDS and M2 WDS are the WDS catalog values. M1 new stands for measured M1, dm1 stands for delta between M1 WDS and M1 new. M2 new stands for measured M2, dm2 stands for delta M1 WDS and M1 new. Err M1 stands for the estimated error range calculated from the average delta Vmag over all reference stars used in the image and the SNR value of the star with the formula SQRT(dVmag^2+(2.5*LOG10(1+1/SNR))^2 WDS ID Name M1 WDS M1 new dm1 Err M1 M2 WDS M2 new dm2 Err M2 Notes 18511+3524 J110 AB 10.47 10.710-0.240 0.130 11.81 12.050-0.240 0.130 Overlapping star disks - no separate photometry possible. Combined magnitude 10.436 with SNR 132.41 gives estimated M1 new and M2 new values confirming rather well the current WDS values 19018+3337 J112 AB 6.39 6.504-0.114 0.180 13.30 12.582 0.718 A too bright for reliable photometry 0.182 No resolution of B 18497+3223 J131 AB 10.77 10.767 0.003 0.150 13.00 - - - suggests B being far fainter than listed 18386+2937 J525 AB 9.20 11.162-1.962 0.141 9.40 11.342-1.942 0.141 18225+3130 J760 AB 9.50 11.524-2.024 0.130 13.00 12.914 0.086 0.133 18274+3137 J761 AB 9.60 11.211-1.611 0.140 11.20 12.801-1.601 0.143 18300+4033 J762 AB 10.00 12.404-2.404 0.082 12.50 13.643-1.143 0.090 18301+4325 J763 AB 9.70 11.975-2.275 0.076 9.70 12.250-2.550 0.081 Touching/Overlapping star disks 18349+4053 J764 AB 12.56 11.751 0.809 0.052 13.70 12.395 1.305 0.055 18494+3324 J765 AB 12.30 11.385 0.915 0.160 12.50 11.408 1.092 0.160 Touching star disks 19030+3729 J766 AB 10.80 11.718-0.918 0.131 11.40 12.425-1.025 0.131 Touching star disks 19030+3729 J766 AC 10.80 11.718-0.918 0.131 12.10 12.780-0.680 0.132 19064+3750 J767 AB 10.51 11.587-1.077 0.141 12.00 13.140-1.140 0.146 19064+3750 J767 AC 10.51 11.587-1.077 0.141 13.00 13.994-0.994 0.150 19131+2946 J768 AB 10.50 12.356-1.856 0.152 12.20 14.681-2.481 0.174 SNR for B <20 19203+2914 J769 AB 9.70 11.603-1.903 0.160 9.90 12.185-2.285 0.161 19031+2757 J811 AB 11.90 11.699 0.201 0.151 12.40 12.973-0.573 Touching star disks. 0.164 SNR for B <20 18381+3000 J1138 AB 9.80 11.910-2.110 0.102 9.80 12.011-2.211 0.102 Touching star disks 19075+2728 J1205 AB 10.00 12.094-2.094 0.161 10.20 12.250-2.050 0.162 19117+2712 J1206 AB 11.94 13.373-1.433 0.174 12.20 13.479-1.279 0.175 18491+2834 J1208 AB 9.50 11.538-2.038 0.131 10.00 12.051-2.051 0.131 19045+3406 J1209 AB 9.50 11.529-2.029 0.190 10.00 12.303-2.303 0.191 No double star at this position. Nearby A 19 11 46.012 +27 12 02.68 and B 19 11 45.900 +27 12 04.86 with dra 0.14 and ddec 0.15 giving Sep 2.643" with Err 0.205 and PA 325.573 with Err 4.439 Minor position issue: A 18 49 14.783 +28 34 46.97 18 49 14.627 +28 34 51.17 with dra 0.14 and ddec 0.15 giving Sep 4.676" with Err 0.205 and PA 333.930 with Err 2.413 Table 4 concludes on next page.

Page 355 Jonckheere Double Star Photometry Part III: Lyra, Equuleus, and Eridanus Table 4 (conclusion). Bessel epoch 2015.713 photometry results for the J objects in Lyr. M1 WDS and M2 WDS are the WDS catalog values. M1 new stands for measured M1, dm1 stands for delta between M1 WDS and M1 new. M2 new stands for measured M2, dm2 stands for delta M1 WDS and M1 new. Err M1 stands for the estimated error range calculated from the average delta Vmag over all reference stars used in the image and the SNR value of the star with the formula SQRT(dVmag^2+(2.5*LOG10(1+1/SNR))^2 WDS ID Name M1 WDS M1 new dm1 Err M1 M2 WDS M2 new dm2 Err M2 Notes 19115+2953 J1263 AB 7.62 7.466 0.154 0.140 13.00 12.917 0.083 0.142 A too bright for reliable measurement, star disk looks elongated, might be a close double itself 19115+2953 J1263 BC 13.00 12.917 0.083 0.142 14.10 14.040 0.060 0.151 SNR for C <20 19047+2850 J2941 AB 10.80 12.361-1.561 0.141 12.50 14.402-1.902 0.150 SNR for B <20 19056+2848 J2942 AB 11.80 13.155-1.355 0.152 13.00 14.433-1.433 0.165 SNR for B <20 19079+3043 J2945 AC 10.81 10.616 0.194 0.150 14.10 13.685 0.415 Mag for HLM16 B measured with 12.340 with 0.156 SNR 51.98 (WDS lists 12.7mag) Notes regarding the notes column: Touching star disks indicates that the rims of the star disks are touching and that the measurement results might be a bit less precise than with clearly separated star disks Overlapping/Touching star disks indicates that the star disks overlap to the degree of an elongation and that the measurement results is probably less precise than with clearly separated star disks Overlapping star disks indicates star disk overlap to the degree that photometry for the separated components was no longer possible and that it was necessary to resort to the measurement of the combined magnitude Low SNR <20 indicates that the measurement result might be a bit less precise than desired due to a low SNR value but this is already included in the calculation of the error range estimation too bright for reliable photometry indicates a star far brighter than the for plate solving used range 10.5 to 14.5mag despite this most such cases showed a reasonable measurement result anyway In case of questionable astrometric data separation and position angle is calculated based on the RA/Dec coordinates of the components. This is done using the formulas provided by Buchheim 2008 Specifications of the used telescope: T24: 610mm CDK with 3962mm focal length. Resolution 0.625 arcsec/pixel. V-filter. No transformation coefficients available. Located in Auberry, California. Elevation 1405m

Page 356 Jonckheere Double Star Photometry Part III: Lyra, Equuleus, and Eridanus Table 5. Bessel epoch 2015.837 astrometry and photometry results for the J objects in Equ plus BRT1355 as bonus. Number of observations is 1. RA and Dec are the coordinates based on plate solving with UCAC4 reference stars in the 10.5 to 14.5mag range. Sep is separation calculated as SQRT(((RA2-RA1)*cos(Dec1))^2+(Dec2-Dec1)^2) in radians. Err Sep is the error estimation for Sep calculated as SQRT(dRA^2+dDec^2). The position angle PA is calculated as arctan((ra2-ra1)*cos (Dec1))/(Dec2-Dec1)) in radians and Err_PA is the error estimation for PA calculated as arctan(err_sep/sep) in degrees assuming the worst case that Err_Sep points in the right angle to the direction of the separation means perpendicular to the separation vector. Err Mag stands for the estimated error range calculated from the average delta Vmag over all reference stars used in the image and the SNR value of the star with the formula SQRT(dVmag^2+(2.5*LOG10(1+1/SNR))^2) Name RA Dec Sep Err Sep PA Err PA Mag Err Mag Notes J 158 A 21 02 08.841 10 17 33.41 10.641 0.191 it27 1x3s. SNR for 5.386 0.270 168.621 2.872 B<20 B 21 02 08.913 10 17 28.13 12.861 0.207 J 159 A 21 08 35.186 09 37 44.36 9.843 0.100 4.171 0.336 245.192 4.606 B 21 08 34.930 09 37 42.61 11.652 0.104 it27 1x3s J 161 J 576 J 608 J 848 J 913 J 914 J 1039 A 21 22 28.149 10 57 17.73 10.163 0.091 it27 1x3s. Touching/ 2.488 0.236 289.735 5.420 Overlapping star B 21 22 27.990 10 57 18.57 10.306 0.091 disks A 21 12 25.542 07 45 06.52 10.791 0.092 it27 1x3s. Touching/ 2.357 0.297 237.681 7.182 Overlapping star B 21 12 25.408 07 45 05.26 10.844 0.092 disks A 20 59 27.719 11 13 22.35 10.965 0.102 it27 1x3s. SNR for 5.003 0.304 112.567 3.479 B<10, barely to see B 20 59 28.033 11 13 20.43 14.233 0.227 A 21 09 07.719 04 28 56.66 9.982 0.081 it27 1x3s. Touching/ 2.806 0.348 140.646 7.074 Overlapping star B 21 09 07.838 04 28 54.49 12.324 0.090 disks A 20 59 09.859 11 28 40.68 10.811 0.111 it27 1x3s. Touching/ 2.686 0.374 123.697 7.937 Overlapping star B 20 59 10.011 11 28 39.19 12.485 0.121 disks A 21 24 11.162 02 46 59.33 10.800 0.071 it27 1x3s. Touching/ 2.040 0.311 0.842 8.671 Overlapping star B 21 24 11.164 02 47 01.37 10.978 0.071 disks A 21 25 37.490 02 47 41.91 12.160 0.073 it27 1x3s. SNR for 4.722 0.291 343.598 3.523 B<20 B 21 25 37.401 02 47 46.44 14.117 0.093 J 1356 A 21 22 26.526 09 52 37.01 7.993 0.255 175.653 1.827 11.936 0.111 it27 1x3s B 21 22 26.567 09 52 29.04 12.847 0.113 J 1721 A 21 19 20.592 03 40 56.73 3.161 0.205 272.357 3.714 11.248 0.061 it27 1x3s B 21 19 20.381 03 40 56.86 12.587 0.066 Table 5 concludes on next page.

Page 357 Jonckheere Double Star Photometry Part III: Lyra, Equuleus, and Eridanus Table 5 (conclusion). Bessel epoch 2015.837 astrometry and photometry results for the J objects in Equ plus BRT1355 as bonus. Number of observations is 1. RA and Dec are the coordinates based on plate solving with UCAC4 reference stars in the 10.5 to 14.5mag range. Sep is separation calculated as SQRT(((RA2-RA1)*cos(Dec1))^2+(Dec2-Dec1)^2) in radians. Err Sep is the error estimation for Sep calculated as SQRT(dRA^2+dDec^2). The position angle PA is calculated as arctan((ra2- RA1)*cos(Dec1))/(Dec2-Dec1)) in radians and Err_PA is the error estimation for PA calculated as arctan(err_sep/sep) in degrees assuming the worst case that Err_Sep points in the right angle to the direction of the separation means perpendicular to the separation vector. Err Mag stands for the estimated error range calculated from the average delta Vmag over all reference stars used in the image and the SNR value of the star with the formula SQRT(dVmag^2+(2.5*LOG10(1+1/SNR))^2) Name RA Dec Sep Err Sep PA Err PA Mag Err Mag Notes J 1781 A 21 06 38.930 11 36 54.99 7.499 0.355 116.447 2.711 10.718 0.101 it27 1x3s B 21 06 39.387 11 36 51.65 12.405 0.103 J 2341 A 21 19 43.114 05 37 11.38 7.424 0.292 349.926 2.249 12.090 0.092 it27 1x3s B 21 19 43.027 05 37 18.69 13.156 0.094 J 2576 A 21 06 55.769 10 29 50.38 14.453 0.127 5.393 0.382 57.973 4.050 B 21 06 56.079 10 29 53.24 14.146 0.139 it27 1x3s. SNR for A and B<20. No good match with the original Jonckheere 12/13 mags J 2605 BRT1355 A 21 22 21.445 11 13 50.63 12.333 0.088 it27 1x3s. Touching/ 2.055 0.318 226.301 8.802 Overlapping star B 21 22 21.344 11 13 49.21 12.369 0.090 disks A 21 22 25.570 11 11 01.00 11.491 0.082 it27 1x3s. Touching 3.912 0.318 194.373 4.651 star disks B 21 22 25.504 11 10 57.21 12.528 0.087 Notes regarding the notes column: it27 1x3s indicates that the given values base on one it27 image with 3 seconds exposure time. Touching star disks indicates that the rims of the star disks are touching and that the measurement results might be a bit less precise than with clearly separated star disks. Overlapping/Touching star disks indicates that the star disks overlap to the degree of an elongation and that the measurement results is probably less precise than with clearly separated star disks. Overlapping star disks indicates star disk overlap to the degree that photometry for the separated components was no longer possible and that it was necessary to resort to the measurement of the combined magnitude. Low SNR <20 indicates that the measurement result might be a bit less precise than desired due to a low SNR value but this is already included in the calculation of the error range estimation. too bright for reliable photometry indicates a star far brighter than the range used in plate solving (mag. 10.5 to 14.5), despite this most such cases showed a reasonable measurement result anyway. Specifications of the used telescope: it27: 700mm CDK with 4531mm focal length. CCD: FLI PL09000. Resolution 0.53 arcsec/pixel. V-filter. No B-V transformation coefficients available. Located in Siding Spring, Australia. Elevation 1122m

Page 358 Jonckheere Double Star Photometry Part III: Lyra, Equuleus, and Eridanus Table 6. Bessel epoch 2015.966 astrometry and photometry results for the J objects in Eri. Number of observations is 1. RA and Dec are the coordinates based on plate solving with UCAC4 reference stars in the 10.5 to 14.5mag range. Sep is separation calculated as SQRT(((RA2-RA1)*cos(Dec1))^2+(Dec2-Dec1)^2) in radians. Err Sep is the error estimation for Sep calculated as SQRT(dRA^2+dDec^2). The position angle PA is calculated as arctan((ra2-ra1)*cos(dec1))/(dec2-dec1)) in radians and Err_PA is the error estimation for PA calculated as arctan(err_sep/sep) in degrees assuming the worst case that Err_Sep points in the right angle to the direction of the separation means perpendicular to the separation vector. Err Mag stands for the estimated error range calculated from the average delta Vmag over all reference stars used in the image and the SNR value of the star with the formula SQRT(dVmag^2+(2.5*LOG10(1+1/SNR))^2) Name RA Dec Sep Err Sep PA Err PA Mag Err Mag Notes J 318 A 04 53 10.255-10 39 17.09 11.319 0.061 4.816 0.219 286.031 2.607 B 04 53 09.941-10 39 15.76 11.738 0.061 it27 1x3s J 319 A 05 04 21.336-05 12 59.55 10.982 0.061 3.399 0.213 233.958 3.579 B 05 04 21.152-05 13 01.55 11.821 0.061 it27 1x3s J 708 A 04 23 23.450-06 34 15.70 10.596 0.062 it27 1x3s. Touching/ 2.279 0.248 286.045 6.199 Overlapping star B 04 23 23.303-06 34 15.07 10.836 0.061 disks J 709 04 29 42.350-03 34 40.90-0.248 - - 10.245 0.051 it27 1x3s. No resolution but elongation according to the listed WDS PA. Combined magnitude 10.245 suggests 10.93/11.07mag for A/ B keeping the given delta_m J 710 A 04 38 19.368-02 42 55.82 10.478 0.061 3.096 0.227 315.817 4.189 B 04 38 19.224-02 42 53.60 11.706 0.066 it27 1x3s. Touching star disks J 1003 A 04 58 26.324-09 06 00.31 11.287 0.061 5.536 0.262 236.317 2.707 B 04 58 26.013-09 06 03.38 13.151 0.063 it27 1x3s J 1004 A 05 08 49.953-08 30 58.89 12.305 0.062 3.233 0.233 320.371 4.130 B 05 08 49.814-08 30 56.40 12.402 0.062 it27 1x3s J 1087 A 04 30 12.763-03 37 13.78 11.047 0.101 it27 1x3s. Touching/ 2.965 0.361 16.723 6.935 Overlapping star B 04 30 12.820-03 37 10.94 13.149 0.109 disks J 1245 A 02 47 29.959-06 00 52.63 10.402 0.076 it27 1x3s. Touching/ 2.642 0.304 20.149 6.568 Overlapping star B 02 47 30.020-06 00 50.15 10.615 0.083 disks Table 6 concludes on next page.

Page 359 Jonckheere Double Star Photometry Part III: Lyra, Equuleus, and Eridanus Table 6 (conclusion). Bessel epoch 2015.966 astrometry and photometry results for the J objects in Eri. Number of observations is 1. RA and Dec are the coordinates based on plate solving with UCAC4 reference stars in the 10.5 to 14.5mag range. Sep is separation calculated as SQRT(((RA2-RA1)*cos(Dec1))^2+(Dec2-Dec1)^2) in radians. Err Sep is the error estimation for Sep calculated as SQRT(dRA^2+dDec^2). The position angle PA is calculated as arctan((ra2-ra1)*cos(dec1))/(dec2- Dec1)) in radians and Err_PA is the error estimation for PA calculated as arctan(err_sep/sep) in degrees assuming the worst case that Err_Sep points in the right angle to the direction of the separation means perpendicular to the separation vector. Err Mag stands for the estimated error range calculated from the average delta Vmag over all reference stars used in the image and the SNR value of the star with the formula SQRT(dVmag^2+(2.5*LOG10(1+1/SNR))^2) Name RA Dec Sep Err Sep PA Err PA Mag Err Mag Notes J 1453 A 02 50 07.009-06 16 12.02 10.977 0.092 9.500 0.336 200.296 2.027 B 02 50 06.788-06 16 20.93 11.287 0.092 it27 1x3s J 1453 A 02 50 07.009-06 16 12.02 10.977 0.092 38.360 0.336 68.096 0.502 C 02 50 09.396-06 15 57.71 12.974 0.101 it27 1x3s J 1455 A 03 03 07.440-02 14 54.05 11.577 0.080 6.257 0.178 63.008 1.630 B 03 03 07.812-02 14 51.21 11.941 0.081 it27 1x3s J 1456 A 03 17 30.417-12 22 51.62 11.098 0.101 3.890 0.311 325.603 4.577 B 03 17 30.267-12 22 48.41 11.014 0.101 it27 1x3s J 1457 A 03 36 04.465-03 20 04.95 10.104 0.131 it27 1x3s. Touching 3.277 0.318 220.809 5.548 star disks B 03 36 04.322-03 20 07.43 10.368 0.134 J 1459 A 04 22 00.001-06 25 32.96 10.996 0.052 it27 1x3s. Touching 3.155 0.278 240.369 5.036 star disks B 04 21 59.817-06 25 34.52 10.919 0.051 Notes regarding the notes column: it27 1x3s indicates that the given values base on one it27 image with 3 seconds exposure time. Touching star disks indicates that the rims of the star disks are touching and that the measurement results might be a bit less precise than with clearly separated star disks. Overlapping/Touching star disks indicates that the star disks overlap to the degree of an elongation and that the measurement results are probably less precise than with clearly separated star disks. Overlapping star disks indicates star disk overlap to the degree that photometry for the separated components was no longer possible and that it was necessary to resort to the measurement of the combined magnitude. Low SNR <20 indicates that the measurement result might be a bit less precise than desired due to a low SNR value but this is already included in the calculation of the error range estimation. too bright for reliable photometry indicates a star far brighter than the for plate solving used range 10.5 to 14.5mag despite this most such cases showed a reasonable measurement result anyway. Specifications of the used telescope: -it27: 700mm CDK with 4531mm focal length. CCD: FLI PL09000. Resolution 0.53 arcsec/pixel. V-filter. No B-V transformation coefficients available. Located in Siding Spring, Australia. Elevation 1122m

Page 360 Jonckheere Double Star Photometry Part III: Lyra, Equuleus, and Eridanus (Continued from page 351) 3. Summary All result tables show, with some exceptions, quite large differences for the magnitudes compared with the WDS data often even in cases where double digit values suggest recent precise measurements. But it is obvious that the Jonckheere objects in more southern constellations have been visited rather often compared to the J-objects in the more northern constellations also with the effect of a far better data quality. A few cases suggest errors in position, separation, and position angle as the difference to the WDS data is larger than the given error estimation. In some cases the available equipment did not allow separate measurement due to heavily overlapping star disks. The measurement of the combined magnitude allowed an estimation of the components on the basis of the given m using the formula provided by Greaney 2012. Special cases: J131B in Lyr: No resolution, B probably fainter than +13mag J1206 in Lyr: WDS gives here for unknown reasons a position slightly different from the WDS ID. The measured position is a better match with the WDS ID (assumed to be the original position given by Jonckheere) and is also confirmed by an elongation in the 2MASS image J1208 in Lyr: Position error in WDS catalog by about 72 arcseconds. Measured position confirmed by UCAC4 catalog with 593-069152 and 593-069151 J2576 in Equ: No good match with the original Jonckheere 12/13 mag estimation. J2576 was not found at the given IDS position by Heintz according to his 1990 paper and the current precise WDS position seems to be given for a potential candidate with similar parameters for separation and position angle but at the cost of a rather bad match of the estimated magnitudes compared with the measured 14.45/14.15mag regarding not only delta_m but also position of the primary. Measurement results confirmed by UCAC4 catalog objects 503-140424 and 503-140426. Unfortunately the star field around the given position does not offer another better matching candidate so we can either take what we have or declare J2576 as lost Jonckheere object. Acknowledgements The following tools and resources have been used for this research: AAVSO APASS (via the UCAC4 catalog) AAVSO VPhot Aladin Sky Atlas v8.0 Astrometrica v4.8.2.405 AstroPlanner v2.2 itelescope it24 & it27 MaxIm DL6 v6.08 SIMBAD, VizieR, UCAC4, URAT1, GAIA UCAC4 catalog via the University of Heidelberg website and directly from USNO DVD Washington Double Star Catalog References Buchheim, Robert 2008, CCD Double-Star Measurements at Altimira Observatory in 2007, Journal of Double Star Observations, Vol. 4 No. 1 Page 28 Greaney, Michael 2012, "Some Useful Formulae" in R.W. Argyle, Observing and Measuring Visual Double Stars, 2nd Edition 2012, Chapter 25, Page 359 Heintz, W.D. 1990, Observations of double stars and new pairs. XIV. Astrophysical Journal Supplement Series Vol. 74, p. 275-290 Knapp, Wilfried; Nanson, John 2016, Jonckheere Double Star Photometry Part I: Cyg, Journal of Double Star Observing, Vol. 12 No 2 pp. nn-mm Knapp, Wilfried 2016, Jonckheere Double Star Photometry Part II: Del, Journal of Double Star Observing, Vol. 12 No 3 pp. nn-mm

Page 361 STT Doubles with Large ΔM Part IV: Ophiuchus and Hercules Wilfried R.A. Knapp Vienna, Austria wilfried.knapp@gmail.com John Nanson Star Splitters Double Star Blog Manzanita, Oregon jnanson@nehalemtel.net Abstract: The results of visual double star observing sessions suggested a pattern for STT doubles with large M of being harder to resolve than would be expected based on the WDS catalog data. It was felt this might be a problem with expectations on one hand, and on the other might be an indication of a need for new precise measurements, so we decided to take a closer look at a selected sample of STT doubles and do some research. We found that like in the other constellations covered so far (Gem, Leo, UMa, etc.) at least several of the selected objects in Ophiuchus and Hercules show parameters quite different from the current WDS data. 1. Introduction As follow up to our reports STT Doubles with Large delta_m Part I, II and III we continued in the constellations of Ophiuchus (Oph) and Hercules (Her), which contained 9 objects from our list (see Table 1) conveniently located with reasonable altitude at the time of observation. All values are from the WDS data as of the end of 2014. 2. Further Research Following the procedure for parts I, II, and III of our report we concluded again that the best approach would be to check historical data on all objects, observe them visually with the target of comparing with the existing data and obtain as many images as possible suitable for photometry. 2.1 Historical Research and Catalog Comparisons Of the nine stars in this survey, five of them have notable aspects worth further investigation. Three main research sources were used for this section of the paper, the first of which was W.J. Hussey s Micrometrical Observations of the Double Stars Discovered at Pulkovo, published in 1901, which provided preliminary historical information on each of the stars. Hussey s book includes his observations and measures of all the stars originally listed in Otto Wilhelm Struve s 1845 Pulko- Table 1. WDS 2014.96 values for the selected STT objects in Oph and Her Name Comp ID RA Dec Con Sep PA M1 M2 ΔM STT 326 AB 17183+0931 17:18:15.811 +09:31:03.899 Oph 17.9 223 8.10 12.40 4.30 STT 342 AB 18073+0934 18:07:21.019 +09:33:49.199 Oph 24.8 298 3.73 14.00 10.27 STT 310 AB 16254+3755 16:25:25.459 +37:54:36.796 Her 3.0 226 8.40 11.00 2.60 STT 314 AB 16389+2028 16:38:51.498 +20:27:57.599 Her 3.8 234 8.80 11.70 2.90 STT 317 AB 16530+4424 16:52:57.219 +44:24:08.000 Her 24.8 200 8.21 12.00 3.79 STT 324 AB 17080+3112 17:08:00.700 +31:12:22.497 Her 3.5 220 6.60 11.10 4.50 STT 328 AB 17173+3306 17:17:19.568 +33:06:00.406 Her 4.2 59 4.80 10.20 5.40 STT 338 AC 17520+1520 17:51:58.462 +15:19:34.899 Her 32.8 201 7.21 13.60 6.39 STT 585 BP 16450+0605 16:44:57.961 +06:02:37.099 Her 77.4 3 10.4 13.10 2.70

Page 362 STT Doubles with Large ΔM Part IV: Ophiuchus and Hercules vo Catalog, as well as data beginning with the date of first measure and continuing through the following years up to 1900. That data, plus inclusion of the background for the Pulkovo Catalog, makes Hussey s book a valuable source of reference. Also consulted was S.W. Burnham s A General Catalogue of Double Stars Within 121 of the North Pole, Part II, for information on STT 585. In addition, Bill Hartkopf of the USNO graciously supplied text files for STT 324, 326, 338, 342, and 585, as well as other information. STT 317 (Her) stood out immediately as a star worth further investigation because of the very noticeable changes in position angle and separation of the AB pair. According to Hussey s data (Hussey, 1910, p. 137), Johann Heinrich Mädler made the first measurements of STT 317 AB in 1843, which were 234.1 and 15.39". The most recent WDS data (dated 2013) at the time we made observations of STT 317 showed a position angle of 200 and a separation of 24.80". That considerable change in PA and separation is due to the two stars moving in opposite directions, which is shown in Figure 2. Also notable in the image is the high proper motion of the C component relative to A and B. However, there is less change between the first AC measures in 1874 (318.1 and 113.40") and the 2013 WDS measures (316 and 130.40") due to the two stars moving in similar directions. found almost all of the fourteen measures between 1867 and 2000 (Table 2) showed a position angle in the range of 219 to 221. The separations are more erratic, ranging from a high of 4.05" in 1869 by Dembowski to a low of 3.5" in 2000. Hussey (1901, p. 139) shows the first measures of STT 324 in 1848 were made by Otto Struve, and he also shows a follow-up measure of 218.5 and 3.87" by Struve in 1853 which is not listed in the WDS text file. So in general, it appears the position angle of this pair has been rather consistently in the 220 range, while the separation has fluctuated somewhat, averaging out to 3.79". Table 2. Data from WDS Text File for STT 324 Figure 1. Proper Motion of STT 317 Components STT 324 (Her) shows measurements changing from 213.6 and 3.8" in 1848 to 219.9 and 3.5" in 2000, the date of the most recent measures in the WDS. We requested the text file to see what changes had taken place in the 152 years between those two dates and STT 326 (Oph) stood out because of a consistent change in position angle and separation, which is a result of the two stars moving away from each other. The WDS proper motion numbers show the primary is moving east and south at a relatively slow rate of +027-020, while the secondary is moving west and south at similar rate, -015-021. When the 139 years of data of shown in the WDS is plotted, the consistent trend is very obvious, see Figure 2. STT 342 (Oph) has a strange history which began with Otto Struve s 1841 observation of a companion at an estimated distance of 1.5". He recorded eight additional observations (Figure 3) of what he identified as an eighth magnitude companion, several of which described it as suspect. (Hussey, 1901, pp. 144-45). (Continued on page 364)

Page 363 STT Doubles with Large ΔM Part IV: Ophiuchus and Hercules Figure 2. STT 326 Measures from WDS Text File Figure 3. Otto Struve's Observations of Close Companion of STT 342 (from Hussey, 1901, p. 145).

Page 364 STT Doubles with Large ΔM Part IV: Ophiuchus and Hercules (Continued from page 362) But as Hussey states, Struve also recorded another eight observations in which he failed to see the companion. Although other observers also reported measures between 1845 and 1884, no one reported the sighting of the companion when using large refractors, specifically the 26 inch at the USNO and the 36 inch at Lick. Hussey, S.W. Burnham, and R.G. Aitken each used the 36 inch Lick Refractor with no success during the period 1889 to 1898, which seems to have effectively decided the matter. Burnham credits Simon Newcomb with the first measure of the star now identified as B, which surprisingly didn t occur until 1890, perhaps because of all the attention focused on the spurious close companion. The star now identified as C was discovered by John Herschel in 1827, which he cataloged as H 5943. STT 585 (Her) is included here because of its anomalous numbering. When Otto Struve published his first Dorpat catalog in 1845, it ended at number 514. That catalog also was restricted to pairs with separations of 16 or less for companions fainter than ninth magnitude. All of the components of STT 585 are well over that limit, and all are fainter than tenth magnitude. The pairs wider than 16 of separation were added to Struve s appendix, which included a total of 254 stars. So STT 585 stands out as being peculiarly numbered, which is significant also because the first measures of it weren t made until 1854. Research in Burnham s 1906 General Catalog (Burnham, 1901, p. 725) shows STT 585 is referred to only as 41 Herculis, and a 1996 copy of the WDS shows the star and its components referred to only as STT, with no number attached. However, a look at a 2001 copy of the WDS found the system had been designated as STT 585. A request to Bill Hartkopf at the WDS for background on the numbering provided information that stars such as this, which were not numbered in the IDS catalog (the predecessor to the WDS), were later given designations by Brian Mason of the WDS. 2.2 Visual Observations Both Nanson and Knapp made visual observations of the stars included in this report. Nanson used a 152 mm f/10 refractor and a 235 mm SCT, while Knapp utilized 140 mm and 185 mm refractors and a 235 mm SCT, as well as a masking device to evaluate what could be seen at lesser apertures. STT 310 (Her): This was a difficult pair with a magnitude differential of 2.4 and a separation of 3 according to the WDS data. Nanson observed it at the meridian with a six inch f/10 refractor and detected a definite elongation at 380x, and had a brief glimpse of a dot of light at the correct PA. Given the difficulty, he estimated the secondary was slightly fainter than the WDS magnitude of 11.0. Knapp observed the secondary at 200x in a 140 mm refractor and could still see it when the aperture was reduced to 110 mm, suggesting a magnitude slightly brighter than 11.0. STT 314 (Her): Knapp observed this pair twice with a 185 mm refractor and resolved the secondary at 250x and 360x. He noticed a comparison star with a Vmag of 13.021 (UCAC4 553-056558) was a bit fainter than the secondary, but since he could still see the secondary with averted vision when the aperture was reduced to 130mm, he concluded the WDS magnitude of 11.7 was correct. Nanson used the same comparison star and concluded the secondary was just slightly brighter, but also felt the Vmag of 13.021 for the comparison star was too faint. He estimated the secondary to be of about 12.5 magnitude, which was in line with the difficulty he had in resolving it. STT 317 (Her): Nanson r esolved the B component at 109x and 152x in the six inch refractor, and concluded it was definitely fainter than the WDS magnitude of 12.0. It appeared to be slightly fainter than a 12.340 magnitude comparison star, suggesting the WDS magnitude is a bit too bright. Knapp resolved B in the 140 mm refractor with averted vision at a magnification of 280x, and could still detect it with the aperture reduced to 100 mm, which he concluded confirmed the WDS magnitude. STT 324 (Her): Knapp resolved the secondary in a 185 mm refractor at 100x and could still detect it at 180x with the aperture reduced to 170 mm. Comparison stars with Vmags of 11.635 and 11.812 appeared to be similar in brightness to the secondary, suggesting it s slightly fainter than the WDS magnitude of 11.1. Nanson attempted this pair twice with the six inch refractor, but seeing conditions were too poor each time to allow visual detection. STT 326 (Oph): Nanson observed this pair once with a 235 mm SCT and resolved the secondary at 136x. It appeared to be similar in magnitude to a comparison star with a Vmag of 12.660, suggesting the WDS magnitude of 12.4 for B is about right. Knapp observed STT 326 twice, catching a glimpse of it through a thin veil of clouds in the 140mm refractor at 180x, and during the next observation detected it at 40x in the 185 mm refractor, with confirmations at 100x, 180x, and 250x. He could still detect the secondary with averted vision when the aperture was reduced to 110mm, suggesting the secondary is brighter (about 11.8) than the WDS s 12.4. A comparison star with a Vmag of 13.477 seemed somewhat fainter than the secondary. STT 328 (Her): Knapp resolved the secondary

Page 365 STT Doubles with Large ΔM Part IV: Ophiuchus and Hercules at 140x and 200x in the 140 mm refractor, and could still detect it with the aperture reduced to 115 mm, which seems to confirm the WDS magnitude of 10.2. Nanson observed this pair twice with the six inch refractor, finding the secondary easier to resolve each time than would be expected for a pair with a M of 5.4 and a separation of 4.2". No comparison stars were available, but based on both his experience and Knapp s, it s possible that either the separation is wider than 4.2" or the magnitude of the secondary is brighter than the WDS s 10.2 STT 338 (Her): Using a 235 mm SCT at 196x Nanson found C was slightly fainter than a comparison star with a Vmag of 12.951, suggesting it may be a bit brighter than the WDS magnitude of 13.60. Knapp came to the same conclusion using a 185mm refractor at 180x, but found the limit aperture for resolution was 150 mm, which would seem to suggest a magnitude for C of 12.4. A second observation with the same refractor resulted in a limiting aperture of 160 mm, which still suggests C is brighter than the WDS s 13.60 magnitude. STT 342 (Oph): Knapp was unable to resolve B using 140 mm and 180 mm refractors. C was resolved with the 185 mm refractor at 180x, but was more difficult than expected based on the data. A comparison star with a Vmag of 11.934 was similar in brightness to C, suggesting the WDS magnitude for it of 11.48 is close. However, a limiting aperture for C of 130mm suggests C may be slightly fainter than 11.48. Nanson found B very difficult with a 235 mm SCT, but finally got a glimpse of it at 408x. Further attempts to see it failed, but based on the one observation, it s likely that B is a bit brighter than the 14.0 magnitude listed for it in the WDS. Using the same comparison star for C that Knapp used, he also found the two to be similar in magnitude. STT 585 (Her): Using a 235 mm SCT and two comparison stars, Nanson found P was obviously brighter than the WDS magnitude of 13.10, perhaps by as much as half a magnitude. Knapp observed P twice, resolving it at 100x in the 185mm refractor on the first observation. Based on a limiting aperture of 170 mm for P, he estimated its magnitude in the 12.5 to 12.6 range. A second observation with the 185 mm refractor resulted in a limiting aperture of 120 mm, again pointing toward P being brighter than the WDS s 13. 2.3 Photometry and Astrometry Results Several hundred images taken with itelescope remote telescopes were in a first step plate solved and stacked with AAVSO VPhot. The stacked images were then plate solved with Astrometrica with UCAC4 reference stars with Vmags in the range 10.5 to 14.5mag. The RA/Dec coordinates resulting from plate solving were used to calculate Sep and PA using the formula provided by R. Buchheim (2008). Photometry was also performed with Astrometrica based on the Vmags of the UCAC4 reference stars used for plate solving. The results are shown in Table 3. 3. Summary Tables 4 and 5 below compare the final results of our research with the WDS data that was current at the time we began working on the group of stars in Oph and Her. In Table 4 the results of our photometry have been averaged for each star. Because we re aware that both the NOMAD-1 and the UCAC4 catalogs are frequently consulted when making WDS evaluations of magnitudes changes, the data from those catalogs has also been included for each of the stars. Red type has been used in Tables 4 and 5 to call attention to significant differences from the WDS data. With regard to Table 4, those magnitudes that differ by two tenths of a magnitude or more from the WDS values have been highlighted. In Table 5 differences in separation in excess of two-tenths of an arc second are highlighted, as are all position angles which differ by more than a degree. Subsequent to our measures, as a quality check for our astrometry results we turned to the URAT1 catalog for the most recent precise professional measurements available. We used its coordinates to calculate the Sep and PA for all objects in this report for which URAT1 data was available and compared these values with our results, which are shown below in Table 6. With the exception of STT 585 BP, the Sep results are all within the given error range, so this comparison can be considered as confirmation for the reported results. In the case of STT 585 BP, a rather high rate of proper motion for B (GAIA shows a PM of -219-255) seems to be the cause of the discrepancy. We calculated a 0.3 shift in position of B between the 2013.735 URAT1 data and the 2015.497 date of our measure. With regard to the use of URAT1 as a quality check on our astrometry, we contacted Norbert Zacharias at the USNO, who was closely involved in the URAT1 project. He referred us to a paper on which he was lead author which contains this information: "URAT1 can serve as accurate reference star catalog before Gaia data become available. The position accuracy of URAT1 is about 4 times higher than for UCAC4 data at its faint end and the sky density of URAT1 is about 4 times larger than that of UCAC4, similar to the sky density of 2MASS." (Zacharias, 2015, p. 11). (Continued on page 373)

Page 366 STT Doubles with Large ΔM Part IV: Ophiuchus and Hercules Table 3: Photometry and astrometry results for the selected STT objects in Oph and Her. RA and Dec are the coordinates based on plate solving with UCAC4 reference stars in the 10.5 to 14.5mag range. Sep is separation calculated as SQRT (((RA2-RA1)*cos(Dec1))^2+(Dec2-Dec1)^2) in radians. Err_Sep is calculated as SQRT(dRA^2+dSep^2) with dra and ddec as average RA and Dec plate solving errors. PA is calculated as arctan((ra2-ra1)*cos(dec1))/(dec2-dec1)) in radians depending on quadrant and Err_PA is the error estimation for PA calculated as arctan(err_sep/sep) in degrees assuming the worst case that Err_Sep points in the right angle to the direction of the separation means perpendicular to the separation vector. Mag is the photometry result based on UCAC4 reference stars with Vmags between 10.5 and 14.5mag. Err_Mag is calculated as square root of (dvmag^2 + (2.5*Log10(1+1/SNR))^2) with dvmag as the average Vmag error over all used reference stars and SNR is the signal to noise ratio for the given star. Date is the Bessel epoch in 2015 and N is the number of images (usually with 1s exposure time) used for the reported values. it in the Notes column indicates the telescope used with number of images and exposure time given. The average results over all used images are given in the line below the individual stacks in red and bold. The error estimation over all used images is calculated as root mean square over the individual Err values. The N column in the summary line gives the total number of images used and Date the average Bessel epoch. STT 326 RA Dec Sep Err Sep PA Err PA Mag Err Mag Date 2015 N Notes A 17 18 15.842 09 31 03.51 18.038 0.233 223.934 0.741 8.036 0.120 519 5 it11 stack 5x1s B 17 18 14.996 09 30 50.52 12.190 0.127 A 17 18 15.863 09 31 03.35 18.143 0.234 224.004 0.740 7.979 0.110 B 17 18 15.011 09 30 50.30 12.034 0.113 A 17 18 15.844 09 31 03.33 18.170 0.234 224.182 0.739 7.934 0.110 B 17 18 14.988 09 30 50.30 11.983 0.114 A 17 18 15.845 09 31 03.49 18.029 0.163 223.766 0.517 8.013 0.060 B 17 18 15.002 09 30 50.47 12.088 0.064 A 17 18 15.849 09 31 03.52 18.099 0.156 223.814 0.492 7.999 0.090 B 17 18 15.002 09 30 50.46 12.039 0.093 A 17 18 15.853 09 31 03.53 18.187 0.276 223.419 0.869 8.074 0.151 B 17 18 15.008 09 30 50.32 12.143 0.155 A 17 18 15.848 09 31 03.57 18.077 0.198 223.880 0.629 7.993 0.080 B 17 18 15.001 09 30 50.54 12.071 0.085 A 17 18 15.849 09 31 03.471 18.106 0.217 223.857 0.688 8.004 0.107 B 17 18 15.001 09 30 50.416 12.078 0.111 478 2 it24 stack 2x1s 476 5 it24 stack 5x1s 511 5 it24 stack 5x1s_2 522 5 it24 stack 5x1s_3 516 5 it24 stack 5x1s_4 524 5 it24 stack 5x1s_5 507 32 Summary line STT342 RA Dec Sep Err Sep PA Err PA Mag Err Mag Date 2015 N Notes A 18 07 20.934 09 33 51.60 4.658 0.131 it24 stack 4x1s. 24.941 0.270 295.965 0.621 519 4 B 18 07 19.418 09 34 02.52 13.780 0.152 SNR for B <20 A 18 07 20.917 09 33 51.28 24.659 0.212 297.405 0.493 4.707 0.190 B 18 07 19.437 09 34 02.63 14.003 0.211 A 18 07 20.943 09 33 51.36 25.129 0.184 297.055 0.419 5.021 0.140 B 18 07 19.430 09 34 02.79 13.864 0.154 A 18 07 20.932 09 33 50.90 25.397 0.234 298.427 0.529 4.569 0.120 B 18 07 19.422 09 34 02.99 13.868 0.130 A 18 07 20.930 09 33 50.57 25.326 0.213 298.411 0.481 4.969 0.120 B 18 07 19.424 09 34 02.62 13.903 0.126 A 18 07 20.918 09 33 50.75 25.249 0.198 298.299 0.449 5.054 0.120 B 18 07 19.415 09 34 02.72 13.799 0.124 A 18 07 20.916 09 33 51.54 24.698 0.191 297.358 0.443 4.060 0.140 B 18 07 19.433 09 34 02.89 13.822 0.157 A 18 07 20.927 09 33 51.143 25.055 0.216 297.565 0.495 4.720 0.139 B 18 7 19.426 09 34 02.737 13.863 0.153 524 5 511 5 it24 stack 5x1s. SNR for B <20 it24 stack 5x1s_2. SNR for B <20 628 5 it24 stack 5x3s 628 5 it24 stack 5x6s 628 5 it24 stack 5x9s 522 6 566 35 it24 stack 6x1s. SNR for B <20 SNR for B in some images <20. A too bright for reliable photometry Table 3 continues on next page.

Page 367 STT Doubles with Large ΔM Part IV: Ophiuchus and Hercules Table 3 (continued). Photometry and astrometry results for the selected STT objects in Oph and Her. RA and Dec are the coordinates based on plate solving with UCAC4 reference stars in the 10.5 to 14.5mag range.... STT 310 RA Dec Sep Err Sep PA Err PA Mag Err Mag Date 2015 N Notes A 16 25 25.445 37 54 36.33 2.936 0.150 222.629 2.925 8.230 0.080 467 5 it24 stack 5x1s B 16 25 25.277 37 54 34.17 11.123 0.085 A 16 25 25.445 37 54 36.31 3.064 0.184 221.634 3.444 8.215 0.070 522 5 it24 stack 5x1s_2 B 16 25 25.273 37 54 34.02 11.081 0.074 A 16 25 25.446 37 54 36.22 3.432 0.184 222.257 3.066 8.209 0.080 516 5 it24 stack 5x1s_3 B 16 25 25.251 37 54 33.68 11.325 0.084 A 16 25 25.445 37 54 36.37 8.209 0.070 it24 stack 3.209 0.163 221.869 2.904 525 5 B 16 25 25.264 37 54 33.98 11.066 0.073 5x1s_4 A 16 25 25.445 37 54 36.307 8.216 0.075 Touching/ 3.160 0.171 222.094 3.095 507 20 overlapping star B 16 25 25.266 37 54 33.962 11.149 0.079 disks STT 314 RA Dec Sep Err Sep PA Err PA Mag Err Mag Date 2015 N Notes A 16 38 51.508 20 27 57.45 3.576 0.277 235.218 4.423 8.313 0.100 B 16 38 51.299 20 27 55.41 11.139 0.104 A 16 38 51.497 20 27 57.43 3.639 0.213 234.950 3.343 8.278 0.100 B 16 38 51.285 20 27 55.34 11.301 0.109 A 16 38 51.492 20 27 57.64 3.729 0.198 232.311 3.039 8.123 0.100 B 16 38 51.282 20 27 55.36 11.110 0.111 A 16 38 51.492 20 27 57.29 3.557 0.170 232.202 2.732 8.223 0.070 B 16 38 51.292 20 27 55.11 11.278 0.073 A 16 38 51.497 20 27 57.35 3.393 0.194 228.915 3.275 8.236 0.070 B 16 38 51.315 20 27 55.12 10.979 0.075 A 16 38 51.494 20 27 57.35 3.740 0.261 231.068 3.989 8.234 0.061 B 16 38 51.287 20 27 55.00 11.019 0.070 A 16 38 51.499 20 27 57.28 3.720 0.172 229.412 2.648 8.206 0.070 B 16 38 51.298 20 27 54.86 11.254 0.073 A 16 38 51.495 20 27 57.05 3.530 0.248 235.094 4.012 8.280 0.100 B 16 38 51.289 20 27 55.03 11.430 0.111 A 16 38 51.499 20 27 57.28 3.720 0.172 229.412 2.648 8.206 0.070 B 16 38 51.298 20 27 54.86 11.254 0.073 A 16 38 51.497 20 27 57.347 3.619 0.215 232.056 3.399 8.233 0.084 B 16 38 51.294 20 27 55.121 11.196 0.091 472 5 it11 stack 5x1s 521 5 it18 stack 5x1s 470 5 it21 stack 5x1s 473 5 it24 stack 5x1s 478 5 it24 stack 5x1s_2 476 5 it24 stack 5x1s_3 524 5 it24 stack 5x1s_4 516 5 it24 stack 5x1s_5 524 5 it24 stack 5x1s_6 495 45 Summary line Table 3 continues on next page.

Page 368 STT Doubles with Large ΔM Part IV: Ophiuchus and Hercules Table 3 (continued). Photometry and astrometry results for the selected STT objects in Oph and Her. RA and Dec are the coordinates based on plate solving with UCAC4 reference stars in the 10.5 to 14.5mag range.... STT 317 RA Dec Sep Err Sep PA Err PA Mag Err Mag Date N Notes A 16 52 57.208 44 24 09.33 24.713 0.355 199.744 0.823 7.900 0.070 530 4 it21 stack 4x1s. SNR B<20 B 16 52 56.429 44 23 46.07 12.677 0.103 A 16 52 57.196 44 24 09.67 24.808 0.141 200.349 0.327 8.030 0.070 476 3 it24 stack 3x1s B 16 52 56.391 44 23 46.41 12.517 0.078 A 16 52 57.187 44 24 09.81 24.852 0.178 200.154 0.410 7.757 0.060 467 5 it24 stack 5x1s B 16 52 56.388 44 23 46.48 12.471 0.068 A 16 52 57.189 44 24 09.83 24.925 0.164 200.276 0.377 7.822 0.050 473 5 it24 stack 5x1s_2 B 16 52 56.383 44 23 46.45 12.472 0.057 A 16 52 57.200 44 24 09.60 24.760 0.149 200.444 0.344 7.769 0.070 511 5 it24 stack 5x1s_3 B 16 52 56.393 44 23 46.40 12.499 0.076 A 16 52 57.195 44 24 09.60 24.713 0.163 200.485 0.377 7.850 0.060 522 5 it24 stack 5x1s_4 B 16 52 56.388 44 23 46.45 12.501 0.067 A 16 52 57.194 44 24 09.63 24.741 0.163 200.460 0.377 7.852 0.080 516 5 it24 stack 5x1s_5 B 16 52 56.387 44 23 46.45 12.484 0.087 A 16 52 57.196 44 24 09.639 24.787 0.200 200.273 0.462 7.854 0.066 499 32 Summary line B 16 52 56.394 44 23 46.387 12.517 0.078 STT 324 RA Dec Sep Err Sep PA Err PA Mag Err Mag Date N Notes it24 stack 5x1s. A 17 08 00.683 31 12 22.06 6.098 0.070 Overlapping star 2.974 0.191 218.411 3.676 473 5 disks. SNR for B 17 08 00.539 31 12 19.73 10.530 0.095 B<20 it24 stack A 17 08 00.682 31 12 22.08 6.039 0.070 5x1s_2. Overlapping star disks. 3.550 0.212 221.957 3.420 473 5 B 17 08 00.497 31 12 19.44 10.883 0.095 SNR for B<20 A 17 08 00.691 31 12 21.72 5.953 0.090 it24 stack 3.669 0.177 227.256 2.761 478 5 5x1s_3. Overlapping star disks B 17 08 00.481 31 12 19.23 10.657 0.102 A 17 08 00.678 31 12 21.98 5.820 0.090 it24 stack 3.676 0.205 219.173 3.195 476 5 5x1s_4. Overlapping star disks B 17 08 00.497 31 12 19.13 10.039 0.102 A 17 08 00.685 31 12 22.11 6.130 0.080 it24 stack 3.786 0.200 218.081 3.024 511 5 5x1s_5. Overlapping star disks B 17 08 00.503 31 12 19.13 11.197 0.094 A 17 08 00.670 31 12 22.41 5.801 0.120 it24 stack 3.084 0.212 205.639 3.935 516 5 5x1s_6. Overlapping star disks B 17 08 00.566 31 12 19.63 10.180 0.127 A 17 08 00.683 31 12 22.21 6.076 0.080 it24 stack 3.612 0.184 217.395 2.922 525 5 5x1s_7. Overlapping star disks B 17 08 00.512 31 12 19.34 10.980 0.090 A 17 08 00.683 31 12 22.21 6.085 0.080 it24 stack 4.196 0.184 218.366 2.516 525 5 5x1s_8. Overlapping star B 17 08 00.480 31 12 18.92 11.523 0.089 disks A 17 08 00.682 31 12 22.097 3.552 0.196 218.535 3.161 6.000 0.086 497 40 Summary line B 17 08 00.509 31 12 19.319 10.749 0.100 Table 3 continues on next page.

Page 369 STT Doubles with Large ΔM Part IV: Ophiuchus and Hercules Table 3 (continued). Photometry and astrometry results for the selected STT objects in Oph and Her. RA and Dec are the coordinates based on plate solving with UCAC4 reference stars in the 10.5 to 14.5mag range.... STF2127 RA Dec Sep Err Sep PA Err PA Mag Err Mag Date N Notes A 17 07 04.412 31 05 34.78 15.127 0.191 280.475 0.724 8.423 0.070 473 5 it24 stack 5x1s B 17 07 03.254 31 05 37.53 11.555 0.072 A 17 07 04.417 31 05 34.74 15.163 0.212 280.411 0.802 8.404 0.070 473 5 it24 stack 5x1s_2 B 17 07 03.256 31 05 37.48 11.569 0.072 A 17 07 04.424 31 05 34.47 15.301 0.177 281.574 0.662 8.356 0.090 478 5 it24 stack 5x1s_3 B 17 07 03.257 31 05 37.54 11.615 0.092 A 17 07 04.407 31 05 34.56 15.056 0.205 281.144 0.781 8.217 0.090 476 5 it24 stack 5x1s_4 B 17 07 03.257 31 05 37.47 11.669 0.094 A 17 07 04.420 31 05 34.81 15.213 0.200 280.376 0.753 8.453 0.080 511 5 it24 stack 5x1s_5 B 17 07 03.255 31 05 37.55 11.528 0.082 A 17 07 04.403 31 05 35.10 14.955 0.212 279.585 0.813 8.186 0.120 516 5 it24 stack 5x1s_6 B 17 07 03.255 31 05 37.59 11.521 0.122 A 17 07 04.409 31 05 34.86 15.148 0.184 280.113 0.697 8.424 0.080 525 5 it24 stack 5x1s_7 B 17 07 03.248 31 05 37.52 11.528 0.082 A 17 07 04.413 31 05 34.760 15.137 0.198 280.528 0.749 8.352 0.087 493 35 Summary line B 17 07 03.255 31 05 37.526 11.569 0.089 STT 328 RA Dec Sep Err Sep PA Err PA Mag Err Mag Date N Notes it24 stack 4x1s. A 17 17 19.563 33 06 00.05 4.808 0.070 Overlapping star 4.549 0.184 57.708 2.321 470 4 disks. SNR for B 17 17 19.869 33 06 02.48 10.328 0.112 B<20 it24 stack 5x1s. A 17 17 19.559 33 06 00.36 4.848 0.080 Overlapping star 4.694 0.219 61.082 2.675 473 5 disks, SNR for B 17 17 19.886 33 06 02.63 10.461 0.117 B<20 it24 stack A 17 17 19.565 33 06 00.38 4.837 0.080 5x1s_2. Overlapping star disks, 4.533 0.214 57.730 2.703 478 5 B 17 17 19.870 33 06 02.80 10.147 0.122 SNR for B<20 it24 stack A 17 17 19.556 33 06 00.46 4.096 0.080 5x1s_3. Overlapping star disks, 4.326 0.198 60.960 2.627 516 5 B 17 17 19.857 33 06 02.56 10.118 0.097 SNR for B<20 it24 stack A 17 17 19.563 33 06 00.42 4.810 0.080 5x1s_4. Overlapping star disks, 4.508 0.163 59.469 2.068 522 5 B 17 17 19.872 33 06 02.71 10.301 0.109 SNR for B<20 A 17 17 19.561 33 06 00.334 4.520 0.197 59.386 2.494 4.680 0.078 492 24 Summary line B 17 17 19.871 33 06 02.636 10.271 0.112 Table 3 continues on next page.

Page 370 STT Doubles with Large ΔM Part IV: Ophiuchus and Hercules Table 3 (continued). Photometry and astrometry results for the selected STT objects in Oph and Her. RA and Dec are the coordinates based on plate solving with UCAC4 reference stars in the 10.5 to 14.5mag range.... STT338 RA Dec Sep Err Sep PA Err PA Mag Err Mag Date N Notes AB 17 51 58.466 15 19 35.28 32.525 0.250 202.077 0.440 6.363 0.150 472 5 it11 stack 5x1s. SNR for B<20 C 17 51 57.621 15 19 05.14 13.239 0.169 AB 17 51 58.470 15 19 34.96 32.617 0.262 202.148 0.460 6.309 0.090 521 4 it18 stack 4x1s. SNR for C<10 C 17 51 57.620 15 19 04.75 13.157 0.143 AB 17 51 58.461 15 19 34.91 32.648 0.184 202.236 0.323 5.985 0.140 470 5 it21 stack 5x1s. SNR for C<20 C 17 51 57.607 15 19 04.69 13.033 0.167 AB 17 51 58.461 15 19 35.15 32.789 0.191 202.053 0.334 6.091 0.080 473 5 it24 stack 5x1s C 17 51 57.610 15 19 04.76 13.022 0.088 AB 17 51 58.453 15 19 35.22 32.649 0.227 201.961 0.398 6.062 0.080 467 5 it24 stack 5x1s_2 C 17 51 57.609 15 19 04.94 13.041 0.089 AB 17 51 58.451 15 19 35.02 32.270 0.226 202.094 0.402 6.005 0.080 478 5 it24 stack 5x1s_3 C 17 51 57.612 15 19 05.12 12.988 0.089 AB 17 51 58.458 15 19 35.24 32.660 0.191 202.008 0.335 6.215 0.070 511 5 it24 stack 5x1s_4 C 17 51 57.612 15 19 04.96 13.124 0.079 AB 17 51 58.449 15 19 35.30 32.885 0.226 201.388 0.394 6.101 0.090 516 5 it24 stack 5x1s_5 C 17 51 57.620 15 19 04.68 13.176 0.099 AB 17 51 58.448 15 19 35.34 32.726 0.212 202.015 0.371 6.073 0.080 522 5 it24 stack 5x1s_6 C 17 51 57.600 15 19 05.00 13.037 0.089 AB 17 51 58.457 15 19 35.158 32.641 0.220 201.997 0.387 6.134 0.099 492 44 Summary line C 17 51 57.612 15 19 04.893 13.091 0.117 STT338 RA Dec Sep Err Sep PA Err PA Mag Err Mag Date N Notes AB 17 51 58.466 15 19 35.28 96.303 0.250 246.786 0.149 6.363 0.150 472 5 it11 stack 5x1s D 17 51 52.348 15 18 57.32 11.834 0.154 AB 17 51 58.470 15 19 34.96 96.338 0.262 246.846 0.156 6.309 0.090 521 4 it18 stack 4x1s D 17 51 52.347 15 18 57.08 11.819 0.104 AB 17 51 58.461 15 19 34.91 96.291 0.184 246.847 0.109 5.985 0.140 530 5 it21 stack 5x1s D 17 51 52.341 15 18 57.05 11.110 0.148 AB 17 51 58.461 15 19 35.15 96.367 0.191 246.828 0.114 6.091 0.080 473 5 it24 stack 5x1s D 17 51 52.337 15 18 57.23 11.666 0.082 AB 17 51 58.453 15 19 35.22 96.288 0.227 246.762 0.135 6.062 0.080 467 5 it24 stack 5x1s_2 D 17 51 52.337 15 18 57.23 11.650 0.082 AB 17 51 58.451 15 19 35.02 96.251 0.226 246.837 0.135 6.005 0.080 478 5 it24 stack 5x1s_3 D 17 51 52.334 15 18 57.16 11.019 0.087 AB 17 51 58.458 15 19 35.24 96.328 0.191 246.773 0.114 6.215 0.070 511 5 it24 stack 5x1s_4 D 17 51 52.339 15 18 57.25 11.660 0.072 AB 17 51 58.449 15 19 35.30 96.131 0.226 246.631 0.135 6.101 0.090 516 5 it24 stack 5x1s_5 D 17 51 52.349 15 18 57.17 11.734 0.092 AB 17 51 58.448 15 19 35.34 96.329 0.212 246.728 0.126 6.073 0.080 522 5 it24 stack 5x1s_6 D 17 51 52.331 15 18 57.28 11.633 0.082 AB 17 51 58.457 15 19 35.158 96.292 0.220 246.782 0.131 6.134 0.099 499 44 Summary line D 17 51 52.34 15 18 57.197 11.569 0.104 Table 3 concludes on next page.

Page 371 STT Doubles with Large ΔM Part IV: Ophiuchus and Hercules Table 3 (conclusion). Photometry and astrometry results for the selected STT objects in Oph and Her. RA and Dec are the coordinates based on plate solving with UCAC4 reference stars in the 10.5 to 14.5mag range.... STT 585 RA Dec Sep Err Sep PA Err PA Mag Err Mag Date N Notes B 16 44 57.753 06 02 33.08 89.669 0.255 5.202 0.163 10.369 0.092 472 5 it11 stack 5x1s. SNR for P<20 P 16 44 58.298 06 04 02.38 12.940 0.113 B 16 44 57.734 06 02 33.16 89.754 0.228 5.092 0.146 10.321 0.113 515 2 it18 stack 5x1s. SNR for P<10 P 16 44 58.268 06 04 02.56 13.125 0.169 B 16 44 57.726 06 02 33.22 89.801 0.333 5.414 0.212 9.887 0.161 515 9 it21 stack 5x1s. SNR for P<20 P 16 44 58.294 06 04 02.62 12.544 0.174 B 16 44 57.733 06 02 33.14 89.624 0.177 10.272 0.160 5.233 0.113 473 5 it24 stack 5x1s P 16 44 58.281 06 04 02.39 12.742 0.163 B 16 44 57.731 06 02 33.19 89.640 0.205 5.280 0.131 10.259 0.081 467 5 it24 stack 5x1s_2 P 16 44 58.284 06 04 02.45 12.783 0.086 B 16 44 57.735 06 02 33.24 89.565 0.177 5.246 0.113 10.263 0.071 476 5 it24 stack 5x1s_3 P 16 44 58.284 06 04 02.43 12.749 0.081 B 16 44 57.733 06 02 33.11 89.666 0.205 5.250 0.131 10.275 0.071 511 5 it24 stack 5x1s_4 P 16 44 58.283 06 04 02.40 12.763 0.076 B 16 44 57.741 06 02 32.98 89.615 0.248 5.243 0.159 10.326 0.121 516 5 it24 stack 5x1s_5 P 16 44 58.290 06 04 02.22 12.876 0.126 B 16 44 57.736 06 02 33.10 89.929 0.227 5.263 0.144 10.303 0.120 524 5 it24 stack 5x1s_6 P 16 44 58.289 06 04 02.65 12.838 0.125 B 16 44 57.736 06 02 33.136 89.696 0.233 10.253 0.115 5.247 0.149 497 46 Summary line P 16 44 58.286 06 04 02.456 12.818 0.129 Specifications of the used telescopes: it11: 510mm CDK with 2280mm focal length. CCD: FLI ProLine PL11002M. Resolution 0.81 arcsec/pixel. B- and V- Filter. Transformation coefficients B-V available. Located in Mayhill, New Mexico. Elevation 2225m it18: 318mm CDK with 2541mm focal length. CCD: SBIG-STXL-6303E. Resolution 0.73 arcsec/pixel. V-filter. No transformation coefficients available. Located in Nerpio, Spain. Elevation 1650m it21: 431mm CDK with 1940mm focal length. CCD: FLI-PL6303E. Resolution 0.96 arcsec/pixel. V-filter. Transformation coefficients V-R available, but not used. Located in Mayhill, New Mexico. Elevation 2225m it24: 610mm CDK with 3962mm focal length. CCD: FLI-PL09000. Resolution 0.62 arcsec/pixel. V-filter. No transformation coefficients available. Located in Auberry, California. Elevation 1405m

Page 372 STT Doubles with Large ΔM Part IV: Ophiuchus and Hercules WDS Mag NOMAD-1 VMag Table 4. Photometry and Visual Results Compared to WDS UCAC4 VMa UCAC4 f. mag Average of Photometry Measures STT 326 B 12.40 12.060-12.307 12.078 STT 342 B 14.00 - - 13.711 13.863 STT 310 B 11.00 - - - 11.149 STT 314 B 11.70 - - - 11.196 STT 317 B 12.00 12.220-12.475 12.517 STT 324 B 11.10 - - - 10.749 Results of Visual Observations Three observations: one concluded B was slightly brighter, one that it was close to the WDS value, and one that it was fainter. One observation of B found it was slightly brighter than the WDS value. Two observations: one found B slightly brighter, one estimated it to be slightly fainter than the WDS value. Two observations: one found the WDS magnitude to be about right, one estimated B at 12.5. Two observations: one found the WDS magnitude to be about right, the other concluded B was a bit fainter than the WDS value. One observation suggested B was slightly fainter than the WDS magnitude. STF 2127 B 12.30 11.030-11.342 11.569 No visual observations made. STT 328 B 10.20 - - - 10.271 STT 338 C 13.60 13.80-12.746 13.091 One observation tended to confirm the WDS magnitude; the other felt B was either brighter than the WDS magnitude or the separation was slightly wider than the WDS value. Three observations indicated C was brighter than the WDS value. STT 338 D 10.60 11.950 11.671 11.289 11.569 No visual estimates made. STT 585 P 13.10 11.960 12.799 12.812 12.818 Three observations, all indicating P was brighter than the WDS magnitude. STT 326 AB STT 342 AB STT 310 AB STT 314 AB STT 317 AB STT 324 AB STF 2127 AB STT 328 AB STT 338 AB-C STT 338 AB-D STT 585 BP** WDS Coordinates WDS Sep 17 18 15.81 +09 31 03.9 18 07 21.02 +09 33 49.2 16 25 25.46 +37 54 36.8 16 38 51.50 +20 27 57.6 16 52 57.22 +44 24 08.0 17 08 00.70 +31 12 22.5 17 07 04.42 +31 05 35.1 17 17 19.57 +33 06 00.4 17 51 58.46 +15 19 34.9 17 51 58.46 +15 19 34.9 16 44 57.96 +06 02 37.1 Table 5. Astrometry Results Compared to WDS WDS PA 17.90" 223 24.90" 298 3.00" 226 3.80" 234 24.80" 200 3.50" 220 14.80" 276 4.20" 59 32.80" 201 95.60" 247 85.90" 3 Astrometry Coordinates 17 18 15.849 +09 31 03.471 18 07 20.927 +09 33 51.143 16 25 25.445 +37 54 36.307 16 38 51.497 +20 27 57.347 16 52 57.196 +44 24 09.639 17 08 00.682 +31 12 22.097 17 07 04.413 +31 05 34.760 17 17 19.561 +33 06 00.334 17 51 58.457 +15 19 35.158 17 51 58.457 +15 19 35.158 16 44 57.736 +06 02 33.136 Astrometry Sep Astrometry PA 18.106" 223.857 25.055" 297.565 3.160" 222.094 3.619" 232.056 24.787" 200.273 3.552" 218.535 15.137" 280.528 4.520" 59.386 32.641" 201.997 96.292" 246.782 89.696" 5.247 ** At the time we first pulled data from the WDS for STT 585 BP, it listed the 2001 (most recent) separation as 77.40. However, a look at the text file for that pair of stars showed a separation of 85.858 for the 2001 measure. That error is now corrected in the current WDS listing of STT 585 BP.

Page 373 STT Doubles with Large ΔM Part IV: Ophiuchus and Hercules Object URAT1 Sep Table 6. Astrometry Results Compared with URAT1 Coordinates itelescope Sep Err Sep Within Error Range? URAT1 PA itelescope PA Err PA Within Error Range? STT 326 AB 18.031" 18.106" 0.217 Yes 223.648 223.857 0.688 Yes STT 342 AB 25.040" 25.055" 0.216 Yes 297.562 297.565 0.495 Yes STT 317 AB 24.710" 24.787" 0.200 Yes 200.574 200.273 0.462 Yes STF 2127 AB 15.219" 15.137" 0.198 Yes 280.579 280.528 0.749 Yes STT 338 AB-C 32.588" 32.641" 0.220 Yes 202.149 201.997 0.387 Yes STT 338 AB-D 96.349" 96.292 0.220 Yes 246.862 246.782 0.131 Yes STT 585 BP 89.254" 89.696 0.233 No 5.033 5.247 0.149 No (Continued from page 365) References Buchheim, Robert 2008, CCD Double-Star Measurements at Altimira Observatory in 2007, Journal of Double Star Observations, Vol. 4 No. 1 Page 28 Burnham, S.W. 1906, A General Catalogue of Double Stars Within 120 of the North Pole, Part II. University of Chicago Press, Chicago Greaney, Michael 2012, "Some Useful Formulae" in R.W. Argyle, Observing and Measuring Visual Double Stars, 2nd Edition 2012, Chapter 25, Page 359 Hussey, W.J. 1901, Micrometrical Observations of the Double Stars Discovered at Pulkowa Made with the Thirty-Six-Inch and Twelve-Inch Refractors of Lick Observatory, pp. 14-16. A.J. Johnston, Sacramento Knapp, Wilfried; Nanson, John; Smith, Steven 2015, STT Doubles with Large Delta_M Part I: Gem, Journal of Double Star Observing, Vol. 11 No. 4 pp. 390-401. Knapp, Wilfried; Nanson, John; Smith, Steven 2016, STT Doubles with Large Delta_M Part II: Leo and UMa, Journal of Double Star Observing, Vol. 12 No 2 pp. 110-126. Knapp, Wilfried; Nanson, John 2015, STT Doubles with Large Delta_M Part III: Vir, Ser, CrB, Com and Boo, Journal of Double Star Observing, Vol. 12 No 2 pp. 127-141. Zacharias, Norbert, et al 2015, The First U.S. Naval Observatory Robotic Astrometric Telescope Catalog (URAT1), The Astronomical Journal, Vol 150, Issue 4 (August 19, 2015), pp. 1-12. Acknowledgements Our thanks to Bill Hartkopf at the USNO/WDS for his enthusiastic aid and advice. The following tools and resources have been used for this research: Washington Double Star Catalog itelescope AAVSO VPhot AAVSO APASS UCAC4 catalog via the University of Heidelberg website and directly from USNO DVD Aladin Sky Atlas v8.0 SIMBAD, VizieR 2MASS All Sky Catalog URAT1 Survey AstroPlanner v2.2 MaxIm DL6 v6.08 Astrometrica v4.8.2.405

Page 374 Measurements with Reticle Micrometer Performed by a New Double Stars Observing Group from Poland Marcin Biskupski, Natalia Banacka, Justyna Cupryjak, Małgorzata Malinowska, Kamil Bujel, Zdzisław Kołtek, Jarosław Mazur, Marcin Muskała, Łukasz Płotkowski, Barłomiej Prowans, and Paweł Szkaplewicz Polish Astronomy Amateur Association Szczecin Divison, Poland Email: marcin.biskupski@ptma.szczecin.pl Abstract: Measurements of 19 double stars using a reticle micrometer eyepiece are reported. The observational program was held in spring and summer of 2015 as an extended workshop for a new double stars observing group from Szczecin, Poland. The goal of the program was to learn how to measure position angle and separation using a reticle micrometer eyepiece. Introduction A new group of double stars observers has been informally founded as a part of the Polish Astronomy Amateur Association, division Szczecin. None of the observers had previous experience in double star astronomy, so it was clearly an educational program to learn how to use a reticle micrometer eyepiece and to spark an interest in double stars in general. The purpose was also to learn the basics before taking the next steps in the vast field of double star astronomy. The program was based on the observing list generated by Brian Mason from the USNO, previously requested by the first author. The list contained 54 stars with the following specifications: RA: from 13h to 18h DEC: from 15 o to 60 o Magnitudes: > 10 mag, no lower limit Separation: from 10'' to 80'' Last observation: 2005 The limits were mainly determined by the observatory location close to the city center where the measurements were carried out. The telescope used was the Zeiss Coude-Refractor 150/2250 from the year 1980. Method Calibration was performed via the drift method and led to value 9.253 for one division at the linear scale of the Celestron Micrometer Eyepiece. Measurements were carried out in two to five person groups at the time, with an exception of 1 night when only 1 person ran observations. Each person's position angle and separation results were noted and averaged. Ten out of 20 observed stars was measured during two or more nights. In those cases Bessellian dates were averaged. For each system, the measurement errors were calculated as a standard deviation of all results. Results Nineteen double stars were measured from May to September 2015, giving a total of 245 single observations. The vast spread of errors is due to a few factors like poor telescope drive and lack of experience for the program participants. Table 1 gives the measurements and uncertainties. Acknowledgements Special thanks to people who made this program possible - Bob Argyle and Bruce MacEvoy for basic knowledge and patiently showing directions, also Brian Mason for great help with the observing list. The authors are all amateur astronomers with a special interest in double stars and photometry. All participants of the described program are members of the Astronomy Amateur Association, Szczecin Division.

Page 375 Measurements with Reticle Micrometer Performed by a New Double Stars Observing Group from Poland Table 1. Measurements of the Double Stars disc wds mags PA err SEP err date HZG 8AC 11045+3814 6.04, 7.56 83.75 0.76 150.64 0.77 2015.368 HJL1062 11202+1707 7.92, 9.13 187 0 103.63 0 2015.390 HJL1065AC 11390+4109 8.11, 9.18 3.63 0.29 132.32 2.37 2015.553 ARG 101 11512+3322 6.27, 9.28 273.75 0.5 46.08 0.77 2015.390 STTA112AB 11545+1925 8.28, 8.49 36.75 0.35 73.79 0.33 2015.384 STFA 25AC 13135+6717 6.64, 8.89 223.38 0.18 105.02 1.31 2015.550 HJ 1231AC 13253+4028 8.67, 8.85 233.25 1.06 92.53 0 2015.550 STF1831AC 14161+5643 7.16, 6.73 221.69 0.74 112.19 0.33 2015.381 STF1830CE 14161+5643 6.73, 9.33 246.67 0.58 139.03 0.89 2015.384 ARY 42 15174+3022 9.3, 9.63 188.33 0.58 92.76 1.58 2015.409 STTA138BC 15201+6023 7.76, 9.28 48.81 0.49 91.6 0.59 2015.550 BAR 41CD 15520+4238 7.8, 9.7 51.5 0.58 66.62 0.76 2015.409 ARY 12 15599+6914 8.9, 8.95 248.38 0.48 124.22 0.89 2015.384 STFA 30BC 16362+5255 6.42, 5.5 16.86 0.43 91.47 0.4 2015.396 BU 953AB,D 16366+6948 8.04, 8.03 46.39 0.47 147.96 1.05 2015.507 POP1222AD 16448+3544 9.37, 8.91 7 0.61 158.5 0.41 2015.444 STTA151AB 17039+5314 7.93, 9.34 171.4 0.67 88.42 1 2015.537 S 689AB 17246+3913 7.48, 8.44 198.15 0.84 91.19 0.58 2015.529 STTA157AB 17407+3117 6.43, 7.92 106.2 0.69 118.28 0.83 2015.537

Page 376 CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs:The Autumn 2015 Observing Program at Brilliant Sky Observatory, Part 1 Richard W. Harshaw Brilliant Sky Observatory, Cave Creek, AZ Rharshaw2@cox.net Abstract: A set of 66 stars with known rectilinear solutions was observed with a CCD camera at f/30 22 known rectilinear pairs, 18 strongly linear pairs and 26 possible linear pairs. Data reduction showed that all but one of the 22 rectilinear measurements fell within the estimated positions of the ephemerides as reported in the Fourth Catalog of Rectilinear Elements. The lone exception was only 0.040 arc seconds off the predicted value of rho. The other 44 cases show varying degrees of linearity, some probably being at the point of deriving a rectilinear solution. The Observing Program From October 23 to December 1, 2015, a vigorous program of measuring double stars with a Skyris 618C CCD camera was done at Brilliant Sky Observatory (Cave Creek, Arizona). Over 18 different nights, over 220 double stars were imaged and their FITS cubes reduced using Plate Solve 3.47B. In this report, I describe the measurements of 66 pairs that are known rectilinear systems or showing signs of being such. These stars were chosen for two reasons: (1) to check the accuracy of my measurements, and (b) to add data to the validation (or correction) of the ephemerides in the Fourth Catalog of Rectilinear Elements (Hartkopf, Mason, October 2015). Equipment Used Brilliant Sky Observatory (so-named for the street on which it is located) is a roll-off roof structure that houses a Celestron C-11 SCT telescope mounted on a Celestron CGEM-DX GoTo mount controlled by a laptop using TheSky 6.0. To keep the focal length as consistent as possible, a JMI digital motorized focus control moves the primary mirror in extremely tiny increments to bring star images to a sharp focus. The difference in the readout spans about 20 counts between winter and summer (due to thermal expansion and contraction of the entire optical train). Since a complete turn of the focus knob causes a change of 100 counts on the JMI digital readout, this corresponds to a mirror shift of approximately 0.16 mm, an insignificant effect on the system s overall focal length, which in turn assures that the camera pixel scale remains constant for each observing session at a given focal ratio. The camera was calibrated as described in Harshaw (2015). The Skyris 618C, being a color camera, is run in black and white mode using FireCapture software. FITS frames are sent to a 2 TB external USB hard drive and later compiled into FITS cubes and reduced with Plate Solve 3.47B software. Plate Solve 3.47B was written by David Rowe of PlaneWave Instruments. Mr. Rowe is an ardent supporter of astronomers doing speckle interferometry and high-resolution CCD imaging of double stars. Plate Solve 3.47B has a number of powerful features and is still in development and not yet ready for general release. The observer can calibrate the camera s angle (orientation with respect to celestial north) with drift files of a bright stars. By capturing drift files of a reference star (a bright star where one can use camera integration times of 20ms or less, thus generating a large number of frames for the short transit across the camera s chip), Plate Solve can compute the RMS line-ofbest-fit of the star s image and then accurately determine celestial north (to within a tenth of a degree). I run ten drift files per observing run to drive down the standard errors to an acceptable level. Plate Solve also can use the same data in the drift file to compute the camera s pixel scale, but I find that it takes many dozens of drifts to drive the standard error down to an acceptable level. This new feature is a great addition and makes the grating calibration method described by the author (Harshaw, 2015) and Cotterell (2015) unnecessary, thus saving an observer the expense of making a grating and procuring an H Alpha filter.

Page 377 CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs... Figure 1. Unprocessed autocorrelogram of SMA 30. In addition to that, Plate Solve can also compile the FITS images made at the telescope into FITS cubes, and then pre-process those cubes to reduce file size and greatly reduce processing time during reduction. Procedure For CCD measures, I find that taking 100 frames and then selecting the best 25% for signal to noise ratio yields 25 frames that Plate Solve can work with very nicely. I find that as a general rule, Plate Solve gives more accurate solutions than lucky imaging. When measuring the autocorrelograms with Plate Solve, I take advantage of the fact that an autocorrelogram produces an image with axial symmetry. The autocorrelogram is not technically an image of the pair, but is instead a graphical representation of the pair s power spectrum, a process covered in detail in the Plate Solve User s Guide (Rowe, Genet, 2013; PDF copy available upon request). As such, one of the images of the companion star will be the true one (at the proper value of theta and rho) while the other will be its mirror image (same rho, 180 complement of theta). I always measure both companion images when doing reduction. In a high-quality FITS cube, both measurements will be identical, of course (with the exception of the quadrant flip for the complementary image); in cubes of lesser quality, there may be very small differences in the two measurements. These are reported in the tables as two measurements, although only one FITS cube is being analyzed. Figure 1 shows a noisy image the integration time had to be run up to 1.05 seconds due to the faintness of Figure 2: SMA 30 after enhancement using Plate Solve 3.47B s tools. the stars (10.03 and 10.44 magnitudes respectively). Figure 2 shows the same image after processing to remove noise. Note the small pink circle Plate Solve drew on the companion image at the 7 0 clock position. This indicates that Plate Solve thinks this is the companion star to be measured. (As it turns out in this case, this is in fact the location of the companion, the image at 1 o clock being the complement produced by the symmetric solution of the Fourier transform.) Plate Solve has a tool that allows the user to remove the pink circle and manually select the other image to perform a measurement of the complement (or, in many cases, the actual companion as Plate Solve does not always correctly select the companion star since it does not have the measurement history available to it). The largeness of the stars images is an indication of the usually poor seeing in Arizona. (Most nights while collecting data, the stars were forming images approximately 2 arc seconds across. Such is the price one pays for strong thermals rising off the desert floor. But the dry air also makes for exceptional transparency, which is why Arizona figures so prominently as the Continental United States premier observing location for deep sky objects.) Since fainter stars require longer integration times (or shutter speeds ) in the camera, the roiling of the atmosphere produces a smudged out image. Results Part 1: 22 Rectilinear Pairs Observed In Table 1, I present the results of the measures of 22 pairs with known rectilinear solutions. In this table,

Page 378 CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs... Table 1: Measures on 22 Rectilinear Pairs WDS Number Disc Comp Date Last Last Last Year Meas. Made Meas Meas Resid Resid Note 00032+4508 HJ 1927 2015.836 72.8 9.83 2011 4 73.362 9.524-0.562 0.306 00033+6053 HJ 1928 AB 2015.858 183.6 15.34 2010 2 183.096 15.231 0.504 0.109 00047+3416 STF3056 AB, C 2015.915 3.0 26.04 2012 6 3.859 26.034-0.859 0.002 1 00047+3416 STF3056 AB, C 2015.836 3.0 26.04 2012 6 3.303 26.060-0.303-0.024 00272+4959 STF 30 AB 2015.849 314.2 13.20 2014 6 314.361 13.430-0.161-0.230 2 00305+2208 HJ 1027 2015.852 217.0 18.21 2010 2 217.809 18.458-0.809-0.248 00384+4059 STF 44 2015.852 273.9 12.72 2012 2 274.069 12.815-0.169-0.095 00413+5240 AG 299 2015.855 69.0 29.86 2010 2 68.882 30.410 0.118-0.550 00444+7713 STF 50 2015.863 95.7 22.10 2007 4 96.621 22.489-0.921-0.385 3 00504+5038 BU 232 AB, C 2015.901 299.2 24.53 2010 6 299.991 24.444-0.791 0.086 4 00584+5426 HJ 2003 2015.910 332.4 17.00 2010 6 332.145 16.843 0.255 0.157 00595+8341 STF 69 2015.855 32.5 28.59 2010 2 33.101 28.815-0.601-0.225 01207+4620 STF 112 AB 2015.852 336.5 19.17 2011 2 336.789 18.990-0.289 0.180 5 01268+4908 ARG 50 2015.910 137.3 15.48 2010 6 135.768 15.182 1.532 0.298 01276+6429 STF 121 AB 2015.877 268.0 12.00 2012 6 267.824 12.001 0.176-0.001 01352+8321 STF 118 2015.855 93.8 15.33 2010 2 93.741 15.522 0.059-0.192 01374+5838 STT 33 AB 2015.855 77.5 26.64 2011 6 77.081 26.861 0.419-0.221 6 01383+7235 HJ 2053 2015.904 36.3 33.03 2010 6 36.621 32.871-0.321 0.159 7 01395+3216 SEI 19 2015.910 347.6 18.86 2011 6 348.405 18.698-0.805 0.162 01459+7142 HJ 1089 AB 2015.904 89.2 26.34 2012 6 89.340 26.234-0.140 0.106 01581+4123 S 404 AB 2015.882 82.7 28.90 2012 10 84.367 29.247-1.667-0.347 8 02407+6117 STF 284 AB 2015.904 190.4 6.82 2011 6 189.953 6.903 0.447-0.083 9 Notes: 1. The parallax for A is given as 5.64 mas (±1.42), while B shows 34.52 mas (±30.8). Clearly the parallax for B is meaningless. The uncertainty in the parallax of A (25.18%) makes it a poor guide to the star s actual distance, but the star could be 177 parsecs away. If at that distance, the minimum mean distance between the two stars would be 2,307 AU. 2. The parallaxes of this system are close (4.03 mas ±1.13 for A, 3.92 mas ±2.69 for B), yet the error estimates make these values virtually unusable as true distance indicators. Having said that, there is a likely chance that the two could be bound as both have a projected mean distance of 248 pc (A) or 255 pc (B). In either case, the minimum mean separation at present would be between 1,665 AU and 1,712 AU. 3. The parallax of A is known, and is 167.98 mas ±0.48. This implies a distance of 6 pc with a probable minimum mean separation of the two stars at present of 67 AU. 4. Curious parallax case. A has a parallax of 9.89 mas ±2.19, while B s is negative and hence unusable. If the system is at the distance indicated by A, the two stars can be no closer at present than 1,235 AU. 5. The parallaxes in this case are unusable. The primary is shown to have a parallax of 10.01 mas ±3.60 (a 36% uncertainty, hence not reliable as a distance indicator), while B s parallax has an error estimate three times its value! If the system is truly at the distance suggested by A s parallax (100 pc), the minimum separation of the two stars at present is 948 AU. 6. Although this pair has a rectilinear solution, the parallaxes leave open the possibility they are physical. The given parallaxes are 15.60 mas ±0.96 and 16.52 mas ±0.72, suggesting the pair lies somewhere between 61 and 64 pc away. At this distance, the minimum separation at present would be between 813 and 861 AU. 7. This pair shows only a parallax for the primary (3.54 mas ±0.74). The uncertainty of 21% puts this pair just off the uncertainty cutoff of 20%, but is close enough to let us conjecture the pair, if physical, could be 282 pc away with the stars lying some 4,641 AU apart. 8. A case of vastly different parallaxes, the primary showing 31.99 mas ±0.86, with the companion showing 15.02 mas ±6.12. Tossing out the companion s value as too uncertain, a solution using the primary s value suggests a distance of 31 pc with a minimum separation of 457 AU. Given the fact that there is a very low probability that the parallaxes could actually have any overlap, and the system is almost certainly optical. 9. Only the primary has a parallax (-3.67 mas ± 1.94), so no safe conclusions about distance or separation can be drawn.

Page 379 CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs... Last and Last are the last measures of and on record, the year of that measurement being given in the Last Year column. Meas. Made indicates how many measurements of that system I made (bearing in mind that I measured both the actual companion and its complementary image). Meas and Meas are the values I obtained from my measurements, being the means of all the measurements. Resid and Resid are residuals of the 2015 measurements compared to the last measure on record. The Note flag refers to notes that appear at the end of Table 1. Table 2 presents the ephemerides and residuals for these 22 pairs based on the values for and predicted in the Fourth Catalog of Rectilinear Elements. The mean of all the residuals for these 22 pairs was -0.099 for and +0.044 arc sec for. It is noteworthy that every pair measured yielded and values that fell well within the uncertainty bars for each pair except for WDS 01489+7142 (HJ 1089), where the value of fell just outside the upper limit from the ephemerides (0.040" over the limit). Measures of Likely Linear Pairs Analysis of the Measurement History With Excel Microsoft s Excel spreadsheet program has a useful tool for working with the Cartesian plots of a pair s historical measurements. After plotting the data for a given pair, the mouse may be right-clicked on any data point which brings up a menu that has, among other options, the ability to insert a trend line. Selecting that option and asking for a linear trend helps identify data that may be emerging as a rectilinear case. It is possible to ask Excel to display the R 2 value (the RMS value of the line of best fit). A value of 1.00 indicates a perfect fit of all the data points to a line; a value of 0.00 indicates no pattern whatsoever exists. Values between 0.00 and 1.00 suggest varying degrees of the fit of the data to a straight line. In my data plots, I sort linear cases into one of five classes, depending on the R 2 value. Graphs with an R 2 value of 0.80 and up are assigned to Class 1 (very strong linear tendency). Values between 0.60 and 0.79 are assigned Class 2; values between 0.40 and 0.59 Class 3; 0.20 to 0.39, Class 4; and all others Class 5. However, it must be noted that Excel s linear trend line function is a non-weighted function. All data points Table 2: Ephemerides and Residuals for the Rectilinear Pairs WDS Number Disc Comp Meas Meas 2015 Err 2015 Err Resid Resid 00032+4508 HJ 1927 73.362 9.524 72.7 3.7 9.713 0.436-0.662 0.189 00033+6053 HJ 1928 AB 183.096 15.231 183.2 1.8 15.700 2.174 0.104 0.469 00047+3416 STF3056 AB, C 3.859 26.034 3.1 2.5 25.982 1.120-0.759-0.052 00047+3416 STF3056 AB, C 3.303 26.060 3.1 2.5 25.982 1.120-0.203-0.078 00272+4959 STF 30 AB 314.361 13.430 314.6 1.4 13.370 0.322 0.239-0.060 00305+2208 HJ 1027 217.809 18.458 217.8 3.0 19.083 0.967-0.009 0.625 00384+4059 STF 44 274.069 12.815 273.9 0.9 12.719 0.490-0.169-0.096 00413+5240 AG 299 68.882 30.410 68.6 1.3 30.389 0.656-0.282-0.021 00444+7713 STF 50 96.621 22.489 96.2 3.2 22.339 0.736-0.421-0.150 00504+5038 BU 232 AB, C 299.991 24.444 298.9 3.7 24.610 1.633-1.091 0.166 00584+5426 HJ 2003 332.145 16.843 331.8 1.5 17.071 0.346-0.345 0.228 00595+8341 STF 69 33.101 28.815 32.7 0.6 28.858 0.322-0.401 0.043 01207+4620 STF 112 AB 336.789 18.990 336.5 3.6 18.987 1.556-0.289-0.003 01268+4908 ARG 50 135.768 15.182 136.3 1.5 15.648 0.401 0.532 0.466 01276+6429 STF 121 AB 267.824 12.001 267.7 4.1 11.946 1.112-0.124-0.055 01352+8321 STF 118 93.741 15.522 93.9 1.7 15.493 0.472 0.159-0.029 01374+5838 STT 33 AB 77.081 26.861 77.3 9.5 26.922 4.217 0.219 0.061 01383+7235 HJ 2053 36.621 32.871 36.2 0.5 32.984 0.286-0.421 0.113 01395+3216 SEI 19 348.405 18.698 347.7 1.2 18.735 0.597-0.705 0.037 01459+7142 HJ 1089 AB 89.340 26.234 89.0 0.3 26.568 0.141-0.340 0.334 01581+4123 S 404 AB 84.367 29.247 83.9 1.7 29.008 1.315-0.467-0.239 02407+6117 STF 284 AB 189.953 6.903 190.3 8.8 6.911 2.134 0.347 0.008

Page 380 CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs... are given equal weight in determining the final fit of the line. In working with double stars this is not how we evaluate the historical data, of course. To be precise, each measurement must be assigned a weight based on a number of factors (see http://ad.usno.navy.mil/wds/ orb6/orb6text.html#grading for more information). Hence, the Excel linear trend line function can serve as an indicator that a pair may be linear, but not as a definitive statement. One must exercise caution when assigning a linear nature to a pair. There are two mitigating factors that can actually rule against linearity. These factors are (1) the number of measurements (some pairs have fewer than a dozen measurements), and (2) the total displacement of the companion over the history of the measurements (in some cases, the companion has only moved 3 arc seconds in nearly 200 years). When a pair has significant change in over the years, it is more likely that the pair is linear. Even then, however, one must be careful that we are not observing a nearly edge-on orbit in which the companion is transiting in front of (or behind) the primary in its normal orbit. (A similar problem exists with common proper motions, which will be covered in another paper.) Results, Part 2: 18 Pairs That Are Showing Definite Rectilinear Motion Having said all of that, I present Table 3, which shows 18 pairs that have high R 2 values but for which no rectilinear solutions presently exist. (Continued on page 385) Table 3. 18 Likely Rectilinear Pairs WDS Number Disc Comp Date Last Last Last Year Meas. Made Meas Meas Resid Resid R2 Note 00042+4959 HJ 1931 2015.849 117.0 22.40 2014 2 117.491 22.843-0.491-0.443 n/a 10 00071+6309 ES 1934 AB 2015.915 70.4 6.77 2004 4 70.949 6.835-0.549-0.065 0.8787 11 00099+1125 HJ 1939 2015.915 168.7 31.09 2010 6 169.569 30.630-0.869 0.460 0.9243 12 00099+7329 WFC 1 2015.877 36.5 6.42 2010 6 34.806 6.277 1.694 0.143 0.7922 13 00167+4104 FAB 2 AB 2015.852 308.8 12.17 2010 2 304.499 12.940 4.301-0.770 0.9972 14 00287+5801 MLB 107 AB 2015.910 2.8 34.97 2011 6 3.219 34.443-0.419 0.525 0.8825 15 00304+6059 STI 82 AB 2015.863 81.7 11.19 2011 2 84.524 11.122-2.824 0.071 0.9508 16 00324+4455 HJ 1029 2015.852 289.1 14.80 2010 2 289.098 15.002 0.002-0.202 0.9980 17 00395+6002 HJ 1042 2015.863 63.3 15.34 2014 2 63.690 15.349-0.390-0.009 0.7965 18 00458+4951 ES 446 2015.901 256.6 13.83 2007 6 257.022 13.846-0.422-0.016 0.8015 19 00552+3814 KU 71 2015.855 248.9 22.50 2013 2 248.311 22.328 0.589 0.172 0.8092 20 01107+8021 STF 89 2015.855 322.2 16.57 2006 2 319.640 16.803 2.560-0.233 0.9287 21 01246+5311 ES 2583 2015.882 343.8 26.39 2011 10 345.133 25.949-1.333 0.438 0.9129 22 01495+2842 STF 176 2015.915 330.5 23.70 2006 6 331.513 23.695-1.013 0.005 0.9395 23 01594+5036 AG 302 2015.893 2.6 14.65 2010 6 3.134 14.595-0.534 0.055 0.7978 24 02108+5624 ARG 7 2015.893 252.9 16.79 2009 6 252.945 16.930-0.045-0.140 0.8857 25 02124+7256 HJ 1107 2015.915 99.5 21.21 2012 6 98.805 21.126 0.695 0.084 0.9363 26 02481+3733 AG 51 2015.915 285.5 11.10 2010 6 284.654 11.256 0.846-0.156 0.9183 27

Page 381 CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs... Table 3 Notes: 10. It is ironic that the first pair in this table does not yield a linear trend line solution, as the data plots in almost a perfectly north-south line and Excel tries to draw the trend line horizontally! Nonetheless, the plot shows a nearly straight line with the companion moving in the general direction of = 180. Figure 3 is a plot of the measurements showing 2015.849 as the red box: 12. Figure 5 is a weighted plot of the data. Figure 5. Plot of WDS 00099+1125. 13. The WFC 1897.75 measurement should be heavily discounted as it plots well away from the rest of the data. (If it is included, the R2 value drops to 0.3863.) Figure 6 is the plot with WFC 1897.75 removed: Figure 3: Data plot of WDS 00042+4959 showing strong linear nature in the motion of the companion. 11. Figure 4 is the data plot for this pair, based on weighted measurements (more reliable than Excel s equal weight line). Figure 6. Plot of WDS 00099+7329 without WFC 1897.75. Figure 4. Plot of WDS 00071+6309 AB.

Page 382 CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs... 14. Figure 7 is a data plot of WDS 00167_4104 16. Only seven measures for this pair make classification a bit premature despite the high R2 value. See Figure 9. Figure 7: Plot of WDS 00167_4104. Figure 9: Plot of WDS 00304+6059 AB; premature classification may be the case here. 15. Figure 8 is a plot of WDS 00287+5801 AB. 17. A plot of this pair is shown in Figure 10. Figure 8. Plot of WDS 00287+5801 AB. Figure 10: Plot of WDS 00324+4455.

Page 383 CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs... 18. Here is a plot (Figure 11) using weighted measurements: 20. A plot of this pair is given in Figure 13. Figure 11. Plot of WDS 00395+6002. 19. Both CLL 1980 and TOB 1989.43 plot well away from the data (See Figure 12.) and, if included, drop the R2 value down to 0.0009. They should be given very little, if any, weight for analysis. Figure 13. Plot of WDS 00552+3814. 21. Apparently EGB 1879.75 flipped the protractor on his micrometer as his data point plots well away from the historical trend. If we subtract his q from 360, his data point falls right on the trend line. Figure 14 is a weighted plot of the data: Figure 12: Plot of WDS 00458+4951 without CLL 1980 and TOB 1989.43. Figure 14: Plot of WDS 01107+8021 with EGB 1879.75 corrected for quadrant flip.

Page 384 CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs... 22. This pair is plotted in Figure 15. 24. Figure 17 is a plot of this pair. Figure 15. Plot of WDS 01246+5311. Figure 16. Plot of WDS 01594+5036. 23. See Figure 16. CLL 1980.8 should be given no weight. It plots well away from the trend and its presence drops the R2 value from 0.9395 to 0.8084. 25. Figure 18 is a plot of this pair. Figure 16. Plot of WDS 01495+2842 without CLL 1980.8. Figure 18. Plot of WDS 02108+5624.

Page 385 CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs... 26. John Herschel s measurements are very poor and should be given a very low weight during analysis. The plot of this pair, without HJ 1828 and HJ 1831.83, is shown in Figure 19. 27. A plot of this pair is given in Figure 20. Figure 19. Plot of WDS 02124+7256 without HJ 1828 and HJ 1831.83. Figure 20. Plot of WDS 2481+3733. (Continued from page 380) Results, Part 3: 26 Pairs That Are Showing Possible Rectilinear Motion In Table 4, I present the measurements on 26 pairs that show some possibility of rectilinear motion. These cases are very vague at this time, but these pairs deserve extra attention by astrometrists in the years ahead to help determine their true nature. In Table 4, Last, Last, and Last Year are the year and latest recorded measures for and. Meas. Made shows how many measurements I made of the pair (using both the companion and its complement image). Meas and Meas report my measurements of the pair. Resid and Resid show the residuals of my measurement compared to the last measurement on record. Discussion The Autumn 2015 observing program at Brilliant Sky Observatory produced many useful and accurate CCD measurements of 66 known (or possibly) rectilinear pairs. The measurements confirmed the accuracy of the ephemerides of the known pairs in all but one case, and that exception was marginal. In addition, 18 cases were uncovered that are likely at or nearly at a solvable state for determining the rectilinear elements and producing ephemerides. The utility and accuracy of Plate Solve 3.47B is well established by this observing program. The ability of the Skyris to capture data on close and faint pairs was demonstrated by this program. Recommended Future Observations I plan to measure the same stars early in 2016 after their early evening positions make them easily observed on the west side of the meridian and then compare east-meridian measurements to west-meridian measurements to identify systemic errors (if any) and provide a second set of measures for these stars. (Continued on page 387)

Page 386 CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs... WDS Number Disc Comp Date Last Last Last Year Table 4. 26 Possible Rectilinear Pairs Meas. Made Meas Meas Resid Resid R2 Note 00059+1805 STF3060 AB 2015.904 133.6 3.35 2012 6 134.528 3.444-0.928-0.099 0.5181 00091+5938 ARG 1 AB 2015.836 329.0 25.94 2012 4 328.757 25.961 0.243-0.021 1 00100+4623 STF 3 2015.904 80.9 4.95 2011 6 82.409 5.012-1.509-0.062 0.3247 2 00229+5420 ES 42 2015.882 206.1 7.26 2003 8 208.633 7.202-2.533 0.059 0.6613 00253+3724 ES 1938 2015.910 8.4 7.14 2010 6 8.106 7.038 0.294 0.102 0.4393 00303+5624 STI1364 2015.852 6.7 14.64 2012 2 7.309 14.682-0.609-0.042 0.6164 00318+3658 STT 13 AB 2015.893 131.4 6.85 2011 6 132.211 6.762-0.811 0.088 00403+2403 BU 1348 AC 2015.852 233.1 46.44 2011 2 53.128 46.516-0.028-0.076 0.0169 00444+3332 STF 54 2015.855 188.5 18.52 2010 2 188.426 18.301 0.074 0.223 0.3848 00505+7538 HJ 1997 2015.855 47.3 17.60 2014 2 47.273 17.598 0.027 0.002 0.6379 00538+5242 STF 70 AB 2015.915 247.7 8.04 2011 6 247.244 8.132 0.456-0.092 0.6059 01134+7137 HJ 2022 2015.877 154.1 11.85 2012 6 154.406 11.929-0.306-0.079 0.6938 3 01147+4255 ARG 49 AC 2015.893 99.8 22.71 2003 6 102.929 23.489-3.129-0.779 0.6105 01245+3902 STTA 17 AB 2015.890 101.5 35.80 2014 10 101.141 35.376 0.359 0.424 01279+7807 HJ 2038 2015.855 358.1 26.20 2010 2 358.030 25.959 0.070 0.241 0.2585 4 01301+4131 HJ 1081 2015.893 318.1 8.89 2003 6 319.380 8.419-1.280 0.471 0.3954 5 01317+6103 STF 128 2015.877 309.1 11.28 2007 10 310.169 11.360-1.069-0.077.02492 01342+4800 STF 134 2015.910 354.6 11.11 2010 6 356.415 10.989-1.815 0.121 0.7090 01344+5553 HJ 2047 2015.855 55.4 13.33 2005 2 56.702 13.320-1.302 0.010 0.7453 6 01364+7909 STF 127 2015.855 190.4 23.71 2010 2 190.226 23.395 0.174 0.315 7 01393+3901 HJ 1087 2015.910 74.5 13.26 2014 6 75.072 13.077-0.572 0.183 0.0472 8 01393+5257 STF 139 AB 2015.893 38.9 9.21 2011 5 39.117 9.212-0.217-0.002 0.3689 9 01456+7721 HJ 2065 2015.915 156.2 21.65 2012 4 155.737 21.320 0.463 0.330 0.7648 01523+3355 HU 805 AC 2015.910 257.2 14.82 2012 6 256.967 14.793 0.233 0.030 0.7155 02011+7358 STF 184 2015.863 14.9 17.03 2010 2 14.474 16.989 0.426 0.041 0.6478 02109+1341 STF 224 2015.915 243.5 6.00 2011 6 243.862 5.942-0.362 0.058 0.5726 10 Table 4 Notes: 1. The plot shows a vague suggestion of sinusoidal motion of the companion. 2. Just starting to show a linear trend. 3. HJ 1831.83 should be heavily discounted in the analysis. 4. HJ 1831.86 should be heavily discounted in the analysis. 5. HJ 2818.0 should be heavily discounted in the analysis. 6. HJ 1831.94 should be heavily discounted in the analysis. 7. FmY 2012.85 should be heavily discounted in the analysis. 8. HJ 2818.0 should be heavily discounted in the analysis. 9. HJ 1831.85 should be heavily discounted in the analysis. 10. HJ 2818.0 should be heavily discounted in the analysis.

Page 387 CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs... (Continued from page 385) Acknowledgments This research has made use of the Washington Double Star Catalog maintained at the U. S. Naval Observatory. Use was also made of the VizieR service of the Centre de Données astronomiques de Strasbourg and the Hipparcos 2 Output Catalog, and the Fourth Catalog of Rectilinear Elements produced by the U. S. Naval Observatory. The author thanks Dr. William H. Hartkopf of the U. S. Naval Observatory for reviewing the draft of this paper. References Cotterell, J. David 2015. Calibrating the Plate Scale of a 20 cm Telescope with a Multiple-Slit Diffraction Mask. JDSO Vol 11 No 4, 387-389. Viewable online at JDSO.org. Harshaw, Richard 2015. Calibrating a CCD Camera for Speckle Interferometry. JDSO Vol 11 No 1s, 314-322.

Page 388 CCD Measurements of 8 Double Stars With Binary Nature The Autumn 2015 Observing Program at Brilliant Sky Observatory, Part 2 Richard W. Harshaw Rharshaw2@cox.net Brilliant Sky Observatory, Cave Creek, AZ Abstract: Results of CCD measures of five pairs are reported as well as three cases of speckle interferometry. Results show that the Skyris 618 CCD camera and an 11-inch SCT can do serious and accurate double star astrometry The Observing Program From October 23 to December 1, 2015, a vigorous program of measuring double stars with a Skyris 618C CCD camera was done at Brilliant Sky Observatory (Cave Creek, Arizona). Over 18 different nights, over 220 double stars were imaged and their FITS cubes reduced using Plate Solve 3.47B. This report focuses on 8 pairs that either have known orbits (one case), or are showing strong arc-like shapes of the plots of their measurements (four pairs), or are close pairs (three) best analyzed with speckle interferometry. Equipment Used The equipment used in this observing program is described in detail in Harshaw 2016. This includes the telescope (a C-11), the mount (CGEM-DX), camera (Celestron Skyris 618c), and data reduction software (Plate Solve 3.47B). Procedure When doing speckle interferometry, I select pairs that are no farther apart than 7 arc seconds and with both magnitudes being brighter than 8.50, since fainter stars require integration times of greater than 100ms. (The rule of thumb for speckle integration times says 50ms or less, which is considered by many to be about as long as one can image without smearing out the speckles created by the atmosphere. But this rule was established with large research-grade telescopes which must look through many millions of Fried turbulence cells compared to a smaller telescope s thousands of cells. A member of our speckle community, Clif Ashcraft of New Jersey, has been getting good speckle results with integration times in the 100ms range.) The magnitude limit comes into play when one considers that when obtaining speckles, I use a Johnson-Cousins R filter to reduce atmospheric dispersion. This means that there are only a little over 180 pairs that can be analyzed with speckle using a Skyris 618C on a C-11. For speckle, I obtain 1,000 FITS frames (which Plate Solve converts into a FITS cube for processing), and generally run 3 to 8 sets of frames. The speckle procedure also requires obtaining 1,000 FITS frames of a single deconvolution star. The Fourier Transform that Plate Solve develops for the deconvolution star is then applied to the double star to enhance the clarity of the data and produce a highquality autocorrelogram. For CCD measures, I find that taking 100 frames and then selecting the best 25% for signal to noise ratio yields 25 frames that Plate Solve can work with very nicely. I find that as a general rule, Plate Solve gives more accurate solutions than lucky imaging. For a description of my processing method, see Harshaw 2016. Results, Part 1: One Grade 3 Orbit First to report is the one pair with a known orbit

Page 389 CCD Measurements of 8 Double Stars With Binary Nature... that was imaged during the Autumn 2015 observing season at Brilliant Sky Observatory. The results are shown in Table 1. In Table 1, Last and Last are the measures of and (respectively) in the year shown in Last Year. Meas. Made is the number of measurements made of the autocorrelograms. Meas. and Meas. and Resid. and Resid. are the measurements (and residuals) of the measurement made. With only six measures made of three FITS cubes, the standard error is of little value. The PNG file for this pair from the U. S. Naval Observatory is shown in Figure 1. After obtaining the measurement history of this pair from the U. S. Naval Observatory, the past measurements were corrected for precession of the equinoxes and plotted in Cartesian coordinates using Microsoft s Excel. The result of that plot, showing the 2015.855 measure, is the red box in Figure 2. Results, Part 2: 4 Pairs That Show A Short Arc Short arc binaries are pairs whose data plot is beginning to show an arc, the telltale sign that the pair is probably physically bound, as the arc is the projection of the orbital path on the plane of the sky. However, do not interpret short arc to mean short period. In some cases, the arc may be revealing itself at periastron (or apastron) and the arc may be a small piece of a huge and highly inclined orbit. But the arcing does suggest, no matter the orbital period that may someday be derived, that the pair is gravitationally bound. It may take centuries more of measurement to collect enough data to permit an orbital solution, but the existence of such pairs should warrant special attention by astrometrists in the future. To determine a pair to be a short arc binary, it is necessary to obtain the measurement data from the U. S. Naval Observatory and then to enter the values of theta and rho into a spreadsheet that can then translate the values into X, Y coordinates, thus allowing the user to plot the data in Cartesian space. This is done by the simple mathematical conversions of X = * sin( Y = * cos( ) In addition, we must adjust for the precession of the equinoxes to normalize the measurements for different epochs to the present day. All of this is done in an Excel program I wrote for the purpose of plotting the measurement histories. Excel has a trend line function that can be invoked by right-clicking on any data point in the graph of the measurements and selecting Insert Trend Line. This allows us to select a polynomial line that takes on the shape of an arc. We can also ask for the R 2 value, a number that reflects the goodness of the fit of the data to the curve. However, Excel assigns equal weights to all the data points, which is not how we analyze historical data in double star astrometrics. The higher the R 2 value, the more likely it is that we are indeed seeing the emergence of a short arc and hence have a clue about the physical/binary nature of the pair. The lower the R 2 value, the more scatter or noise in the data and the less likely we are looking at a true binary system. The format of Table 2 is the same as Table 1 but with the addition of the R 2 value column. Results, Part 3: 3 Speckle Interferometry Pairs In the autumn 2015 observing program at Brilliant Sky Observatory, three pairs were measured using speckle interferometry. This process has been documented in Harshaw (2015). All three speckle measurements were made at f/30 and consisted of pairs bright enough to image at integration times of under 50ms and with separations of 7 arc seconds or less, using a Johnson-Cousins R filter. (Two stars are borderline cases for. As a general rule, stars wider than 7 arc seconds will probably have their light passing through different isoplanatic patches, so true speckle interferometry is not usually reliable at these separations. However, exceptionally good seeing might extend the patch a bit.) In all three pairs, the stars have common proper motion. The data for the speckle measurements are in Table 3. Discussion The Autumn 2015 observing program at Brilliant Sky Observatory proved that speckle interferometry on close double stars can be done with amateur-class equipment and inexpensive CCD cameras. The one known orbit pair that was measured showed results that are in good conformance with the ephemerides from the Sixth Catalog of Orbits of Visual Binary Stars. The short arc binaries deserve special attention by astrometrists in the coming years. Recommended Future Observations Observations of the pairs featured in Table 2 would be a good investment of amateur observing time as we may be only a few measurements away from deriving (Continued on page 393)

Page 390 CCD Measurements of 8 Double Stars With Binary Nature... Table 1: Measure of WDS 00491+5749 (STF 60 AC) WDS Number Disc Comp Date Last Last Last Year Meas. Made Meas Meas Resid Resid Notes 00491+5749 STF 60 AB 2015.855 324.3 12.78 2014 6 324.783 13.696-0.483-0.916 1 Table 2: Short Arc Binaries WDS Number Disc Comp Date Last Last Last Meas. Year Made Meas Meas Resid Resid R2 Note 00089+6627 FAB 1 2015.858 178.9 14.65 2011 2 181.034 14.905-2.134-0.255 0.5461 2 00311+5648 ES 2 AB 2015.890 112.1 5.93 2012 8 112.686 5.854-0.586 0.076 0.7661 3 00546+3910 STF 72 2015.855 172.5 23.03 2014 2 172.969 23.339-0.469-0.309 0.7203 4 01373+6344 MLB 383 AD 2015.877 165.6 31.96 2011 6 164.809 31.752 0.791 0.208 0.0478 5 Table 3: Speckle Interferometry on Three Pairs WDS Number Disc Comp Date Last Last Last Year Meas. Made Meas Meas Resid Resid Plot 00499+2743 STF 61 2015.855 115.0 4.50 2014 20 113.529 4.200 1.471 0.300 6 01001+4443 STF 79 2015.855 194.1 7.90 2013 10 192.327 7.842 1.773 0.058 7 01535+1918 STF 180 AB 2015.855 0.9 7.41 2014 10 359.704 7.362-0.604 0.048 8 Notes to Tables: 1. Using the Sixth Orbit Catalog ephemerides and extrapolating for 2015.855, the projected values for and are 323.642 and 13.346". The residuals for the 2015.855 measurement are +1.141 and +0.353". See Figures 1 and 2. 2. The trend line (Figure 3) is actually reversed the concave side of the curve points away from the system s center of mass. May not be a true short arc binary. 3. In this case, the trend line has the pair s center of mass on the correct side of the curve. See Figure 4. 4. Parallaxes for both stars are known, but neither is reliable as a test for distance and physical separation of the two stars. The parallax values are 1.33 ±1.30 mas for the primary and 12.33 ±5.51 mas for the companion. See Figure 5. 5. See Figure 6 for a plot of WDS 01373+6344. 6. See Figure 7 for a plot of WDS 00499+2743, a speckle measurement. 7. See Figure 8 for a plot of WDS 01001+4443, a speckle measurement. 8. See Figure 9 for a plot of WDS 01535+1918 AB, a pair with several anomalous measurements. Figure 1: PNG plot of WDS 00401+5749. Figure 2: Plot of WDS 00491+5749 AB history showing the 2015.855 measurement (red box).

Page 391 CCD Measurements of 8 Double Stars With Binary Nature... Figure 3: Plot of WDS 00089+6627, a curious case of a reverse trend curve. Figure 4: Plot of WDS 00311+5648 AB. Figure 5. Plot of WDS 00546+3910. Figure 6: Plot of WDS 01373+6344 AD.

Page 392 CCD Measurements of 8 Double Stars With Binary Nature... Figure 7. Plot of WDS 00499+2743, a speckle measurement. Figure 8. Plot of WDS 01001+4443. Figure 9. Plot of WDS 01535+1918 AB, a pair with several anomalous measurements.

Page 393 CCD Measurements of 8 Double Stars With Binary Nature... an orbital solution. Acknowledgments This research has made use of the Washington Double Star Catalog maintained at the U.S. Naval Observatory. Use was also made of the VizieR service of the Centre de Données astronomiques de Strasbourg and the Hipparcos 2 Output Catalog as well as the Sixth Catalog of Orbits of Visual Binary Stars (Hartkopf and Mason, June 2015). References Cotterell, J. David 2015. Calibrating the Plate Scale of a 20 cm Telescope with a Multiple-Slit Diffraction Mask. JDSO Vol 11 No 4, 387-389. Viewable online at JDSO.org. Harshaw, Richard 2015. Calibrating a CCD Camera for Speckle Interferometry. JDSO Vol 11 No 1s, 314-322. Harshaw, Richard 2016. CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs. JDSO, in submission.

Page 394 CCD Measurements of 141 Proper Motion Stars: The Autumn 2015 Observing Program at the Brilliant Sky Observatory, Part 3 Richard W. Harshaw Rharshaw2@cox.net Brilliant Sky Observatory, Cave Creek, AZ Abstract: The use of a Skyris 618C camera on a Celestron C-11 SCT proved to be a reliable means of obtaining accurate data for double star astrometry. 141 systems were examined, with all but one result plotting within the scattered data from the historical measurements. The Observing Program From October 23 to December 1, 2015, a vigorous program of measuring double stars with a Skyris 618C CCD camera was done at Brilliant Sky Observatory (Cave Creek, Arizona). Over 18 different nights, over 220 double stars were imaged and their FITS cubes reduced using Plate Solve 3.47B. This report focuses on 141 pairs that share some degree of proper motion. Equipment Used The equipment used for this project is described in Harshaw 2016. Procedure See Harshaw 2016 for a complete description of the procedure used for these observations. Results: 141 Pairs That Are Proper Motion Related This set of measurements deals with stars that share proper motion to some degree. I list three types of proper motion classes, based on the relative differences in the proper motions. The proper motion of a star can be depicted as a vector. When the resultant of the two vectors is divided by the largest vector, the result will either be zero (or very near it) if the proper motions are identical, somewhere between 20% and 60% of the resultant of the vectors, or over 60% of the resultant. Pairs in the first category are classed as Common Proper Motion pairs, or CPM. Pairs in the second category are classed as Similar Proper Motion pairs (SPM), and those in the third category are classed as Different Proper Motion pairs (DPM). Some examples might help illustrate the classification scheme. Case 1 has two stars in which the proper motion (PM) vectors of the stars are +027 +018 for the primary and +026 +018 for the companion. The resultant is found by: R = 1 mas The largest vector is that of the primary, for which the value is V = 31.6 mas The ratio of the resultant to the largest vector is thus 1/31.6 = 3.2%. This is a CPM case. Case 2 has a pair with PM of -026 +005 for the pri-

Page 395 CCD Measurements of 141 Proper Motion Stars: The Autumn 2015 Observing Program... mary and -018 +009 for the companion. The resultant is 8.94 mas while the largest vector has a scalar value of 26.48 mas. The resultant is 33.7% of the scalar, so this is a SPM pair. For Case 3, the primary has PM of +038-076 with a companion of -010 +037. The resultant is 122.7 mas while the scalar for the largest vector is 85.0 mas. The ratio is 69.2%, so this would be a DPM case. Common proper motion stars are a challenge for double star astrometry. First, they appear to be moving across the sky at the same angular rate. If they are at nearly the same distance (established by accurate parallaxes, which are not always available for both stars of a double), they are probably physically related. If close enough to be gravitationally bound, they are probably a true binary (albeit one with an extremely long period). If too far for gravitational binding (and such binding would depend on the total system mass relative to the orbital velocity of the pair, as noted by Rica [2011]), then the pair probably shares a common origin perhaps being ejected together from an open star cluster or stellar association. It might also be the case that stars that show no significant displacement over two or three centuries could be in highly eccentric orbits whose plane is nearly on our line of sight and whose major axis is oriented more or less along our line of sight, and that we are viewing the motion of the companion along one of the longer sides of the orbit as it approaches (or recedes from) earth. In such cases, a star may show no significant angular displacement for thousands of years. Finally, the two stars may not be related to each other at all. They just happen to share angular motion across the sky. If they are at greatly different distances, this implies that the more remote star has a higher absolute motion through space than the nearer star, but other than that, we cannot make any conclusions about the nature of the system, unless accurate parallaxes for both stars are known and the parallaxes place the stars at significantly different distances (too far apart for gravitational binding). Discussion All but one of 141 measurements plotted inside the region of all the historical measurement plots. Only one measurement plotted on the outer edge of the historical grouping (WDS 00142+4612). The capabilities of the Skyris 618 and an 11-inch SCT to do accurate double star astrometry are wellestablished. Recommended Future Observations Four pairs appear to be physical and warrant extra attention: WDS 00528+5638, WDS 01057+2128, WDS 02053+6740 and WDS 02370+2439. Three pairs show an optical nature and could use extra observations in the next few decades: WDS 00028+8017, WDS 00352+3650 and WDS 21543+1943. Four pairs are starting to show what may be a linear trend. These are WDS 00029+7122, WDS 00052+3020, WDS 01420+5547 and WDS 01513+6451. Acknowledgments This research has made use of the Washington Double Star Catalog maintained at the U.S. Naval Observatory. Use was also made of the VizieR service of the Centre de Données astronomiques de Strasbourg and the Hipparcos 2 Output Catalog. References Cotterell, J. David 2015. Calibrating the Plate Scale of a 20 cm Telescope with a Multiple-Slit Diffraction Mask. JDSO Vol 11 No 4, 387-389. Viewable online at JDSO.org. Harshaw, Richard 2015. Calibrating a CCD Camera for Speckle Interferometry. JDSO Vol 11 No 1s, 314-322. Harshaw, Richard 2016. CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs. JDSO in submission. Rica, F. M. 2011. Determining the Nature of a Double Star: The Law of Conservation of Energy and the Orbital Velocity. JDSO Vol 7 No 4, 254-259.

Page 396 CCD Measurements of 141 Proper Motion Stars: The Autumn 2015 Observing Program... Table 1. Measurements on 141 Proper Motion Pairs WDS No. Disc Comp Date Last Last Last Meas. Year Made Meas Meas Resid Resid Type Note 00004+6026 STI1248 2015.855 48.2 12.37 2011 2 48.021 12.254 0.179 0.114 CPM 00005+6713 HJ 1924 2015.858 225.1 8.20 2010 2 224.761 8.087 0.339 0.113 CPM 00020+2347 TVB 2 2015.849 292.2 28.07 2010 6 292.166 27.925 0.034 0.145 CPM 00026+6606 STF3053 AB 2015.833 70.0 14.30 2014 10 70.586 15.159-0.586-0.859 SPM 00027+5958 ARG 47 2015.833 290.0 9.90 2010 6 287.620 9.876 2.380 0.024 DPM 00028+8017 STF3051 2015.836 23.6 16.69 2010 6 22.827 16.768 0.773-0.078 CPM 1 00029+7122 STF3052 2015.836 8.7 34.72 2010 6 8.294 34.649 0.406 0.071 SPM 2 00031+0816 STF3054 2015.836 180.0 34.70 2014 6 181.296 33.597-1.296 1.103 CPM 00039+2759 HJ 1929 AB, C 2015.904 287.3 5.43 2011 6 288.115 5.138-0.815 0.292 SPM 00040+6050 HJ 1930 2015.858 346.4 10.95 2011 2 346.404 10.810-0.004 0.140 CPM 00042+2701 SMA 1 2015.852 161.3 13.12 2010 2 161.356 13.382-0.056-0.262 CPM 00043+4235 HJ 1932 AB 2015.882 306.5 7.11 2011 6 307.037 7.155-0.537-0.045 CPM 00052+3020 STF3058 2015.836 52.2 12.60 2012 6 51.267 12.616 0.933-0.016 CPM 3 00068+5430 ES 611 2015.849 291.0 9.88 2003 2 289.970 10.367 1.030-0.487 CPM 00078+5723 HJ 3241 2015.849 8.1 15.04 2014 4 7.976 14.974 0.124 0.066 CPM 00089+3713 STF 1 2015.836 286.7 9.65 2014 4 286.216 9.855 0.484-0.205 SPM 00096+4758 ES 1126 2015.910 318.3 6.36 2008 6 317.634 6.056 0.666 0.304 SPM 00099+0827 STF 4 2015.904 276.1 5.20 2009 6 276.109 5.243-0.009-0.043 CPM 00099+3014 MLB 552 2015.882 190.0 8.20 2012 8 190.027 8.042-0.027 0.158 DPM 00112+4419 ES 1406 AB 2015.890 331.5 9.35 2011 8 333.136 9.686-1.636-0.336 SPM 00114+5205 HJ 1004 AC 2015.890 314.8 25.10 2014 8 315.279 25.207-0.479-0.107 DPM 4 00115+2949 MLB 441 AB 2015.852 358.7 14.14 2012 2 358.670 14.138 0.030 0.002 CPM 5 00116-0305 STF 8 2015.836 291.8 7.99 2012 6 291.325 7.621 0.475 0.369 CPM 00129+6150 ES 1865 AB 2015.858 121.6 23.60 2012 3 123.289 23.712-1.689-0.112 DPM 00137+4934 STF 9 2015.849 164.5 20.19 2003 4 165.411 19.935-0.911 0.255 CPM 00138+3612 BU 1341 AB 2015.910 319.0 20.51 2014 8 319.330 20.295-0.330 0.215 CPM 00142+4612 ES 1195 2015.910 14.6 6.68 2002 6 12.856 6.788 1.744-0.104 CPM 6 00148+6250 STF 10 AB 2015.849 176.0 17.60 2012 4 175.664 17.503 0.336 0.097 00150+0849 STF 12 2015.836 145.0 11.60 2014 8 147.190 11.527-2.190 0.073 SPM 00152+7801 STF 11 2015.858 191.8 7.97 2010 6 191.522 8.220 0.278-0.250 CPM 00160+4835 HJ 1009 AB 2015.852 27.9 16.79 2003 2 28.287 16.199-0.387 0.591 SPM 00160+4835 HJ 1009 AC 2015.852 138.4 36.46 2002 2 137.085 36.108 1.315 0.352 SPM 00161+6006 HJ 1010 2015.858 117.8 20.40 2008 2 118.246 20.471-0.446-0.071 SPM 00162+2918 STF 17 AB 2015.849 30.0 26.90 2012 4 28.986 26.696 1.014 0.204 SPM 7 00167+5439 STF 16 2015.901 39.1 5.82 2003 6 40.618 5.869-1.518-0.049 SPM 00174+1631 STF 20 2015.849 233.4 11.88 2009 4 233.425 11.913-0.025-0.029 CPM 00174+3550 WEI 1 2015.904 286.6 5.28 2009 6 285.884 5.386 0.716-0.106 CPM 00185+2608 STF 24 2015.904 247.0 5.10 2013 6 247.429 4.950-0.429 0.150 SPM 00203+5412 HDS 44 2015.852 32.1 12.34 2009 4 37.636 12.312-5.536 0.028 DPM 00214+6700 STF 26 AB, C 2015.858 114.4 13.33 2010 4 113.627 13.753 0.773-0.424 CPM 00216+5543 STI1334 2015.910 235.4 6.61 2011 6 235.867 6.600-0.467 0.010 SPM 00220+4213 HJ 1021 2015.910 246.2 6.15 2002 6 247.127 6.016-0.927 0.135 SPM 00239+2930 STF 28 AB 2015.849 224.2 32.80 2013 6 223.919 32.786 0.281 0.014 CPM 00260+6647 HJ 1026 2015.863 192.1 12.35 2012 2 192.393 12.466-0.293-0.116 CPM 00261+3448 HJ 622 2015.852 130.9 19.86 2014 2 130.924 19.794-0.024 0.066 CPM Table 1 continues on next page.

Page 397 CCD Measurements of 141 Proper Motion Stars: The Autumn 2015 Observing Program... Table 1 (cointinued). Measurements on 141 Proper Motion Pairs WDS No. Disc Comp Date Last Last Last Meas. Year Made Meas Meas Resid Resid Type Note 00270+6430 MLB 277 2015.877 72.6 6.34 2011 6 73.272 6.709-0.672-0.369??? 00271+6112 FOX 108 2015.863 26.8 7.58 2012 2 26.919 7.369-0.119 0.211 SPM 00287+5700 STI1358 2015.852 302.6 14.32 2011 2 302.691 14.247-0.091 0.074 SPM 00310+5539 ES 116 2015.882 256.0 7.41 2003 10 257.762 7.409-1.762 0.001 DPM 00327+7807 STF 34 2015.863 339.4 5.79 2006 6 339.111 5.609 0.289 0.181 CPM 00329+3007 FOX 111 2015.852 26.5 23.22 2010 2 26.771 23.081-0.271 0.139 SPM 00333+3731 ALI 249 2015.852 287.3 13.33 2005 2 287.398 13.023-0.098 0.307 CPM 8 00350+5636 ES 3 2015.849 158.6 8.10 2012 4 158.769 7.921-0.169 0.179 CPM 00352+3650 STF 40 AB 2015.849 312.1 11.64 2014 6 311.628 12.015 0.472-0.375 SPM 9 00355+5841 STF 38 2015.852 144.4 16.89 2012 4 144.265 16.900 0.135-0.010 SPM 00369+3343 H 5 17 AB 2015.890 173.5 35.60 2014 10 173.969 35.702-0.469-0.102 SPM 00400+5549 ES 936 2015.901 269.0 6.03 2011 6 270.994 7.886-1.994-1.856 CPM 00403+2403 STF 47 AB 2015.852 205.7 16.40 2011 2 205.464 16.560 0.236-0.160 CPM 00403+4343 HJ 1044 2015.890 138.9 21.73 2005 8 139.389 21.560-0.489 0.170 CPM 00430+4405 ES 1408 2015.901 262.5 7.90 2005 6 265.106 7.558-2.606 0.342 CPM 00474+7239 STF 57 2015.863 197.9 6.29 2010 2 15.271 6.151 182.629 0.139??? 00475+4214 ES 1488 2015.890 280.9 6.91 2004 8 282.638 6.810-1.738 0.100 CPM 00495+5534 STI1437 2015.910 298.6 11.27 2011 2 298.641 11.093-0.041 0.176 SPM 00503+3548 STF 62 2015.855 303.0 11.81 2012 2 303.010 11.757-0.010 0.053 CPM 00514+7010 HJ 1999 2015.863 16.2 25.60 2010 2 16.153 25.312 0.047 0.288 CPM 00528+5638 BU 1 AD 2015.890 194.8 8.96 2012 6 196.763 8.896-1.963 0.064 SPM 00528+5638 BU 1 CD 2015.890 133.0 3.10 2013 6 134.536 3.718-1.536-0.618??? 10 00536+6835 AG 8 2015.855 35.2 17.41 2010 2 34.923 17.387 0.277 0.023 CPM 00543+6903 AG 9 2015.863 70.6 6.49 2003 2 71.112 6.419-0.512 0.070 SPM 00573+6020 ARG 3 2015.855 200.2 20.69 2014 2 199.991 20.677 0.209 0.013 CPM 00581+2655 STF 77 2015.855 118.0 10.37 2005 2 119.324 10.300-1.324 0.070 CPM 00583+5659 STI1492 2015.882 315.9 14.55 2010 8 316.312 14.380-0.412 0.172 DPM 01003+6717 HJ 1061 2015.877 103.6 13.17 2010 4 102.748 13.125 0.852 0.045 CPM 01027+4742 HJ 2010 2015.833 270.7 9.88 2011 8 270.428 9.899 0.272-0.019 CPM 01032+6032 MLB 43 2015.858 297.7 7.53 2012 2 294.973 7.089 2.727 0.441 SPM 01057+2128 STF 88 AB 2015.833 159.0 29.69 2014 10 158.917 29.556 0.083 0.134 CPM 11 01058+0455 STF 90 AB 2015.833 83.4 32.88 2014 8 83.452 32.887-0.052-0.007 CPM 12 01101+5145 STT 23 AB 2015.852 190.9 14.32 2011 4 191.201 14.503-0.301-0.183 SPM 01103+1636 STF 94 AC 2015.852 280.8 20.24 2005 2 281.175 20.279-0.375-0.039 CPM 01107+6515 STI 194 2015.858 21.9 10.21 2011 2 20.387 10.636 1.513-0.426 CPM 01129+3205 STF 98 AB 2015.833 248.0 20.00 2014 8 248.457 19.502-0.457 0.498 CPM 01133+4426 HJ 2027 AB 2015.893 161.2 18.76 2003 6 160.789 18.203 0.411 0.557 CPM 01137+0735 STF 100 AB 2015.833 63.2 22.80 2012 10 62.971 22.752 0.229 0.048 CPM 01146+4102 AG 300 2015.882 44.8 6.58 2008 8 45.119 6.599-0.319-0.019 SPM 01147+4255 ARG 49 AB 2015.893 106.8 36.26 2003 6 105.753 35.328 1.047 0.932 DPM 01170+3828 STF 104 2015.852 321.6 13.33 2010 2 323.037 13.423-1.437-0.093 SPM 01172+6810 HJ 1075 2015.877 104.5 7.78 2010 6 103.365 7.797 1.135-0.017 DPM 01178+4901 STF 102 AB, C 2015.882 223.8 10.08 2012 14 224.002 10.060-0.202 0.020 CPM 01192+5821 STI1560 2015.893 324.4 13.90 2005 6 324.862 13.782-0.462 0.118 CPM 01200+6355 STF 109 AB 2015.877 11.4 7.20 2012 4 8.911 7.254 2.489-0.054 CPM Table 1 continues on next page.

Page 398 CCD Measurements of 141 Proper Motion Stars: The Autumn 2015 Observing Program... Table 1 (continued). Measurements on 141 Proper Motion Pairs WDS No. Disc Comp Date Last Last Last Meas. Year Made Meas Meas Resid Resid Type Note 01283+5329 STF 123 AB 2015.852 162.1 16.30 2007 2 162.121 16.335-0.021-0.035 CPM 01326+5445 ES 2584 2015.890 196.3 15.70 2008 8 196.536 15.649-0.236 0.051 CPM 01330+5340 HJ 2051 2015.910 75.3 23.15 2002 6 76.064 22.812-0.764 0.342 DPM 13 01331+5416 ES 2585 2015.893 29.0 15.05 2006 6 29.782 15.037-0.782 0.013 CPM 01332+6041 STF 131 AB 2015.877 147.7 13.35 2012 10 142.878 13.920 4.822-0.570 CPM 01340+4559 ARG 5 2015.882 319.2 9.93 2006 8 319.825 9.930-0.625 0.000 CPM 01348+5209 ES 759 2015.910 90.9 10.37 2008 6 92.037 10.260-1.137 0.110 CPM 01348+6954 STF 130 2015.877 187.7 7.69 2003 10 187.098 7.608 0.602 0.081 CPM 01373+6714 HJ 1084 2015.877 358.3 15.56 2010 8 358.904 15.584-0.604-0.024 SPM 01409+4952 HU 531 AB, C 2015.890 280.2 6.11 2011 6 279.762 6.092 0.438 0.018 CPM 01420+5547 HJ 2066 2015.910 71.7 20.74 2005 6 72.016 20.677-0.316 0.063 DPM 14 01431+3426 COU 668 AB 2015.910 41.0 25.36 2011 6 41.290 24.932-0.290 0.428 SPM 01447+5607 ES 1772 AB 2015.915 107.5 24.67 2011 4 106.801 23.919 0.699 0.751 DPM 01460+6113 STF 151 2015.863 38.1 7.25 2011 2 38.015 6.814 0.085 0.436 CPM 01461+6114 STF 152 2015.863 106.3 9.28 2012 4 105.898 9.422 0.402-0.142 SPM 01466+6116 STF 153 2015.863 69.1 7.84 2012 4 69.062 7.710 0.038 0.130 CPM 01467+3856 STF 157 AC 2015.890 115.6 12.50 2011 8 115.620 12.475-0.020 0.025 SPM 01487+6150 HJ 1091 2015.863 151.9 28.28 2011 4 151.481 28.106 0.419 0.174 CPM 01487+7528 HJ 2075 AB 2015.863 230.8 30.73 2003 4 230.844 30.514-0.044 0.219 CPM 15 01492+3404 STF 164 2015.890 95.4 9.81 2011 8 95.847 9.825-0.447-0.015 CPM 16 01493+6135 ES 1951 2015.863 158.6 6.41 2011 4 160.639 6.122-2.039 0.288 SPM 01513+6451 STF 163 AB 2015.863 37.2 34.75 2012 4 37.073 34.167 0.127 0.583 CPM 17 01514+4329 HJ 2089 2015.890 306.1 29.07 2011 6 306.464 29.031-0.364 0.039 CPM 01517+4549 ARG 51 2015.890 170.9 15.87 2011 6 171.825 15.839-0.925 0.031 CPM 01527+5717 ARG 6 AB 2015.882 136.4 14.81 2003 8 136.135 14.913 0.265-0.103 SPM 01545+5954 HDS 259 2015.893 211.8 16.79 2008 6 211.734 16.499 0.066 0.291 SPM 01561+3745 HJ 1097 2015.915 39.9 14.82 2011 3 39.796 14.645 0.104 0.175 CPM 01561+6035 AG 301 2015.863 262.3 8.60 2011 2 262.186 8.564 0.114 0.036 CPM 01567+3505 ES 2144 2015.915 143.4 6.33 2011 4 144.010 6.407-0.610-0.077 CPM 01595+6254 STF 188 2015.863 238.1 31.88 2011 4 237.860 31.827 0.240 0.053 SPM 18 02039+4220 STF 205 A, BC 2015.855 63.2 9.39 2013 10 61.952 9.708 1.248-0.318 CPM 02042+5257 HJ 2104 2015.855 169.8 30.61 2003 2 168.411 30.161 1.389 0.449 SPM 02053+6740 STF 199 2015.863 22.2 35.80 2012 4 22.089 35.562 0.111 0.238 CPM 19 02078+5525 SMA 30 2015.915 327.8 11.13 2003 4 329.072 11.141-1.272-0.012 SPM 02091+4048 STF 215 2015.893 59.5 19.71 2011 6 60.031 19.584-0.531 0.126 CPM 02091+4051 AG 32 AB 2015.915 99.8 21.40 2011 4 99.094 21.164 0.706 0.236 CPM 20 02094+4254 FOX 122 2015.915 5.0 17.38 2008 4 6.581 17.351-1.581 0.029 SPM 02103+3322 STF 219 2015.855 184.6 11.40 2011 8 185.638 11.662-1.038-0.262 CPM 21 02109+3902 STF 222 2015.893 35.8 16.68 2013 10 36.515 16.603-0.715 0.077 SPM 02124+3018 STF 227 2015.855 69.0 3.80 2012 10 67.422 3.871 1.578-0.071 CPM 02149+5829 STF 230 2015.901 258.8 24.19 2011 6 259.189 23.788-0.389 0.402 CPM 02172+3729 STF 238 AC 2015.915 355.8 10.93 2012 6 356.464 10.845-0.664 0.085 DPM 22 02216+7212 HJ 2122 2015.904 140.1 31.51 2011 6 139.466 31.269 0.634 0.241 CPM 23 02236+7406 STF 241 2015.904 286.0 20.13 2011 6 285.018 19.989 0.982 0.141 DPM 02370+2439 STFA 5 AB 2015.849 275.0 38.00 2012 6 274.593 37.747 0.407 0.253 CPM 24 Table 1 concludes on next page.

Page 399 CCD Measurements of 141 Proper Motion Stars: The Autumn 2015 Observing Program... Table 1 (conclusion). Measurements on 141 Proper Motion Pairs WDS No. Disc Comp Date Last Last Last Meas. Year Made Meas Meas Resid Resid Type Note 20585+1626 STF2738 AB 2015.816 254.0 14.80 2013 10 254.108 14.929-0.108-0.129 SPM 21105+2227 STF2769 AB 2015.816 299.2 18.14 2014 10 299.310 18.067-0.110 0.073 CPM 21359+2622 HJ 1661 2015.816 84.6 11.93 2011 8 85.207 11.932-0.607-0.002 CPM 21390+5729 STF2816 AD 2015.808 338.4 19.80 2012 10 337.671 19.865 0.729-0.065 CPM 21543+1943 STF2841 A, BC 2015.808 109.8 22.20 2014 10 108.235 22.200 1.565 0.000 CPM 25 22086+5917 STF2872 A, BC 2015.808 315.6 21.61 2014 10 314.825 21.528 0.775 0.082 CPM Notes: 1. The parallax of the primary is 6.72 mas ± 0.80, implying a distance of 148 pc and minimum separation of 1,241 AU. But the parallax for the companion is given as 11.46 mas ± 3.56, which is 31% of the parallax and hence not reliable as a true distance indicator. However, assuming this parallax is close to the real one, the companion would appear to be about 87 pc distant, or some 61 pc closer to earth than the companion. Probably an optical system based on this. 2. Both stars have parallax values but the error estimates are too large to make them reliable as true distance indicators. However, a linear trend does appear to be forming in the data plot. 3. This pair may be starting to show a linear trend. The parallax for each star is known, but the error estimates are so large as to make the values unreliable as true distance indicators. 4. HJ 1828.0 should be given very little weight during analysis. 5. Both BAZ 1935.05 and WFC 1958.32 appear to have quadrant reversals. 6. I am not completely at ease with my measurement. 7. HJ 1828.1 should be discounted heavily during analysis. 8. High velocity pair. 9. Parallaxes of both stars are known, but only the primary is reliable. It is given as 3.85 mas ±0.86, implying a distance of 260 pc. If both stars are at this distance, the minimum separation between the two is 1,600 AU. The parallax of the companion has an uncertainty of 70% of the parallax itself, so is not a reliable indicator. If the companion really is at the distance implied by its parallax (1.61 mas), it is some 260 pc farther away than the primary and thus the system would clearly be optical. 10. Although the pair is shown as CPM, the parallaxes are nearly identical, being 11.86 mas ± 0.68 for the primary and 11.64 mas ± 0.68 for the companion. Using the mean of 11.73 mas, the system is thus 85 pc away and the stars are 512 AU apart. This system is most likely physical. 11. Like STF 88, this pair has nearly identical parallaxes (24.61 mas ± 0.76 and 23.28 mas ± 0.60). Using the mean of 23.95 mas, the pair is then about 42 pc away with the stars 686 AU apart at minimum. This pair is most likely physical. 12. Only the primary has a usable parallax (18.76 mas ± 2.76), which places it 53 pc away. If the pair is physical (and given the companion parallax of 10.64 mas ± 10.93, this is not likely), the minimum separation would be 606 AU. 13. HJ 1831.88 should be assigned a minimal weight during analysis. 14. Starting to show a linear trend? 15. HJ 1831.84 should be given minimal weight during analysis. 16. Both Mad 1834.36 and WFD 1916.20 should be given very low weights during analysis. 17. A linear trend appears to be emerging. The parallax of the primary is given as 0.17 mas ± 0.063, a value which is on the verge of being unreliable. But assuming it is accurate, the distance to the primary is at least 5,880 pc away which would make the minimum separation of the two stars over 100,000 AU. This pair is probably optical. 18. HJ 1828 should be given minimal weight during analysis. 19. HJ 1828 should be given minimal weight during analysis. The parallax of both stars is known with good accuracy and is almost identical. Using the mean of 7.41 mas, the distance to the system works out to 135 pc, making the stars at least 2,348 AU apart. The system is most probably physical. 20. Dob 1912.96 should be assigned a low weight during analysis. 21. The parallaxes of both stars are similar enough to suggest a physical system, but the uncertainty in the companion s motion makes use of its parallax unreliable. Assuming the system to be at the distance suggested by the primary s parallax, the pair is 160 pc with a minimum separation of 934 AU. But the uncertainty in the parallax of the primary means this analysis should be held with a healthy degree of skepticism. 22. HJ 1828 should be given minimal weight during analysis. 23. CLL 1980.8 appears to be a case of quadrant reversal. 24. This is a high proper motion pair, and given that the parallaxes are virtually identical (the mean being 24.24 mas), the distance to the system works out to 41 pc with the stars being at least 778 AU apart. Most likely a physical system. 25. Both stars have a parallax, but only the primary s is reliable. Its value puts the primary at 103 pc with the pair being 1,143 AU apart. The parallax for the companion would imply a distance of 37 pc, so it is possible that this is an optical pair.

Page 400 Measurements of Multi-star Systems LEO 5 and MKT 13 Faisal AlZaben 1, Allen Priest 1, Stephen Priest 1, Rex Qiu 1, Grady Boyce 2, and Pat Boyce 2 1. Army and Navy Academy, Carlsbad, California 2. Boyce Research Initiatives and Education Foundation Abstract: We report measurements of the position angles and separations of two multistar systems observed during the fall of 2015. Image data was obtained using an online 17-inch itelescope system in Nerpio, Spain. Image data was analyzed using Maxim DL Pro 6 and Mira Pro x64 software tools at the Army and Navy Academy in Carlsbad, California. Our measurements of the LEO 5 system are consistent with historical data, although inconclusive as to the nature of the system. Our measurements and the historical data for the MKT 13 system show a consistent linearity in the position angle and separation. Introduction As a part of an educational course on double stars at the Army and Navy Academy in Carlsbad, California, we obtained images for multi-star systems LEO 5 and MKT 13 in order to measure the relative positions and separations of these systems. Using the Washington Double Star catalog (WDS), we chose star systems which would meet a set of criteria which would allow us to make good measurements with the equipment and tools available. These criteria included star systems with separations of 4 arc seconds or more, visual magnitude of 12 or brighter, and difference in visual magnitude less than 3. Our team, shown in Figure 1, selected two candidate star systems which had not recently been measured. Attempts were made to acquire images using an 11- inch Celestron Schmidt-Cassegrain telescope at Tierra Del Sol, near San Diego, California, but weather conditions prevented us from acquiring any useful images. We utilized the itelescope network of remotely operated telescopes to acquire CCD images of the candidate systems. We used the itelescope T7 system located in Nerpio, Spain, which is a 17-inch CDK with a focal ratio of f/6.8, equipped with an SBIG STL11000M monochrome camera (Figure 2). The field of view is 28x42 arcminutes with 0.63 arcseconds per pixel scale. This telescope provided a large enough aperture to acquire high quality images of the 11 th magnitude stars in one of the systems we chose. We chose to use a telescope in Spain because of the good weather available at the time of the observations. Figure 1. Allen Priest, Stephen Priest, Faisal AlZaben, and Rex Qiu. We imaged both LEO 5 and MKT 13 on two different nights. On each night we acquired four images per system using a luminance filter and four images using a hydrogen alpha (H a -7nm) filter. These two filters were chosen in order to ensure that we would have good measurements on the fainter stars while also ensuring that we would not have blooming problems on some of the brighter stars. Star system LEO 5 is a triple system in the constellation Perseus. The AB pair of this system has not had reported observations since 2006, while the AC pair

Page 401 Measurements of Multi-star Systems LEO 5 and MKT 13 Figure 2. T7 17-inch Planewave f/6.8 Corrected Dall-Kirkham (CDK) Astrograph in Spain. was last reported in 2012. The stars in the system are faint, all with visual magnitudes of about 11. The AB pair of stars in this system appear fairly close to one another with a visual separation of about 4.5 arc seconds. The AC pair has a separation of about 48 arc seconds. Star system MKT 13 is a quintuple system in the constellation of Taurus. While there are five stars in this system, the Aa and Bb stars are each actually very close binary stars with separations of 0.1 arc seconds or less and too close for us to measure with our equipment. The AB pair of this system last reported observations were in 2011. The AC pair was last reported in 2000. The WDS catalog reports that the A and B stars in the system have visual magnitudes of about 3.41 and 3.94 while the C star is fainter, measuring about 11.96 in magnitude. Because of the wide difference in brightness, we were unable to obtain measurements on the AC pair with the images we acquired. Thus, we focused on measurements of the AB pair which have a visual separation of about 341 arcseconds. Methods and Procedures Each observation was scheduled via the itelescope internet portal where we designated: RA & Dec coordinates, image time, number of images, date and time to acquire the image, and filters to be used. Once the images were acquired, they were calibrated by the automated itelescope systems and made available to us through an FTP server. The calibration procedure utilized dark frames, bias frames, and flat frames to correct for anomalous effects of the optical system and camera used. Pinpoint Astrometry, a plug-in for the popular Maxim DL software, was then used to obtain a plate solution for each image by locating a number of stars in the image and comparing their positions against the Fourth U.S. Naval Observatory CCD Astrograph Catalogue (UCAC4). This procedure is crucial to determine the exact pixel scale and rotation angle of the image which are then used in determination of the star s separations and angles. This information is placed into the FITS header for the image when saved. Even though all of our images were taken on the same telescope with the same camera, we performed this plate solving process on every image that we used to guarantee highest accuracy of our measurements. This process confirmed a pixel resolution of 0.63ʺ/pixel and a camera rotation angle of 272. Each WCS calibrated image was then opened with Mira Pro x64, a software product from Mirametrics, Inc. This software enables making many different photometric measurements of the stars in the image including visual magnitude, absolute position in RA and Dec, and separation in arc seconds, and relative position angles. As we were initially unfamiliar with these star systems, it was also helpful to use star charting software such as The SkyX and Stellarium to verify the

Page 402 Measurements of Multi-star Systems LEO 5 and MKT 13 Figure 3. Example Position Angle and Separation measurement procedure with Mira Pro. appearance of the stars in our systems. These tools allowed us to visually identify the positions of the star pairs within the field of view of our images to quickly begin the process of measuring the stars separations. Using the point and click Distance & Angle function of Mira Pro x64, we measured the position angle and separation of the binary stars. When the first star is clicked upon, Mira calculates the centroid of the star and synchronizes the start of the measurement from that point. Releasing the mouse button on the second star allows the Mira software to locate that star s centroid position and provide the desired measurement from these centroid positions. An example of this process is shown in Figure 3. The software calculates the centroid of each star based on the image data. In most cases, this provides a very accurate location for the star and minimizes the effects of noise. The parameters of this calculation can be adjusted if necessary to account for the size of the stars in the image. In some cases, where the star might be overexposed resulting in blooming, it is possible to disable this centroid measurement and use other methods of pinpointing a star s location. For example, if there are diffraction spikes in the image, these can be used to locate the center of the star. However, for our images, this was not necessary, and we relied on the centroid measurement. Because this measurement is based on the brightness data for many pixels in the star image, it is possible for this centroid calculation to pinpoint a star s location within a fraction of a pixel. This resulted in very accurate measurements even for the faintest stars. After completion of the position angle and separation measurements, the data were placed into an Excel spreadsheet to calculate the mean, standard deviation, and standard error of the mean for each binary star system. Once these were calculated, each measurement was compared to the data available in the Washington Double Star catalog (WDS). This comparison allowed us to confirm that the measurements are being made appropriately and that our data is in agreement with previously published data. If there had been an error in the processing, such as an incorrect image angle or pixel scale, this error would show up in the comparison and let us know that there was a problem. In one case, early in the process of learning to use the Mira software, it was found that the FITS image was inverted due to an improper setting when opening the file. This gave double star angles which were obviously incorrect based on the historical measurements in the WDS. We were then able to go back to verify the mistake and to correct it. Star System LEO 5 [WDS 02191+5422] The AB pair required an additional effort to obtain accurate measurements because of the small ~4.5 arc second separation. Initially, this required adjustment of the contrast stretching of the image in order to identify the two stars. The default stretching performed by Mira Pro x64 caused the two stars to appear as a single star. By adjusting the amount of stretching, and viewing the image as a negative, it was fairly easy to view the 2 stars. Adjustment of the sample radius of the centroid calculation was necessary so that the centroid measurement accurately identified the 2 stars separately rather than combining them together as a single star. Sixteen images were acquired of this system on 2 nights of observing, October 10 th and 21 st of 2015. An example image with the stars labeled is shown in Figure 4. Eight of these images were taken using the H a filter and eight were taken with a luminance filter. Exposure times on the first observing night were varied from 60 seconds to 120 seconds. The H a -filtered images taken on the first night were found to be under-exposed resulting in poor signal-to-noise ratio on 2 of the images. These 2 images were therefore discarded as no measurements could be obtained. On the second night of observations, the exposure times for the H a -filtered images were doubled and ranged from 120 to 240 seconds. The mean, standard deviation, and the standard error of the mean for the separation distance in arc seconds and the angle in degrees were calculated from these data as shown in Table 1. The date is the mean of (Continued on page 404)

Page 403 Measurements of Multi-star Systems LEO 5 and MKT 13 Table 1. Measured Data Results for LEO 5 WDS No. ID Date Observations 02191+5422 LEO 5AB 2015.79 14 PA Sep. Mean 338.53 4.18 Std Dev 1.075 0.333 Std Error 0.287 0.089 Mean 10.07 47.95 02191+5422 LEO 5AC 2015.79 14 Std Dev 0.095 0.073 Std Error 0.025 0.019 Figure 4. Sample Image of LEO 5 with Stars Labeled. Figure 5. Graphical Representation of Historical Data Points for LEO 5 AB Pair. Figure 6. Graphical Representation of Historical Data Points for LEO 5 AC Pair.

Page 404 Measurements of Multi-star Systems LEO 5 and MKT 13 Table 2. Measured Data Results for MKT 13 WDS No. ID Date Observations PA Sep. Mean 346.72 337.97 04287+1552 MKT13AB 2015.79 13 Std Dev 0.435 3.033 Std Error 0.121 0.841 (Continued from page 402) the two observation dates. Historical Data for LEO 5 We requested the historical data from the US Naval Observatory. The data we received, along with our measured data, are shown graphically in Figures 5 and 6. Discussion of Results for LEO 5 Our data agreed well with the historical data and the calculated standard deviation indicates that our measurements were accurate. The historical trend of the measured data does not provide enough information to draw conclusions about whether these star pairs are physical doubles or not. A search of other databases did not yield any additional information about these stars. Star System MKT13 [WDS 04287+1552] This is a quintuple star system with each of the A and B stars being, themselves, binary pairs with known orbital data. The orbital parameters are available from the Sixth Catalog of Orbits of Visual Binary Stars. As mentioned earlier, the Aa pair and the Bb binary pairs are too close for us to separate using the observing techniques we employed. In addition, while the A and B stars are very visible with magnitudes of 3.41 and 3.94, respectably, the C star in this system is much dimmer with a magnitude of 11.96. Because of this large variation in visual magnitude, we were unable to measure the separation and angle for the AC pair. We were able to make 13 measurements from the images acquired. From these data, we calculated the mean, standard deviation, and the standard error of the mean for the separation distance in arc seconds and the position angle in degrees. These are shown in Table 2. The date observed is the mean of the two observation dates. There were seven and six observations on the first and second nights, respectively. Historical Data for MKT 13 We requested the historical data from the US Naval Observatory. The data we received are shown in Figure 7. Because of the large number of historical data points received (42), we chose to plot the angle and separation vs. observation date in order to look for trends in the data. Discussion of Results for MKT 13 From the graphed data, there does appear to be a trend in the position angle of this pair. A linear fit gives a trend of about 4.7 millidegrees per year with an Figure 7. Graph of Historical Data Points for MKT 13 AB.

Page 405 Measurements of Multi-star Systems LEO 5 and MKT 13 R 2 value of 0.54. The separation appears to be decreasing very slowly but a trend in this data is uncertain. A linear fit to the trend for the separation measures about 3.6 milliarcseconds per year with an R 2 value of 0.04. Acknowledgements We would like to thank Russell Genet for his assistance and guidance which allowed us this opportunity to do research and for introducing our team to the study of binary stars. Additionally, we thank the Boyce Research Initiatives and Education Foundation (B.R.I.E.F.) for their instructional support and financial donation that allowed us to use the itelescope robotic telescope system and the Maxim DL Pro 6 and Mira Pro x64 software tools. This research made extensive use of the Washington Double Star catalog maintained by the U.S. Naval Observatory. References Genet, R. M., Johnson, J. M., Buchheim, R., and Harshaw, R. 2015. Small Telescope Astronomical Research Handbook. In preparation. Hartkopf, W.I. and Mason, B.D 2006, Sixth Catalog of Orbits of Visual Binary Stars. US Naval Observatory, Washington. http://www.usno.navy.mil/usno/ astrometry/optical-ir-prod/wds/orb6 Mason, B. and Hartkopf, W. USNO CCD Astrograph Catalog (UCAC), March 2011. Astrometry Department, U.S. Naval Observatory. http:// www.usno.navy.mil/usno/astrometry/optical-irprod/ucac. Mason, B. and Hartkopf, W. The Washington Double Star Catalog, October 2015. Astrometry Department, U.S. Naval Observatory. http:// ad.usno.navy.mil/wds/wds.html. Stelle Doppie Double Star Database Search Engine, http://stelledoppie.goaction.it

Page 406 GJ 282 AB (WDS 07400-0336 AB = BGH 3 AB) and GICLAS 112-29: A Very Wide System in Process of Dissociation F. M. Rica 1, R. Benavides 2 1 Astronomical Federation of Extremadura, C/José Ruíz Azorín, 14, 4º D, Mérida E-06800, Spain email: frica0@gmail.com 2 Astronomical Observatory of Posadas ( J53 MPC code), Posadas E-14730, Spain Abstract: Very wide binaries are interesting objects that shed light on the binary formation process and their dynamical evolution. Poveda et al. (2009) studied the possible physical relation of the near (14.2 pc) and wide (~58 ) binary star GJ 282 AB and the extremely wide (1.09º; ~55,000 AU) companion, NLTT 18149, and they concluded that this very wide system is in the process of dynamical disintegration. In this work, we confirm the same conclusion but using a different method. We first study dynamically GJ 282 AB, confirmed that it is a bound system and then we determine possible orbital solutions. Later, we calculate the relative velocity of NLTT 18149 with respect to the GJ 282 AB s center mass using their (U, V, W) galactocentric velocity. The relative velocity, V rel = 1.98 ± 0.16 km s -1, is much larger than the escape velocity (0.25 ± 0.01 km s -1 ). Therefore, with a significance level of 11, we also conclude that this very wide system is in a process of dynamical disintegration. 1. Introduction The very wide binaries after formation are subject to dynamical process that causes their evolution. In environments with high or moderate stellar density, most pairs with separations of a few hundreds to a few thousands AU are disintegrated (that is, disrupted) within a few million years (Parker et al. 2009). In the stars field, outside of these high density environments, Galactic tides and weak interactions with passing stars disrupt binary stars with separations of a few times 10,000 AU on a time scale of about 10 Gyr (Heggie 1975; Weinberg et al. 1987). Recently, astronomers discovered that stars of disrupted binaries don t quickly leave the binary environment but escaping stars drift apart with low relative velocity and remain within the Jaboci radius during millions or tens of millions of years. In order to study the process of dissociation of very wide systems, Poveda et al. (2009) presented the very wide and nearby system GJ 282 AB NLTT 18149 as the most interesting object in his very wide common proper motion binary search. GJ 282 AB is a wide pair (~58 arcsec) composed by two red stars of 7.20 and 8.87 magnitudes at 14.2 pc of distance. The high common proper motion, common radial velocity, and common age strongly suggest a bound nature for AB. NLTT 18149 (= Giclas 112-29) is a red dwarf star located at 1.09 deg (0.27 pc) of separation to GJ 282 AB. Its common distance, common age, common proper motion, common radial velocity to GJ 282 AB strongly suggest possible physical relation. Poveda et al. (2009) concluded that the system GJ 282 AB NLTT 18149 is in the process of dynamical disintegration. The large physical separation of very wide binaries such as these is larger than the isolate stars formation regions. Astronomers think that these systems can only form during the dissolution phase of open clusters of low density (Kouwenhoven et al. 2010). The main objective of this work is to confirm the bound status of GJ 282 AB and the dynamical disintegration status of GJ 282 AB NLTT 18149. The organization of this paper is as follows. In Section 2, we detail the characteristic of the AB pair, the

Page 407 GJ 282 AB (WDS 07400-0336 AB = BGH 3 AB) and GICLAS 112-29: A Very Wide System Figure 1. Historical position angle, of GJ 282 AB and its evolution with time. We determined a very significant change of +0.0090 ± 0.0004 deg yr -1 new astrometric measures performed, the dynamic study and the orbital calculation. In Section 3, we present the very wide component, the calculus of the characteristics of the mass center and the study of the possible physical relation of C with respect to AB. 2. The Close System GJ 282 AB S. van den Bergh in 1949 discovered, using the photographic technique with astrograph, two red stars with high common proper motions. This object was catalogued as GJ 282 AB, a wide pair (~58 arcsec, 825 UA) listed as WDS 07400-0336 AB ( = BGH 3 AB) in the Washington Double Star Catalog (hereafter WDS). It is composed of two young stars of 7.20 (K2V) and 8.87 (K6/7V) magnitudes at 14.2 pc of distance The high common proper motion, common radial velocity, and common age strongly suggest a bound nature for AB. To confirm this bound status, we study the relative motion of B component with respect to A by weighted linear fits using d /dt, d /dt, dx/dt, and dy/dt plots (see Figures 1 and 2). The WDS catalog lists 27 astrometric measures from 1890 to 2003 and was kindly provided by Brian Mason. We assign initial weights for astrometric measures using a data-weighting scheme and process based on Rica et al. (2012). To confirm the bound status, we study the relative motion of B component with respect to A by weighted Figure 2. Historical distance, of GJ 282 AB and its evolution with time. We determined a change of -0.0021 ± 0.0005 arcsec yr -1. linear fits using d /dt, d /dt, dx/dt, and dy/dt plots (see Figures 1 and 2). The WDS catalog lists 27 astrometric measures from 1890 to 2003 and was kindly provided by Brian Mason. We assign initial weights for astrometric measures using a data-weighting scheme and process based on Rica et al. (2012). In this work, we add two more astrometric measures to the WDS for epochs 2010.5589 and 2014.131 using the catalogs WISE and URAT1 (Zacharias et al. 2015). In addition to this, Rafael Benavides used a f/10 Celestron telescope of 0.3 m with a ASCOM QHY9 CCD camera, to take 5 CCD images of 0.6 seconds of exposition on 2015 February 8 th. The telescope is located at the Posadas Observatory (Córdoba, Spain) with the MPC code J53. The pixel size of the camera was of 5.4 m (0.86" in the focal plane). We use Astrometrica 4.8.2 for the calibration and astrometric process. All the astrometric measures, with a time baseline of 125 years, are listed in Table 1. This table lists, from the left to right, the observational epoch, the position angle (2000 equinox), and distance as listed in WDS in the three first columns. The number of nights (N), the reference (as used in WDS), the aperture of the telescope (in meters), the observational technique (as listed in WDS), the weights assigned to and, and the O C residuals are also listed. The United State Naval Observatory (USNO) per-

Page 408 GJ 282 AB (WDS 07400-0336 AB = BGH 3 AB) and GICLAS 112-29: A Very Wide System Table 1. Astrometric data, weights and residuals for the linear trend of GJ 282 AB Date º " N Ref. Ap Tec w w O-C O-C " 1890.600 112.1 57.623 2 WFD1906b 0.2 T 0 9 1.10-0.49 1893.200 111.0 57.963 1 WFC1998 0.3 Pa 20 22-0.04-0.14 1894.180 110.7 57.799 1 WFC1998 0.3 Pa 20 22-0.35-0.30 1903.500 111.8 59.240 4 WFD1940 0.2 T 3 0 0.62 1.16 1933.500 111.6 57.654 1 WFC1945b 0.1 Pa 20 22 0.00-0.37 1946.000 112.2 58.200 1 Bgh1958 0.1 Pa 20 32 0.42 0.21 1968.650 112.1 57.943 4 WFC1992 0.2 Pa 79 86 0.01-0.01 1970.235 112.1 57.943 1 USN1974 0.7 Po 6596 16020 0.00 0.00 1970.238 112.1 57.935 1 USN1974 0.7 Po 6596 16020 0.00-0.01 1970.915 112.1 57.957 1 USN1974 0.7 Po 6596 16020-0.01 0.01 1971.174 112.1 57.943 1 USN1974 0.7 Po 6596 16020 0.01 0.00 1971.185 112.1 57.947 1 USN1974 0.7 Po 6596 16020 0.00 0.00 1971.185 112.1 57.940 1 USN1974 0.7 Po 6596 16020-0.01 0.00 1975.876 112.2 57.919 1 USN1978 0.7 Po 3298 8010-0.02-0.01 1975.876 112.2 57.917 1 USN1978 0.7 Po 6596 8010-0.01-0.02 1976.092 112.2 57.932 1 USN1978 0.7 Po 6596 16020 0.00 0.00 1976.155 112.2 57.946 1 USN1978 0.7 Po 6596 16020-0.01 0.01 1976.155 112.2 57.928 1 USN1978 0.7 Po 6596 16020 0.00 0.00 1976.158 112.2 57.928 1 USN1978 0.7 Po 6596 16020 0.00 0.00 1976.158 112.2 57.933 1 USN1978 0.7 Po 6596 16020 0.01 0.00 1981.200 112.3 58.011 2 WFC1999 0.2 Pa 56 61 0.03 0.09 1985.960 112.6 58.105 4 WFC1994 0.2 Pa 79 86 0.26 0.19 1987.800 112.8 58.340 4 WFD1985 0.2 T 6 6 0.44 0.43 1991.850 112.5 57.920 1 TYC2002 0.3 Ht 79 86 0.08 0.02 1998.860 112.7 57.960 1 TMA2003 1.3 E2 99 108 0.18 0.07 2000.102 112.6 57.974 6 UC_2013b 0.2 Eu 40 43 0.07 0.09 2003.068 113.0 58.260 1 Arn2003e 0.2 Mg 3 2 0.43 0.38 2010.559 112.7 57.710 1 WISE 0.4 Hw 123 123 0.02-0.15 2014.131 112.7 57.900 1 URAT1 0.2 E 1111 1111 0.01 0.05 2015.108 112.79 57.85 1 Benavides 0.3 C 400 400 0.12 0.00

Page 409 GJ 282 AB (WDS 07400-0336 AB = BGH 3 AB) and GICLAS 112-29: A Very Wide System Table 2. Positional, Dynamical, and Kinematic Parameters for GJ 282 AB. Mean Epoch 1990.000 (deg) for mean epoch 112.445 ± 0.007 (arcsec) for mean epoch 57.904 ± 0.009 x (AU) [East-West] +763 ± 14 y (AU) [North-South] -315 ± 6 d /dt (mas yr -1 ) -2.06 ± 0.51 d /dt (deg yr -1 ) +0.0090 ± 0.0004 dx/dt (mas yr -1 ) -5.31 ± 0.53 dy/dt (mas yr -1 ) -7.65 ± 0.41 Vx (km s -1 ) [East-West] -0.36 ± 0.04 Vy (AU) [North-South] -0.52 ± 0.03 Vz (km s -1 ), radial velocity -0.1 ± 0.2 Vtot (km s -1 ) 0.67 ± 0.04 Vesc_max (km s -1 ) 1.74 ± 0.05 Mass of A (Msun) 0.80 ± 0.05 Mass of B (Msun) 0.65 ± 0.05 Distance (pc) 14.3 ± 0.3 formed a very accurate series (root mean square, RMS, of ~0.01º and ~0.01 for position angles and distances) of astrometric measures using the Alvan Clark 0.7 m refractor telescope. For the observing condition, the correction of relative astrometry for atmospheric refraction is negligible for position angle (< 0.01º) but significant (+0.02 ) for the USNO distances. We correct for atmospheric refraction in the USNO distances. Our dynamic study shows that the angular separation decreases about 2.06 ± 0.51 mas yr -1 while the position angle clearly increases 0.0090 ± 0.0004 deg yr -1. The total relative motion (9.3 ± 0.5 mas yr -1 ) has a significance of 13, therefore we can reject the nonmotion hypothesis. The positional, dynamical, and kinematical parameters for the linear fit are shown in Table 2. The RMS of this fit is 0.02º and 0.013 and the mean absolute, MA, 0.01º and 0.007. The RMS gives the mean spread of the measures with respect to the mean. And the MA gives the uncertainty of the near future ephemerids. The adopted values for the stellar masses are 0.80 and 0.65 solar mass. The total relative velocity of B with respect to A is 0.67 ± 0.04 km s -1 much smaller than the upper limit of the escape velocity (1.74 ± 0.05 km s -1 ). By using the work of Winsberg et al. (1987) about dynamic evolution, we can conclude that GJ 282 AB is immune to external perturbations (gravitational binding energy of -8.8 x 10-42 ergs) and that is a high common proper motion, common distance, common age binary, composed by stars gravitationally bound. We determined orbital solutions for GJ 282 AB using the method of orbital calculation presented by Hauser & Marcy (1999). This method only needs instant position (x, y, z) and velocity vectors (V x, V y, V z ) in addition to a parallax and stellar masses to obtain a family of orbits depending on z (the line-of-sight position of the component). The input parameters are those of Table 2. The only unknown input data is the z parameter. We constrained the value of z following the procedure in Hauser & Marcy (1999) and one orbit for each value of z is obtained. We study the empirical distribution of r (in arcsecond) as a function of. For this task, we select about 300 grade 1-2 orbital solutions from the Sixth Catalog of Orbits of Visual Binary (Hartkopf & Mason 2003), calculate the ephemerides for and r for different epochs. The comparison between and r give us the distribution of r as a function of s. We see that the values for r/ are highly dependent on the orbital inclination (see Figure 3). For highly-inclined orbits, the 3D effect is greater and therefore we could find r-values much greater than. Figure 4 shows the cumulative distribution. Table 3 shows same numbers (quartiles, percentiles, mean, median, etc.) about the distribution of r/. The median happens for r/ = 1.11 (that is, 50% of possible orbital solutions have values of r/ from 1.0 to 1.11). If we center over the median, 50% of the orbital solutions ranges from 1.02 to 1.38 (from 1.00 to 1.38 for the 75% of the possible orbital solutions). Finally, the 90% of possible orbital solutions have r/ 2.0 approximately. Only the high-inclined orbits have greater Table 3. Statistics for the r/ Distribution Name Mean Minimum Maximum Q10 Quartile1 Median Quartile3 Q90 r/ 1.40 1.00 17.14 1.00 1.02 1.11 1.38 1.96 (Continued on page 411)

Page 410 GJ 282 AB (WDS 07400-0336 AB = BGH 3 AB) and GICLAS 112-29: A Very Wide System Figure 3. The relation of r/ with the orbital inclination (in degrees). Figure 4. Cumulative distribution of r/s in AU (or r/ in arcseconds).

Page 411 GJ 282 AB (WDS 07400-0336 AB = BGH 3 AB) and GICLAS 112-29: A Very Wide System (Continued from page 409) values. The maximum value is 17.14. Table 4 lists orbital solutions for different values of the radius-vector (r) chosen in function of the empirical distribution of r (in arcsecond) in function of. An orbital solution for the minimum value of the radiusvector, r = s (that is z = 0 AU) is shown. In the 50th percentile of the distribution of r in function of s, r = 1.11s (z = ± 396 UA) and in the 75th percentile, r = 1.38s (z = ± 783 UA) two orbital solutions. Therefore, in this table is represented the 75% range of possible orbital solutions. Figure 5 shows orbital solutions for the AB components calculated in this work. The thick black ellipse is the orbital solution for z = +396 UA (when r = 1.11 s, the median value) while the dash ellipse is for z = -396 UA. The legends in the inner box are self-explicative. The possible regions ( zone possible in the inner box) of possible orbital solutions cover the 90% of the confidence interval for z parameter. 3. The Very Wide Companion NLTT 18149 Giclas 112-29 (= NLTT 18149) is a red dwarf (M1.5V) star located at 1.09 deg of separation to GJ 282 AB. Its common distance, common age, common proper motion, and common radial velocity to GJ 282 AB strongly suggest a possible physical relation: It is not listed in WDS. Poveda et al. (2009) concluded that the system GJ 282 AB NLTT 18149 is in the process of dynamical disintegration. They determined that the perspective effect for the wide pair and the orbital motion of GJ 282 AB cannot explain the large difference in proper motion between GJ 282 and NLTT 18149. In this work, we want to confirm the dynamical disintegration status of GJ 282 AB NLTT 18149 by the Table 4. Computed Orbital Parameters COMPUTED ORBITAL PARAMETERS FOR WDS 07400-0336 = BGH 3 AB WITH r = s r = 1.11 s and r = 1.38 s Parameter -783 AU -396 AU 0 AU +396 AU +783 AU P (yr) 15000 10172 8493 10172 15000 T (yr) 9259 6728 5776 6365 8274 e 0.651 0.724 0.761 0.742 0.681 a (arcsec) 48.4 37.4 33.2 37.4 48.4 a (AU) 688.4 531.3 471.2 531.3 688.4 i (deg) 45.7 29.0 9.4 25.8 43.6 (deg) 72.8 60.6 355.9 270.2 260.0 (deg) -135.6-127.8-67.6 15.9 25.6 q (AU) 240.18 146.52 112.74 136.93 219.31 study of the relative velocity of NLTT 18149 with respect to the center of mass of GJ 282 AB (CM AB ). To determine the properties (AR and DEC, proper motion and radial velocity) for CM AB, we assign weights to the A and B members in function of the stellar masses, as in Kiselev, Romanenko & Gorynya (2009). The values for the weights are p A = 0.55 and p B = 0.45 for A and B components respectively. The adopted values for the stellar masses are 0.80 and 0.65 solar mass for A and B components. In 1991.25, the CM AB has an offset of 23.42 East and 9.66 South to GJ 282 A. To obtain the (AR, DEC) coordinate for CM AB in this epoch, we use the Hipparcos coordinate for GJ 282 A and the offset determined previously. For the proper motion and radial velocity of CM AB, we calculate the weighted mean of the values for A and B using the weights p A and p B. We assume that the CM AB is at the same distance that the A component. The (U, V, W) galactocentric velocities were calculated following the work of Przybylski (1962). We calculate the relative velocity of NLTT 18149 with respect to the CM AB from the difference of their (U, V, W) velocities: V rel U U V V W W 2 2 2 C CMab C CMab C CMab The positional, kinematical, and dynamical data of the stellar components and the CM AB are listed in Table 5. The relative velocity (V rel ) obtained using formula (1) is 1.98 ± 0.16 km s -1. We determined the errors using a Monte Carlo approach with Gaussian errors for the input data. From the Tycho-2, 2MASS and URAT1 AR and DEC coordinates of the three components, we determine the relative position of C with respect to CM AB : (1) (Continued on page 413)

Page 412 GJ 282 AB (WDS 07400-0336 AB = BGH 3 AB) and GICLAS 112-29: A Very Wide System Figure 5 Orbital solutions for the AB components calculated in this work. The legends in the inner box are selfexplanatory. The possible regions ( zone possible in the inner box) of possible orbital solutions cover the 90% if the confidence interval for z parameter. Table 5. Data for the Stellar Components and the CM AB A Component B Component CM AB C Component 2000 for 1991.25 07h 39m 59.29s... 07h 40m 00.85s 07 36 07.06 2000 for 1991.25-03º 35' 48.6"... -03º 35' 58.26" -03 06 36.6 (mas yr -1 ) 2) +71.7 ± 1.2 +66.8 ± 1.3 +69.5 ± 0.9 +36.3 ± 1.6 (mas yr -1 ) 2) -276.1 ± 1.3-286.2 ± 1.4-280.5 ± 1.0-253.5 ± 0.8 V rad (km s -1 ) 1) -21.8 ± 0.2-22.0 ± 0.2-21.9 ± 0.2-22.7 ± 0.2 Parallax (mas) 3) 70.37 ± 0.64... 70.37 ± 0.64 70.55 ± 1.64 U (km s -1 )...... +28.12 ± 0.15 +27.59 ± 0.15 V (km s -1 )...... +0.13 ± 0.13 +1.28 ± 0.13 W (km s -1 )...... -8.22 ± 0.03-9.34 ± 0.03 1) Poveda et al. (2009); 2) Tycho-2 catalog; 3) Hipparcos

Page 413 GJ 282 AB (WDS 07400-0336 AB = BGH 3 AB) and GICLAS 112-29: A Very Wide System (Continued from page 411) Tycho-2: 296.649 ± 0.001º and 3899.61 ± 04 (1991.78) 2MASS: 296.652 ± 0.001º and 3899.81 ± 0.08 (1998.865) URAT1: 296.650 ± 0.001º and 3899.88 ± 0.06 (2014.05) The errors in the relative measures were determined using the (AR, DEC) astrometry uncertainties listed in the Tycho-2, 2MASS and URAT1 catalogs. At the distance of this system, the angular separation corresponds to a projected physical separation (s) of 55,345 UA (= 0.268 pc). So s is the lower limit of radius-vector (r) which allows us to calculate an upper limit for the escape velocity (V esc_max ) of 0.25 ± 0.01 km s -1. The binding energy for GJ 282 AB NLTT 18149 is -2.0x10 41 ergius and in the Fig. 15 and 16 of Close et al. (2007) we can see that there is no binary with such as low binding energy. And in his Fig. 17, our very wide system is located in the field unstable region. Weinberg, Shapiro and Wasserman (1987) studied the dynamical evolution and survival probability of very wide binaries. GJ 282 AB NLTT 18149 has a binding energy between the curves for a o = 0.063 pc (-2.7x10 41 ergius) and a o = 0.16 pc (-1.1x10 41 ergius) in their Fig. 6, therefore the probability of survival at the age of the system (300-500 Myr) is about 80%. But our result shows that V rel > V esc_max with a significance of nearly 11. Trigonometric parallax listed in Hipparcos catalog for the A and C components yield greater values for r and therefore smaller values for V esc reinforcing our conclusion. Our result confirms that GJ 282 AB NLTT 18149 is in the process of gravitational dissociation with significance of at least 11. Acknowledgements This publication makes use of data products from the Wide-field Infrared Survey Explorer (WSIE), which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This research has made use of the Washington Double Star Catalog maintained at the U.S. Naval Observatory and the Simbad database operated at CDS, Strasbourg, France. References Close. L. M. et al., 2007, ApJ, 660, 1492 Gaidos E. et al., 2014, MNRAS, 443, 2561 Hartkopf W. I., Mason B. D., 2003, Sixth Catalog of Orbits of Visual Binary Stars, U.S. Naval Observatory, Washington, http://ad.usno.navy.mil/wds/ orb6.html Hauser, H. M. and Marcy, G. W., 1999, PASP, 111, 321. Heggie, D. C. 1975, MNRAS, 173, 729 Kordopatis G. et al., 2013, AJ, 146, 134 Kiselev, A. A.; Romanenko, L. G.; Gorynya, N. A., 2009, ARep, 53, 1136 Kouwenhoven, M. B. N. et al. 2010, MNRAS, 404, 1835 Parker, R. J., Goodwin, S. P., Kroupa, P., & Kouwenhoven, M. B. N. 2009, MNRAS, 397, 1577 Poveda A., Allen C., Costero R., Echevarría J., & Hernández-Alcántara A., 2009, ApJ, 706, 343 Przybylski, A., 1962, PASP, 74, 230 Rica F. M., Barrena R., Vázquez G., Henríquez J. A., Hernández F., 2012, MNRAS, 419, 197 Takeda G., Ford E. B., Sills A., Rasio F. A., Fischer D. A., Valenti J. A., 2007, ApJS, 168, 297 Weinberg, M.D., Shapiro, S.L., and Wasserman, I., 1987, ApJ, 312, 367 Zacharias, N. et al., 2015, AJ, 150, 101

Page 414 Opportunities for Student Astronomical Research in Southern California Workshop on Sunday, June 12, 2016 Presented by InStAR The Institute for Student Astronomical Research http://in4star.org inst4star@gmail.com Hosted by BRIEF Boyce Research Initiatives and Education Foundation http://www.boyce-astro.org info@boyce-astro.org At The San Diego Hilton Bay Front Hotel Meet and Greet -- 11:00 to 12:30 No host brunch gathering at the Fox Sports Grill at the Hilton Meeting -- 12:30 to 5:00 in the Cobalt Room Here are some of our experienced speakers and the topics we will cover: Dr. Russ Genet, past President of the Astronomy Society of the Pacific Bob Buchheim, President of the Society for Astronomical Sciences (SAS) Dr. John Kenney, Chair of the Astronomy and Physics Department of Concordia University and more to be announced at our website soon. Overview of small telescope research opportunities for amateurs, professionals and students The Astronomy Research Seminar - its importance, history and future as a key STEM component The astronomy community and its connections to SAS, AAVSO, schools and universities How to publish your seminar student research through InStAR and Collins Foundation Press InStAR and BRIEF resources provided for schools, instructors and students nationwide Student experiences and outcomes - lessons learned and impact on their careers Expansion of the astronomy community, seminar, resources and research areas Q&A - How to start the seminar at your school and tailor it to your school's needs and programs For more information and to sign up for this free workshop, go to Research Opportunities Workshop. http://in4star.org/instar-events/san-diego-opportunities-workshop-june-12-2016/