Journal of Double Star Observations

Transcription

1 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 AB = BGH 3 AB) and GICLAS : 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, 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,

2 Page 308 Astronomical Association of Queensland Program of Measurements of Seven Southern Multiple Stars Graeme Jenkinson Astronomical Association of Queensland. 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 Slow movement HO554A-B Oph Definite change in PA HO554A-C Oph Possible increase in sep. I 428 Circinus No probable movement I 1282 Scorpius Definite change in PA SEE114A-B Antlia Changes since 1 st measure SEE234 Lupus Little change * Epochs of new measures given in Besselian years as the average of the observations making up the measure.

3 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, V Napier-Munn, T. J. and Jenkinson, G. 2009, "Measurement of Some Neglected Southern Multiple Stars in Pavo", Webb Society Double Star Section Circular 17, 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, Argyle, Bob, 2004, Observing and Measuring Visual Double Stars, Springer Table 2. Measurements of B 2350 B2350 RA DEC Last Measure 1999 Libra MAG. 6.8 & 12.5 PA SEP. 9.3" Date No. images PA Sep" 19 Apr Apr Apr Apr May May May Mean Standard dev % CI +/ P(t) movement 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 DEC Last Measure 1999 Ophiuchus MAG & PA SEP. 35.3" Date No. images PA Sep" 27 June June June July July July July Mean Standard dev % CI +/ P(t) movement COMMENTS: A small increase in separation may have occurred in the last 15 years.

4 Page 310 Measurements of Seven Southern Multiple Stars Table 4. Measurements of I 428 I 428 RA DEC Last Measure 2000 Circinus MAG. 5.8 & 11.6 PA SEP. 11.0" Date No. images PA Sep" 18 Apr Apr Apr Apr Apr May May Mean Standard dev % CI +/ P(t) movement COMMENTS: No probable movement in the last 14 years. Table 5. Measurements of I 1282 I 1282 RA DEC Last Measure 1998 Scorpius MAG & 13.0 PA SEP. 12.1" Date No. images PA Sep" 25 May June June June June June June Mean Standard dev % CI +/ P(t) movement COMMENTS: Definite movement in PA, small increase in separation possible.

5 Page 311 Measurements of Seven Southern Multiple Stars Table 6. Measurements of SEE 114 AB SEE114 A-B RA DEC Last Measure 1999 Antlia MAG. 6.0 & 12.8 PA SEP. 47.3" Date No. images PA Sep" 28 Feb Mar Mar Mar Mar Mar April Mean Standard dev % CI +/ P(t) movement COMMENTS: Considerable increase in separation since the first measure of 23.6" in Position angle has also increased from 283 at that time. Table 7. Measurements of SEE 234 SEE234 RA DEC Last Measure 1999 LUPUS MAG. 6.1 & 12.5 PA SEP. 13.0" Date No. images PA Sep" 25 Apr May May May May May June Mean Standard deviation % CI +/ P(t) movement COMMENTS: Very slow changes since the first measure in 1897 of 31 and 14.0"

6 Page 312 Measurements of Seven Southern Multiple Stars Table 8. Measurements of HO 554 AB HO554A-B RA DEC Last Measure 1904 Ophiuchus MAG. 7.9 & 12.9 PA SEP. 9.8" Date No. images PA Sep" 27 June June June July July July July Mean Standard deviation % CI +/ P(t) movement COMMENTS: Definite movement in PA and negligible change in separation in the last 110 years.

7 Page 313 Astronomical Association of Queensland Program of Measurement of Nine Neglected Southern Multiple Stars Graeme Jenkinson Astronomical Association of Queensland 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 ICX x582 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 to 0.978, with a mean figure of " 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 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

8 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 ± 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, V Napier-Munn, T. J. and Jenkinson, G. 2009,"Measurement of Some Neglected Southern Multiple Stars in Pavo", Webb Society Double Star Section Circular 17, 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, 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 Possible small PA change SEE98 Puppis Little evident movement B2659 Pyxis Large apparent movement B2263 Vela Considerable movement CPO327 Centaurus Movement RST3746AB Cen Clear movement ARA1790 Corvus Questionable Sep. change RSS370 Lupus Possible small PA RSS386 TrA Questionable PA change * Epochs of new measures given in Besselian years as the average of the observations making up the measure.

9 Page 315 Measurement of Nine Neglected Southern Multiple Stars Table 2. Measurements of BU 1419 BC. RA DEC Last Measure 1903 BU1419BC MAG & Puppis PA SEP. 7.8" 13.0 Date No. images PA Sep" 16 January January January January February February February Mean Standard dev % CI +/ P(t) movement COMMENTS: Possible slight movement in PA over the last 112 years. Table 3. Measurements of HO 554 AC. SEE98 RA DEC Last Measure 1928 Puppis MAG. 6.7 & 12.7 PA. 67 SEP. 5.9" Date No. images PA Sep" 6 January January January January January January January Mean Standard dev % CI +/ P(t) movement COMMENTS:Little movement evident since 1929.

10 Page 316 Measurement of Nine Neglected Southern Multiple Stars Table 4. Measurements of B RA DEC Last Measure 1932 B2659 MAG. 7.7 & Pyxis PA SEP. 8.0" 13.2 Date No. images PA Sep" 17 January January January February February February February Mean Standard dev % CI +/ P(t) movement COMMENTS: Large apparent movement in both axes since the only previous measurement in 1932 warrants further investigation. B2263 Vela Table 5. Measurements of B RA DEC Last Measure 1932 MAG. 7.8 & 13.0 PA SEP. 7.0" Date No. images PA Sep" 17 January January February February February February February Mean Standard dev % CI +/ P(t) movement COMMENTS: Poor seeing on 21 February 2015 results deleted from calculation of mean. Considerable movement apparent since the only previous measure in 1932.

11 Page 317 Measurement of Nine Neglected Southern Multiple Stars Table 6. Measurements of CPO 327. CPO327 RA DEC Last Measure 1930 Centaurus MAG. 8.0 & 12.8 PA SEP. 7.6" Date No. images PA Sep" 21 February February March March March March March Mean Standard dev % CI +/ P(t) movement COMMENTS: Increase in PA and decrease in separation appear consistent with the two previous measures in 1902 and Table 7. Measurements of RST 3746 AB. RST3746AB RA DEC Last Measure 1944 CENTAURUS MAG & 11.5 PA SEP. 16.0" Date No. images PA Sep" 21 February February March March March March March Mean Standard dev % CI +/ P(t) movement COMMENTS: Changes in PA & separation consistent with two previous measures in 1937 & 1944.

12 Page 318 Measurement of Nine Neglected Southern Multiple Stars Table 8. Measurements of ARA ARA 1790 RA DEC Last Measure 1922 Corvus MAG. 8.8 & 11.1 PA SEP. 11.3" Date No. images PA Sep" 16 April April April April April April April Mean Standard dev % CI +/ P(t) movement 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 DEC Last Measure 1976 Lupus MAG & -- PA SEP. 7.2" Date No. images PA Sep" 14 April April April April April May May Mean Standard dev % CI +/ P(t) movement COMMENTS: Possible small increase in PA since the only previous measure in 1976.

13 Page 319 Measurement of Nine Neglected Southern Multiple Stars Table 10. Measurements of RSS 386. RSS 386 RA DEC Last Measure 1974 Triangulum Aust. MAG. 8.6 & 12.0 PA. 270 SEP. 10.3" Date No. images PA Sep" 16 April April April April May May May Mean Standard dev % CI +/ P(t) movement COMMENTS: No change in separation makes large change in PA questionable over the last 41 years.

14 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 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 = 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

15 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 Mason B.D. et al: 2001, Astron. J., 122, Zacharias N. et al: 2013, Astron. J., 145, 44Z 5. Figure 2. Standard errors in positional angle (left) and separation vs separation.

16 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 Table 1 continues on next page.

17 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 Table 1 continues on next page.

18 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 Table 1 continues on next page.

19 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 ** ** Table 1 concludes on next page.

20 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 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.

21 Page 327 Jonckheere Double Star Photometry Part II: Delphinus Wilfried R.A. Knapp Amateur visual double star astronomer Vienna, Austria 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 Photometry For each of the listed J-objects one single image was taken (in Bessel epoch ) 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 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 m 1` 2 Buchheim, Robert, 2008, "CCD Double-Star Measurements at Altimira Observatory in 2007", Journal of Double Star Observations, 4,

22 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, 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 v 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 WDS J1 AB 20:32: :44: WDS J3 AB 20:31: :50: WDS J135 AB 20:15: :02: WDS J142 AB 20:34: :37: WDS J156 AB 20:40: :50: WDS J157 AB 20:55: :34: WDS J191 AB 20:40: :37: WDS J192 AB 20:42: :00: WDS J193 AB 20:42: :21: WDS J194 AB 20:49: :24: WDS J194 AB,C 20:49: :24: WDS J195 AB 20:50: :06: WDS J284 AB 21:03: :53: WDS J510 AB 20:29: :11: WDS J553 AB 20:18: :54: WDS J559 AB 20:27: :48: WDS J562 AB 20:31: :46: WDS ROE14 AB 20:31: :48: WDS J563 BC 20:31: :48: WDS J566 AB 20:35: :32: WDS J572 AB 20:52: :26: WDS J573 AB 20:53: :22: WDS J604 AB 20:15: :42: WDS J605 AC 20:52: :26: WDS J605 AB 20:52: :26: WDS J607 AB 20:57: :00: WDS J790 AB 20:34: :56: WDS J797 AB 21:05: :49: WDS J837 AB 20:19: :03: WDS J838 AB 20:21: :28: Table 1 continues on next page.

23 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 WDS J839 AB 20:23: :10: WDS J840 AB 20:24: :23: WDS J841 AB 20:24: :08: WDS J841 AB.C 20:24: :08: WDS J842 AB 20:24: :51: WDS J844 AB 20:30: :53: WDS J845 AB 20:43: :12: WDS J846 AB 20:54: :02: WDS J912 AB 20:39: :09: WDS J1073 AB 20:38: :16: WDS J1173 AB 20:20: :31: WDS J1234 AB 20:15: :56: WDS J1241 AB 20:28: :44: WDS J1242 AB 20:38: :18: WDS J1243 AB 20:30: :54: WDS J1296 AB 20:14: :17: WDS J1297 AB 20:27: :44: WDS J1318 AB 20:55: :35: WDS J1342 AB 20:24: :05: WDS J1343 AB 20:27: :11: WDS J1344 AB 20:34: :20: WDS J1345 AB 20:43: :39: WDS J1346 AB 20:56: :35: WDS J1704 AB 20:26: :11: WDS J1715 AB 20:58: :23: WDS J1716 AB 20:59: :43: WDS J1879 AB 20:16: :02: WDS J1879 AC 20:16: :02: WDS J1880 AB 20:17: :04: WDS J1883 AB 20:30: :20: WDS J1884 AB 20:31: :50: WDS J1885 AB 20:31: :47: WDS J1887 AB 20:35: :13: WDS J1888 AB 20:43: :53: WDS J1889 AB 20:44: :31: WDS J1890 AB 20:48: :50: WDS J2192 AB 20:36: :15: WDS J2313 AB 20:30: :29: WDS J2314 AB 20:32: :52: WDS J2314 AC 20:32: :52: WDS J2319 AB 20:41: :12: WDS J2321 AB 20:48: :11: WDS J2325 AB 20:51: :36: WDS J2572 AB 20:23: :28: WDS J2573 AB 20:32: :29: Table 1 concludes on next page.

24 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 WDS J2575 AB 20:41: :05: WDS J2603 AB 20:39: :59: WDS J2604 AB 20:39: :26: WDS J2702 AB 21:05: :40: WDS J3066 AB 20:15: :00: WDS J3066 AC 20:15: :00: WDS J3079 AB 20:22: :45: WDS J3080 AB 20:22: :22: WDS J3081 AB 20:22: :22: WDS J3082 AB 20:23: :47: WDS J3084 AB 20:25: :02: WDS J3085 AB 20:26: :45: WDS J3087 AB 20:27: :13: WDS J3088 AB 20:29: :27: WDS J3089 AB 20:29: :31: WDS J3091 AB 20:31: :51: WDS J3092 AB 20:32: :23: WDS J3093 AB 20:33: :58: WDS J3094 AB 20:33: :14: WDS J3095 AB 20:36: :35: WDS J3096 AB 20:36: :43: WDS J3096 BC 20:36: :44: WDS J3098 AB 20:36: :21: WDS J3099 AB 20:37: :38: WDS J3102 AB 20:38: :49: WDS J3103 AB 20:39: :03: WDS J3104 AB 20:39: :06: WDS J3107 AB 20:41: :39: WDS J3108 AB 20:43: :38: WDS J3109 AB 20:43: :27: WDS J3110 AB 20:46: :31: WDS J3113 AB 20:51: :19: WDS J3115 AB 20:51: :46: WDS J3116 AB 20:52: :56: WDS J3116 BC 20:52: :57: WDS J3118 AB 20:58: :06: WDS J3125 AB 21:08: :57: WDS J3220 AB 20:28: :41: WDS J3221 AB 20:31: :59: WDS J3223 AB 20:48: :05: WDS J3244 AB 20:31: :45: WDS J3245 AB 20:51: :01: WDS J3263 AB 20:28: :23: WDS J3264 AB 20:29: :19: WDS J3277 AB 20:50: :42: WDS J3328 AB 20:55: :29:

25 Page 331 Jonckheere Double Star Photometry Part II: Delphinus Table 2. Bessel epoch (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 J1 AB Overlapping star disks - no separate photometry possible. Combined magnitude with SNR gives estimated M1 new and M2 new values not confirming the current, seemingly a bit too faint, WDS values J3 AB Touching/overlapping star disks J135 AB Touching star disks J142 AB J156 AB Touching/overlapping star disks J157 AB Touching star disks J191 AB Overlapping star disks - no separate photometry possible. Combined magnitude with SNR gives estimated M1 new and M2 new values suggesting much fainter magnitudes than currently WDS listed J192 AB Very low SNR <10 for B J193 AB J194 AB Overlapping star disks - no separate photometry possible. Combined magnitude with SNR gives estimated M1 new and M2 new values confirming rather well the current WDS values J194 AB. C mag WDS gives here obviously M1 for A and not AB combined. WDS value for C well confirmed J195 AB J284 AB Touching star disks J510 AB J553 AB J559 AB Overlapping/Touching star disks J562 AB Overlapping star disks ROE14 AB ROE14 AB as "bonus" J563 BC J566 AB J572 AB Touching star disks J573 AB Table 2 continues on next page.

26 Page 332 Jonckheere Double Star Photometry Part II: Delphinus Table 2 (continued). Bessel epoch (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 J604 AB Overlapping star disks - no separate photometry possible. Combined magnitude with SNR gives estimated M1 new and M2 new values confirming rather well the current WDS values J605 AC WDS values for A with 11.4 and not consistent J605 AB Overlapping star disks J607 AB Touching star disks J790 AB Touching star disks J797 AB J837 AB Overlapping/Touching star disks J838 AB J839 AB Overlapping/Touching star disks J840 AB J841 AB Overlapping star disks - no separate photometry possible. Combined magnitude with SNR gives estimated M1 new and M2 new values confirming rather well the current WDS values J841 AB.C J842 AB J844 AB J845 AB J846 AB J912 AB Touching star disks J1073 AB Low SNR <20 for B J1173 AB Touching star disks J1234 AB Very low SNR <10 for B J1241 AB Overlapping star disks - no separate photometry possible. Combined magnitude with SNR gives estimated M1 new and M2 new values confirming rather the current WDS values J1242 AB J1243 AB it27. Bessel epoch J1296 AB it27. Bessel epoch Table 2 continues on next page.

27 Page 333 Jonckheere Double Star Photometry Part II: Delphinus Table 2 (continued). Bessel epoch (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 J1297 AB Overlapping star disks - no separate photometry possible. Combined magnitude with SNR gives estimated M1 new and M2 new values confirming rather well the current WDS values J1318 AB Overlapping star disks - no separate photometry possible. Combined magnitude with SNR gives estimated M1 new and M2 new values confirming rather well the current WDS values J1342 AB Overlapping/Touching star disks J1343 AB Overlapping/Touching star disks. Bessel epoch J1344 AB Overlapping/Touching star disks. Bessel epoch J1345 AB Low SNR <20 for B J1346 AB it27. Touching star disks. Bessel epoch J1704 AB Bessel epoch J1715 AB Low SNR <20 for B J1716 AB J1879 AB Low SNR <20 for B. Bessel epoch J1879 AC Very low SNR <10 for B. Bessel epoch J1880 AB J1883 AB J1884 AB J1885 AB Low SNR <20 for B J1887 AB J1888 AB Low SNR <10 for B. Bessel epoch J1889 AB Low SNR <20 for A and very low SNR <10 for B. Bessel epoch J1890 AB J2192 AB Bessel epoch J2313 AB Low SNR <20 for B J2314 AB Low SNR <20 for B J2314 AC No resolution, C fainter than 14mag J2319 AB J2321 AB Table 2 continues on next page.

28 Page 334 Jonckheere Double Star Photometry Part II: Delphinus Table 2 (continued). Bessel epoch (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 J2325 AB Low SNR <20 for B. Similar pair UCAC /UCAC nearby J2572 AB Very low SNR<10 for B. Image quality questionable J2573 AB Low SNR<20 for B J2575 AB Overlapping star disks - no separate photometry possible. Combined magnitude with SNR questionable object, Bogus assumed. If double at all than A could be not brighter than 11.8mag J2603 AB Overlapping star disks - no trace of a secondary, no separate photometry possible. Combined magnitude with SNR questionable object, potential bogus J2604 AB Overlapping star disks - no trace of a secondary, no separate photometry possible. Combined magnitude with SNR questionable object, potential bogus J2702 AB J3066 AB J3066 AC Very low SNR<5 for C J3079 AB Bessel epoch J3080 AB Large dvmag Bessel epoch J3081 AB Large dvmag Bessel epoch J3082 AB Most probably position error. Only very faint single star with mag and SNR in the given position. But nearby UCAC :23: :47: Vmag with companion UCAC mag model fit, no Vmag. Bessel epoch J3084 AB Low SNR<20 for B. Bessel epoch J3085 AB Bessel epoch Table 2 continues on next page.

29 Page 335 Jonckheere Double Star Photometry Part II: Delphinus Table 2 (continued). Bessel epoch (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 J3087 AB Large dvmag Bessel epoch J3088 AB Low SNR<20 for A and B. Bessel epoch J3089 AB Low SNR<20 for A and very low SNR<5 for B. Bessel epoch J3091 AB Bessel epoch J3092 AB No resolution, no photometry possible. Both components probably much fainter than WDS value. UCAC fmag, UCAC fmag. Given Vmag for A seems questionable, especially as the same value is given for B and similar bright stars nearby are listed with Vmag. Bessel epoch J3093 AB No resolution, no photometry possible. Both components probably much fainter than WDS value. UCAC fmag, 4UCAC fmag. Vmag 12.79mag for A seems questionable, especially as similar bright stars nearby are listed with Vmag. Bessel epoch J3094 AB Companion too faint for resolution, thus rather confirming WDS value. Image quality questionable. Bessel epoch J3095 AB Low SNR<20 for A and B, image quality questionable. Bessel epoch J3096 AB Low SNR<20 for B. Bessel epoch J3096 BC Low SNR<20 for B, no resolution for C, thus probably much fainter than 13.1mag. Questionable image quality. Bessel epoch J3098 AB Low SNR<20 for A and B. Bessel epoch Table 2 concludes on next page.

30 Page 336 Jonckheere Double Star Photometry Part II: Delphinus Table 2 (conclusion). Bessel epoch (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 J3099 AB Bessel epoch J3102 AB Bessel epoch J3103 AB Bessel epoch J3104 AB Bessel epoch J3107 AB Bessel epoch J3108 AB Bessel epoch J3109 AB Bessel epoch J3110 AB Bessel epoch J3113 AB Bessel epoch J3115 AB Low SNR<20 for B. Bessel epoch J3116 AB A too bright for reliable photometry, low SNR<20 for B. Bessel epoch J3116 BC C too faint to be resolved, inconsistent WDS data for B (12.88 vs 13.3mag). Bessel epoch J3118 AB Bessel epoch J3125 AB Low SNR<20 for B. Bessel epoch J3220 AB Bessel epoch J3221 AB Very low SNR <10 for B. Bessel epoch J3223 AB No resolution, not even an elongation. Probably WDS catalog mismatch. Bessel epoch J3244 AB Very low SNR <10 for B. Same image as for J562. Bessel epoch J3245 AB Low SNR<20 for A and B. Bessel epoch J3263 AB Low SNR<20 for A and very low SNR<10 B. Bessel epoch J3264 AB Very low SNR <10 for B. Bessel epoch J3277 AB Very low SNR <10 for B. Bessel epoch J3328 AB Low SNR<20 for A and very low SNR<10 B. Bessel epoch Table 2 notes on next page.

31 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 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, Specifications of the used telescopes: it24: 610.mm CDK with 3962 mm focal length. Resolution 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 PL Resolution 0.53 arcsec/pixel. V-filter. No B-V transformation coefficients available. Located in Siding Spring, Australia. Elevation 1122 m.

32 Page 338 Double Star Measurements for December 2013 Frank Smith 20 Coburn Way Jaffrey, NH Abstract: I report 288 measurements of binary systems from The observations were conducted with the T24 robotic telescope located at the itelescope Observatory, Auberry CA, USA ( 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 seconds for 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

33 Page 339 Double Star Measurements for December 2013 References itelecopes. Mason, B.D., 2006 Requesting double star data from the US Naval Observatory. JDSO. 2, UCAC3 Catalog (Zacharias, et al. 2010). UCAC4 Catalog (Zacharias, et al. 2012). Warner, Brian MPO Canopus, 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 UCAC Position 06:42: :26: APASS V mag proper motion PA 8.4 DEC B Star is UCAC MASS J mag proper motion PA -1.8 DEC C star is UCAC MASS J mag C is also URAT proper motion PA 0.9 DEC D star is UCAC MASS J mag proper motion: PA 6.4 DEC 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.

34 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 POU862 AB POU 863 AC POU POU POU POU POU POU POU ALI POU POU POU POU POU POU POU POU SLE POU SLE 833 AB SLE 833 AC ALI BTG BTG 10 AC J 1092 AB POU POU POU POU POU POU POU POU POU POU POU POU POU POU POU POU POU POU 1508 AB Table 1 continues on next page.

35 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 POU 1509 AC POU POU POU POU POU POU POU 1556 AB POU 1557 AC POU POU POU POU POU POU POU POU POU POU POU POU POU POU POU POU POU POU POU POU POU POU POU POU 1681 AB POU 1682 AC POU 1688 AB POU 1689 AC POU 1690 AD POU POU POU POU 1700 AB POU POU POU POU POU POU POU POU POU POU POU POU POU Table 1 continues on next page.

36 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 POU POU POU POU POU POU POU POU POU POU POU POU POU POU 1757 AB POU 1758 AC POU POU BAL POU POU 1768 AB POU 1769 AC POU POU POU POU POU POU BAL POU TOK POU 1779 AB POU 1780 AC BAL POU POU POU HJ POU POU POU POU POU POU SLE POU POU POU POU POU POU POU POU POU 1806 AB POU 1807 AC Table 1 continues on next page.

37 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 POU 1802 AC POU POU POU POU HJ 2331 AB HJ 2331 AC POU POU POU POU 1814 AB POU 1815 AC POU 1822 AC BAL POU POU POU POU 1831 AB POU 1832 AC POU 1826 AB POU 1827 AC POU POU POU BAL POU POU 1837 AB POU 1838 AC POU POU POU POU POU POU POU POU POU 1848 AB POU 1849 AC POU POU POU POU POU POU POU POU 1863 AC POU POU POU POU POU POU 1867 AB POU 1868 AC POU Table 1 continues on next page.

38 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 POU POU POU POU POU POU POU POU POU 1883 AB POU POU POU POU POU POU POU POU POU POU POU POU 1903 AB POU 1903 AC POU POU POU POU POU POU POU POU POU POU POU 1912 BC POU 1912 AB POU 1912 AC POU POU POU POU POU POU POU NEW AB NEW AC NEW AD POU POU POU POU POU POU SLE POU POU Table 1 continues on next page.

39 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 POU POU POU POU SLE POU POU POU POU POU POU POU POU POU POU POU POU POU BAL BAL BAL BAL POU POU POU POU Notes: 1. POU894. "A" star is a close binary, see Figure POU610. "B" star faint. 3UCAC has a listed V mag of POU I'm measuring 3UCAC :29: :26:25.3 Mag 14.9 as the "A" star and 3UCAC :29: :26:18.7 Mag as the "B" star. 4. POU1470. "B" star is a close double. See image. I'm measuring to the brighter component 3UCAC Mag The other star is 3UCAC See Figure POU1546. I'm measuring 3UCAC : :55:06.7 Mag 14.6 as the "A"star. "B" is 3UCAC :35: :55:13.3 Mag 15.2 is the "B" star. 6. POU1653."A" star is much fainter in my CCD image. "A" 3UCAC V mag , "B" 3UCAC V mag POU1741.There are two pairs available. One matches the 1906 measure and one matches 1998 measure. POU Measuring 3UCAC V mag and 3UCAC V mag POU Measuring: star at 06:38: :58:36.3 mag 17.37, 06:38: :58:32.6 mag POU1889. 'B" star is a close double. See Figure POU1903. New "C" star. See Figure 5. "C" is UCAC-4 4UC "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

40 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 Mag POU1920. "A" star is a close double. See Figure POU1901. I'm measuring 3UCAC and 3UCAC "A" star is at 06:41: :44: POU1882. Position seems wrong. I'm measuring 3UCAC and 3UCAC "A" is at 06:41: :51: New quadruple star. See "Discussion". Figure 6. POU1912 showing new "C" component. Figure 7. POU1920. Measuring to brighter companion.

41 Page 347 Photometry of Faint and Wide Doubles in Vulpecula Wilfried R.A. Knapp Vienna, Austria Chris Thuemen Double Star Imaging Project Pembroke, Ontario, Canada 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 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 WDS mags. 9.8, UCAC4 fmags and ; Vmag for A 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 and Vmag for A only, 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 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-

42 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 to confirm this in the latter part of August 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 A 264AB WDS mags. of 8.20 and 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 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 M 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 & 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 (UCAC 4 # ) 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 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

43 Page 349 Photometry of Faint and Wide Doubles in Vulpecula ID Name RA Dec Sep PA M1 M2 WDS J 1303 AB Sge 19:15: :54: WDS AG 247 AB Vul 20:08: :20: WDS HJ 1504 AC Vul 20:22: :17: WDS A 264 AB Vul 19:12: :34: WDS A 264 DE Vul 19:12: :34: WDS A 264 AD Vul 19:12: :34: WDS MAD 7 AC Vul 19:12: :34: WDS MAD 7 BC Vul 19:12: :34: WDS HO 445 AB Vul 19:12: :35: WDS DAM 373 AB Vul 19:12: :32: WDS Table 1: WDS 2015 April values for the objectsfurther Research STF 2523 KRU 8 CD Vul 19:26: :06: Table 2: Photometry and measurement results based on itelescope it24 images used with AAVSO VPhot ID Name M1+ Err1 M2+ Err2 Date Notes WDS J 1303 AB WDS AG 247 AB WDS HJ 1504 AB WDS HJ 1504 AC WDS A 264 AB WDS A 264 DE WDS A 264 AD WDS MAD 7 AC WDS MAD 7 BC WDS HO 445 AB WDS DAM 373 AB WDS STF2523 KRU 8 CD 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

44 Page 350 Photometry of Faint and Wide Doubles in Vulpecula Table 3: Summary of results compared to WDS per April With a few exception WDS data changes are suggested ID Name Notes WDS J 1303 AB The components are about 3 mag fainter than listed but delta_m remained similar to Jonckheere s estimation WDS AG 247 AB B is about 1 mag fainter than listed WDS HJ 1504 AB WDS HJ 1504 AC WDS 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 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 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 / separation and / PA rather confirm the current WDS Sep/PA data within the given error range. Latest GAIA measurements with 19:12:42.448/+ 24:34: for A and 19:12:42.231/+ 24:34: for B would give separation and PA WDS A 264 DE WDS mag for E 15.5 quite confirmed with WDS A 264 AD WDS mag for D 15 quite confirmed with WDS MAD 7 AC WDS 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: with an average error of 0.15 and Dec +24:34:37.18 with an average error of 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 WDS HO 445 AB Both components fainter than listed, especially B WDS DAM 373 AB Both components fainter than listed, especially A WDS 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

45 Page 351 Jonckheere Double Star Photometry Part III: Lyra, Equuleus, and Eridanus Wilfried R.A. Knapp Vienna, Austria 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 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 ) 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 m 1` 2 according to Greaney Measurements of the J-objects in Lyra are given in Table 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 Measurements of the J-objects in Equ are given in Table 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 Table 6 gives the measurements of the J-objects in Eri. (Continued on page 360)

46 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 J110 AB 18:51: :24: J112 AB 19:01: :37: J131 AB 18:49: :23: J525 AB 18:38: :37: J760 AB 18:22: :30: J761 AB 18:27: :36: J762 AB 18:30: :34: J763 AB 18:30: :26: J764 AB 18:34: :54: J765 AB 18:49: :25: J766 AB 19:02: :27: J766 AC 19:02: :27: J767 AB 19:06: :49: J767 AC 19:06: :49: J768 AB 19:13: :46: J769 AB 19:20: :12: J811 AB 19:03: :56: J1138 AB 18:38: :00: J1205 AB 19:07: :28: J1206 AB 19:11: :12: J1208 AB 18:49: :34: J1209 AB 19:04: :06: J1263 AB 19:11: :53: J1263 BC 19:11: :53: J2941 AB 19:04: :51: J2942 AB 19:05: :49: J2945 AC 19:07: :43: J3213 AB 19:06: :15: J3313 AB 19:14: :45:

47 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 J158 AB 21:02: :17: J159 AB 21:08: :37: J161 AB 21:22: :57: J576 AB 21:12: :45: J608 AB 20:59: :13: J848 AB 21:09: :28: J913 AB 20:59: :28: J914 AB 21:24: :46: J1039 AB 21:25: :47: J1356 AB 21:22: :52: J1721 AB 21:19: :40: J1781 AB 21:06: :36: J2341 AB 21:19: :37: J2576 AB 21:06: :29: J2605 AB 21:22: :13: 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 J318 AB 04:53: :39: J319 AB 05:04: :12: J708 AB 04:23: :34: J709 AB 04:29: :34: J710 AB 04:38: :42: J1003 AB 04:58: :06: J1004 AB 05:08: :30: J1087 AB 04:30: :37: J1245 AB 02:47: :00: J1453 AB 02:50: :16: J1453 AC 02:50: :16: J1455 AB 03:03: :14: J1456 AB 03:17: :22: J1457 AB 03:36: :20: J1459 AB 04:21: :25:

48 Page 354 Jonckheere Double Star Photometry Part III: Lyra, Equuleus, and Eridanus Table 4. Bessel epoch 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 J110 AB Overlapping star disks - no separate photometry possible. Combined magnitude with SNR gives estimated M1 new and M2 new values confirming rather well the current WDS values J112 AB A too bright for reliable photometry No resolution of B J131 AB suggests B being far fainter than listed J525 AB J760 AB J761 AB J762 AB J763 AB Touching/Overlapping star disks J764 AB J765 AB Touching star disks J766 AB Touching star disks J766 AC J767 AB J767 AC J768 AB SNR for B < J769 AB J811 AB Touching star disks SNR for B < J1138 AB Touching star disks J1205 AB J1206 AB J1208 AB J1209 AB No double star at this position. Nearby A and B with dra 0.14 and ddec 0.15 giving Sep 2.643" with Err and PA with Err Minor position issue: A with dra 0.14 and ddec 0.15 giving Sep 4.676" with Err and PA with Err Table 4 concludes on next page.

49 Page 355 Jonckheere Double Star Photometry Part III: Lyra, Equuleus, and Eridanus Table 4 (conclusion). Bessel epoch 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 J1263 AB A too bright for reliable measurement, star disk looks elongated, might be a close double itself J1263 BC SNR for C < J2941 AB SNR for B < J2942 AB SNR for B < J2945 AC Mag for HLM16 B measured with with SNR (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 arcsec/pixel. V-filter. No transformation coefficients available. Located in Auberry, California. Elevation 1405m

50 Page 356 Jonckheere Double Star Photometry Part III: Lyra, Equuleus, and Eridanus Table 5. Bessel epoch 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 it27 1x3s. SNR for B<20 B J 159 A B it27 1x3s J 161 J 576 J 608 J 848 J 913 J 914 J 1039 A it27 1x3s. Touching/ Overlapping star B disks A it27 1x3s. Touching/ Overlapping star B disks A it27 1x3s. SNR for B<10, barely to see B A it27 1x3s. Touching/ Overlapping star B disks A it27 1x3s. Touching/ Overlapping star B disks A it27 1x3s. Touching/ Overlapping star B disks A it27 1x3s. SNR for B<20 B J 1356 A it27 1x3s B J 1721 A it27 1x3s B Table 5 concludes on next page.

51 Page 357 Jonckheere Double Star Photometry Part III: Lyra, Equuleus, and Eridanus Table 5 (conclusion). Bessel epoch 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 it27 1x3s B J 2341 A it27 1x3s B J 2576 A B it27 1x3s. SNR for A and B<20. No good match with the original Jonckheere 12/13 mags J 2605 BRT1355 A it27 1x3s. Touching/ Overlapping star B disks A it27 1x3s. Touching star disks B 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 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 PL Resolution 0.53 arcsec/pixel. V-filter. No B-V transformation coefficients available. Located in Siding Spring, Australia. Elevation 1122m

52 Page 358 Jonckheere Double Star Photometry Part III: Lyra, Equuleus, and Eridanus Table 6. Bessel epoch 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 B it27 1x3s J 319 A B it27 1x3s J 708 A it27 1x3s. Touching/ Overlapping star B disks J it27 1x3s. No resolution but elongation according to the listed WDS PA. Combined magnitude suggests 10.93/11.07mag for A/ B keeping the given delta_m J 710 A B it27 1x3s. Touching star disks J 1003 A B it27 1x3s J 1004 A B it27 1x3s J 1087 A it27 1x3s. Touching/ Overlapping star B disks J 1245 A it27 1x3s. Touching/ Overlapping star B disks Table 6 concludes on next page.

53 Page 359 Jonckheere Double Star Photometry Part III: Lyra, Equuleus, and Eridanus Table 6 (conclusion). Bessel epoch 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 B it27 1x3s J 1453 A C it27 1x3s J 1455 A B it27 1x3s J 1456 A B it27 1x3s J 1457 A it27 1x3s. Touching star disks B J 1459 A it27 1x3s. Touching star disks B 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 PL Resolution 0.53 arcsec/pixel. V-filter. No B-V transformation coefficients available. Located in Siding Spring, Australia. Elevation 1122m

54 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 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 and 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 and 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 v 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 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

55 Page 361 STT Doubles with Large ΔM Part IV: Ophiuchus and Hercules Wilfried R.A. Knapp Vienna, Austria John Nanson Star Splitters Double Star Blog Manzanita, Oregon 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 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 values for the selected STT objects in Oph and Her Name Comp ID RA Dec Con Sep PA M1 M2 ΔM STT 326 AB :18: :31: Oph STT 342 AB :07: :33: Oph STT 310 AB :25: :54: Her STT 314 AB :38: :27: Her STT 317 AB :52: :24: Her STT 324 AB :08: :12: Her STT 328 AB :17: :06: Her STT 338 AC :51: :19: Her STT 585 BP :44: :02: Her

56 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 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 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 ") and the 2013 WDS measures (316 and ") 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 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 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 and 3.8" in 1848 to 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 , while the secondary is moving west and south at similar rate, 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 ). (Continued on page 364)

57 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).

58 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 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 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 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 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 (UCAC ) 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 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 It appeared to be slightly fainter than a 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 and appeared to be similar in brightness to the secondary, suggesting it s slightly fainter than the WDS magnitude of 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 , 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 A comparison star with a Vmag of seemed somewhat fainter than the secondary. STT 328 (Her): Knapp resolved the secondary

59 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 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 , suggesting it may be a bit brighter than the WDS magnitude of 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 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 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 was similar in brightness to C, suggesting the WDS magnitude for it of is close. However, a limiting aperture for C of 130mm suggests C may be slightly fainter than 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 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 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 ) seems to be the cause of the discrepancy. We calculated a 0.3 shift in position of B between the URAT1 data and the 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)

60 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 it11 stack 5x1s B A B A B A B A B A B A B A B it24 stack 2x1s it24 stack 5x1s it24 stack 5x1s_ it24 stack 5x1s_ it24 stack 5x1s_ it24 stack 5x1s_ Summary line STT342 RA Dec Sep Err Sep PA Err PA Mag Err Mag Date 2015 N Notes A it24 stack 4x1s B SNR for B <20 A B A B A B A B A B A B A B it24 stack 5x1s. SNR for B <20 it24 stack 5x1s_2. SNR for B < it24 stack 5x3s it24 stack 5x6s it24 stack 5x9s 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.

61 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 it24 stack 5x1s B A it24 stack 5x1s_2 B A it24 stack 5x1s_3 B A it24 stack B x1s_4 A Touching/ overlapping star B disks STT 314 RA Dec Sep Err Sep PA Err PA Mag Err Mag Date 2015 N Notes A B A B A B A B A B A B A B A B A B A B it11 stack 5x1s it18 stack 5x1s it21 stack 5x1s it24 stack 5x1s it24 stack 5x1s_ it24 stack 5x1s_ it24 stack 5x1s_ it24 stack 5x1s_ it24 stack 5x1s_ Summary line Table 3 continues on next page.

62 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 it21 stack 4x1s. SNR B<20 B A it24 stack 3x1s B A it24 stack 5x1s B A it24 stack 5x1s_2 B A it24 stack 5x1s_3 B A it24 stack 5x1s_4 B A it24 stack 5x1s_5 B A Summary line B STT 324 RA Dec Sep Err Sep PA Err PA Mag Err Mag Date N Notes it24 stack 5x1s. A Overlapping star disks. SNR for B B<20 it24 stack A x1s_2. Overlapping star disks B SNR for B<20 A it24 stack x1s_3. Overlapping star disks B A it24 stack x1s_4. Overlapping star disks B A it24 stack x1s_5. Overlapping star disks B A it24 stack x1s_6. Overlapping star disks B A it24 stack x1s_7. Overlapping star disks B A it24 stack x1s_8. Overlapping star B disks A Summary line B Table 3 continues on next page.

63 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 it24 stack 5x1s B A it24 stack 5x1s_2 B A it24 stack 5x1s_3 B A it24 stack 5x1s_4 B A it24 stack 5x1s_5 B A it24 stack 5x1s_6 B A it24 stack 5x1s_7 B A Summary line B STT 328 RA Dec Sep Err Sep PA Err PA Mag Err Mag Date N Notes it24 stack 4x1s. A Overlapping star disks. SNR for B B<20 it24 stack 5x1s. A Overlapping star disks, SNR for B B<20 it24 stack A x1s_2. Overlapping star disks, B SNR for B<20 it24 stack A x1s_3. Overlapping star disks, B SNR for B<20 it24 stack A x1s_4. Overlapping star disks, B SNR for B<20 A Summary line B Table 3 continues on next page.

64 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 it11 stack 5x1s. SNR for B<20 C AB it18 stack 4x1s. SNR for C<10 C AB it21 stack 5x1s. SNR for C<20 C AB it24 stack 5x1s C AB it24 stack 5x1s_2 C AB it24 stack 5x1s_3 C AB it24 stack 5x1s_4 C AB it24 stack 5x1s_5 C AB it24 stack 5x1s_6 C AB Summary line C STT338 RA Dec Sep Err Sep PA Err PA Mag Err Mag Date N Notes AB it11 stack 5x1s D AB it18 stack 4x1s D AB it21 stack 5x1s D AB it24 stack 5x1s D AB it24 stack 5x1s_2 D AB it24 stack 5x1s_3 D AB it24 stack 5x1s_4 D AB it24 stack 5x1s_5 D AB it24 stack 5x1s_6 D AB Summary line D Table 3 concludes on next page.

65 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 it11 stack 5x1s. SNR for P<20 P B it18 stack 5x1s. SNR for P<10 P B it21 stack 5x1s. SNR for P<20 P B it24 stack 5x1s P B it24 stack 5x1s_2 P B it24 stack 5x1s_3 P B it24 stack 5x1s_4 P B it24 stack 5x1s_5 P B it24 stack 5x1s_6 P B Summary line P 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-PL Resolution 0.62 arcsec/pixel. V-filter. No transformation coefficients available. Located in Auberry, California. Elevation 1405m

66 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 STT 342 B STT 310 B STT 314 B STT 317 B STT 324 B 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 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 No visual observations made. STT 328 B STT 338 C 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 No visual estimates made. STT 585 P 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 Table 5. Astrometry Results Compared to WDS WDS PA 17.90" " " " " " " " " " " 3 Astrometry Coordinates Astrometry Sep Astrometry PA " " " " " " " " " " " ** At the time we first pulled data from the WDS for STT 585 BP, it listed the 2001 (most recent) separation as However, a look at the text file for that pair of stars showed a separation of for the 2001 measure. That error is now corrected in the current WDS listing of STT 585 BP.

67 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 " " Yes Yes STT 342 AB " " Yes Yes STT 317 AB " " Yes Yes STF 2127 AB " " Yes Yes STT 338 AB-C " " Yes Yes STT 338 AB-D " Yes Yes STT 585 BP " No 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 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 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 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 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 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 v

68 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 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 Method Calibration was performed via the drift method and led to value 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.

69 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 , HJL , HJL1065AC , ARG , STTA112AB , STFA 25AC , HJ 1231AC , STF1831AC , STF1830CE , ARY , STTA138BC , BAR 41CD , ARY , STFA 30BC , BU 953AB,D , POP1222AD , STTA151AB , S 689AB , STTA157AB ,

70 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 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.

71 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 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,

72 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 HJ HJ 1928 AB STF3056 AB, C STF3056 AB, C STF 30 AB HJ STF AG STF BU 232 AB, C HJ STF STF 112 AB ARG STF 121 AB STF STT 33 AB HJ SEI HJ 1089 AB S 404 AB STF 284 AB Notes: 1. The parallax for A is given as 5.64 mas (±1.42), while B shows 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 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 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 mas ±0.96 and 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 mas ±0.86, with the companion showing 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.

73 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 for and 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 (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 HJ HJ 1928 AB STF3056 AB, C STF3056 AB, C STF 30 AB HJ STF AG STF BU 232 AB, C HJ STF STF 112 AB ARG STF 121 AB STF STT 33 AB HJ SEI HJ 1089 AB S 404 AB STF 284 AB

74 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 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 Likely Rectilinear Pairs WDS Number Disc Comp Date Last Last Last Year Meas. Made Meas Meas Resid Resid R2 Note HJ n/a ES 1934 AB HJ WFC FAB 2 AB MLB 107 AB STI 82 AB HJ HJ ES KU STF ES STF AG ARG HJ AG

75 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 as the red box: 12. Figure 5 is a weighted plot of the data. Figure 5. Plot of WDS The WFC 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 ) Figure 6 is the plot with WFC removed: Figure 3: Data plot of WDS 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 without WFC Figure 4. Plot of WDS AB.

76 Page 382 CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs Figure 7 is a data plot of WDS 00167_ 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 AB; premature classification may be the case here. 15. Figure 8 is a plot of WDS AB. 17. A plot of this pair is shown in Figure 10. Figure 8. Plot of WDS AB. Figure 10: Plot of WDS

77 Page 383 CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs 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 Both CLL 1980 and TOB plot well away from the data (See Figure 12.) and, if included, drop the R2 value down to They should be given very little, if any, weight for analysis. Figure 13. Plot of WDS Apparently EGB 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 without CLL 1980 and TOB Figure 14: Plot of WDS with EGB corrected for quadrant flip.

78 Page 384 CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs This pair is plotted in Figure Figure 17 is a plot of this pair. Figure 15. Plot of WDS Figure 16. Plot of WDS See Figure 16. CLL should be given no weight. It plots well away from the trend and its presence drops the R2 value from to Figure 18 is a plot of this pair. Figure 16. Plot of WDS without CLL Figure 18. Plot of WDS

79 Page 385 CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs 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 , is shown in Figure A plot of this pair is given in Figure 20. Figure 19. Plot of WDS without HJ 1828 and HJ Figure 20. Plot of WDS (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)

80 Page 386 CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs... WDS Number Disc Comp Date Last Last Last Year Table Possible Rectilinear Pairs Meas. Made Meas Meas Resid Resid R2 Note STF3060 AB ARG 1 AB STF ES ES STI STT 13 AB BU 1348 AC STF HJ STF 70 AB HJ ARG 49 AC STTA 17 AB HJ HJ STF STF HJ STF HJ STF 139 AB HJ HU 805 AC STF STF 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 should be heavily discounted in the analysis. 4. HJ should be heavily discounted in the analysis. 5. HJ should be heavily discounted in the analysis. 6. HJ should be heavily discounted in the analysis. 7. FmY should be heavily discounted in the analysis. 8. HJ should be heavily discounted in the analysis. 9. HJ should be heavily discounted in the analysis. 10. HJ should be heavily discounted in the analysis.

81 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 Calibrating the Plate Scale of a 20 cm Telescope with a Multiple-Slit Diffraction Mask. JDSO Vol 11 No 4, Viewable online at JDSO.org. Harshaw, Richard Calibrating a CCD Camera for Speckle Interferometry. JDSO Vol 11 No 1s,

82 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 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 Results, Part 1: One Grade 3 Orbit First to report is the one pair with a known orbit

83 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 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)

84 Page 390 CCD Measurements of 8 Double Stars With Binary Nature... Table 1: Measure of WDS (STF 60 AC) WDS Number Disc Comp Date Last Last Last Year Meas. Made Meas Meas Resid Resid Notes STF 60 AB Table 2: Short Arc Binaries WDS Number Disc Comp Date Last Last Last Meas. Year Made Meas Meas Resid Resid R2 Note FAB ES 2 AB STF MLB 383 AD Table 3: Speckle Interferometry on Three Pairs WDS Number Disc Comp Date Last Last Last Year Meas. Made Meas Meas Resid Resid Plot STF STF STF 180 AB Notes to Tables: 1. Using the Sixth Orbit Catalog ephemerides and extrapolating for , the projected values for and are and ". The residuals for the measurement are and ". See Figures 1 and 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 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 ±5.51 mas for the companion. See Figure See Figure 6 for a plot of WDS See Figure 7 for a plot of WDS , a speckle measurement. 7. See Figure 8 for a plot of WDS , a speckle measurement. 8. See Figure 9 for a plot of WDS AB, a pair with several anomalous measurements. Figure 1: PNG plot of WDS Figure 2: Plot of WDS AB history showing the measurement (red box).

85 Page 391 CCD Measurements of 8 Double Stars With Binary Nature... Figure 3: Plot of WDS , a curious case of a reverse trend curve. Figure 4: Plot of WDS AB. Figure 5. Plot of WDS Figure 6: Plot of WDS AD.

86 Page 392 CCD Measurements of 8 Double Stars With Binary Nature... Figure 7. Plot of WDS , a speckle measurement. Figure 8. Plot of WDS Figure 9. Plot of WDS AB, a pair with several anomalous measurements.

87 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 Calibrating the Plate Scale of a 20 cm Telescope with a Multiple-Slit Diffraction Mask. JDSO Vol 11 No 4, Viewable online at JDSO.org. Harshaw, Richard Calibrating a CCD Camera for Speckle Interferometry. JDSO Vol 11 No 1s, Harshaw, Richard CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs. JDSO, in submission.

88 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 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 for the primary and 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 for the pri-

89 Page 395 CCD Measurements of 141 Proper Motion Stars: The Autumn 2015 Observing Program... mary and for the companion. The resultant is 8.94 mas while the largest vector has a scalar value of mas. The resultant is 33.7% of the scalar, so this is a SPM pair. For Case 3, the primary has PM of with a companion of The resultant is 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 ). 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 , WDS , WDS and WDS Three pairs show an optical nature and could use extra observations in the next few decades: WDS , WDS and WDS Four pairs are starting to show what may be a linear trend. These are WDS , WDS , WDS and WDS 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 Calibrating the Plate Scale of a 20 cm Telescope with a Multiple-Slit Diffraction Mask. JDSO Vol 11 No 4, Viewable online at JDSO.org. Harshaw, Richard Calibrating a CCD Camera for Speckle Interferometry. JDSO Vol 11 No 1s, Harshaw, Richard CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs. JDSO in submission. Rica, F. M Determining the Nature of a Double Star: The Law of Conservation of Energy and the Orbital Velocity. JDSO Vol 7 No 4,

90 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 STI CPM HJ CPM TVB CPM STF3053 AB SPM ARG DPM STF CPM STF SPM STF CPM HJ 1929 AB, C SPM HJ CPM SMA CPM HJ 1932 AB CPM STF CPM ES CPM HJ CPM STF SPM ES SPM STF CPM MLB DPM ES 1406 AB SPM HJ 1004 AC DPM MLB 441 AB CPM STF CPM ES 1865 AB DPM STF CPM BU 1341 AB CPM ES CPM STF 10 AB STF SPM STF CPM HJ 1009 AB SPM HJ 1009 AC SPM HJ SPM STF 17 AB SPM STF SPM STF CPM WEI CPM STF SPM HDS DPM STF 26 AB, C CPM STI SPM HJ SPM STF 28 AB CPM HJ CPM HJ CPM Table 1 continues on next page.

91 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 MLB ??? FOX SPM STI SPM ES DPM STF CPM FOX SPM ALI CPM ES CPM STF 40 AB SPM STF SPM H 5 17 AB SPM ES CPM STF 47 AB CPM HJ CPM ES CPM STF ??? ES CPM STI SPM STF CPM HJ CPM BU 1 AD SPM BU 1 CD ??? AG CPM AG SPM ARG CPM STF CPM STI DPM HJ CPM HJ CPM MLB SPM STF 88 AB CPM STF 90 AB CPM STT 23 AB SPM STF 94 AC CPM STI CPM STF 98 AB CPM HJ 2027 AB CPM STF 100 AB CPM AG SPM ARG 49 AB DPM STF SPM HJ DPM STF 102 AB, C CPM STI CPM STF 109 AB CPM Table 1 continues on next page.

92 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 STF 123 AB CPM ES CPM HJ DPM ES CPM STF 131 AB CPM ARG CPM ES CPM STF CPM HJ SPM HU 531 AB, C CPM HJ DPM COU 668 AB SPM ES 1772 AB DPM STF CPM STF SPM STF CPM STF 157 AC SPM HJ CPM HJ 2075 AB CPM STF CPM ES SPM STF 163 AB CPM HJ CPM ARG CPM ARG 6 AB SPM HDS SPM HJ CPM AG CPM ES CPM STF SPM STF 205 A, BC CPM HJ SPM STF CPM SMA SPM STF CPM AG 32 AB CPM FOX SPM STF CPM STF SPM STF CPM STF CPM STF 238 AC DPM HJ CPM STF DPM STFA 5 AB CPM 24 Table 1 concludes on next page.

93 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 STF2738 AB SPM STF2769 AB CPM HJ CPM STF2816 AD CPM STF2841 A, BC CPM STF2872 A, BC 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 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 should be given very little weight during analysis. 5. Both BAZ and WFC appear to have quadrant reversals. 6. I am not completely at ease with my measurement. 7. HJ 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 mas ± 0.68 for the primary and mas ± 0.68 for the companion. Using the mean of 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 mas ± 0.60). Using the mean of 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 mas ± 10.93, this is not likely), the minimum separation would be 606 AU. 13. HJ should be assigned a minimal weight during analysis. 14. Starting to show a linear trend? 15. HJ should be given minimal weight during analysis. 16. Both Mad and WFD 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 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 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 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.

94 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 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

95 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 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 The AC pair was last reported in 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 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

96 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 ] 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 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)

97 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 LEO 5AB PA Sep. Mean Std Dev Std Error Mean LEO 5AC Std Dev Std Error 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.

98 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 MKT13AB Std Dev Std Error (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 ] 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 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.

99 Page 405 Measurements of Multi-star Systems LEO 5 and MKT 13 R 2 value of 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 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 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. astrometry/optical-ir-prod/wds/orb6 Mason, B. and Hartkopf, W. USNO CCD Astrograph Catalog (UCAC), March Astrometry Department, U.S. Naval Observatory. Mason, B. and Hartkopf, W. The Washington Double Star Catalog, October Astrometry Department, U.S. Naval Observatory. ad.usno.navy.mil/wds/wds.html. Stelle Doppie Double Star Database Search Engine,

100 Page 406 GJ 282 AB (WDS AB = BGH 3 AB) and GICLAS : 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 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 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 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 (= Giclas ) 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 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 The organization of this paper is as follows. In Section 2, we detail the characteristic of the AB pair, the

101 Page 407 GJ 282 AB (WDS AB = BGH 3 AB) and GICLAS : 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 ± 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 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 ± 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 and 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 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-

102 Page 408 GJ 282 AB (WDS AB = BGH 3 AB) and GICLAS : 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 " WFD1906b 0.2 T WFC Pa WFC Pa WFD T WFC1945b 0.1 Pa Bgh Pa WFC Pa USN Po USN Po USN Po USN Po USN Po USN Po USN Po USN Po USN Po USN Po USN Po USN Po USN Po WFC Pa WFC Pa WFD T TYC Ht TMA E UC_2013b 0.2 Eu Arn2003e 0.2 Mg WISE 0.4 Hw URAT1 0.2 E Benavides 0.3 C

103 Page 409 GJ 282 AB (WDS AB = BGH 3 AB) and GICLAS : A Very Wide System Table 2. Positional, Dynamical, and Kinematic Parameters for GJ 282 AB. Mean Epoch (deg) for mean epoch ± (arcsec) for mean epoch ± x (AU) [East-West] +763 ± 14 y (AU) [North-South] -315 ± 6 d /dt (mas yr -1 ) ± 0.51 d /dt (deg yr -1 ) ± dx/dt (mas yr -1 ) ± 0.53 dy/dt (mas yr -1 ) ± 0.41 Vx (km s -1 ) [East-West] ± 0.04 Vy (AU) [North-South] ± 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 ± 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 and the mean absolute, MA, 0.01º and 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 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/ (Continued on page 411)

104 Page 410 GJ 282 AB (WDS AB = BGH 3 AB) and GICLAS : 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).

105 Page 411 GJ 282 AB (WDS AB = BGH 3 AB) and GICLAS : A Very Wide System (Continued from page 409) values. The maximum value is 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 Giclas (= 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 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 In this work, we want to confirm the dynamical disintegration status of GJ 282 AB NLTT by the Table 4. Computed Orbital Parameters COMPUTED ORBITAL PARAMETERS FOR WDS = 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) T (yr) e a (arcsec) a (AU) i (deg) (deg) (deg) q (AU) study of the relative velocity of NLTT 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 , the CM AB has an offset of 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 with respect to the CM AB from the difference of their (U, V, W) velocities: V rel U U V V W W 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)

106 Page 412 GJ 282 AB (WDS AB = BGH 3 AB) and GICLAS : 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 h 39m 59.29s... 07h 40m 00.85s for º 35' 48.6" º 35' 58.26" (mas yr -1 ) 2) ± ± ± ± 1.6 (mas yr -1 ) 2) ± ± ± ± 0.8 V rad (km s -1 ) 1) ± ± ± ± 0.2 Parallax (mas) 3) ± ± ± 1.64 U (km s -1 ) ± ± 0.15 V (km s -1 ) ± ± 0.13 W (km s -1 ) ± ± ) Poveda et al. (2009); 2) Tycho-2 catalog; 3) Hipparcos

107 Page 413 GJ 282 AB (WDS AB = BGH 3 AB) and GICLAS : A Very Wide System (Continued from page 411) Tycho-2: ± 0.001º and ± 04 ( ) 2MASS: ± 0.001º and ± 0.08 ( ) URAT1: ± 0.001º and ± 0.06 ( ) 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 (= 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 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 has a binding energy between the curves for a o = 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 ( 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 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, 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

108 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 Hosted by BRIEF Boyce Research Initiatives and Education Foundation 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.