COMMISSIONS 27 AND 42 OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS Number 6xxx
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1 COMMISSIONS 27 AND 42 OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS Number 6xxx Konkoly Observatory Budapest x Xxxx 2012 HU ISSN MINIMA OF ECLIPSING BINARIES AND NEW EPHEMERIDES FOR GSC AND EZ LAC BANFI, M. 1 ; ACETI, P. 1,2 ; ARENA, C. 1,3 ; BIANCIARDI, G. 1,4 ; BONAVENTURA, G. 1,3 ; CHIAP- PINI, M. 5 ; CORFINI, G. 1 ; DE PONTI, J.M. 2 ; LO SAVIO, E. 3 ; LUCIDI, F. 1 ; MARCHINI, A. 1,5 ; MARINO, G. 1,3 ; MARTINENGO, M. 1 ; NASIMI, H. 5 ; PESENTI, L. 2 ; PRANDONI, F. 2 ; RUOCCO, N. 1,6 ; SALVAGGIO, F. 1,3 ; VINCENZI, M. 1 ; ZAMBELLI, R. 1 1 Sezione Stelle Variabili Unione Astrofili Italiani (UAI), stellevariabili@uai.it 2 Liceo Scientifico Iris Versari, Cesano Maderno (MI), ITALY 3 Gruppo Astrofili Catanesi - via Milo, 28 I Catania, ITALY 4 Skylive/Telescopio remoto UAI - ITALY 5 University of Siena Astronomical Observatory - Via Roma, 56 I Siena, ITALY 6 Astrocampania, Sez. Stabia Penisola Sorrentina - ITALY The list herebelow contains 163 times of minimum for 79 eclipsing binary stars (including the cataclysmic AM Her) calculated from CCD observations made by participants in the SSV-UAI Eclipsing Binaries Program. All the observatories are located in Italy; one is managed by the Physics Department of the University of Siena, while the others are privately operated. Some light curves were remotely obtained (via Internet) using the Italian and Australian telescopes of the Skylive-UAI Project, that are publicly available on the web site The observations were reduced following standard procedures (see next section) and the light curves were analyzed using the Kwee van Woerden algorithm (Kwee & van Woerden, 1956) to determine the times of minimum. All the times of minimum listed in this paper are heliocentric. It is worth noting that most of the observed stars are neglected objects. Observatory and telescope: University of Siena Astron. Observatory: 32-cm Maksutov Cassegrain (MC32) Australian Skylive remote telescope: 36-cm Schmidt Cassegrain (SC36) Other private astronomical stations: 30-cm Schmidt Cassegrain (SC30) 23-cm Schmidt Cassegrain (SC23) 25-cm Newton (NW25) 25-cm Schmidt Cassegrain (SC25) 20-cm Newton (NW20) 20-cm Schmidt Cassegrain (SC20) 13-cm Maksutov Cassegrain (MK13) 8-cm ED Refractor (ED8)
2 2 IBVS 6xxx Detector: Meade DSI Pro II Monochromatic CCD camera (DSI) QSI 516wsg CCD Camera SBIG ST-7 CCD Camera (ST7) SBIG ST-8XME CCD Camera (ST8) SBIG ST-9 CCD Camera (ST9) Sony ICX429ALL based CCD camera (CCD-UAI) Canon Eos 1100D DSLR(Eos) Method of data reduction: Frame calibration (dark subtraction and flat field correction) and photometric analysis (differential photometry on each image) were performed using MaxIm DL or Mira Pro software packages. Method of minimum determination: Times of minima, expressed as Heliocentric Julian Day (see the attached Table), were computed adopting the KW method (Kwee & van Woerden, 1956) using AVE (Barberá, 1996). This algorithm also provides an error estimate, that is the formal internal error of the KW method, which can be considered as a lower limit of the actual uncertainty on times of minimum. Together with that error, we provide an alternative estimate error according to the Arlot s (modified) method (Arlot et al., 2009) by adopting the formula σ ToM = 1 σ m 2 m t, where σ m is the error in magnitude and m is the magnitude drop during a time range t delimiting the part of the light curve where the speed of decrease in magnitude is the highest. The types of minimum quoted in the Table were deduced according to the ephemeris provided by Kreiner s (2004) web site ( by B.R.N.O. O C Gateway web site ( or by our updated elements. In the latter case we are sure that the primary minimum (conventionally at zero phase) is the deepest one. V473 And a b I V Martinengo/SC20/QSI 516 V473 And II V Martinengo/SC20/QSI 516 V473 And I V Martinengo/SC20/QSI 516 V473 And II V Banfi/SC25/ST7 V473 And I V Banfi/SC25/ST7 V473 And I V Banfi/SC25/ST7 V473 And I V Vincenzi/SC30/ST9 V480 And I V Zambelli/SC25/ST8 V487 And I V Banfi/SC25/ST7 V502 And I V Banfi/SC25/ST7 V502 And I Corfini/NW20/CCD-UAI V502 And I V Corfini/NW20/CCD-UAI XX Ant II r Marino/SC36/ST8 CK Aqr I V Vincenzi/SC30/ST9 GS Aqr II Corfini/NW20/CCD-UAI AL Ari I R Marino/NW25/ST7 EM Aur II R Marino/NW25/ST7 MM Aur I Ruocco/SC25/ST7 MR Aur I Ruocco/SC25/ST7 V562 Aur I Y 495 Corfini/NW20/CCD-UAI V594 Aur : I Ruocco/SC25/ST7 TU Boo I V Vincenzi/SC30/ST9
3 IBVS 6xxx 3 EF Boo I R Marino et al./nw20/st7 XZ CMi I V Vincenzi/SC30/ST9 AE Cas I R Marino/NW25/ST7 DO Cas I R Marino/NW20/ST7 V541 Cas II R Marino/NW25/ST7 DM CVn I Ruocco/SC25/ST7 EL CVn I V Martinengo/SC20/QSI 516 EV CVn II Ruocco/SC25/ST7 EV CVn I Ruocco/SC25/ST7 UX CrB I Ruocco/SC25/ST7 V997 Cyg II V Banfi/SC25/ST7 V1187 Cyg I V Banfi/SC25/ST7 V1187 Cyg I V Zambelli/SC25/ST8 V1191 Cyg II V Banfi/SC25/ST7 V1905 Cyg I Ruocco/SC25/ST7 V1763 Cyg I V Banfi/SC25/ST7 V2287 Cyg I V Banfi/SC25/ST7 V2486 Cyg I Ruocco/SC25/ST7 CR Del II V Banfi/SC25/ST7 KO Del I Corfini/NW20/CCD-UAI HL Dra I Corfini/NW20/CCD-UAI G Dra I Corfini/NW20/CCD-UAI G Dra I V Marchini et al./mc32/st7 G Dra II V Marchini et al./mc32/st7 G Dra I V Marchini et al./mc32/st7 G Dra II V Marchini et al./mc32/st7 G Dra I V Marchini et al./mc32/st7 G Dra II V Marchini et al./mc32/st7 G Dra II Arena/NW20/DSI G Dra I Arena/NW20/DSI G Dra II Arena/NW20/DSI G Dra I R Arena/NW20/ST7 G Dra II V Aceti et al./sc20/st8 VV Eri I V Vincenzi/SC30/ST9 VV Eri I V Vincenzi/SC30/ST9 VV Eri II V Vincenzi/SC30/ST9 VV Eri I V Zambelli/SC25/ST8 VV Eri I r Corfini/NW20/CCD-UAI AM Her c I V Banfi/SC25/ST7 V1072 Her II Arena/NW20/DSI V1088 Her II Ruocco/SC25/ST7 V1088 Her I Ruocco/SC25/ST7 V1088 Her I Ruocco/SC25/ST7 V1088 Her II Ruocco/SC25/ST7 V1106 Her I Corfini/NW20/CCD-UAI V1106 Her I Corfini/NW20/CCD-UAI V1106 Her I V Banfi/SC25/ST7 V1106 Her II V Marchini/MC32/ST7 V1106 Her I Corfini/NW20/CCD-UAI V1106 Her I Corfini/NW20/CCD-UAI V1106 Her I V Marchini/MC32/ST7 V1106 Her II Corfini/NW20/CCD-UAI V1106 Her II Bonaventura/MK13/Eos
4 4 IBVS 6xxx G Her I Arena/NW20/DSI G Her II Arena/NW20/DSI G Her II V Aceti et al./sc25/st8 EZ Lac I Ruocco/SC25/ST7 EZ Lac I Vincenzi/SC30/ST9 EZ Lac I Ruocco/SC25/ST7 EZ Lac I V Marchini/MC32/ST7 EZ Lac I Marchini/MC32/ST7 EZ Lac I Marchini/MC32/ST7 EZ Lac II I Zambelli/SC25/ST8 EZ Lac II Corfini/NW20/CCD-UAI EZ Lac II Banfi/SC25/ST7 EZ Lac II Marchini/MC32/ST7 EZ Lac II V Martinengo/SC20/QSI 516 EZ Lac II Marchini/MC32/ST7 FU Lac I Ruocco/SC25/ST7 FU Lac II Ruocco/SC20/ST7 FU Lac I Ruocco/SC25/ST7 XX Leo II V Salvaggio,Lo Savio/SC23/ST7 VW LMi I Bonav., Marino/MK13/Eos WZ LMi II Ruocco/SC25/ST7 AA Lyn I Ruocco/SC25/ST7 CW Lyn I V Martinengo/SC20/QSI 516 DI Lyn II H Corfini/NW20/CCD-UAI EH Lyn I Corfini/NW20/CCD-UAI EH Lyn I Zambelli/SC25/ST8 EH Lyn I Zambelli/SC25/ST8 EH Lyn II Corfini/NW20/CCD-UAI EH Lyn II Corfini/NW20/CCD-UAI HY Lyr II V Banfi/SC25/ST7 PV Lyr I V Banfi/SC25/ST7 QQ Lyr I Ruocco/SC25/ST7 V574 Lyr II BV RI Arena/NW20/ST7 V574 Lyr I BV RI Arena/NW20/ST7 V574 Lyr II BV RI Arena/NW20/ST7 V574 Lyr I BV RI Arena/NW20/ST7 V574 Lyr II BV RI Arena/NW20/ST7 V574 Lyr I BV RI Arena/NW20/ST7 V574 Lyr II BV RI Arena/NW20/ST7 V574 Lyr II BV RI Arena/NW20/ST7 V574 Lyr I BV RI Arena/NW20/ST7 V574 Lyr II BV RI Arena/NW20/ST7 G Lyr I Arena/NW20/DSI DD Mon I R Marino/NW25/ST7 V383 Mon I Ruocco/SC25/ST7 V383 Mon I Ruocco/SC25/ST7 V383 Mon II Ruocco/SC25/ST7 V464 Mon I Marino/SC36/ST8 V527 Mon I Marino/SC36/ST8 ET Ori I Bianciardi, Ruocco/SC36/ST8 BW Peg I Ruocco/SC20/ST7 BW Peg I Corfini/NW20/CCD-UAI V365 Peg II V Banfi/SC25/ST7 V963 Per I Ruocco/SC25/ST7 V963 Per II Ruocco/SC25/ST7 V963 Per I Ruocco/SC25/ST7 GR Psc II V Banfi/SC25/ST7 CP Sge I V Banfi/SC25/ST7
5 IBVS 6xxx 5 V423 Tau II Ruocco/SC25/ST7 V423 Tau II Ruocco/SC25/ST7 V423 Tau : I Ruocco/SC25/ST7 V423 Tau II Ruocco/SC25/ST7 V1374 Tau I Y 495 Corfini/NW20/CCD-UAI V1374 Tau I r Corfini/NW20/CCD-UAI BE Tri I V Banfi/SC20/ST7 BE Tri I Corfini/NW20/CCD-UAI BM Tri I V Banfi/SC25/ST7 BX Tri II V Banfi/SC25/ST7 BX Tri II V Banfi/SC25/ST7 BX Tri I V Banfi/SC25/ST7 BX Tri II V Banfi/SC25/ST7 CM Tri I V Banfi/SC25/ST7 CN Tri I V Banfi/SC25/ST7 CS Tri I V Banfi/SC25/ST7 XY UMa I Bonaventura/MK13/Eos GZ UMa : I V Lucidi/ED8/DSI LL UMa I Ruocco/SC25/ST7 LL UMa II Ruocco/SC25/ST7 MS UMa I V Aceti et al./sc25/st7 EY Vul I V Banfi/SC25/ST7 V384 Vul II V Banfi/SC25/ST7 V384 Vul II V Banfi/SC25/ST7 V384 Vul II V Vincenzi/SC30/ST9 V384 Vul II V Vincenzi/SC30/ST9 V384 Vul I V Vincenzi/SC30/ST9 V384 Vul II V Marchini/MC32/ST7 V467 Vul II V Corfini/NW20/CCD-UAI V467 Vul II Corfini/NW20/CCD-UAI Explanation of the remarks in the table: Rem.: Observer[s]/Telescope/Detector a Arlot s modified method b as given by KW method c cataclysmic variable : uncertain
6 6 IBVS 6xxx Remarks: GSC We found relevant discrepancies between our observed times of the minima and the computed times of the minima based on the period of 0 d given by Devor et al. (2008). Our data better fit to the 0 d value given by Gettel et al. (2006). The best linear fit of the O C vs. the epoch, leaving the initial epoch and period free to vary, including the time of minimum given by the VSX catalogue (deduced from Devor et al., 2008 data), leads to the following updated ephemeris: T min (HJD) = (± ) + 0 d (± ) E Figure 1 shows the O C diagram computed using our new ephemeris. EZ Lac Considering our data together with those found in literature, the best linear fit of the O C leads to the following average ephemeris: T min (HJD) = (±0.0263) + 2 d (± ) E Figure 2 shows the O C diagram computed using the above mentioned average ephemeris. The high dispersion of the old data (photographic) does not allow to establish with certainty a variation of O C or period in the range from the first observations (1938) up to our observations. However, the average ephemeris leads to a discrepance of about half an hour with respect to the recent times of minimum. Our minima better fit to the following updated ephemeris: T min (HJD) = (±0.0013) + 2 d (± ) E obtained taking into account only our primary minima, whose depth allows a more precise timing of the minima. Figure 1. O C diagram for GSC Empty symbols for secondary minima.
7 IBVS 6xxx 7 Figure 2. O C diagram for EZ Lac. Empty symbols for secondary minima. References: Arlot, J.-E. et al., 2009, A&A, 493, 1171 Devor, J., Charbonneau, D., O Donovan, F. T., Mandushev, G., Torres, G., 2008, AJ, 135, 850 Gettel, S.J., Geske, M.T., McKay, T.A., 2006, AJ, 131, 621 Kreiner, J. M., 2004, AcA, 54, 207, Kwee, K. K., van Woerden, H., 1956, Bull. Astr. Inst. Neth., 12, 327, (No. 464)
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