Access to Astronomical Catalogues

← Click to display the menu
J/A+A/456/599       Light curves of 5 cataclysmic variables    (Papadaki+, 2006)

Photometric study of selected cataclysmic variables. Papadaki C., Boffin H.M.J., Sterken C., Stanishev V., Cuypers J., Boumis P., Akras S., Alikakos J. <Astron. Astrophys. 456, 599 (2006)> =2006A&A...456..599P (SIMBAD/NED BibCode)
ADC_Keywords: Stars, variable ; Photometry Keywords: accretion, accretion discs - stars: novae, cataclysmic variables Abstract: We present time-resolved photometry of five relatively poorly-studied cataclysmic variables: V1193 Ori, LQ Peg, LD 317, V795 Her and MCT 2347-3144. The observations were made using four 1m-class telescopes for a total of more than 250h of observation and almost 16,000 data points. For LQ Peg WHT spectroscopic data have been analysed as well. The light curves show a whole range of variability on different time scales, from minutes to months. We detect for the first time a brightness variation of 0.05mag in amplitude in V1193 Ori on the same timescale as the orbital period, that we interpret as the result of the irradiation of the secondary. A 20-min Quasi-Periodic Oscillation is also detected. The mean brightness of the system has changed by 0.5mag on a three month interval, while the flickering was halved. In LQ Peg a 0.05mag modulation was revealed with a period of about 3h. The flickering was much smaller, of the order of 0.025mag. A possible Quasi-Periodic Oscillation could exist near 30min. For this object, the WHT spectra are single peaked and do not show any radial-velocity variations. The data of LD 317 show a decrease in the mean magnitude of the system. No periodic signal was detected but this is certainly attributable to the very large flickering observed: between 0.07 and 0.1mag. For V795 Her, the 2.8-hour modulation, thought to be a superhump arising from the precession of the disc, is present. We show this modulation not to be stable in terms of periodicity, amplitude and phase. Finally, for MCT 2347-3144, a clear modulation is seen in a first dataset obtained in October 2002. This modulation is absent in August 2003, when the system was brighter and showed much more flickering. Description: tablea1.dat describes the observing log. We have performed photometric observations of five relatively poorly-studied cataclysmic variables: V1193 Ori, LQ Peg, LD 317, V795 Her and MCT 2347-3144. For each target, we give the UT dates it was observed, the site where the observations took place, the Heliocentric Julian Date at the beginning of each observing night, the total duration of each run and which filter, if any, was used. table1.dat shows (for V1193 Ori, LD 317 and MCT 2347-3144) the mean nightly magnitude of each CV along with the variation of the difference between two comparison stars. figA2.dat-figA6.dat give the light curves of V1193 Ori, LQ Peg, LD 317, V795 Her and MCT 2347-3144, respectively. In figA3.dat, figA4.dat and figA5.dat the magnitude is in arbitrary units. Objects: ---------------------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------------------- 05 16 26.7 -00 12 14 V1193 Ori = V* V1193 Ori 21 36 19.1 +11 40 55 LQ Peg = V* LQ Peg 23 44 57.5 +43 31 23 LD 317 = FBS 2342+432 17 12 56.1 +33 31 21 V795 Her = V* V795 Her 23 50 30.8 -31 27 29 MCT 2347-3144 = MCT 2347-3144 ---------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablea1.dat 47 70 Log of observations table1.dat 32 30 Long-term behaviour of three CVs figa2.dat 19 3750 V1193 Ori light curve figa3.dat 19 2014 LQ Peg light curve figa4.dat 19 2984 LD 317 light curve figa5.dat 19 4496 V795 Her light curve figa6.dat 19 1435 MCT 2347-3144 light curve
Byte-by-byte Description of file: tablea1.dat
Bytes Format Units Label Explanations
1- 13 A13 --- Name Cataclysmic variable name 15- 24 A10 --- UT UT date at beginning of the night 26- 29 A4 --- Site Observing site (1) 31- 41 F11.3 d HJDstart Heliocentric Julian Date at start 43- 45 F3.1 h Dur Duration of observing run 47 A1 --- Band [RV-] Band used (2)
Note (1): Observing site as follows: SAAO = South African Astronomical Observatory OHL = Observatorium Hoher List, Germany KR = Kryoneri Observatory, Greece SK = Skinakas Observatory, Greece Note (2): Bands as follows: R = Johnson R filter V = Johnson V filter - = unfiltered runs
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 8 A8 --- UT UT date 9 A1 --- Star [a-c] Flag for the star observed (1) 11- 15 F5.2 mag <mag> Mean nightly magnitude of our object 17- 20 F4.2 mag e_<mag> Error in mean(CV) 22- 26 F5.3 mag <shift> Nightly mean of the shift between 2comp. stars 28- 32 F5.3 mag e_<shift> Error in mean(shift)
Note (1): Flag for the star observed as follows: a = observing runs of V1193 Ori, b = observing runs of LD 317 c = observing runs of MCT 2347-3144
Byte-by-byte Description of file: figa?.dat
Bytes Format Units Label Explanations
1- 12 F12.8 d Time Number of days after the beginning of observation (1) 14- 19 F6.3 mag mag ? Magnitude (2)
Note (1): Days from HJD=2452570 for V1193 Ori Days from HJD=2453158 for LQ Peg Days from HJD=2452894 for LD 317 Days from HJD=2452794 for V795 Her Days from HJD=2452572 for MCT 2347-3144 Note (2): The magnitude is in mag units for V1193 Ori (figa2) and MCT 2347-3144 (figa6). The magnitude is in arbitrary units for LQ Peg (figa3), LD 317 (figa4) and V795 Her (figa5).
Acknowledgements: Christina Papadaki, christip(at)ksb-orb.oma.be
(End) C. Papadaki [Royal Obs. of Belgium, VUB], P. Vannier [CDS] 31-Mar-2006
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

catalogue service

© UDS/CNRS

Contact