Peremennye Zvezdy

"Peremennye Zvezdy",
Prilozhenie
,
vol. 13, N 13 (2013)

VBIc Photometry for Five Eclipsing Variables

L. N. Berdnikov#1, E. N. Pastukhova#2
#1. Sternberg Astronomical Institute, Lomonosov State University, Moscow, Russia
#2. Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia

Received:   9.04.2013;   accepted:   7.10.2013
(E-mail for contact: leonid.berdnikov@gmail.com, pastukhova@sai.msu.ru)


#NameOtherCoord (J2000)TypeMaxMinSystemPeriodEpoch (JD)typeSpCommentL.CurveFind.ChartData
1 ASAS 052606-6710.905 26 06.19, -67 10 56.8EB12.3212.70V3.3015352454816.370minOBComm. 11lc.jpg1ch.jpg1.txt
2 ASAS 063847-3108.006 38 47.58, -31 07 56.2EW13.0513.50V0.7067652454844.319min Comm. 22lc.jpg2ch.jpg2.txt
3EZ MonASAS 070525-0510.607 05 25.39, -05 10 37.0EW12.6013.40V0.7523342455578.488min Comm. 33lc.jpg3ch.jpg3.txt
4 ASAS 074522-2400.207 45 22.32, -24 00 13.5EB11.6511.85V2.2426372454480.449min Comm. 44lc.jpg4ch.jpg4.txt
5 ASAS 200559-0159.920 05 58.40, -01 59 53.0EW:12.2312.45V1.0521822456063.540min Comm. 55lc.jpg5ch.jpg5.txt

Comments:


1. MinII = 12m.65. B–V = –0.11, J–K = –0.2.

2. MinII = 13m.43. B–V = 0.42, J–K = 0.21. This star was discovered in the ASAS-3 survey and enters their variable-star catalog as EC/DCEP-F0 but with a wrong period (2d.4179).

3. MinII = 13m.35. B–V = 0.60, J–K = 0.22.

4. MinII = 11m.80. B–V = 0.35, J–K = 0.09.

5. MinII = 12m.40. B–V = 0.81, J–K = 0.41.

Remarks:
In 2006–2012, we performed photometric observations of selected variable stars with the 76-cm telescope of the South African Astronomical Observatory (SAAO, Republic of South Africa). Photoelectric photometer was used before JD 2454480 and an SBIG ST-10XME CCD camera was used after JD 2454480. For all frames, we used BVI filters of the Kron–Cousins system (Cousins 1976). We found that 4 stars which were suspected to be pulsating variables (EZ Mon is in GCVS, Samus et al. 2007–2012; stars 1, 4, and 5 are in the ASAS-3 project, Pojmanski 2002), have proved to be eclipsing binaries. Later we revealed that EZ Mon was already detected in the ASAS-3 project as an eclipsing variable with a period of 0.75234 days. Periods for other stars were determined by us and we could confirm the value of period thanks to the publicly available electronic archives of CCD observations of the ASAS-3 project.

Acknowledgments: Our studies are supported by grants from the Russian Foundation for Basic Research (grants No. 10-02-00489, 11-02-00495, 13-02-00203 and 13-02-00664) and from the Program "Origin and Evolution of Stars and Galaxies" of the Presidium of Russian Academy of Science. We wish to thank the administration of the SAAO for allocation of the telescope time.

References:
Cousins, A.W.J., 1976, Mem. R. Astron. Soc., 81, 25
Pojmanski, G., 2002, Acta Astronomica, 52, 397
Samus, N.N., Durlevich, O.V., Kazarovets, E V., Kireeva, N.N., Pastukhova E.N., et al., 2007–2012, General Catalogue of Variable Stars, Centre de Données Astronomiques de Strasbourg, B/gcvs



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