Peremennye Zvezdy

Article in PDF
"Peremennye Zvezdy",
Prilozhenie
,
vol. 20, N 4 (2020)

Seven New Eclipsing Binaries

A. V. Khruslov#1,2, A. V. Kusakin#3, I. Reva#3
#1. Sternberg Astronomical Institute, Lomonosov Moscow State University, Moscow, Russia;
#2. Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia;
#3. Fesenkov Astrophysical Institute, Almaty, Kazakhstan.

ISSN 2221–0474 DOI: 10.24411/2221-0474-2020-10017

Received:   19.03.2020;   accepted:   22.12.2020
(E-mail for contact: khruslov@bk.ru, un7gbd@gmail.com)


#NameOtherCoord (J2000)TypeMaxMinSystemPeriodEpoch (JD)typeSpCommentL.CurveFind.ChartData
1 USNO-B1.0 1466-005461401 32 41.85 +56 40 41.4EW17.4517.98V0.44192456954.324min Comm. 1lc_1.PNGch_1.PNGdt1_B.txt dt1_V.txt dt1_R.txt
2 USNO-B1.0 1423-043769121 13 02.09 +52 20 45.6EW17.8018.45V0.301622456870.111min Comm. 2lc_2.PNGch_2.PNGdt2_B.txt dt2_V.txt dt2_R.txt
3 2MASS 22014813+545221722 01 48.13 +54 52 21.7EA16.2216.49V0.701252456955.220min Comm. 3lc_3.PNGch_3.PNGdt3_B.txt dt3_V.txt dt3_R.txt
4 USNO-B1.0 1446-038613522 02 16.44 +54 40 00.9EA15.2815.49V2.103182457230.274min Comm. 4lc_4.PNGch_4.PNGdt1_B.txt dt1_V.txt dt1_R.txt
5 USNO-B1.0 1446-038620122 02 20.09 +54 36 59.3EW17.0017.44V0.388082457200.055min Comm. 5lc_5.PNGch_5.PNGdt1_B.txt dt1_V.txt dt1_R.txt
6 USNO-B1.0 1447-038486122 02 50.86 +54 43 47.8EA16.2016.78V0.534052456947.288min Comm. 6lc_6.PNGch_6.PNGdt1_B.txt dt1_V.txt dt1_R.txt
7 USNO-B1.0 1447-038488922 02 53.59 +54 46 17.4EW16.8317.47V0.4582322457006.139min Comm. 7lc_7.PNGch_7.PNGdt1_B.txt dt1_V.txt dt1_R.txt

Comments:


1. MinII = 17m.95 (V). For the B band, 18m.15 – 18m.7, MinII = 18m.7. for the R band, amplitude 0m.50; MinII = 0m.48 (delta R).

2. MinII = 18m.40 (V). For the B band, 19m.35 – 20m.1, MinII = 19m.9; for the R band, amplitude 0m.63.

3. D = 0.16 P. MinII = 16m.46 (V). For the B band, 17m.52 – 17m.76: ; for the R band, amplitude 0m.24, MinII = 0m.24 (delta R). Close companion (distance 6″) 2MASS 22014778+5452166, in USNO-B1.0 catalog pair is not resolved.

4. D = 0.14 P. MinI exhibits s total eclipse, d = 0.06 P. MinII = 15m.36 (V). For the B band, 15m.78 – 15m.99, MinII = 15m.86; for the R band, amplitude 0m.20, MinII = 0m.09 (delta R).

5. MinII = 17m.42 (V). For the B band, 17m.81 – 18m.32, MinII = 18m.32; for the R band, amplitude 0m.45, MinII = 0m.42 (delta R);

6. D = 0.19 P. For the B band, 17m.15 – 17m.80; for the R band, amplitude 0m.54.

7. MinII = 17.41 (V). For the B band, 17m.85 – 18m.5, MinII = 18m.45; for the R band, amplitude 0m.63, MinII = 0m.57 (delta R)

Remarks:
We present our discovery of seven new eclipsing binaries. Our CCD observations in the Johnson B, V and R bands were performed at the Tien Shan Astronomical Observatory of the V.G. Fesenkov Astrophysical Institute, at the altitude of 2750 m above the sea level. Our observations were performed with the eastern Zeiss 1000-mm reflector (the focal length of the system was 6650 mm; the detector was an Apogee U9000 D9 CCD camera; the chip was cooled to –40°C).

Reductions were performed using the MaxIm DL aperture photometry package. Magnitudes of the comparison stars (in Johnson's B and V bands) were taken from the AAVSO Photometric All-Sky Survey (APASS) catalog. The R-band observations could be presented only as magnitude differences with respect to the comparison star. In the Comments for the R band, the total variability amplitude is given.

These observations were analyzed using the period-search software developed by Dr. V.P. Goranskij. The coordinates were drawn from the Gaia DR2 catalog (Gaia Collaboration et al. 2018). All studied stars are not detected as a variables in Gaia DR2 project. The variables were classified according to the GCVS classifications (Samus et al. 2017).

The light elements for one star (No. 4) were calculated using ASAS-SN data (Shappee et al. 2014 and Kochanek et al. 2017)

Acknowledgments: The authors are grateful to Dr. V. P. Goranskij for providing light-curve analysis software. We wish to thank M.A. Krugov, N.V. Lichkanovsky, I.V. Rudakov, and R.I. Kokumbaeva for their assistance during the observations. This study was carried out within the framework of Project No. BR05236322 "Studies of physical processes in extragalactic and galactic objects and their subsystems", financed by the Ministry of Education and Science of the Republic of Kazakhstan.

References:
Gaia Collaboration, Brown, A.G.A., Vallenari, A., et al., 2018, Astron. and Astrophys., 616, A1
Kochanek, C. S., Shappee, B. J., Stanek, K. Z., et al., 2017, Publ. Astron. Soc. Pacific, 129, 104502
Samus, N.N., Kazarovets, E.V., Durlevich, O.V., Kireeva, N.N., Pastukhova, E.N., 2017, General Catalogue of Variable Stars: Version GCVS 5.1, Astron. Rep., 61, No. 1, 80
Shappee, B. J., Prieto, J. L., Grupe, D., et al., 2014, Astrophys. J., 788, 48



Main Page | Search
Astronet | SAI | INASAN

Report problems