|Article in PDF||
vol. 20, N 3 (2020)
|#1. Sternberg Astronomical Institute, Lomonosov Moscow State University, Moscow,
#2. Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia.
|ISSN 2221–0474||DOI: 10.24411/2221-0474-2020-10016|
Received: 17.03.2020; accepted: 22.12.2020
(E-mail for contact: firstname.lastname@example.org)
1. D = 0.07 P. MinII = 10m.89 (V). From the 1SWASP data, 11m.08 – 11m.30, MinII = 11m.16; from the ROTSE-I/NSVS data, 11m.21 – 11m.43 (R), MinII = 11m.31 in the R band. J–K = 0.08 (2MASS).
2. D = 0.10 P. Total eclipse with duratioh d = 0.02 P is possible. MinII = 13m.35 (V). From the 1SWASP data, 13m.52 – 13m.93, MinII = 13m.57; from the ROTSE-I/NSVS data, 13m.25 – 13m.60 (R), MinII = 13m.31: in the R band. J–K = 0.43 (2MASS).
3. D = 0.09 P. MinII = 11m.135 (V). From the 1SWASP data, 11m.16 – 11m.30, MinII = 11m.28; from the ROTSE-I/NSVS data, 11m.16 – 11m.27, MinII = 11m.27 in the R band. J–K = 0.22 (2MASS).
4. Asymmetrical phases of maxima: 0.28 P for MaxI, 0.72 P for MaxII. MinII = 11m.52 (V). From the 1SWASP data, 11m.47 – 11m.55, MinII = 11m.52; from the ROTSE-I/NSVS data, 11m.31 – 11m.40, MinII = 11m.35 in the R band. J–K = 0.26 (2MASS).
5. MinII = 11m.855 (V). From the 1SWASP data, 12m.04 – 12m.11; from the ROTSE-I/NSVS data, 12m.05 – 12m.13 in the R band. J–K = 0.15 (2MASS).
6. D = 0.07 P. From the 1SWASP data, 15m.1 – 15m.5; J–K = 0.56 (2MASS).
7. MinII = 12.105 (V). From the 1SWASP data, 12m.26 – 12m.31, MinII = 12m.305; J–K = 0.33 (2MASS).
8. Period varies. Two systems of the light elements for two series of data. Elements for the ASAS-SN are given in table; from the 1SWASP the light elements are HJD(min) = 2454111.320 + 0.45648×E ; MinII = 11m.73 (V). From the 1SWASP data, 11m.91 – 11m.94, MinII = 11m.94. J–K = 0.24 (2MASS).
9. D = 0.10 P. MinII = 10m.38 (V). From the 1SWASP data, 10m.57 – 10m.80, MinII = 10m.60; from the ROTSE-I/NSVS data, 10m.80 – 11m.06, MinII = 10m.84 in the R band. J–K = 0.31 (2MASS). The reflection effect with amplitude 0m.04 is well visible in all series of observations.
10. D = 0.08 P. MinII = 9m.71 (V). From the 1SWASP data, 9m.76 – 9m.95, MinII = 9m.88; from the ROTSE-I/NSVS data, 9m.93 – 10m.12, MinII = 10m.07 in the R band. J–K = 0.23 (2MASS).
11. D = 0.06 P. MinII = 14m.12 (g). From the ASAS-SN data, V-band range 12m.85 – >13m.29 (V), phase 0.00 was not observed, MinII = 13m.35 (V). Blend of two stars in the NSVS and the 1SWASP data (distance 25"), amplitude is underestimated. From the 1SWASP data, 12m.65 – 13m.05, MinII = 12m.99; from the ROTSE-I/NSVS data, 12m.20 – 12m.68, MinII = 12m.60 in the R band. J–K = 0.93 (2MASS). Included in the ASAS-SN Catalog of Variable Stars I with type L.
12. Mean magnitudes of the ASAS-SN data for two cameras are shifted by 0m.1 to each other. The V-band range of the ba camera is given in the table, MinII = 10m.18 (V). Range of the bb camera 10m.21 – 10m.31, MinII = 10m.27 (V) in the ASAS-SN data. From the 1SWASP data, 10m.44 – 10m.54, MinII = 10m.50; from the ROTSE-I/NSVS data, 10m.50 – 10m.61, MinII = 10m.57 in the R band. The apsidal motion is possible. In the 1SWASP and the NSVS data phase of MinII is 0.545 (1SWASP) and 0.535 (NSVS), in the ASAS-SN data phase of MinII is 0.505 (cam bb) and 0.510 (cam ba). J–K = 0.09 (2MASS).
13. MinII = 11m.67 (V). From the 1SWASP data, 11m.60 – 11m.73, MinII = 11m.70; from the ROTSE-I/NSVS data, 11m.86 – 12m.00 in the R band. O'Connell effect: from the ASAS-SN data, MaxII = 11m.59 (V); from the 1SWASP, MaxII = 11m.64; J–K = 0.27 (2MASS).
14. MinII = 12m.07 (V). From the ROTSE-I/NSVS data, 12m.05 – 12m.15, MinII = 12m.14 in the R band. from the ASAS-3 data, 11m.92 – 12m.02 (V). J–K = 0.37 (2MASS).
I present a study of 14 new eclipsing variable stars. I analyzed all observations of these stars available in the Northern Sky Variability Survey (NSVS, Woźniak et al. 2004), Wide Angle Search for Planets (SuperWASP, Butters et al. 2010), All-Sky Automated Survey for Supernovae (ASAS-SN, Shappee et al. 2014 and Kochanek et al. 2017). For one of the cases I used data of the All Sky Automated Survey (ASAS-3, Pojmanski 2002).
The variability of most stars (No. 1-5 and 9-14) was suspected by J.S. Shaw and his colleagues in 2008. They described the project at a website. The authors searched for variability of the objects automatically in the NSVS data. I looked through the data available in untyped.cat. Shaw and coauthors list two possible periods for each star in this catolog. Detected periods for some stars are often incorrect. There are many cases of false variability (these stars were not confirmed with other available photometric data archives). Therefore, the suspected variables of the untyped.cat are not included in the ASAS and the VSX databases. The appendix for this paper provides the periods 1 and 2 of suspected variables according to the list from untyped.cat.
One star (No. 11) is included in the ASAS-SN Catalog of Variable Stars I (Jayasinghe et al. 2018) as an irregular variable (L-type).
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 were not detected as a variables in Gaia DR2 project. The variables were classified according to the GCVS classification (Samus et al. 2017).
The SuperWASP observations are available as FITS tables, which were converted into ASCII tables using the OMC2ASCII program as described by Sokolovsky (2007).
The table photometric magnitudes are given according to ASAS-SN data (also, magnitude of MinII in Comments).
Appendix. Possible periods of the suspected variables according to J.S. Shaw and colaborators (see above).
No. P1, days P2, days 1 4.21649697 2.10776135 2 5.0930874 2.54292742 3 2.39467158 1.1973764 4 3.71987474 0.92951574 5 12.92821174 2.58447116 9 2.18699034 2.18736215 10 1.29633705 1.2966482 11 93.3874471 96.34513098 12 2.31682144 1.15893086 13 0.83800075 0.41898316 14 1.18178128 0.16451686
Acknowledgements: Thanks are due to Dr. K.V. Sokolovsky for his advice concerning data retrieving. The author wishes to thank Dr. V.P. Goranskij for providing his software.
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