CC BY
42"Peremennye Zvezdy", Prilozhenle,
vol. 20, N 3 (2020)
14 New Eclipsing Variables
A. V. Khruslov#1'2
#1. Sternberg Astronomical Institute, Lomonosov Moscow State University, Moscow, Russia; #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: khruslov@bk.ru)
# |Name| Other Coord (J2000) Type Max Min System Period Epoch (JD) iype Sp. Comment L.Curve Find.Chart Data
1 GSC 03695-01701 02 27 49.01 +56 39 43.4 EA 10.79 11.00 V 4.21857 2454000.650 min Comm. 1 lc 01.PNG ch 10.PNG dt a 01.txt dt n 01.txt dt w 01.txt
2 GSC 03699-01986 02 37 11.20 +58 22 02.3 EA 13.30 13.69 V 2.544617 2457777.594 min Comm. 2 lc 02.PNG ch 02.PNG dt a 02.txt dt n 02.txt dt w 02.txt
3 GSC 03713-00648 02 54 16.39 +58 30 25.1 EA 11.01 11.14 V 2.394144 2457778.69 min Comm. 3 lc 03.PNG ch 03.PNG dt a 03.txt dt n 03.txt dt w 03.txt
4 GSC 03709-00539 02 54 24.96 +58 01 59.7 EB 11.47 11.56 V 1.85959 2457777.74 min Comm. 4 lc 04.PNG ch 04.PNG dt a 04.txt dt n 04.txt dt w 04.txt
5 GSC 03331-00963 04 05 17.67 +48 29 47.9 ELL 11.79 11.86 V 5.16915 2457779.29 min Comm. 5 lc 05.PNG ch 05.PNG dt a 05.txt dt n 05.txt dt w 05.txt
6 USN0-B1.0 1371-0127827 04 28 22.67 +47 11 47.9 EA 14.80 15.15 V 1.193945 2457778.188 min Comm. 6 lc 06.PNG ch 06.PNG dt a 06.txt dt w 06.txt
7 GSC 02897-00549 04 47 34.83 +41 03 52.0 ELL 12.06 12.11 V 0.519415 2457777.357 min Comm. 7 lc 07.PNG ch 07.PNG dt a 07.txt dt w 07.txt
8 GSC 02897-00982 04 48 21.23 +39 39 21.2 ELL 11.71 11.74 V 0.456521 2457777.021 min Comm. 8 lc 08.PNG ch 08.PNG dt a 08.txt dt w 08.txt
9 GSC 02898-00479 04 53 43.01 +41 01 54.3 EA 10.36 10.59 V 2.187770 2457778.897 min Comm. 9 lc 09.PNG ch 09.PNG dt a 09.txt dt n 09.txt dt w 09.txt
10 GSC 02898-01983 04 54 53.60 +39 52 11.7 EA 9.59 9.80 V 2.592917 2457779.180 min Comm. 10 lc 10.PNG ch 10.PNG dt a 10.txt dt n 10.txt dt w 10.txt
11 GSC 02902-03186 04 57 36.94 +42 23 15.8 EA 13.63 14.24 g 185.19 2458465.9 min Comm. 11 lc 11.PNG ch 11.PNG dt a 11.txt dt n 11.txt dt w 11.txt
12 GSC 02397-00879 05 06 35.04 +35 17 45.7 EB 10.11 10.21 V 2.31662 2457778.36 min Comm. 12 lc 12.PNG ch 12.PNG dt a 12.txt dt n 12.txt dt w 12.txt
13 GSC 03345-02514 05 11 49.75 +45 24 57.1 EB 11.56 11.70 V 0.838287 2457777.012 min Comm. 13 lc 13.PNG ch 13.PNG dt a 13.txt dt n 13.txt dt w 13.txt
14 GSC 00733-01267 06 37 30.10 +08 15 16.5 ELL 11.97 12.07 V 0.329092 2457777.300 min Comm. 14 lc 14.PNG ch 14.PNG dt a 14.txt dt n 14.txt dt a3 14.txt
Comments:
1. D = 0.07 P. Minll = 10m.89 (V). From the 1SWASP data, 11m.08 - 11m.30, Minll = 11m. 16; from the ROTSE-I/NSVS data, 11m.21 - 11m.43 (R), Minll = 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. Minll = 13m.35 (V). From the 1SWASP data, 13m.52 - 13m.93, Minll = 13m.57; from the ROTSE-I/NSVS data, 13m.25 - 13m.60 (R), Minll = 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. Minll = 11m52 (V). From the 1SWASP data, 11m47 - 11m55, Minll = 11m52; from the ROTSE-I/NSVS data, 11m.31 - 11m.40, Minll = 11m35 in the R band. J-K = 0.26 (2MASS).
5. Minll = 11m.855 (V). From the 1SWASP data, 12m.04 - 12m11; 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 + 0.45648xE ; 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). Remarks:
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. Wozniak 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 theOMC2ASCII 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. Pi, 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. References:
Butters, O.W., West, R.G., Anderson, D.R., et al., 2010, Astron. and Astrophys., 520, L10 Gaia Collaboration, Brown, A.G.A., Vallenari, A., et al., 2018, Astron. and Astrophys., 616, A1 Jayasinghe, T., Kochanek, C.S., Stanek, K.Z., et al., 2018, Mon. Not. Royal Astron. Soc., 477, 3145 Kochanek, C.S., Shappee, B.J., Stanek, K.Z., et al., 2017, Publ. Astron. Soc. Pacific, 129, 104502 Pojmanski, G., 2002, Acta Astron., 52, 397
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
Sokolovsky, K.V., 2007, Perem. Zvezdy Prilozh., 7, No. 30
Wozniak, P.R., Vestrand, W.T., Akerlof, C.W., et al., 2004, Astron. J., 127, 2436
