New Light Elements for Seventeen Stars of Different Variability Types

E. V. Kazarovets
Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia

Received:   22.05.2023;   accepted:   6.07.2023
(E-mail for contact: helene@inasan.ru)

Comments:


1. Min II = 13.69 V, D = 0.20 P. The star was included in ASAS-SN Variable Stars Database (Jayasinghe et al. 2018) with a type EA and P = 1.3888681 d.

2. M – m = 0.35 P. The star was included in ASAS-SN Variable Stars Database (Jayasinghe et al. 2018) with a type CWB and P = 1.1509774 d.

3. Min II = 14.24 g, D = 0.12 P. Variability was discovered by the author using the ASAS-SN photometric data.

4. = ASASSN-V J180240.32-331414.9 (see Iwanek et al. 2022). Variability of this star was independently discovered by the author using the STScI plates archive.

5. Variability of this star was discovered by the author using the STScI plates archive.

6. Variability of this star was discovered by the author using the STScI plates archive. The star was included in ASAS-SN Variable Stars Database (Jayasinghe et al. 2018) with the type YSO and no period. The ASAS-SN photometry in V- and g-bands in common was used for period determination. Magnitudes in g were adjusted by –1 mag.

7. N-comp. of 3" pair. Variability of this star was discovered by the author using the STScI plates archive. The ASAS-SN photometry in V- and g-bands, and ZTF photometry in zr-band in common were used for period determination. Magnitudes in g were adjusted by –1 mag.

8. Min II = 11.23 g. The star was suspected by Borrelly (1885) who did not publish a finding chart. Recovered by the author using the ASAS-SN photometric data.

9. Min II = 15.89 zg, D = 0.02 P. Min II – Min I = 0.785 P. The variability was discovered by Lapukhin et al. (2018a) who published an incorrect P = 4.16: d.

10. Min II = 14.55 zr, D = 0.02 P. Min II – Min I = 0.68 P. The variability was discovered by Lapukhin et al. (2018b) who published an incorrect P = 1.7708: d.

11. M – m = 0.40 P. Blazhko effect. The variability was discovered by Lapukhin et al. (2018a) who gave type BY and erroneous P = 16.24 d.

12. Pulsation cycle P ~ 73 d. The variability was discovered by Lapukhin et al. (2020) with a type LB. The star was included in the ZTF Catalog of Variable Stars (Chen et al. 2020) with a type SR and P = 70.4 d.

13. Min II = 14.06 zr, D = 0.04 P. The variability of 2MASS J22451103+5455516 was discovered by Lapukhin et al. (2020) with incorrect P = 1.4045: d.

14. Min II = 14.42 g, D = 0.08 P. The variability of 2MASS J22462507+5416558 was discovered by Lapukhin et al. (2020) with incorrect P = 0.68802 d and a type EW. There is a faint companion at 2".2 N. It is not excluded that the companion is the actual variable.

15. Min II = 15.22 zr, D = 0.08 P. Distortion wave P = 7.36 d. The variability of 2MASS J22470097+5252338 was discovered by Lapukhin et al. (2020) with incorrect P = 2.3786: d and a type EA.

16. Min II = 13.81 V, D = 0.03 P. Min II - Min I = 0.460. The variability of 2MASS J22503120+5351341 was discovered by Lapukhin et al. (2021) with incorrect P = 1.8013: d.

17. Min II = 15.62 zg, D = 0.05 P. The variability of 2MASS J22515854+5318505 was discovered by Lapukhin et al. (2021) with incorrect P = 0.727191 d.

Remarks:
While working on compiling of the next Name-List for Version 5.1 of the General Catalogue of Variable Stars (GSVS, Samus et al. 2017), I determined types, light elements and improved coordinates for 4 new variable stars, 3 more stars from the NSV catalogue (Kazarovets et al. 2022) and 10 new variables, discovered and published by other authors to transfer them to the GCVS. The study of the variables was made using the publicly available electronic archive of CCD observations of the Sky Patrol of the All-Sky Automated Survey for Supernovae (ASAS-SN) project (Shappee et al. 2014, Kochanek et al. 2017) and the Zwicky Transient Facility (ZTF) photometric data (Masci et al. 2019). For each star, I present archive observations. Information on the filter can be found in corresponding files.

To find periods I applied the WinEfk software provided by Dr. V.P. Goranskij and the on-line lightcurve analysis tool created by Dr. K.V. Sokolovsky.

References:
Borrelly, M.A., 1885, Bulletin astronomique, 2, 62
Chen, X., Wang, S., Deng, L., et al., 2020, Astrophys. J. Suppl., 249, 18
Iwanek, P., Soszyński, I., Kozłowski, S., et al., 2022, Astrophys. J. Suppl. Ser., 260, 46
Jayasinghe, T., Stanek, K.Z., Kochanek, C.S., et al., 2018, Mon. Not. Royal Astron. Soc., 486, No. 2, 1907
Kochanek, C.S., Shappee, B.J., Stanek, K.Z., et al., 2017, Publ. Astron. Soc. Pacific, 129, No. 980, 104502
Kazarovets, E.V., Samus, N.N., and Durlevich, O.V., 2022, Astron. Rep., 66, No. 7, 555
Lapukhin, E.G., Veselkov, S.A., and Zubareva, A.M., 2018a, Perem. Zvezdy Prilozh. (Var. Stars Suppl.), 18, No. 1
Lapukhin, E.G., Veselkov, S.A., and Zubareva, A.M., 2018b, Perem. Zvezdy Prilozh. (Var. Stars Suppl.), 18, No. 2
Lapukhin, E.G., Zubareva, A.M., Kryukova, E., and Khamrakulov, F., 2020, Perem. Zvezdy Prilozh. (Var. Stars Suppl.), 20, No. 2
Lapukhin, E.G., Zubareva, A.M., Kryukova, E., and Khamrakulov, F., 2021, Perem. Zvezdy Prilozh. (Var. Stars Suppl.), 21, No. 3
Masci, F.J., Laher, R.R., Rusholme, B., et al., 2019, Publ. Astron. Soc. Pacific, 131, No. 995, 018003
Samus, N.N., Kazarovets, E.V., Durlevich, O.V., Kireeva, N.N., Pastukhova, E.N., 2017, Astron. Rep. 61, No. 1, 80
Shappee, B.J., Prieto, J.L., Grupe, D., et al., 2014, Astrophys. J., 788, 48