Received: 2.12.2019; accepted: 18.12.2019
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1. X-ray source 1WGA J2035.8+3257.
2. Min II = 13.98 V. The star was included in the ASAS-SN Catalog of Variable Stars II (Jayasinghe et al. 2018) with a type ROT and period of 9d.8185186 .
3. The star was suspected by Leavitt (1906) without published finding chart. It recovered by me using the ASAS-SN photometric data. Min II = 15.02 V, D = 0.10 P.
4. Min II = 14.45 V, D = 0.20 P.
5. The star was suspected by Leavitt (1906) without published finding chart. It recovered by us using the ASAS-SN photometric data.
6. Min II = 14.74 V, D = 0.12 P.
7. Mira type and Min <17.0 V are not excluded. I measured minimal brightness using DSS images of the STScI Archive: V = 17.0 on the Quick-V Northern plate (1983-08-12), B = 18.4 on the POSS-II blue plate (1989-07-01), R = 15.7 on the POSS-II red plate (1992-06-29).
8. Min II = 15.8 V, D = 0.04 P.
9. Min II = 15.08 V.
10. Neighbor of NSV 13535. Variability of this star was discovered by me using DSS images of the STScI Archive. For example, R = 15.0 on the POSS-I red plate (1954-07-05) and R = 18.0 on the POSS-II red plate (1991-07-09).
11. Min II = 15.96 V, D = 0.08: P.
13. Min II = 16.14 V.
14. The star was suspected by Shapley and Hughes (1934) without published finding chart. It was found, upon my request, by the late Dr. M. Hazen in Harvard Observatory's logbooks. M – m = 0.30 P.
15. The star was suspected by Shapley and Hughes (1934) without published finding chart. It was found, upon my request, by the late Dr. M. Hazen thanks to the author's marks on Harvard Observatory's photographic plates. The star was included in the ASAS-SN Catalog of Variable Stars II (Jayasinghe et al. 2018) with a type SR and period of 81d.9892624.
In the current paper, I continue to announce the preparation of the new electronic version of the New Suspected Variables Catalogue. While working on compiling of the Name-List No. 82 for Version 5.1 of GCVS (Samus et al. 2017), I determined types, light elements and improved coordinates for 1 new variable star and 14 more stars from the NSV catalogue (Kukarkin et al. 1982) to transfer them to the General Catalogue of Variable Stars. The study of the variables was made using the publicly available electronic archive of CCD observations of the Sky Patrol All-Sky Automated Survey for Supernovae (ASAS-SN) project (Shappee et al. 2014, Kochanek et al. 2017). I measured brightness of large part of the Mira variables using Digitized Sky Survey images (B, V, R bands) of the Space Telescope Science Institute Archive (the STScI Digitized Sky Survey). To find periods, I applied the WinEfk software provided by Dr. V.P. Goranskij and the on-line lightcurve analysis tool of Dr. K.V. Sokolovsky.
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
Kukarkin, B. V., Kholopov, P. N., et al., 1982, New catalogue of suspected variable stars. Moscow: "Nauka"
Leavitt, H.S., 1906, Harvard Circ., No. 107
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, pp. 80–88
Shapee, B. J., Prieto, J. L., Grupe, D., et al., 2014, Astrophys. J., 788, No. 1, article id. 48
Shapley, H., and Hughes, E.M., 1934, Harvard Annals, 90, No. 4, 163