Received: 18.07.2016; accepted: 29.12.2016
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3. Superposed variations with P = 47.3 d.
5. Superposed variations with P = 119 d.
6. Was suspected by Innes (1917). Recovered by us.
7. HV 10075 = 1RXS J185057.0-561148.
8. Was suspected by Luyten (1937). Recovered by us.
11. Was suspected by Luyten (1937). Recovered by us.
15. Was suspected by Luyten (1937). Recovered by us.
16. Was suspected by Luyten (1937). Recovered by us.
21. Discovered by Kooreman (1965).
22. M. Sitek and G. Pojmanski (2014) gave Mira type with a wrong period of 1173 d.
26. Was suspected by Luyten (1937). Recovered by us.
27. Was suspected by Luyten (1937). Recovered by us.
31. We proofed our P = 306 d using the NSVS data.
32. Was suspected by Luyten (1932). Recovered by us.
38. Was suspected by Luyten (1933). Recovered by us.
39. Was suspected by Luyten (1935). Recovered by us.
41. Was suspected by Hoffleit (1932). Recovered by us.
In the process of improving coordinates of variable stars in the electronic version of NSV catalog (Samus et al. 2007–2015), we determined light elements and types of variability for 40 red suspected variables. 1 variable was discovered when we were searching for Luyten's star NSV 11908. Finding charts for recovered variable stars mentioned in the comments are published for the first time. The study of the variables was made using the publicly available electronic archives of CCD observations of the ASAS-3 project (Pojmanski 2002) and the Catalina Sky Survey photometric data (Drake et al. 2009). We studied the variability of NSV 11740 and NSV 12009 in the Northern Sky Variability Survey (NSVS) data (Woźniak et al. 2004). We measured minimal brightness for many Mira variables using Digitized Sky Survey images (R-band) of the STScI Archive. Variability of 10 stars was discovered in the ASAS-3 survey; the stars enter in variable-star catalog as a MISC-type with a wrong periods: 72.35 d for #1, 182.75 d for NSV 11102, 52.96 d for NSV 11155, 121.9 d for NSV 11258, 97.1 d for NSV 11360, 127.1 d for NSV 11560, 128.8 d for NSV 11733, 67.91 d for NSV 11860, 240.2 d for NSV 11890, and 483.9 d for NSV 11941.
Acknowledgments: Our studies are partialy supported by a grant from the Program "Transition and explosive processes in the Universe" of the Presidium of Russian Academy of Science
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