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NSVS 5907410 = MISAO V1119: a Mira variable confirmed

by Siarhey Hadon in November-December 2013 (#3)

Abstract: Details of a Mira variable in the constellation of Cygnus are presented. The variability of the NSVS 5907410 source was detected in January of 2012 by Ivan Adamin, based on photometric data from the Northern Sky Variability Survey, as a part of data mining project, the VS-COMPAS. Lately, by the time the star's data was finally analyzed in 2013, the object was identified as the Mis V1119 classified as possible semi-regular. Thus, a revision with actual data was submitted.
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Mira variables named after the star Mira (o Ceti), belong to a class of pulsating variable stars characterized by very red colors, pulsation periods mostly between 100 and 800 days, and amplitudes greater than one magnitude in infrared and 2.5 magnitude at visual wavelengths by definition.

In this paper a revision of MISAO V1119 variable is presented. Initially, the star discovered by Seiichi Yoshida, MISAO Project; Nobuo Ohkura, Okayama, Japan; and Ken-ichi Kadota, MISAO Project.

During the candidates selection process in the constellation of Cygnus as a part of data mining activity performed by VS-COMPAS Project team in January of 2012, the source identified as NSVS 5907410 was considered a variable. Later, by combining MISAO data with the photometry from the Northern Sky Variability Survey the variability class was determined as Mira.

The Northern Sky Variability Survey (Woniak etź al., 2004) has a moderate resolution, so there are cases when the source object for the photometric set is uncertain in the crowded fields. The pictures made by the MISAO clearly demonstrate that the object in the area referencing by NSVS 5907410 is the unique variable source among its neighbors.

Detailed analysis was made by Siarhey Hadon in November of 2013. Periodogram analysis of data for MISAO V1119 revealed a strong peak (cf. Figure 2) around a period value of 450 days. Photometric data points used were gathered by Nobuo Ohkura. This value has a good match with the blended NSVS data, for which a deblending was performed. Otherwise, the NSVS data is not enough to make a reliable decision about the proper period.

The target star is in a crowded area, so the light curve data from the NSVS database was contaminated by the following non-variable neighbor stars:
2MASS J21255941+4149369 (J-K= 0.81, V= 17.4, sep. 14"),
2MASS J21255855+4150082 (J-K= 0.64, V= 17.3, sep. 19"),
2MASS J21255780+4150086 (J-K= 0.77, V= 17.5, sep. 23"),
2MASS J21260015+4149259 (J-K= 0.56, V= 16.3, sep. 27"),
2MASS J21255733+4150122 (J-K= 0.93, V= 17.3, sep. 29"),
2MASS J21255585+4149505 (J-K= 0.96, V= 14.5, sep. 35"),
2MASS J21255877+4149089 (J-K= 0.61, V= 16.0, sep. 41"),
2MASS J21260005+4149088 (J-K= 0.74, V= 17.2, sep. 43"),
2MASS J21255800+4149051 (J-K= 0.70, V= 16.9, sep. 46").

Performed deblending of the light curve data allowed to find the real magnitude range. Taking in to consideration other properties of the star and its color index, it was classified as a Mira variable. The revision is submitted to the VSX.

Below there is a phased light curve along with a short summary for the NSVS 5907410 is presented. This is a typical light curve for Miras (cf. Figure 3).

In October 2013 ESA had to postpone Gaia's original launch date, due to a precautionary replacement of two of Gaia's transponders, which are used to generate timing signals for the downlink of science data. Around 3 weeks is needed for Gaia to reach its designated orbit around the L2 point.This research has made use of the SIMBAD and VizieR databases operated at the Centre de Données Astronomiques (Strasbourg) in France; of the International Variable Star Index (AAVSO), and of the Two Micron All Sky Survey (2MASS). Period search and analysis software is created by Andrey Prokopovich and Ivan Adamin, members of the VS-COMPAS data mining project.

Appendix. Table1 provides a summary data about the target star.

View Issue Contents (November-December 2013)

  • S. Yoshida, 2012, MISAO Project (online: http://www.aerith.net/misao/data/misv.cgi?1119)
  • S. Yoshida, 2000, MISAO New Variable Stars (online: http://www.aerith.net/misao/data/misv.cgi).
  • Watson, C.; Henden, A. A.; Price, A.,2006-2010, AAVSO International Variable Star Index VSX, VizieR On-line Data Catalog: B/vsx
  • Percy, J. R., 2007, "Understanding variable stars", Cambridge University Press
  • Samus, N. N.; Durlevich, O. V.; Kazarovets, E. V.; Kireeva, N. N.; Pastukhova, E. N.; Zharova, A. V. et al., 2007-2013, General Catalogue of Variable Stars, VizieR On-line Data Catalog, B/gcvs
  • Sterken, C.; Jaschek, C., 1996, "Light Curves of Variable Stars, A Pictorial Atlas", Cambridge University Press
  • Lafler, J.; Kinman, T. D., 1965, Astrophysical Journal Supplement, 11, 216
  • Henden, Arne A.; Smith, T. C.; Levine, S. E.; Terrell, D., AAS Meeting #220, #133.06
  • Woniak, P. R. et al., 2004, The Astronomical Journal, 127, 2436

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