, Volume 57, Issue 4, pp 510–519 | Cite as

Investigation of Faint Galactic Carbon Stars from the First Byurakan Spectral sky Survey. Optical Variability. I. N-Type AGB Carbon Stars. K-band Absolute Magnitudes and Distances

  • K. S. Gigoyan
  • A. Sarkissian
  • D. Russeil
  • N. Mauron
  • G. Kostandyan
  • R. Vartanian
  • H. V. Abrahamyan
  • G. M. Paronyan

The goal of this paper is to present an optical variability study of the comparatively faint carbon (C) stars which have been discovered by searching the First Byurakan Survey (FBS) low-resolution (lr) spectral plates at high Galactic latitudes using recent wide-area variability databases. The light curves from the Catalina Sky Survey (CSS) and Northern Sky Variability Survey (NSVS) databases were exploited to study theit variability nature. In this paper, first in this series, the variability classes are presented for 54 N-type Asymptotic Giant Branch (AGB) C stars. One finds that 9 stars belongs to the group of Mira-type, 43 are Semi-Regular (SR), and 2 stars are Irregular (Irr)-type variables. The variability types of 27 objects has been established for the first time. K-band absolute magnitudes, distances, and height from the Galactic plane were estimated for all of them. We aim to better understand the nature of the selected C stars through spectroscopy, 2MASS photometric colors, and variability data. Most of the tools used in this study are developed within the framework of the Astronomical Virtual Observatory.


stars N-type AGB stars variability K-band luminosity distances 


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Copyright information

© Springer Science+Business Media New York 2014

Authors and Affiliations

  • K. S. Gigoyan
    • 1
  • A. Sarkissian
    • 2
  • D. Russeil
    • 3
  • N. Mauron
    • 4
  • G. Kostandyan
    • 1
  • R. Vartanian
    • 5
  • H. V. Abrahamyan
    • 1
  • G. M. Paronyan
    • 1
  1. 1.V.A. Ambartsumian Byurakan Astrophysical ObservatoryByurakanArmenia
  2. 2.Universite de Versailles Saint-Quentin, CNRS/INSU, LATMOS-IPSLVersaillesFrance
  3. 3.Laboratoire d’Astrophysique de Marseille, CNRS-AMUMarseilleFrance
  4. 4.Laboratoire Univers et Particules de Montpellier, UMR 5299 CNRS & Universite Montpellier IIMontpellierFrance
  5. 5.LA TestingSouth PasadenaUSA

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