, Volume 60, Issue 1, pp 70–82 | Cite as

Investigation of Faint Galactic Carbon Stars from the First Byurakan Spectral Sky Survey. III. Infrared Characteristics

  • K. S. GigoyanEmail author
  • A. Sarkissian
  • C. Rossi
  • D. Russeil
  • G. Kostandyan
  • M. Calabresi
  • F. Zamkotsian
  • M. Meftah

InfraRed (IR) astronomical databases, namely, IRAS, 2MASS, WISE, and Spitzer, are used to analyze photometric data of 126 carbon (C) stars whose spectra are visible in the First Byurakan Survey (FBS) low-resolution(lr) spectral plates. Among these, six new objects, recently confirmed on the digitized FBS plates, are included. For three of them, moderate-resolution CCD optical spectra are also presented. In this work several IR color-color diagrams are studied. Early and late-type C stars are separated in the JHK Near-InfraRed (NIR) color-color plots, as well as in the WISE W3-W4 versus W1-W2 diagram. Late N-type Asymptotic Giant Branch (AGB) stars are redder in W1-W2, while early-types (CH and R giants) are redder in W3-W4 as expected. Objects with W2-W3 > 1.0 mag. show double-peaked spectral energy distribution (SED), indicating the existence of the circumstellar envelopes around them. Twnty-six N-type stars have IRAS Point Source Catalog (PSC) associations. For FBS 1812+455, IRAS Low-Resolution Spectra (LRS) in the wavelength range 7.7 ÷ 22.6 μm and Spitzer Space Telescope Spectra in the range 5 ÷ 38μm are presented, clearly showing absorption features of C2H2 (acetylene) molecule at 7.5 and 13.7 μm, and the SiC (silicone carbide) emission at 11.3 μm. The mass-loss rates for eight Mira-type variables are derived from the K-[12] color and from the pulsation periods. The reddest object among the targets is N-type C star FBS 2213+421, which belongs to the group of the cold post-AGB R Coronae Borealis (R CrB) variables.


stars carbon stars Mira-type stars InfraRed characteristics mass-loss rate 


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Copyright information

© Springer Science+Business Media New York 2017

Authors and Affiliations

  • K. S. Gigoyan
    • 1
    Email author
  • A. Sarkissian
    • 2
  • C. Rossi
    • 3
  • D. Russeil
    • 4
  • G. Kostandyan
    • 1
  • M. Calabresi
    • 5
  • F. Zamkotsian
    • 4
  • M. Meftah
    • 2
  1. 1.V.A.Ambartsumian Byurakan Astrophysical ObservatoryByurakanArmenia
  2. 2.Universite de Versailles Saint-Quentin, CNRS/INSU, LATMOS-IPSLParisFrance
  3. 3.Dipartimento di FisicaUniversity di Roma La SapienzaRomaItaly
  4. 4.Laboratoire d Astrophysique de Marseille, CNRS-AMUMarseilleFrance
  5. 5.Associazione Romana Astrofili - Frasso Sabino ObservatoryFrasso Sabino RIItaly

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