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A Spectroscopic Study of Blue Stragglers in M67

Published online by Cambridge University Press:  01 April 2008

G. Q. Liu ,
L. Deng ,
M. Chávez  and
E. Bertone
G. Q. Liu
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, P. R. China email: lgq@bao.ac.cn, licai@bao.ac.cn Graduate University of ChineseAcademy of Sciences, Beijing 100049, P. R. China
L. Deng
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, P. R. China email: lgq@bao.ac.cn, licai@bao.ac.cn
M. Chávez
Affiliation:
INAOE - Instituto Nacional de Astrofísica, Óptica y Electrónica, Luis Enrique Erro 1 - 72840 Tonantzintla, Puebla, Mexico email: mchavez@inaoep.mx, ebertone@inaoep.mx
E. Bertone
Affiliation:
INAOE - Instituto Nacional de Astrofísica, Óptica y Electrónica, Luis Enrique Erro 1 - 72840 Tonantzintla, Puebla, Mexico email: mchavez@inaoep.mx, ebertone@inaoep.mx
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Abstract

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Spectrophotometric observations of the complete sample of twenty four blue stragglers (BSs) in the old galactic open cluster M67 (NGC2682) have been collected, using the Guillermo Haro Observatory in Cananea, Mexico. All the calibrated spectra were re-calibrated by the Beijing Arizona Taipei Connecticut (BATC) photometric system which includes fluxes in 11 photometric bands covering ~3600–10000 Å. The goal of the current work is to provide observational constraints on spectral properties of BSs by determining the effective temperature (Teff) and surface gravity (log g). The overall results, obtained by applying the flux fitting method, indicate that Teff and surface gravities of BSs in M67 are fully compatible with those expected for main sequence stars.

Keywords

Stars: blue stragglers – Stars: Hertzsprung-Russell (HR) diagram – Galaxy: open clusters and associations: individual: M67
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S252: The Art of Modeling Stars in the 21st Century , April 2008 , pp. 391 - 397
Copyright
Copyright © International Astronomical Union 2008

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