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Properties of AGB variables in the intermediate-age cluster NGC 419 in the SMC

Published online by Cambridge University Press:  12 April 2016

Toshihiko Tanabé ,
Yoshifusa Ita ,
Noriyuki Matsunaga ,
Yoshikazu Nakada  and
IRSF/SIRIUS team
Toshihiko Tanabé
Affiliation:
Institute of Astronomy, School of Science, The University of Tokyo, Mitaka, Tokyo, 181-0015, Japan
Yoshifusa Ita
Affiliation:
Institute of Astronomy, School of Science, The University of Tokyo, Mitaka, Tokyo, 181-0015, Japan
Noriyuki Matsunaga
Affiliation:
Institute of Astronomy, School of Science, The University of Tokyo, Mitaka, Tokyo, 181-0015, Japan
Yoshikazu Nakada
Affiliation:
Institute of Astronomy, School of Science, The University of Tokyo, Mitaka, Tokyo, 181-0015, Japan Kiso Observatory, School of Science, The University of Tokyo, Mitake, Kiso, Nagano, 397-0101, Japan
IRSF/SIRIUS team
Affiliation:
Department of Astrophysics, Nagoya University, Chikusa-ku, Nagoya, 464-8602, Japan National Astronomical Observatory of Japan, Mitaka, Tokyo, 181-0015, Japan

Abstract

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We found that the OGLE database contains most AGB stars associated with the SMC cluster NGC 419. Combining these data with our near-infrared (NIR) data, we obtained the following results: 1) Almost all AGB stars above the TRGB are variables. 2) Large amplitude variables tend to show more regular light curves. 3) Only the tip AGB stars (in this case, carbon stars) increase their amplitudes with their J – K colors and only the most evolved ones can become large amplitude (Mira-like) variables. 4) AGB variables may explain the sequences found by Wood et al. (1999).

Type
Part 5. Red Giants, Miras, post-AGB stars and proto-planetary nebulae
Information
International Astronomical Union Colloquium , Volume 193: Variable Stars in the Local Group , 2004 , pp. 295 - 303
Copyright
Copyright © Astronomical Society of the Pacific 2004

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