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Period-K magnitude relations of variable stars in the LMC

Published online by Cambridge University Press:  12 April 2016

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

Abstract

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We cross-correlated the OGLE-II database with the SIRIUS JHK survey data in the Large Magellanic Cloud (LMC). After eliminating obvious spurious variables, we determined the pulsation periods for 9 681 stars by applying the Phase Dispersion Minimization (PDM) technique to the OGLE-II data. Based on these data, we studied the period-K magnitude (PK) relations of variable stars in the LMC and found a new sequence. Comparison between the theoretical pulsation model (Wood & Sebo 1996) and observational data suggests that the variable stars on the new sequence are Mira variables pulsating in the first overtone mode.

Type
Part 2. What variable stars tell us about the Local Group, including the distance scale
Information
International Astronomical Union Colloquium , Volume 193: Variable Stars in the Local Group , 2004 , pp. 50 - 54
Copyright
Copyright © Astronomical Society of the Pacific 2004

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