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Red supergiant stars in NGC 4449, NGC 5055, and NGC 5457

Published online by Cambridge University Press:  28 July 2017

Sang-Hyun Chun
Affiliation:
Astronomy Program, Department of Physics and Astronomy, Seoul National University email: shyunc.m@gmail.com Research School of Astronomy & Astrophysics, Australian National University
Yong-Jong Sohn
Affiliation:
Department of Astronomy, Yonsei University
Martin Asplund
Affiliation:
Research School of Astronomy & Astrophysics, Australian National University
Luca Casagrande
Affiliation:
Research School of Astronomy & Astrophysics, Australian National University
Corresponding
E-mail address:
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Abstract

Nearby galaxies are ideal objects for the study of the mechanisms of galaxy formation and evolution, and massive stars in nearby galaxies are useful sources to investigate the structures and formation of the galaxies. It is important to gather the contents of massive stars for a number of galaxies spanning various metallicities. We focus on the red supergiants (RSGs) in nearby galaxies NGC 4449, NGC 5055, and NGC 5457, and the photometric properties of RSGs of three galaxies were investigated using near-infrared (JHK) imaging data obtained from WFCAM UKIRT. The (JK, K)0 CMDs are investigated and compared with theoretical isochrones (Figure 1). The majority of RSGs in three galaxies have common age ranges from log(t yr ) = 6.9 to log(t yr ) = 7.3, and this indicates that these galaxies have experienced recent star formation within 20 Myr. Spatial correlation of RSGs with H II regions and their colour distribution were also investigated. For NGC 4449 and NGC 5457, the RSGs are spatially correlated with the H II regions, which however is not the case for NGC 5055. We found a similar colour distribution and a constant peak magnitude of M K = −11.9 for the RSGs in the three galaxies.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2017 

References

Bressan, A., Marigo, P., Girardi, L., Salasnich, B., Dal Cero, C., Rubele, S., & Nanni, A., 2012, MNRAS, 427, 127 CrossRefGoogle Scholar

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