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An Analysis of M31 and its Satellite Galaxies Using RR Lyrae Variables

Published online by Cambridge University Press:  30 October 2019

Nahathai Tanakul Open the ORCID record for Nahathai Tanakul [Opens in a new window]  and
Ata Sarajedini
Nahathai Tanakul
Affiliation:
National Astronomical Research Institute of Thailand, 260 Moo 4, T. Donkaew, A. Maerim, Chiangmai, 50180, Thailand email: [email protected]
Ata Sarajedini
Affiliation:
Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA Department of Physics, Florida Atlantic University, 777 Glades Rd, SE-43, Room 256 Boca Raton, FL 33431, USA
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Abstract

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RR Lyrae stars are powerful tools to study their host populations. Information such as distance, metallicity, reddening, and age can be obtained from their pulsation properties. Dwarf spheroidal (dSph) galaxies are the most common type of galaxy in the Local Group. They are found around massive hosts such as the Milky Way (MW) and M31 and are suggested to be the present-day counterparts to systems from which spheroids and stellar halos of larger galaxies were assembled. By comparing RR Lyraes in these dSphs with their host galaxies, we hope to understand more about the formation of these galaxies. In order to achieve this goal, we have analyzed six fields in M31 using archival imaging from the Hubble Space Telescope. Published data for M31, M33, and several M31 dSphs are also included. The results are then compared with those in the MW to better constrain the early history of these systems.

Keywords

stars: variables: othergalaxies: dwarf
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S344: Dwarf Galaxies: From the Deep Universe to the Present , August 2018 , pp. 147 - 150
Copyright
© International Astronomical Union 2019 

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