Tidal Dwarf Galaxies around a Post-merger Galaxy, NGC 4922
Yun-Kyeong Sheen, Hyunjin Jeong, Sukyoung K. Yi, Ignacio Ferreras,, Jennifer M. Lotz, Knut A. G. Olsen, Mark Dickinson, Sydney Barnes, Jang-Hyun, Park, Chang H. Ree, Barry F. Madore, Tom A. Barlow, Tim Conrow, Karl Foster,, Peter G. Friendman, Young-Wook Lee
TL;DR
This paper reports the discovery of young tidal dwarf galaxy candidates in the post-merger galaxy NGC 4922, highlighting the role of UV observations in understanding their formation and properties.
Contribution
It presents the detection and analysis of tidal dwarf galaxy candidates around NGC 4922 using UV data and a two-component stellar population model, emphasizing their young age and typical dwarf galaxy mass.
Findings
Tidal tail mainly composed of young stars (a few Myr old).
Stellar mass of candidates is approximately 10^{6-7} solar masses.
UV data was crucial for age and mass estimation.
Abstract
One possible channel for the formation of dwarf galaxies involves birth in the tidal tails of interacting galaxies. We report the detection of a bright UV tidal tail and several young tidal dwarf galaxy candidates in the post-merger galaxy NGC 4922 in the Coma cluster. Based on a two-component population model (combining young and old stellar populations), we find that the light of tidal tail predominantly comes from young stars (a few Myr old). The Galaxy Evolution Explorer (GALEX) ultraviolet data played a critical role in the parameter (age and mass) estimation. Our stellar mass estimates of the tidal dwarf galaxy candidates are ~ 10^{6-7} M_sun, typical for dwarf galaxies.
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