http://arxiv.org/abs/2305.01719
Stellar counter-rotation in disk galaxies directly relates to the complex phenomenon of the disk mass assembly believed to be driven by external processes, such as accretion and mergers. The detailed study of such systems makes it possible to reveal the source of external accretion and establish the details of this process. In this paper, we investigate the galaxy PGC 66551 (MaNGA ID~1-179561) which hosts two large-scale counter-rotating stellar disks suspected in the SDSS MaNGA data and then confirmed using deep follow-up spectroscopy with the 10-m Southern African Large Telescope. We measured properties of ionized gas and stellar populations of both counter-rotating disks in PGC 66551. We found that the counter-rotating disk is compact, contains young stars with subsolar metallicity, and has a stellar mass $5\times10^{9}$ M$_\odot$ which amounts to $\approx$20\% of the galaxy’s total. Surprisingly, the main 8 Gyr old disk has a significantly lower metallicity -0.8 dex than other counter-rotating galaxies. We developed a simple analytic model for the metal enrichment history, which we applied to PGC 66551 and constrained the parameters of the galactic outflow wind and estimated the metallicity of the infalling gas that formed the counter-rotating disk to be $-0.9 … -0.5$ dex. Our interpretation prefers a merger with gas-rich satellite over cold accretion from a cosmic filament as a source of gas, which then formed the counter-rotating disk in PGC 66551.
I. Katkov, D. Gasymov, A. Kniazev, et. al.
Thu, 4 May 23
56/60
Comments: 18 pages, 10 figure, submitted to ApJ
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