SDSS IV MaNGA: characteristics of edge-on galaxies with a counter-rotating gaseous disc
Abstract
ABSTRACT Counter-rotating components in galaxies are one of the most direct forms of evidence for past gas accretion or merging. We discovered 10 edge-on disc gaseous counter-rotators in a sample of 523 edge-on galaxies identified in the final MaNGA (Mapping Nearby Galaxies at APO) IFU sample. The counter-rotators tend to located in small groups. The gaseous counter-rotators have intermediate stellar masses and and located in the green valley and red sequence of the colour–magnitude diagram. The average vertical extents of the stellar and ionized gas discs are the same as for the rest of the sample while their radial gas and stellar distributions are more centrally concentrated. This may point at angular momentum loss during the formation process of the counter-rotating discs. The counter-rotators have low gas and dust content, weak emission-line strengths, and low star formation rates. This suggests that the formation of counter-rotators may be an efficient way to quench galaxies. One counter-rotator, SDSS J080016.09+292817.1 (Galaxy F), has a post-starburst region and a possible AGN at the centre. Another counter-rotator, SDSS J131234.03+482159.8 (Galaxy H), is identified as a potential ongoing galaxy interaction with its companion satellite galaxy, a gas-rich spiral galaxy. This may be representative case of amore »
- Publication Date:
- Sponsoring Org.:
- USDOE
- OSTI Identifier:
- 1887477
- Resource Type:
- Published Article
- Journal Name:
- Monthly Notices of the Royal Astronomical Society
- Additional Journal Information:
- Journal Name: Monthly Notices of the Royal Astronomical Society Journal Volume: 516 Journal Issue: 3; Journal ID: ISSN 0035-8711
- Publisher:
- Oxford University Press
- Country of Publication:
- United Kingdom
- Language:
- English
Citation Formats
Beom, Minje, Bizyaev, Dmitry, Walterbos, René A. M., and Chen, Yanmei. SDSS IV MaNGA: characteristics of edge-on galaxies with a counter-rotating gaseous disc. United Kingdom: N. p., 2022.
Web. doi:10.1093/mnras/stac1499.
Beom, Minje, Bizyaev, Dmitry, Walterbos, René A. M., & Chen, Yanmei. SDSS IV MaNGA: characteristics of edge-on galaxies with a counter-rotating gaseous disc. United Kingdom. https://doi.org/10.1093/mnras/stac1499
Beom, Minje, Bizyaev, Dmitry, Walterbos, René A. M., and Chen, Yanmei. Thu .
"SDSS IV MaNGA: characteristics of edge-on galaxies with a counter-rotating gaseous disc". United Kingdom. https://doi.org/10.1093/mnras/stac1499.
@article{osti_1887477,
title = {SDSS IV MaNGA: characteristics of edge-on galaxies with a counter-rotating gaseous disc},
author = {Beom, Minje and Bizyaev, Dmitry and Walterbos, René A. M. and Chen, Yanmei},
abstractNote = {ABSTRACT Counter-rotating components in galaxies are one of the most direct forms of evidence for past gas accretion or merging. We discovered 10 edge-on disc gaseous counter-rotators in a sample of 523 edge-on galaxies identified in the final MaNGA (Mapping Nearby Galaxies at APO) IFU sample. The counter-rotators tend to located in small groups. The gaseous counter-rotators have intermediate stellar masses and and located in the green valley and red sequence of the colour–magnitude diagram. The average vertical extents of the stellar and ionized gas discs are the same as for the rest of the sample while their radial gas and stellar distributions are more centrally concentrated. This may point at angular momentum loss during the formation process of the counter-rotating discs. The counter-rotators have low gas and dust content, weak emission-line strengths, and low star formation rates. This suggests that the formation of counter-rotators may be an efficient way to quench galaxies. One counter-rotator, SDSS J080016.09+292817.1 (Galaxy F), has a post-starburst region and a possible AGN at the centre. Another counter-rotator, SDSS J131234.03+482159.8 (Galaxy H), is identified as a potential ongoing galaxy interaction with its companion satellite galaxy, a gas-rich spiral galaxy. This may be representative case of a gaseous counter-rotator forming through a merger origin. However, tidal distortions expected in mergers are only found in a few of the galaxies and we cannot rule out direct gas accretion as another formation mechanism.},
doi = {10.1093/mnras/stac1499},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 3,
volume = 516,
place = {United Kingdom},
year = {Thu Jun 09 00:00:00 EDT 2022},
month = {Thu Jun 09 00:00:00 EDT 2022}
}
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