SDSS-IV MaNGA: global properties of kinematically misaligned galaxies

Author:

Zhou Yuren123ORCID,Chen Yanmei123,Shi Yong123ORCID,Bizyaev Dmitry45ORCID,Guo Hong6,Bao Min123,Xu Haitong123,Yu Xiaoling123ORCID,Brownstein Joel R7ORCID

Affiliation:

1. School of Astronomy and Space Science, Nanjing University , Nanjing 210093, China

2. Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education , Nanjing 210093, China

3. Collaborative Innovation Center of Modern Astronomy and Space Exploration , Nanjing 210093, China

4. Apache Point Observatory and New Mexico State University , PO Box 59, Sunspot, NM 88349-0059, USA

5. Sternberg Astronomical Institute, Moscow State University , Moscow 119992, Russia

6. Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory , Nandan Road 80, Shanghai 200030, China

7. Department of Physics and Astronomy, University of Utah , 115 S. 1400 E., Salt Lake City, UT 84112, USA

Abstract

ABSTRACT We select 456 gas–star kinematically misaligned galaxies from the internal Product Launch-10 of MaNGA survey, including 74 star-forming (SF), 136 green-valley (GV), and 206 quiescent (QS) galaxies. We find that the distributions of difference between gas and star position angles for galaxies have three local peaks at ∼0°, 90°, and 180°. The fraction of misaligned galaxies peaks at log (M*/M⊙) ∼ 10.5 and declines to both low- and high-mass end. This fraction decreases monotonically with increasing star formation rate and specific star formation rate. We compare the global parameters including gas kinematic asymmetry Vasym, H i detection rate and mass fraction of molecular gas, effective radius Re, Sérsic index n as well as spin parameter $\lambda _{R_e}$ between misaligned galaxies and their control samples. We find that the misaligned galaxies have lower H i detection rate and molecular gas mass fraction, smaller size, higher Sérsic index, and lower spin parameters than their control samples. The SF and GV misaligned galaxies are more asymmetric in gas velocity fields than their controls. These pieces of observational evidence point to the gas accretion scenario followed by angular momentum redistribution from gas–gas collision, leading to gas inflow and central star formation for the SF and GV misaligned galaxies. We propose three possible origins of the misaligned QS galaxies: (1) external gas accretion, (2) merger, and (3) GV misaligned galaxies evolve into QS galaxies.

Funder

National Key Research and Development Program of China

National Natural Science Foundation of China

China Manned Space

RSCF

Alfred P. Sloan Foundation

U.S. Department of Energy

Office of Science

University of Utah

Carnegie Mellon University

Johns Hopkins University

University of Tokyo

Lawrence Berkeley National Laboratory

Leibniz-Institut für Astrophysik Potsdam

New Mexico State University

New York University

University of Notre Dame

MCTI

Ohio State University

Pennsylvania State University

Universidad Nacional Autónoma de México

University of Arizona

University of Colorado Boulder

Oxford University

University of Portsmouth

University of Virginia

University of Washington

Vanderbilt University

Yale University

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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1. Different Influence of Gas Accretion on the Evolution of Star-forming and Non-star-forming Galaxies;The Astrophysical Journal;2024-09-01

2. Starburst-induced Gas–Star Kinematic Misalignment;The Astrophysical Journal Letters;2024-01-29

3. The Study of the Circumgalactic Medium with Quasar Pairs;The Astrophysical Journal Supplement Series;2023-03-29

4. The SAMI Galaxy Survey: physical drivers of stellar-gas kinematic misalignments in the nearby Universe;Monthly Notices of the Royal Astronomical Society;2022-10-07

5. The luminosity function of ringed galaxies;Monthly Notices of the Royal Astronomical Society;2022-09-09

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