From large-scale environment to CGM angular momentum to star forming activities – II. Quenched galaxies

Author:

Lu Shengdong1ORCID,Xu Dandan1,Wang Sen1,Cai Zheng1,He Chuan234,Xu C Kevin24ORCID,Xia Xiaoyang5,Mao Shude12,Springel Volker6ORCID,Hernquist Lars7

Affiliation:

1. Department of Astronomy, Tsinghua University, Beijing 100084, China

2. National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China

3. School of Astronomy and Space Sciences, University of Chinese Academy of Sciences, Beijing 100049, China

4. Chinese Academy of Sciences South America Center for Astronomy, Beijing 100101, China

5. Tianjin Astrophysics Center, Tianjin Normal University, Tianjin 300387, China

6. Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85748, Garching, Germany

7. Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA

Abstract

Abstract The gas needed to sustain star formation in galaxies is supplied by the circumgalactic medium (CGM), which in turn is affected by accretion from large scales. In a series of two papers, we examine the interplay between a galaxy’s ambient CGM and central star formation within the context of the large-scale environment. We use the IllustrisTNG-100 simulation to show that the influence exerted by the large-scale galaxy environment on the CGM gas angular momentum results in either enhanced (Paper I) or suppressed (Paper II, this paper) star formation inside a galaxy. We find that for present-day quenched galaxies, both the large-scale environments and the ambient CGM have always had higher angular momenta throughout their evolutionary history since at least z = 2, in comparison to those around present-day star-forming disk galaxies, resulting in less efficient gas inflow into the central star-forming gas reservoirs. A sufficiently high CGM angular momentum, as inherited from the larger-scale environment, is thus an important factor in keeping a galaxy quenched, once it is quenched. The process above naturally renders two key observational signatures: (1) a coherent rotation pattern existing across multiple distances from the large-scale galaxy environment, to the circumgalactic gas, to the central stellar disk; and (2) an anti-correlation between galaxy star-formation rates and orbital angular momenta of interacting galaxy pairs or groups.

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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