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Quenching massive galaxies across cosmic time with the semi-analytic model SHARK v2.0

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arxiv 2309.02310 v2 pith:B6BIRDBT submitted 2023-09-05 astro-ph.GA

Claudia D.P. Lagos (1 , 2 , 3) , Matias Bravo , Rodrigo Tobar , Danail Obreschkow , Chris Power , Aaron S.G. Robotham
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Katy L. Proctor Samuel Hansen Angel Chandro-Gomez Julian Carrivick ((1) International Centre for Radio Astronomy Research (ICRAR) M468 University of Western Australia Crawley WA Australia (2) ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions ASTRO 3D (3) Cosmic Dawn Center (DAWN) Denmark)
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abstract

We introduce version 2.0 of the SHARK semi-analytic model of galaxy formation after many improvements to the physics included. The most significant being: (i) a model describing the exchange of angular momentum (AM) between the interstellar medium and stars; (ii) a new active galactic nuclei feedback model which has two modes, a wind and a jet mode, with the jet mode tied to the jet energy production; (iii) a model tracking the development of black hole (BH) spins; (iv) more sophisticated modelling of environmental effects on satellite galaxies; and (v) automatic parameter exploration using Particle Swarm Optimisation. We focus on two timely research topics: the structural properties of galaxies and the quenching of massive galaxies. For the former, SHARK v2.0 is capable of producing a more realistic stellar size-mass relation with a plateau marking the transition from disk- to bulge-dominated galaxies, and scaling relations between specific AM and mass that agree well with observations. For the quenching of massive galaxies, SHARK v2.0 produces massive galaxies that are more quenched than the previous version, reproducing well the observed relations between star formation rate (SFR) and stellar mass, and specific SFR and BH mass at $z=0$. SHARK v2.0 produces a number density of massive-quiescent galaxies >1dex higher than the previous version, in good agreement with JWST observations at $z\le 5$; predicts a stellar mass function of passive galaxies in reasonably good agreement with observations at $0.5<z<5$; and environmental quenching to already be effective at $z=5$.

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Cited by 2 Pith papers

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    astro-ph.GA 2025-02 conditional novelty 6.0 of 10

    An abundance-matched SFR-halo accretion relation plus halo quenching reproduces low-redshift galaxy abundances and quenched fractions, with extra low-mass quenching required for the faint end.

  2. Cosmological Simulations of Galaxies

    astro-ph.GA 2025-07 unverdicted

    A comprehensive introductory review of cosmological galaxy simulation methods, covering initial conditions, numerical solvers, star formation and feedback, analysis, and validation.

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