Reeves, Andrew MM, Balogh, Michael L, van der Burg, Remco FJ, Finoguenov, Alexis, Kukstas, Egidijus 
ORCID: 0000-0001-6902-501X, McCarthy, Ian G, Webb, Kristi, Muzzin, Adam, McGee, Sean, Rudnick, Gregory et al (show 11 more authors)
(2021)
The GOGREEN survey: dependence of galaxy properties on halo mass a <i>z</i> > 1 and implications for environmental quenching.
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 506 (3).
pp. 3364-3384.
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Abstract
We use photometric redshifts and statistical background subtraction to measure stellar mass functions in galaxy group-mass ($4.5-8\times10^{13}~\mathrm{M}_\odot$) haloes at $1<z<1.5$. Groups are selected from COSMOS and SXDF, based on X-ray imaging and sparse spectroscopy. Stellar mass ($M_{\mathrm{stellar}}$) functions are computed for quiescent and star-forming galaxies separately, based on their rest-frame $UVJ$ colours. From these we compute the quiescent fraction and quiescent fraction excess (QFE) relative to the field as a function of $M_{\mathrm{stellar}}$. QFE increases with $M_{\mathrm{stellar}}$, similar to more massive clusters at $1<z<1.5$. This contrasts with the apparent separability of $M_{\mathrm{stellar}}$ and environmental factors on galaxy quiescent fractions at $z\sim 0$. We then compare our results with higher mass clusters at $1<z<1.5$ and lower redshifts. We find a strong QFE dependence on halo mass at fixed $M_{\mathrm{stellar}}$; well fit by a logarithmic slope of $\mathrm{d}(\mathrm{QFE})/\mathrm{d}\log (M_{\mathrm{halo}}) \sim 0.24 \pm 0.04$ for all $M_{\mathrm{stellar}}$ and redshift bins. This dependence is in remarkably good qualitative agreement with the hydrodynamic simulation BAHAMAS, but contradicts the observed dependence of QFE on $M_{\mathrm{stellar}}$. We interpret the results using two toy models: one where a time delay until rapid (instantaneous) quenching begins upon accretion to the main progenitor ("no pre-processing") and one where it starts upon first becoming a satellite ("pre-processing"). Delay times appear to be halo mass dependent, with a significantly stronger dependence required without pre-processing. We conclude that our results support models in which environmental quenching begins in low-mass ($<10^{14}M_\odot$) haloes at $z>1$.
| Item Type: | Article |
|---|---|
| Additional Information: | Accepted July 6, 2021, MNRAS |
| Uncontrolled Keywords: | galaxies: clusters: general, galaxies: evolution, galaxies: groups: general, galaxies: haloes, galaxies: high-redshift, galaxies: star formation |
| Divisions: | Faculty of Science and Engineering > School of Physical Sciences |
| Depositing User: | Symplectic Admin |
| Date Deposited: | 21 Jul 2021 10:50 |
| Last Modified: | 18 Oct 2023 08:37 |
| DOI: | 10.1093/mnras/stab1955 |
| Related URLs: | |
| URI: | https://livrepository.liverpool.ac.uk/id/eprint/3130827 |
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