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Halo histories versus Galaxy properties at z = 0 – I. The quenching of star formation

Tinker, Jeremy L. and Wetzel, Andrew R. and Conroy, Charlie and Mao, Yao-Yuan (2017) Halo histories versus Galaxy properties at z = 0 – I. The quenching of star formation. Monthly Notices of the Royal Astronomical Society, 472 (2). pp. 2504-2516. ISSN 0035-8711. doi:10.1093/mnras/stx2066.

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We test whether halo age and galaxy age are correlated at fixed halo and galaxy mass. The formation histories, and thus ages, of dark matter haloes correlate with their large-scale density ρ, an effect known as assembly bias. We test whether this correlation extends to galaxies by measuring the dependence of galaxy stellar age on ρ. To clarify the comparison between theory and observation, and to remove the strong environmental effects on satellites, we use galaxy group catalogues to identify central galaxies and measure their quenched fraction, f_Q, as a function of large-scale environment. Models that match halo age to central galaxy age predict a strong positive correlation between f_Q and ρ. However, we show that the amplitude of this effect depends on the definition of halo age: assembly bias is significantly reduced when removing the effects of splashback haloes – those haloes that are central but have passed through a larger halo or experienced strong tidal encounters. Defining age using halo mass at its peak value rather than current mass removes these effects. In  Sloan Digital Sky Survey data, at M* ≳ 10^(10)M⊙ h^(−2), there is a ∼5 per cent increase in f_Q from low-to-high densities, which is in agreement with predictions of dark matter haloes using peak halo mass. At lower stellar mass there is little to no correlation of f_Q with ρ. For these galaxies, age matching is inconsistent with the data across the range of halo formation metrics that we tested. This implies that halo formation history has a small but statistically significant impact on quenching of star formation at high masses, while the quenching process in low-mass central galaxies is uncorrelated with halo formation history.

Item Type:Article
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URLURL TypeDescription Paper
Wetzel, Andrew R.0000-0003-0603-8942
Conroy, Charlie0000-0002-1590-8551
Mao, Yao-Yuan0000-0002-1200-0820
Additional Information:© 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2017 August 8. Received 2017 August 8; in original form 2016 September 9. Published: 18 August 2017. The authors wish to thank Andrew Hearin for useful discussions, as well as the anonymous referee, whose comments significantly improved the paper. We thank Matthew R. Becker for providing the Chinchilla simulation used in this work. The Chinchilla simulation and related analysis were performed using computational resources at SLAC. We thank the SLAC computational team for their consistent support. JLT acknowledges support from NSF grant AST-121189. ARW was supported by a Moore Prize Fellowship through the Moore Center for Theoretical Cosmology and Physics at Caltech and by a Carnegie Fellowship in Theoretical Astrophysics at Carnegie Observatories. CC acknowledges support from NASA grant NNX15AK14G, NSF grant AST-1313280 and the Packard Foundation.
Funding AgencyGrant Number
Moore Center for Theoretical Cosmology and Physics, CaltechUNSPECIFIED
Carnegie FellowshipUNSPECIFIED
David and Lucile Packard FoundationUNSPECIFIED
Subject Keywords:galaxies: clusters: general – galaxies: evolution – galaxies: groups: general – cosmology: observations
Issue or Number:2
Record Number:CaltechAUTHORS:20171102-144554972
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Official Citation:Jeremy L. Tinker, Andrew R. Wetzel, Charlie Conroy, Yao-Yuan Mao; Halo histories versus Galaxy properties at z = 0 – I. The quenching of star formation, Monthly Notices of the Royal Astronomical Society, Volume 472, Issue 2, 1 December 2017, Pages 2504–2516,
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:82909
Deposited By: Tony Diaz
Deposited On:03 Nov 2017 02:05
Last Modified:15 Nov 2021 19:53

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