Introducing decorated HODs: modelling assembly bias in the galaxy–halo connection

Hearin, Andrew P.; Zentner, Andrew R.; Bosch, Frank C. van den; Campbell, Duncan; Tollerud, Erik

doi:10.1093/mnras/stw840

Cited by 170 publications

(171 citation statements)

References 108 publications

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“…They found that vacc or v peak were best able to reproduce clustering statistics when modelling a sample of SDSS galaxies with M * > 10 10 M . More recently, Lehmann et al (2015) have shown that stellar content likely depends not just on halo mass but also concentration, while Hearin et al (2016) have developed a flexible scheme for incorporating dependencies on multiple halo properties in the context of halo occupation distribution models.…”

Section: Choice Of Stellar Mass Proxymentioning

confidence: 99%

The upper bound on the lowest mass halo

Jethwa¹,

Erkal²,

Belokurov³

2017

Monthly Notices of the Royal Astronomical Society

181

207

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We explore the connection between galaxies and dark matter halos in the Milky Way (MW) and quantify the implications on properties of the dark matter particle and the phenomenology of low-mass galaxy formation. This is done through a probabilistic comparison of the luminosity function of MW dwarf satellite galaxies to models based on two suites of zoom-in simulations. One suite is dark-matter-only while the other includes a disk component, therefore we can quantify the effect of the MW's baryonic disk on our results. We apply numerous Stellar-Mass-Halo-Mass (SMHM) relations allowing for multiple complexities: scatter, a characteristic break scale, and subhalos which host no galaxy. In contrast to previous works we push the model/data comparison to the faintest dwarfs by modeling observational incompleteness, allowing us to draw three new conclusions. Firstly, we constrain the SMHM relation for 10 2 < M * /M < 10 8 galaxies, allowing us to bound the peak halo mass of the faintest MW satellite to M vir > 2.4 × 10 8 M (1σ). Secondly, by translating to a Warm Dark Matter (WDM) cosmology, we bound the thermal relic mass m WDM > 2.9 keV at 95% confidence, on a par with recent constraints from the Lyman-α forest. Lastly, we find that the observed number of ultra-faint MW dwarfs is in tension with the theoretical prediction that reionisation prevents galaxy formation in almost all 10 8 M halos. This can be tested with the next generation of deep imaging surveys. To this end, we predict the likely number of detectable satellite galaxies in the Subaru/HSC survey and the LSST. Confronting these predictions with future observations will be amongst our strongest tests of WDM and the effect reionisation on low-mass systems.

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Section: Choice Of Stellar Mass Proxymentioning

confidence: 99%

The upper bound on the lowest mass halo

Jethwa¹,

Erkal²,

Belokurov³

2017

Monthly Notices of the Royal Astronomical Society

181

207

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“…For example, average SFHs can be inferred by integrating the main sequence SFR over time (e.g., Leitner 2012), but this approach leads to inconsistencies (Leja et al 2015). Instead, the most successful theoretical models link the growth of stellar mass to the growth of the dark matter halos that galaxies inhabit, for example, via subhalo abundance matching (e.g., Kravtsov et al 2004;Conroy et al 2006;Behroozi et al 2013b;Moster et al 2013), halo occupation distributions (e.g., Peacock & Smith 2000;Seljak 2000;Hearin et al 2016), semianalytic models (Kauffmann et al 1993;Somerville et al 2001;Guo et al 2011), or other assumptions (Bouché et al 2010;Davé et al 2012;Lilly et al 2013;Tacchella et al 2013;Mitra et al 2017). One important conclusion from these models is that there has to be significant scatter between halo and galaxy masses (and thus growth histories) in order to explain observations (More et al 2009;Behroozi et al 2013b;Reddick et al 2013;Gu et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Log-normal Star Formation Histories in Simulated and Observed Galaxies

Diemer

Sparre

Abramson³

et al. 2017

ApJ

108

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Gladders et al. have recently suggested that the star formation histories (SFHs) of individual galaxies are characterized by a log-normal function in time, implying a slow decline rather than rapid quenching. We test their conjecture on theoretical SFHs from the cosmological simulation Illustris and on observationally inferred SFHs. While the log-normal form necessarily ignores short-lived features such as starbursts, it fits the overall shape of the majority of SFHs very well. In particular, 85% of the cumulative SFHs are fitted to within a maximum error of 5% of the total stellar mass formed, and 99% to within 10%. The log-normal performs systematically better than the commonly used delayed-τ model, and is superseded only by functions with more than three free parameters. Poor fits are mostly found in galaxies that were rapidly quenched after becoming satellites. We explore the log-normal parameter space of normalization, peak time, and full width at half maximum, and find that the simulated and observed samples occupy similar regions, though Illustris predicts wider, later-forming SFHs on average. The ensemble of log-normal fits correctly reproduces complex metrics such as the evolution of Illustris galaxies across the star formation main sequence, but overpredicts their quenching timescales. SFHs in Illustris are a diverse population not determined by any one physical property of galaxies, but follow a tight relation, where µ ( ) width peak time 3 2 . We show that such a relation can be explained qualitatively (though not quantitatively) by a close connection between the growth of dark matter halos and their galaxies.

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“…When the observable property is a count of galaxies above some size (luminosity, stellar mass, etc.) threshold, the MPR is analogous to the Halo Occupation Distribution (HOD, Berlind & Weinberg 2002;Cooray & Sheth 2002;Hearin et al 2013;Zentner et al 2014;Hearin et al 2016;Zehavi et al 2018). The stellar property statistics of dark matter halos lie within the broad category of the "galaxyhalo connection" which was reviewed recently by Wechsler & Tinker (2018).…”

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confidence: 99%

Stellar property statistics of massive haloes from cosmological hydrodynamics simulations: common kernel shapes

Anbajagane

Evrard

Farahi

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We study stellar property statistics, including satellite galaxy occupation, of massive halo populations realized by three cosmological hydrodynamics simulations: BA-HAMAS + MACSIS, TNG300 of the IllustrisTNG suite, and Magneticum Pathfinder. The simulations incorporate independent sub-grid methods for astrophysical processes with spatial resolutions ranging from 1.5 to 6 kpc, and each generates samples of 1000 or more halos with M halo > 10 13.5 M at redshift z = 0. Applying localized, linear regression (LLR), we extract halo mass-conditioned statistics (normalizations, slopes, and intrinsic covariance) for a three-element stellar property vector consisting of: i) N sat , the number of satellite galaxies with stellar mass, M > 10 10 M within radius R 200c of the halo; ii) M ,tot , the total stellar mass within that radius, and; iii) M ,BCG , the gravitationally-bound stellar mass of the central galaxy within a 100 kpc radius. Scaling parameters for the three properties with halo mass show mild differences among the simulations, in part due to numerical resolution, but there is qualitative agreement on property correlations, with halos having smaller than average central galaxies tending to also have smaller total stellar mass and a larger number of satellite galaxies. Marginalizing over total halo mass, we find the satellite galaxy kernel, p(ln N sat | M halo , z) to be consistently skewed left, with skewness parameter γ = −0.91 ± 0.02, while that of ln M ,tot is closer to log-normal, in all three simulations. The highest resolution simulations find γ −0.8 for the z = 0 shape of p(ln M ,BCG | M halo , z) and also that the fractional scatter in total stellar mass is below 10 percent in halos more massive than 10 14.3 M . We provide a Gaussian mixture fit to the low redshift N sat kernel as well as LLR parameters tabulated for halos more massive than 10 13.5 M in all simulations.

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Introducing decorated HODs: modelling assembly bias in the galaxy–halo connection

Cited by 170 publications

References 108 publications

The upper bound on the lowest mass halo

The upper bound on the lowest mass halo

Log-normal Star Formation Histories in Simulated and Observed Galaxies

Stellar property statistics of massive haloes from cosmological hydrodynamics simulations: common kernel shapes

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