Halo occupation distribution (HOD) modelling of high redshift galaxies using the BlueTides simulation

Bhowmick, Aklant K.; Campbell, Duncan; Matteo, Tiziana Di; Feng, Yu

doi:10.1093/mnras/sty2128

Cited by 16 publications

(10 citation statements)

References 130 publications

(148 reference statements)

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“…The cited works use the virial overdensity at each redshift to define halo masses, so we accordingly let M h correspond to the halo virial mass M vir . For simplicity, we assume that halos host a central galaxy only, since at high redshift the fraction of satellites is expected to be at most a few percent (Rodríguez-Puebla et al 2016;Bhowmick et al 2018). This is also within the theoretical uncertainty of the halo mass function quoted above (Rodríguez-Puebla et al 2016).…”

Section: Halo Mass Functionmentioning

confidence: 85%

Galaxy population constraints on cosmology and star formation in the early Universe

Sahlén,

Zackrisson

2021

Preprint

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We present the first post-cosmic-microwave-background early-Universe observational constraints on σ 8 , Ω m , mean galaxy star-forming efficiency and galaxy UV magnitude scatter at redshifts z = 4 − 10. We perform a simultaneous 11-parameter cosmology and star-formation physics fit using the new code GalaxyMC, with redshift z > 4 galaxy UV luminosity and correlation function data. Consistent with previous studies, we find evidence for redshift-independent star formation physics, regulated by halo assembly. For a flat ΛCDM universe with a low-redshift Hubble constant and a Type Ia supernovae Ω m prior, we constrain σ 8 = 0.81 ± 0.03, and a mean star-forming efficiency peaking at log 10 SFE = −[(0.09±0.20)+(0.58±0.29)×log 10 (1+z)] for halo mass log 10 M p /h −1 M = 11.48±0.09. The suppression of star formation due to feedback is given by a double power law in halo mass with indices α = 0.56 ± 0.08, β = −1.03 ± 0.07. The scatter in galaxy UV magnitude for fixed halo mass is σ M = 0.56 ± 0.08. Without a prior on Ω m we obtain σ 8 = 0.78 ± 0.06, Ω m = 0.33 ± 0.07 and at most 1σ differences in all other parameter values. Our best-fit galaxy luminosity functions yield a reionization optical depth τ ≈ 0.048, consistent with the Planck 2018 value.

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Section: Halo Mass Functionmentioning

confidence: 85%

Galaxy population constraints on cosmology and star formation in the early Universe

Sahlén,

Zackrisson

2021

Preprint

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“…In fact, the calibration step removes first-order differences and typical galaxies at z 5 are expected to have low metallicities. One further basic assumption used to simplify modeling is that each halo is occupied by a single central galaxy, which is justified both by analytical halo occupation models and by analysis of cosmological simulations, which point to a 2% contribution from satellites to the the UVLF at z 6 (Bhowmick et al 2018). Left and middle panels: Sampling of galaxy UV luminosities with the conditional luminosity function from the z ∼ 5 halo mass function.…”

Section: Introductionmentioning

confidence: 99%

The Brightest Galaxies at Cosmic Dawn from Scatter in the Galaxy Luminosity versus Halo Mass Relation

Ren

Trenti

Mason

2019

ApJ

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The Ultraviolet Luminosity Function (UVLF) is a key observable for understanding galaxy formation from cosmic dawn. There has been considerable debate on whether Schechter-like LFs (characterized by an exponential drop-off at the bright end) that well describe the LF in our local Universe are also a sufficient description of the LF at high redshifts (z > 6). We model the UVLF over cosmic history with a semi-empirical framework and include a log-normal scatter, Σ, in galaxy luminosities with a conditional luminosity function approach. We show that stochasticity induces a flattening or a feedback scale in the median galaxy luminosity versus halo mass relation, L c (M h ) to account for the increase of bright objects placed in lower mass halos. We observe a natural broadening in the brightend exponential segment of the UVLF for z > 6 if processes that regulate star-formation acts on the same mass scale as at z ∼ 5, where the degree of broadening is enhanced for larger Σ. Alternatively, if the bright-end feedback is triggered at a near-constant luminosity threshold, the feedback threshold occurs at progressively lower halo masses with increasing redshift, due to galaxies being more luminous on average at a fixed halo mass from rapid halo assembly. Such feedback results in a LF shape with a bright-end closer to that of a Schechter function. We include predictions for the z > 8 UVLFs from future all-sky surveys such as WFIRST which has the potential to both quantify the scatter and type of feedback, and provide insight behind the mechanisms that drive star formation in the early Universe.

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“…where the first term (the halo mass function, HMF) mainly depends on cosmology, whereas the second term (the halo-galaxy connection, which links the mass M h of a DM halo to the absolute magnitude M UV of the galaxy it hosts) depends on astrophysics. Here we implicitly assumed that the halo occupation distribution is unity, i.e., each halo hosts one central galaxy, which is a good approximation at these high redshifts [42].…”

mentioning

confidence: 99%

New Roads to the Small-Scale Universe: Measurements of the Clustering of Matter with the High-Redshift UV Galaxy Luminosity Function

Sabti,

Muñoz,

Blas

2021

Preprint

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Halo occupation distribution (HOD) modelling of high redshift galaxies using the BlueTides simulation

Cited by 16 publications

References 130 publications

Galaxy population constraints on cosmology and star formation in the early Universe

Galaxy population constraints on cosmology and star formation in the early Universe

The Brightest Galaxies at Cosmic Dawn from Scatter in the Galaxy Luminosity versus Halo Mass Relation

New Roads to the Small-Scale Universe: Measurements of the Clustering of Matter with the High-Redshift UV Galaxy Luminosity Function

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