Main Sequence Scatter is Real: The Joint Dependence of Galaxy Clustering on Star Formation and Stellar Mass

Berti, Angela M.; Coil, Alison L.; Hearin, Andrew P.; Behroozi, Peter S.

doi:10.48550/arxiv.2009.02405

Cited by 2 publications

(3 citation statements)

References 39 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Such a dependence is necessary if galaxy properties determining BOSS selection cuts, i.e. luminosity and colour, correlate with halo mass at fixed observed stellar mass (Saito et al 2016;Berti et al 2020). In principle, we could vary the three free parameters for centrals and satellites independently.…”

Section: Galaxy-halo Connectionmentioning

confidence: 99%

“…However, the argument does not work if any secondary galaxy property at fixed intrinsic stellar mass correlates with large scale bias. For example, Berti et al (2020) have shown that at fixed (observed) stellar mass, the specific star formation rate (sSFR) correlates with large-scale clustering, even if one only considers quiescent, red galaxies. Thus, for example, a bias of observed stellar mass as a function of sSFR at fixed intrinsic M could be an alternative explanation for the clustering differences between the three different stellar mass estimates.…”

Section: Precision Of Stellar Mass Estimatesmentioning

confidence: 99%

See 1 more Smart Citation

On the halo-mass and radial scale dependence of the lensing is low effect

Lange,

Leauthaud,

Singh

et al. 2020

Preprint

View full text Add to dashboard Cite

The canonical ΛCDM cosmological model makes precise predictions for the clustering and lensing properties of galaxies. It has been shown that the lensing amplitude of galaxies in the Baryon Oscillation Spectroscopic Survey (BOSS) is lower than expected given their clustering properties. We present new measurements and modelling of galaxies in the BOSS LOWZ sample. We focus on the radial and stellar mass dependence of the lensing amplitude mis-match. We find an amplitude mismatch of around 35% when assuming ΛCDM with Planck Cosmological Microwave Background (CMB) constraints. This offset is independent of halo mass and radial scale in the range M halo ∼ 10 13.3 − 10 13.9 h −1 M and r = 0.1 − 60 h −1 Mpc (0.05 h/Mpc k 20 h/Mpc). The observation that the offset is both mass and scale independent places important constraints on the degree to which astrophysical processes (baryonic effects, assembly bias) can fully explain the effect. This scale independence also suggests that the "lensing is low" effect on small and large radial scales probably have the same physical origin. Resolutions based on new physics require a nearly uniform suppression, relative to ΛCDM predictions, of the amplitude of matter fluctuations on these scales. The possible causes of this are tightly constrained by measurements of the CMB and of the low-redshift expansion history.

show abstract

Section: Galaxy-halo Connectionmentioning

confidence: 99%

Section: Precision Of Stellar Mass Estimatesmentioning

confidence: 99%

On the halo-mass and radial scale dependence of the lensing is low effect

Lange,

Leauthaud,

Singh

et al. 2020

Preprint

View full text Add to dashboard Cite

show abstract

“…As galaxy studies continue to develop our understanding of the connection between large-scale environment and galactic SFRs (e.g. Coil et al 2017;Berti et al 2020), more refined measurements of the AGN fraction as a function of SFR (e.g. Aird et al 2019) may be used to enhance our model.…”

Section: Discussionmentioning

confidence: 99%

The AGN-galaxy-halo connection: The distribution of AGN host halo masses to z=2.5

Aird,

Coil

2020

Preprint

Self Cite

View full text Add to dashboard Cite

It is widely reported by clustering measurements of observed active galactic nuclei (AGN) samples that AGN reside in similar mass host dark matter halos across the bulk of cosmic time, with log M/𝑀 ∼ 12.5 − 13.0 to 𝑧 ∼ 2.5. We show that this is due in part to the AGN fraction in galaxies rising with increasing stellar mass, combined with AGN observational selection effects that exacerbate this trend. Additionally, common methods widely used to convert an observed AGN clustering amplitude to an inferred mean dark matter halo mass can result in systematically biased halo masses. Here we use AGN specific accretion rate distribution functions determined as a function of stellar mass and redshift for star-forming and quiescent galaxies separately, combined with the latest galaxy-halo connection models, to determine the parent and subhalo mass distribution function of AGN. We find that while the mean (sub-)halo mass of AGN, ≈ 2 × 10 12 M , is fairly constant with luminosity, specific accretion rate, and redshift, the full halo mass distribution function is broad, spanning several orders of magnitude. While the AGN satellite fraction rises with increasing parent halo mass, we find that the central galaxy is often not an AGN. Our results elucidate the physical causes for the apparent uniformity of AGN host halos across cosmic time and underscore the importance of accounting for AGN selection biases when interpreting observational AGN clustering results. We further show that AGN clustering is most easily interpreted and understood in terms of the relative bias to galaxy samples, not from absolute bias measurements alone.

show abstract

Main Sequence Scatter is Real: The Joint Dependence of Galaxy Clustering on Star Formation and Stellar Mass

Cited by 2 publications

References 39 publications

On the halo-mass and radial scale dependence of the lensing is low effect

On the halo-mass and radial scale dependence of the lensing is low effect

The AGN-galaxy-halo connection: The distribution of AGN host halo masses to z=2.5

Contact Info

Product

Resources

About