The Integrated Stellar Content of Dark Matter Halos

Leauthaud, Alexie; George, Matthew R.; Behroozi, Peter; Bundy, Kevin; Tinker, Jeremy L.; Wechsler, Risa H.; Conroy, Charlie; Finoguenov, A.; Tanaka, Masayuki

doi:10.1088/0004-637x/746/1/95

Cited by 248 publications

(438 citation statements)

References 111 publications

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“…We also compare our results with the recently published average groups' stellar mass fractions by Leauthaud et al (2012): these authors constrain the fraction of stars in group-sized haloes 3 Note that these values cannot be directly compared with those in Fig. 11 since those are computed by integrating the mass function down to a different stellar mass.…”

Section: The Average Stellar Mass Fraction In Groupsmentioning

confidence: 82%

The galaxy stellar mass function of X-ray detected groups

Giodini

Finoguenov

Pierini

et al. 2012

A&A

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We study the stellar mass distribution for galaxies in 160 X-ray detected groups of 10 13 < Log(M 200 /M ) < 2 × 10 14 and compare it with that of galaxies in the field to investigate the action of environment on the build-up of the stellar mass. We highlight differences in the build-up of the passive population in the field, which imprint features in the distribution of stellar mass of passive galaxies at Log(M/M ) < 10.5. The gradual diminishing of the effect when moving to groups of increasing total masses indicates that the growing influence of the environment in bound structures is responsible for the build-up of a quenched component at Log(M/M ) < 10.5. Differently, the stellar mass distribution of star-forming galaxies is similar in shape in all environments, and can be described by a single Schechter function both in groups and in the field. Little evolution is seen up to redshift 1. Nevertheless at z = 0.2-0.4 groups with M 200 < 6 × 10 13 M (low-mass groups) tend to have a characteristic mass for star-forming galaxies that is 50% higher than in higher mass groups; we interpret it as a reduced action of environmental processes in these systems. Furthermore, we analyse the distribution of sSFR-Log(M) in groups and in the field, and find that groups show on average a lower sSFR (by ∼0.2 dex) at z < 0.8. Accordingly, we find that the fraction of star-forming galaxies is increasing with redshift in all environments, but at a faster pace in the denser ones. Finally, our analysis highlights that low-mass groups have a higher fraction (by 50%) of the stellar mass locked in star-forming galaxies than higher mass systems (i.e. 2/3 of their stellar mass).

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Section: The Average Stellar Mass Fraction In Groupsmentioning

confidence: 82%

The galaxy stellar mass function of X-ray detected groups

Giodini

Finoguenov

Pierini

et al. 2012

A&A

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“…The abundancematching and weak lensing studies (e.g., Moster et al 2010;Behroozi et al 2010;Leauthaud et al 2012) suggest that these halos host central galaxies with a stellar mass of ∼10 11 M . At this stellar mass, the mass quenching is efficient according to Peng et al (2010), and both passive and star-forming galaxies are observed in the low-z Universe (e.g., Baldry et al 2012;Ilbert et al 2013).…”

Section: The Future Of Z ∼ 2 Populationsmentioning

confidence: 98%

“…Finally, weak gravitational lensing can also provide strong constraints on the characteristic halo mass hosting a galaxy population (e.g., Mandelbaum et al 2006). Leauthaud et al (2012) made a combined analysis of z < 1 galaxies combining all these techniques and strongly constrained the M − M h relation. However, only a few studies extended these results at higher redshift.…”

Section: Introductionmentioning

confidence: 99%

Clustering, host halos, and environment ofz ~ 2 galaxies as a function of their physical properties

Béthermin

Kilbinger

Daddi

et al. 2014

A&A

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Using a sample of 25 683 star-forming and 2821 passive galaxies at z ∼ 2, selected in the COSMOS field following the BzK color criterion, we study the hosting halo mass and environment of galaxies as a function of their physical properties. Spitzer and Herschel allow us to obtain accurate star formation rate estimates for starburst galaxies. We measure the autocorrelation and cross-correlation functions of various galaxy subsamples and infer the properties of their hosting halos using both a halo occupation model and the linear bias at large scale. We find that passive and star-forming galaxies obey a similarly rising relation between the halo and stellar mass. The mean host halo mass of star-forming galaxies increases with the star formation rate between 30 M yr −1 and 200 M yr −1 , but flattens for higher values, except if we select only main-sequence galaxies. This reflects the expected transition from a regime of secular coevolution of the halos and the galaxies to a regime of episodic starburst. We find similar large-scale biases for mainsequence, passive, and starburst galaxies at equal stellar mass, suggesting that these populations live in halos of the same mass. However, we detect an excess of clustering on small scales for passive galaxies and showed, by measuring the large-scale bias of close pairs of passive galaxies, that this excess is caused by a small fraction (∼16%) of passive galaxies being hosted by massive halos (∼3 × 10 13 M ) as satellites. Finally, extrapolating the growth of halos hosting the z ∼ 2 population, we show that M ∼ 10 10 M galaxies at z ∼ 2 will evolve, on average, into massive (M ∼ 10 11 M ), field galaxies in the local Universe and M ∼ 10 11 M galaxies at z = 2 into local, massive, group galaxies. We also identify two z ∼ 2 populations which should end up in today's clusters: massive (>M ∼ 10 11 M ), strongly star-forming (>200 M yr −1 ), main-sequence galaxies, and close pairs of massive, passive galaxies.

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“…Tinker et al 2013). The details of the SHMR-based model 3 that we use and how it is constrained from COSMOS data are described in Leauthaud et al (2011Leauthaud et al ( , 2012b. Other models based on the conditional SMF or abundance matching techniques would also our purpose (e.g.…”

Section: E T H O D O L O G Ymentioning

confidence: 99%

The dark matter haloes of moderate luminosity X-ray AGN as determined from weak gravitational lensing and host stellar masses

Leauthaud

Benson

Civano

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Understanding the relationship between galaxies hosting active galactic nuclei (AGN) and the dark matter halos in which they reside is key to constraining how black-hole fueling is triggered and regulated. Previous efforts have relied on simple halo mass estimates inferred from clustering, weak gravitational lensing, or halo occupation distribution modeling. In practice, these approaches remain uncertain because AGN, no matter how they are identified, potentially live a wide range of halo masses with an occupation function whose general shape and normalization are poorly known. In this work, we show that better constraints can be achieved through a rigorous comparison of the clustering, lensing, and cross-correlation signals of AGN hosts to the fiducial stellar-to-halo mass relation (SHMR) derived for all galaxies, irrespective of nuclear activity. Our technique exploits the fact that the global SHMR can be measured with much higher accuracy than any statistic derived from AGN samples alone. Using 382 moderate luminosity X-ray AGN at z < 1 from the COSMOS field, we report the first measurements of weak gravitational lensing from an X-ray selected sample. Comparing this signal to predictions from the global SHMR, we find that, contrary to previous results, most X-ray AGN do not live in medium size groups -nearly half reside in relatively low mass halos with M 200b ∼ 10 12.5 M ⊙ . The AGN occupation function is well described by the same form derived for all galaxies but with a lower normalization-the fraction of halos with AGN in our sample is a few percent. The number of AGN satellite galaxies scales as a power law with host halo mass with a power-law index α = 1. By highlighting the relatively "normal" way in which moderate luminosity X-ray AGN hosts occupy halos, our results suggest that the environmental signature of distinct fueling modes for luminous QSOs compared to moderate luminosity X-ray AGN is less obvious than previously claimed.

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The Integrated Stellar Content of Dark Matter Halos

Cited by 248 publications

References 111 publications

The galaxy stellar mass function of X-ray detected groups

The galaxy stellar mass function of X-ray detected groups

Clustering, host halos, and environment ofz ~ 2 galaxies as a function of their physical properties

The dark matter haloes of moderate luminosity X-ray AGN as determined from weak gravitational lensing and host stellar masses

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