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

Abstract

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.

The Galaxy–Halo Connection in High-redshift Universe: Details and Evolution of Stellar-to-halo Mass Ratios of Lyman Break Galaxies on CFHTLS Deep Fields

“…The ACFs show that the dropout galaxies are more strongly clustered with higher stellar mass thresholds. This trend is also seen in previous clustering studies with stellar-mass limit samples at lower-z (e.g., Béthermin et al 2014;McCracken et al 2015).…”

“…The HOD model was developed to interpret galaxy clustering by characterizing the number of galaxies within dark haloes as probability distributions, assuming that galaxy baryonic properties are primarily governed by the masses of their host dark haloes. Many observational studies have successfully unveiled the relationship between observed galaxies and their host dark haloes for high-redshift Universe (e.g., Geach et al 2012;Béthermin et al 2014;Durkalec et al 2015;Harikane et al 2016;Ishikawa et al 2016;Park et al 2016), as well as z < 1 Universe (e.g., Zehavi et al 2011;Matsuoka et al 2011;Coupon et al 2012Coupon et al , 2015Rodríguez-Torres et al 2016).…”

Faint Submillimeter Galaxies Identified Through Their Optical/Near-Infrared Colors. I. Spatial Clustering and Halo Masses

“…in Hartley et al (2013), Sato et al (2014), McCracken et al (2015, and Lin et al (2016), but contrary to what was reported in Béthermin et al (2014). This finding implies that halo mass could play a major role in quenching the star formation, in line with theoretical models that advocate the halo quenching scenario (e.g., Cen 2011).…”

GAS FRACTION AND DEPLETION TIME OF MASSIVE STAR-FORMING GALAXIES AT z ∼ 3.2: NO CHANGE IN GLOBAL STAR FORMATION PROCESS OUT TO z > 3

“…In Figure 1 we show the location of our z∼3.2 sample in the SFR versus  M plane with respect to the location of the "MS" of star-forming galaxies at redshift » z 3 (Lee et al 2010;Magdis et al 2010;Bethermin et al 2014;Heinis et al 2014;Schreiber et al 2015;Tasca et al 2015;Tomczak et al 2016). 13 Our ALMA detections sample the MS at high stellar mass ( ( [ ]) -…”

“…AGNs are highlighted in red (see the text for details). 13 In the compilation of MSs used by the 2-SFM framework (Sargent et al 2014) and updated with recent sSFR measurements (Bethermin et al 2014;Heinis et al 2014;Steinhardt et al 2014;Schreiber et al 2015;Tasca et al 2015), galaxies with stellar masses of…”