The evolution of the star formation activity per halo mass up to redshift  ~1.6 as seen by<i>Herschel</i>

Popesso, P.; Biviano, A.; Rodighiero, G.; Baronchelli, Ivano; Salvato, M.; Saintonge, A.; Finoguenov, A.; Magnelli, B.; Gruppioni, C.; Pozzi, F.; Lutz, D.; Elbaz, D.; Altiéri, B.; Andreani, P.; Aussel, H.; Berta, S.; Capak, P.; Cava, A.; Cimatti, A.; Coia, D.; Daddi, E.; Dannerbauer, H.; Dickinson, Mark; Dasyra, K. M.; Fadda, D.; Schreiber, N. Förster; Genzel, R.; Hwang, Ho Seong; Kartaltepe, Jeyhan S.; Ilbert, O.; Floc’h, E. Le; Leiton, R.; Magdis, G.; Nordon, R.; Patel, Shannon G.; Poglitsch, A.; Riguccini, L.; Portal, M. Sánchez; Shao, Li; Tacconi, L. J.; Tomczak, Adam; Tran, Kim‐Vy H.; Valtchanov, I.

doi:10.1051/0004-6361/201117973

Cited by 70 publications

(119 citation statements)

References 107 publications

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“…Consistently, only field galaxies exhibit values of the SFR that exceeds 30 M y −1 at z < 0.4. These results point towards a strong evolution of the SFR per unit of halo mass at z < 0.4, in agreement with recent results from Herschel data (Popesso et al 2012).…”

Section: Star-forming Galaxiessupporting

confidence: 92%

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: Star-forming Galaxiessupporting

confidence: 92%

The galaxy stellar mass function of X-ray detected groups

Giodini

Finoguenov

Pierini

et al. 2012

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“…The X-ray selected galaxy group sample All the blank fields considered in our analysis have been observed extensively in the X-ray with Chandra and XMM-Newton. To create a statistically significant sample of galaxy groups, we combined the X-ray selected group sample of Popesso et al (2012) and a newly created X-ray selected group sample of the ECDFS (Ziparo et al 2013). The sample described in Popesso et al (2012) comprises the X-ray selected Notes.…”

Section: Infrared and Spectroscopic Datamentioning

confidence: 99%

“…To create a statistically significant sample of galaxy groups, we combined the X-ray selected group sample of Popesso et al (2012) and a newly created X-ray selected group sample of the ECDFS (Ziparo et al 2013). The sample described in Popesso et al (2012) comprises the X-ray selected Notes. The first column gives the name of the field, the second column the MIPS and PACS band in which the field is observed, the third column the effective area covered, and the fourth column the 3σ detection limit in mJy.…”

Section: Infrared and Spectroscopic Datamentioning

confidence: 99%

“…The resulting "residual" image is then used to identify extended emission with at least 4σ significance with respect to the background. As in Popesso et al (2012) for COSMOS and GOODS-N, Ziparo et al (2013) selected a clean subsample of groups in the ECDFS catalog with clear spectroscopic redshift identification along the line of sight, with at least ten members, the minimum required for a meaningful dynamical analysis, and without close companions, allowing for a clear definition of the spectroscopic members. This selection leads to 22 groups in the ECDFS out of the initial 50 X-ray-selected groups.…”

Section: Infrared and Spectroscopic Datamentioning

confidence: 99%

“…The evidence that more massive galaxies tend to reside in more massive haloes sets a clear link between the galaxy SF activity evolution and their environment. The "galaxy downsizing" scenario could therefore be interpreted in terms of a "halo downsizing" scenario as highlighted in Neistein et al (2006) and Popesso et al (2012).…”

Section: Introductionmentioning

confidence: 99%

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The evolution of galaxy star formation activity in massive haloes

Popesso

Biviano

Finoguenov

et al. 2015

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Context. There is now a large consensus that the current epoch of the cosmic star formation history (CSFH) is dominated by low mass galaxies while the most active phase, between redshifts 1 and 2, is dominated by more massive galaxies, which evolve more quickly. Aims. Massive galaxies tend to inhabit very massive haloes, such as galaxy groups and clusters. We aim to understand whether the observed "galaxy downsizing" could be interpreted as a "halo downsizing", whereas the most massive haloes, and their galaxy populations, evolve more rapidly than the haloes with lower mass. Methods. We studied the contribution to the CSFH of galaxies inhabiting group-sized haloes. This is done through the study of the evolution of the infra-red (IR) luminosity function of group galaxies from redshift 0 to redshift ∼1.6. We used a sample of 39 X-rayselected groups in the Extended Chandra Deep Field South (ECDFS), the Chandra Deep Field North (CDFN), and the COSMOS field, where the deepest available mid-and far-IR surveys have been conducted with Spitzer MIPS and with the Photodetector Array Camera and Spectrometer (PACS) on board the Herschel satellite. Results. Groups at low redshift lack the brightest, rarest, and most star forming IR-emitting galaxies observed in the field. Their IR-emitting galaxies contribute ≤10% of the comoving volume density of the whole IR galaxy population in the local Universe. At redshift 1, the most IR-luminous galaxies (LIRGs and ULIRGs) are mainly located in groups, and this is consistent with a reversal of the star formation rate (SFR) vs. density anti-correlation observed in the nearby Universe. At these redshifts, group galaxies contribute 60-80% of the CSFH, i.e. much more than at lower redshifts. Below z ∼ 1, the comoving number and SFR densities of IR-emitting galaxies in groups decline significantly faster than those of all IR-emitting galaxies. Conclusions. Our results are consistent with a "halo downsizing" scenario and highlight the significant role of "environment" quenching in shaping the CSFH.

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GOODS-Herschel: the impact of galaxy-galaxy interactions on the far-infrared properties of galaxies

Hwang¹,

Elbaz²,

Dickinson³

et al. 2011

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Aims. We study the impact of galaxy-galaxy interactions on the far-infrared properties of galaxies and its evolution at 0 < z < 1.2. Methods. Using the high-z galaxies in the fields of Great Observatories Origins Deep Survey (GOODS) observed by the Herschel Space Observatory in the framework of the GOODS-Herschel key program and the local IRAS or AKARI-selected galaxies in the field of Sloan Digital Sky Survey Data Release 7, we investigate the dependence of galaxy properties on the morphology of and the distance to the nearest neighbor galaxy. Results. We find that the star-formation rates (SFRs) and the specific SFRs (SSFRs) of galaxies on average depend on the morphology of and the distance to the nearest neighbor galaxy in this redshift range. When a late-type galaxy has a close neighbor galaxy, the SFR and the SSFR increase as it approaches a late-type neighbor, which is supported by Kolmogorov-Smirnov (K-S) and Monte Carlo (MC) tests with a significance level of >99%. However, the SFR and the SSFR decrease or do not change much as the galaxy approaches an early-type neighbor. The bifurcations of SFRs and SSFRs depending on the neighbor's morphology seem to occur at R n ≈ 0.5r vir,nei (virial radius of the neighbor), which is supported by K-S and MC tests with a significance level of >98%. For all redshift bins, the SSFRs of late-type galaxies interacting with late-type neighbors are increased by factors of about 1.8 ± 0.7 and 4.0 ± 1.2 compared to those of non-interacting galaxies when the pair separation is smaller than 0.5r vir,nei and 0.1r vir,nei , respectively. The dust temperature of both local and high-z late-type galaxies that strongly interact with late-type neighbors (i.e. R n ≤ 0.1r vir,nei ) appears to be higher than that of non-interacting galaxies with a significance level of 96−99%. However, the dust temperature of local late-type galaxies that strongly interact with early-type neighbors seems to be lower than or similar to that of non-interacting galaxies. Conclusions. Our results suggest that galaxy-galaxy interactions and mergers have been strongly affecting the SFR and the dust properties of star-forming galaxies over at least 8 billion years.

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The evolution of the star formation activity per halo mass up to redshift ~1.6 as seen byHerschel

Cited by 70 publications

References 107 publications

The galaxy stellar mass function of X-ray detected groups

The galaxy stellar mass function of X-ray detected groups

The evolution of galaxy star formation activity in massive haloes

GOODS-Herschel: the impact of galaxy-galaxy interactions on the far-infrared properties of galaxies

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