Where are the stars?

Eke, V. R.; Baugh, C. M.; Cole, Shaun; Frenk, Carlos S.; King, Henry; Peacock, J. A.

doi:10.1111/j.1365-2966.2005.09384.x

Cited by 108 publications

(144 citation statements)

References 31 publications

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“…The fraction of stellar mass in the more massive galaxy clusters is negligible because these are rare objects (Eke et al 2005), and group-sized haloes are the most common high-mass haloes for a galaxy to inhabit. For this reason, we study the evolution of the IR LF of galaxies in groups, and compare it to that of more isolated field galaxies.…”

Section: Introductionmentioning

confidence: 99%

The evolution of galaxy star formation activity in massive haloes

Popesso

Biviano

Finoguenov

et al. 2015

A&A

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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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Section: Introductionmentioning

confidence: 99%

The evolution of galaxy star formation activity in massive haloes

Popesso

Biviano

Finoguenov

et al. 2015

A&A

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“…On the other hand the low-density field is preferentially populated by blue, star forming, spiral galaxies. A third environment, galaxy groups, are the most common environment in the local Universe (Geller & Huchra 1983;Eke et al 2005) and also represent an intermediate-mass regime in which significant populations of both star-forming spirals and passive ellipticals are observed (e.g. Wilman et al 2005;McGee et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Evidence of pre-processing and a dependence on dynamical state for low-mass satellite galaxies

Roberts¹,

Parker²

2017

Monthly Notices of the Royal Astronomical Society

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We study the dependence of satellite star formation rate and morphology on group dynamics for a sample of SDSS groups. We classify the group dynamical state and study satellite properties for populations of galaxies at small and large group-centric radii. For galaxies at large radii we find no differences in the star-forming or disc fraction for those in Gaussian groups compared to those in non-Gaussian groups. By comparing the star-forming and disc fractions of infalling galaxies to field galaxies we find evidence for the pre-processing of both star formation rate and morphology. The strength of pre-processing increases with halo mass and is highest for low-mass galaxies infalling onto high-mass haloes. We show that the star formation rate of galaxies at small radii correlates with group dynamical state, with galaxies in nonGaussian groups showing enhanced star-forming fractions compared to galaxies in Gaussian groups. Similar correlations are not seen for the disc fractions of galaxies at small radii. This seems to suggest that either the mechanisms driving star formation quenching at small halo-centric radii are more efficient in dynamically relaxed groups, or that non-Gaussian groups have assembled more recently and therefore satellites of the groups will have been exposed to these transforming mechanisms for less time.

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“…Galaxies in clusters are known to have suppressed star formation versus galaxies in the field at all redshifts (e.g., Balogh et al 1997Balogh et al , 1999Poggianti et al 1999;Postman et al 2001; Lewis et al 2002;Gomez et al 2003;Kauffmann et al 2004), but relatively few galaxies reside in such dense environments even at low redshift. However, as many as 50% Y70% of all galaxies reside in less massive groups of galaxies (Turner & Gott 1976;Geller & Huchra 1983;Eke et al 2005), meaning that the group environment can play an important role in the evolution of galaxies. Tracing the properties of galaxies versus both the local environment of the surrounding few galaxies and the global group/cluster environment has important implications for the processes responsible for both the morphological transformation of galaxies and the reduction in star formation.…”

Section: Introductionmentioning

confidence: 99%

The Evolution of Galaxies in X‐Ray–luminous Groups

Jeltema

Mulchaey

Lubin

et al. 2007

ApJ

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We investigate the galaxy populations in seven X-rayYselected, intermediate-redshift groups (0:2 < z < 0:6). Overall, the galaxy populations in these systems are similar to those in clusters at the same redshift; they have large fractions of early-type galaxies ( f e $ 70%) and small fractions of galaxies with significant star formation ( f ½O ii $ 30%). We do not observe a strong evolution in the galaxy populations from those seen in X-rayYluminous groups at low redshift. Both f e and f ½O ii are correlated with radius but do not reach the field value out to $r 500 . However, we find significant variation in the galaxy populations between groups, with some groups having fieldlike populations. Comparisons between the morphological and spectral properties of group galaxies reveal both gas-poor mergers and a population of passive spirals. Unlike low-redshift, X-rayYemitting groups, in some of these groups the brightest galaxy does not lie at the center of the X-ray emission, and in several of the groups that do have a central BGG, the BGG has multiple components. These groups appear to represent a range of evolutionary stages in the formation of the BGG. Some groups have relatively large central galaxy densities, and one group contains a string of seven bright galaxies within a radius of 200 kpc that have a lower velocity dispersion than the rest of the system. None of the central galaxies, including those with multiple components, have significant [O ii] emission. These observations support a scenario in which BGGs are formed relatively late through gas-poor mergers.

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Where are the stars?

Cited by 108 publications

References 31 publications

The evolution of galaxy star formation activity in massive haloes

The evolution of galaxy star formation activity in massive haloes

Evidence of pre-processing and a dependence on dynamical state for low-mass satellite galaxies

The Evolution of Galaxies in X‐Ray–luminous Groups

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