CAIRNS: The Cluster and Infall Region Nearby Survey. III. Environmental Dependence of Hα Properties of Galaxies

Rines, Kenneth J.; Geller, Margaret J.; Kurtz, Michael J.; Diaferio, Antonaldo

doi:10.1086/433173

Cited by 97 publications

(167 citation statements)

References 84 publications

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“…A clear trend is observed inward of two to three cluster virial radii: the fraction of gas-rich galaxies decreases monotonically with decreasing cluster-centric distance. This trend is in good agreement with observations that the HI gas depletion increases with decreasing cluster-centric distance inward of about two virial radii (15,18,20,24,(48)(49)(50)(51)(52). Intriguingly, observations indicate that the distribution of star formation rates of cluster galaxies begins to change, compared with the field population, at a cluster-centric radius of about three virial radii.…”

Section: Resultssupporting

confidence: 91%

Gas loss in simulated galaxies as they fall into clusters

Cen

Pop

Bahcall

2014

Proc. Natl. Acad. Sci. U.S.A.

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We use high-resolution cosmological hydrodynamic galaxy formation simulations to gain insights into how galaxies lose their cold gas at low redshift as they migrate from the field to the highdensity regions of clusters of galaxies. We find that beyond three cluster virial radii, the fraction of gas-rich galaxies is constant, representing the field. Within three cluster-centric radii, the fraction of gas-rich galaxies declines steadily with decreasing radius, reaching <10% near the cluster center. Our results suggest galaxies start to feel the effect of the cluster environment on their gas content well beyond the cluster virial radius. We show that almost all gas-rich galaxies at the cluster virial radius are falling in for the first time at nearly radial orbits. Furthermore, we find that almost no galaxy moving outward at the cluster virial radius is gas-rich (with a gas-to-baryon ratio greater than 1%). These results suggest that galaxies that fall into clusters lose their cold gas within a single radial round-trip.cosmology | observations | large-scale structure of universe | intergalactic medium I t has long been known that the local environment affects galaxy properties. Earlier work (1)(2)(3)(4) showed that the fraction of early-type galaxies increases dramatically toward the central regions of clusters of galaxies, whereas the less-dense regions of the field are dominated by spiral galaxies. Similarly, the "color-density relation" (5-8) indicates that red, old galaxies are found preferentially in overdense environments, and galaxies with bluer, younger stellar populations are more common in the field. This color bimodality is linked to a transition in star formation rates between the low-density field and the high-density regions inside clusters (4, 9). However, we still do not have a complete picture of the process through which blue, late-type, star-forming galaxies in the field transform into red, early-type galaxies when entering a cluster. We know that cold gas in galaxies is spatially extended and often distributed far beyond the optical disks (10). Cosmologically, some of the cold gas that feeds galaxy formation may come from the intergalactic medium (11,12). Observations suggest that neutral hydrogen feeds galaxies and turns into molecular hydrogen at a high column density of ∼10 22 cm −2 (13), within which star formation is observed to occur. Together, these facts suggest that the amount of neutral hydrogen supply may ultimately set the rate of star formation. The environmental dependence of galaxy properties may thus be related to the availability of cold gas in or around galaxies. This expectation is supported by observations of galaxies in different environments, showing the well-known depletion of both cold gas and star formation toward the high-density central regions of clusters; this is likely caused by ram pressure stripping of the cold gas by the hot intracluster medium (plus additional gravitational interactions) in the dense environments (refs. 14-24 and references therein). Recent deta...

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Section: Resultssupporting

confidence: 91%

Gas loss in simulated galaxies as they fall into clusters

Cen

Pop

Bahcall

2014

Proc. Natl. Acad. Sci. U.S.A.

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“…Previous studies (Lewis et al 2002;Gray et al 2004;Rines et al 2005;Verdugo et al 2008) have similarly found that star formation of galaxies within infall regions remains suppressed compared to the field out to radii of ∼ 2 − 3 R 200 . This suppression is often attributed to backsplash galaxies which have already made a passage through the halo centre, the pre-processing of galaxies in small groups prior to infall, or some combination of the two.…”

Section: Galaxy Properties At Large Radiimentioning

confidence: 89%

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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“…Ellingson et al (2001) studied the composite radial distributions of different stellar populations as a function of clustercentric radius. They found no evidence at any radius within the clusters for an excess of star formation over that seen in the field (see also Rines et al 2005 andVerdugo et al 2008). The general agreement is that galaxy properties converge to those of field galaxies at 2 − 3 virial radii.…”

Section: Introductionmentioning

confidence: 91%

Galaxies infalling into groups: filaments versus isotropic infall

Martínez

Muriel

Coenda

2015

Mon. Not. R. Astron. Soc.

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We perform a comparative analysis of the properties of galaxies infalling into groups classifying them accordingly to whether they are: falling along filamentary structures; or they are falling isotropically. For this purpose, we identify filamentary structures connecting massive groups of galaxies in the SDSS. We perform a comparative analysis of some properties of galaxies in filaments, in the isotropic infall region, in the field, and in groups. We study the luminosity functions (LF) and the dependence of the specific star formation rate (SSFR) on stellar mass, galaxy type, and projected distance to the groups that define the filaments. We find that the LF of galaxies in filaments and in the isotropic infalling region are basically indistinguishable between them, with the possible exception of late-type galaxies. On the other hard, regardless of galaxy type, their LFs are clearly different from that of field or group galaxies. Both of them have characteristic absolute magnitudes and faint end slopes in between the field and group values. More significant differences between galaxies in filaments and in the isotropic infall region are observed when we analyse the SSFR. We find that galaxies in filaments have a systematically higher fraction of galaxies with low SSFR as a function of both, stellar mass and distance to the groups, indicating a stronger quenching of the star formation in the filaments compared to both, the isotropic infalling region, and the field. Our results suggest that some physical mechanisms that determine the differences observed between field galaxies and galaxies in systems, affect galaxies even when they are not yet within the systems.

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CAIRNS: The Cluster and Infall Region Nearby Survey. III. Environmental Dependence of Hα Properties of Galaxies

Cited by 97 publications

References 84 publications

Gas loss in simulated galaxies as they fall into clusters

Gas loss in simulated galaxies as they fall into clusters

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

Galaxies infalling into groups: filaments versus isotropic infall

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