The Morphology‐Density Relation in<i>z</i>∼ 1 Clusters

Postman, Marc; Franx, Marijn; Cross, Nicholas; Holden, B. P.; Ford, H. C.; Illingworth, G. D.; Goto, Tomotsugu; Demarco, R.; Rosati, P.; Blakeslee, John P.; Tran, Kim-Vy; Benítez, N.; Clampin, M.; Hartig, G.; Homeier, N.; Ardila, D. R.; Bartko, F.; Bouwens, Rychard; Bradley, Larry; Broadhurst, Tom; Brown, Robert A.; Burrows, C. J.; Cheng, E. S.; Feldman, P. D.; Golimowski, D. A.; Grönwall, C.; Infante, L.; Kimble, Randy A.; Krist, John; Lesser, Michael P.; Martel, A. R.; Mei, S.; Menanteau, F.; Meurer, G. R.; Miley, G. K.; Motta, V.; Sirianni, M.; Sparks, W. B.; Tran, H. D.; Tsvetanov, Z.; White, R. L.; Zheng, Wei

doi:10.1086/428881

Cited by 354 publications

(499 citation statements)

References 83 publications

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“…In agreement with previous studies (Postman et al 2005;Smith et al 2005;Capak et al 2007) we see that the morphology-density relation, in luminosity selected volumelimited samples, was already in place at z = 1, but tends to be flatter than at lower redshift. This is also in agreement with the observed trends in the colour-density relation (Cooper et al 2006;Cucciati et al 2006).…”

Section: Discussionsupporting

confidence: 93%

“…In many of these studies the environment is computed following the method first introduced by Dressler et al (1980) and often adopted later on (Dressler et al 1997;Postman et al 2005). The projected number density is calculated by counting the 10 nearest neighbors and dividing by the rectangular area enclosed enclosed by them.…”

Section: Comparison To Previous Studiesmentioning

confidence: 99%

“…They suggest that mechanisms such as starvation or harassment, operating over timescales of several Gyr, could explain the mild trends in the morphological mix. Further studies at high-z are mainly based on groups or clusters (Nuijten et al 2005;Postman et al 2005;Poggianti et al 2008) and the first relevant attempts to extend this analysis to field galaxies (Smith et al 2005;Capak et al 2007;Guzzo et al 2007;Holden et al 2007;van der Wel et al 2007) all make use of local projected surface densities to estimate the environment. In parallel, the redshift and luminosity evolution of the galaxy colour-density relation up to z ∼ 1.5 has been carefully investigated in two fundamental works (Cooper et al 2006;Cucciati et al 2006).…”

Section: Introductionmentioning

confidence: 99%

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The zCOSMOS redshift survey: the role of environment and stellar mass in shaping the rise of the morphology-density relation from z ~ 1

Tasca

Kneib²,

Iovino

et al. 2009

A&A

152

146

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Context. For more than two decades we have known that galaxy morphological segregation is present in the Local Universe. It is important to see how this relation evolves with cosmic time. Aims. To investigate how galaxy assembly took place with cosmic time, we explore the evolution of the morphology-density relation up to redshift z ∼ 1 using about 10 000 galaxies drawn from the zCOSMOS Galaxy Redshift Survey. Taking advantage of accurate HST/ACS morphologies from the COSMOS survey, of the well-characterised zCOSMOS 3D environment, and of a large sample of galaxies with spectroscopic redshift, we want to study here the evolution of the morphology-density relation up to z ∼ 1 and its dependence on galaxy luminosity and stellar mass. The multi-wavelength coverage of the field also allows a first study of the galaxy morphological segregation dependence on colour. We further attempt to disentangle between processes that occurred early in the history of the Universe or late in the life of galaxies. Methods. The zCOSMOS field benefits of high-resolution imaging in the F814W filter from the Advanced Camera for Survey (ACS). We use standard morphology classifiers, optimised for being robust against band-shifting and surface brightness dimming, and a new, objective, and automated method to convert morphological parameters into early, spiral, and irregular types. We use about 10 000 galaxies down to I AB = 22.5 with a spectroscopic sampling rate of 33% to characterise the environment of galaxies up to z ∼ 1 from the 100 kpc scales of galaxy groups up to the 100 Mpc scales of the cosmic web. The evolution of the morphology-density relation in different environments is then studied for luminosity and stellar-mass selected, volume-limited samples of galaxies. The trends are described and related to the various physical processes that could play a relevant role in the build-up of the morphology-density relation. Results. We confirm that the morphological segregation is present up to z ∼ 1 for luminosity-selected, volume-limited samples. The behaviour of the morphology-density relation gets flatter at fixed masses expecially above 10 10.6 M . We suggest the existence of a critical mass above which the physical processes governing galaxy stellar mass also determine the shaping of the galaxy more than its environment. We finally show that at a fixed morphology there is still a residual variation in galaxy colours with density. Conclusions. The observed evolution with redshift of the morphology-density relation offers an opportunity to trace the effect of nature and nurture as a function of environment. Even though it is based mainly on a biased view, the environmental dependence of the morphological evolution for luminosity-selected, volume-limited samples seems to indicate that nurture is in play. On the other hand, the lack of evolution observed for earlytype and spiral galaxies that are more massive than 10 10.8 M independents of the environment indicates that nature has imprinted these properties early in the life of...

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Section: Discussionsupporting

confidence: 93%

Section: Comparison To Previous Studiesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

The zCOSMOS redshift survey: the role of environment and stellar mass in shaping the rise of the morphology-density relation from z ~ 1

Tasca

Kneib²,

Iovino

et al. 2009

A&A

152

146

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“…In particular, galaxies at large radii show enhanced star formation and are more likely to have spiral morphologies compared to galaxies near the centre of the halo (Whitmore et al 1993;Goto et al 2003;Postman et al 2005;Rasmussen et al 2012;Wetzel et al 2012;Fasano et al 2015;Haines et al 2015). Therefore, in order to probe the environmentally driven aspects of galaxy evolution it is crucial to account for both the dependence on the host halo environment as well as the radial position within the group or cluster.…”

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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“…Statistical studies of the galaxy cluster population, in particular the cluster mass function, provide indispensable knowledge of cosmological model parameters (see Allen et al 2011 for a review, Tinker et al 2012), large scale structure (e.g., Bahcall 1988;Einasto et al 2001;Yang et al 2005b;Papovich 2008;Willis et al 2013) and galaxy evolution (e.g., Goto et al 2003;Postman et al 2005;Martínez et al 2008). However, deducing accurate masses of these gravitationally bound structures remains a fundamental challenge for current and future cosmological studies.…”

Section: Introductionmentioning

confidence: 99%

Galaxy Cluster Mass Reconstruction Project – II. Quantifying scatter and bias using contrasting mock catalogues

Old

Wojtak

Mamon

et al. 2015

Monthly Notices of the Royal Astronomical Society

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This article is the second in a series in which we perform an extensive comparison of various galaxy-based cluster mass estimation techniques that utilise the positions, velocities and colours of galaxies. Our aim is to quantify the scatter, systematic bias and completeness of cluster masses derived from a diverse set of 25 galaxy-based methods using two contrasting mock galaxy catalogues based on a sophisticated halo occupation model and a semi-analytic model. Analysing 968 clusters, we find a wide range in the RMS errors in log M 200c delivered by the different methods (0.18 to 1.08 dex, i.e., a factor of ∼1.5 to 12), with abundance matching and richness methods providing the best results, irrespective of the input model assumptions. In addition, certain methods produce a significant number of catastrophic cases where the mass is under-or over-estimated by a factor greater than 10. Given the steeply falling high-mass end of the cluster mass function, we recommend that richness or abundance matching-based methods are used in conjunction with these methods as a sanity check for studies selecting high mass clusters. We see a stronger correlation of the recovered to input number of galaxies for both catalogues in comparison with the group/cluster mass, however, this does not guarantee that the correct member galaxies are being selected. We do not observe significantly higher scatter for either mock galaxy catalogues. Our results have implications for cosmological analyses that utilise the masses, richnesses, or abundances of clusters, which have different uncertainties when different methods are used.

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The Morphology‐Density Relation inz∼ 1 Clusters

Cited by 354 publications

References 83 publications

The zCOSMOS redshift survey: the role of environment and stellar mass in shaping the rise of the morphology-density relation from z ~ 1

The zCOSMOS redshift survey: the role of environment and stellar mass in shaping the rise of the morphology-density relation from z ~ 1

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

Galaxy Cluster Mass Reconstruction Project – II. Quantifying scatter and bias using contrasting mock catalogues

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