The importance of the local density in shaping the galaxy stellar mass functions★

Vulcani, Benedetta; Poggianti, Bianca M.; Fasano, G.; Desai, Vandana; Dressler, Alan; Oemler, A.; Calvi, Rosa; D’Onofrio, M.; Moretti, Alessia

doi:10.1111/j.1365-2966.2011.20135.x

Cited by 53 publications

(87 citation statements)

References 58 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The values of the projected local density that we use are calculated from a circular area enclosing the first 10 most nearby galaxies, which also accounts for background counts as expected from Berta et al (2006) and is corrected for border effect (see Vulcani et al 2012, for details). The local density is expressed as the logarithm of the number of galaxies with M V ≤ −19.5 per Mpc −2 .…”

Section: Emission-line Galaxies In Local Clustersmentioning

confidence: 99%

Wings-Spe

Fritz

Poggianti

Cava

et al. 2014

A&A

View full text Add to dashboard Cite

Context. Cluster galaxies are the ideal sites to look at when studying the influence of the environment on the various aspects of the evolution of galaxies, such as the changes in their stellar content and morphological transformations. In the framework of wings, the WIde-field Nearby Galaxy-cluster Survey, we have obtained optical spectra for ∼6000 galaxies selected in fields centred on 48 local (0.04 < z < 0.07) X-ray selected clusters to tackle these issues. Aims. By classifying the spectra based on given spectral lines, we investigate the frequency of the various spectral types as a function of both the clusters' properties and the galaxies' characteristics. In this way, using the same classification criteria adopted for studies at higher redshift, we can consistently compare the properties of the local cluster population to those of their more distant counterparts. Methods. We describe a method that we have developed to automatically measure the equivalent width of spectral lines in a robust way, even in spectra with a non optimal signal-to-noise ratio. This way, we can derive a spectral classification reflecting the stellar content, based on the presence and strength of the [Oii] and Hδ lines. Results. After a quality check, we are able to measure 4381 of the ∼6000 originally observed spectra in the fields of 48 clusters, of which 2744 are spectroscopically confirmed cluster members. The spectral classification is then analysed as a function of galaxies' luminosity, stellar mass, morphology, local density, and host cluster's global properties and compared to higher redshift samples (MORPHS and EDisCS). The vast majority of galaxies in the local clusters population are passive objects, being also the most luminous and massive. At a magnitude limit of M V < −18, galaxies in a post-starburst phase represent only ∼11% of the cluster population, and this fraction is reduced to ∼5% at M V < −19.5, which compares to the 18% at the same magnitude limit for high-z clusters. "Normal" star-forming galaxies (e(c)) are proportionally more common in local clusters. Conclusions. The relative occurrence of post-starbursts suggests a very similar quenching efficiency in clusters at redshifts in the 0 to ∼1 range. Furthermore, more important than the global environment, the local density seems to be the main driver of galaxy evolution in local clusters at least with respect to their stellar populations content.

show abstract

Section: Emission-line Galaxies In Local Clustersmentioning

confidence: 99%

Wings-Spe

Fritz

Poggianti

Cava

et al. 2014

A&A

View full text Add to dashboard Cite

show abstract

“…In Vulcani et al (2012), we analysed specifically the dependence of the mass function on local density, using collectively the WINGS, PM2GC, ICBS, and EDisCS samples. We found that both in the local and distant universe, in clusters and in the field, local density plays an important role in driving the mass distribution.…”

Section: Global and Local Environmentmentioning

confidence: 99%

The galaxy stellar mass function and its evolution with time show no dependence on global environment

Vulcani

Poggianti

Oemler

et al. 2013

A&A

View full text Add to dashboard Cite

We present an analysis of the galaxy stellar mass function in different environments at intermediate redshift (0.3 ≤ z ≤ 0.8) for two mass-limited galaxy samples. We use the IMACS Cluster Building Survey (ICBS; M * ≥ 10 10.5 M ) to study cluster, group and field galaxies at z = 0.3-0.45, and the ESO Distant Cluster Survey (EDisCS; M * ≥ 10 10.2 M ) to investigate cluster and group galaxies at z = 0.4-0.8. Our analysis thus includes galaxies with masses reaching just below that of the Milky Way. Excluding the brightest cluster galaxies, we show that the shape of the mass distribution does not seem to depend on global environment, Our two main results are: (1) Galaxies in the virialised regions of clusters, in groups, and in the field follow similar mass distributions. (2) Comparing the ICBS and EDisCS mass functions to mass functions in the local universe, we detect evolution from z ∼ 0.4-0.6 to z ∼ 0.07 in the sense that the population of low-mass galaxies has grown with time with respect to the population of massive galaxies. This evolution is independent of environment, i.e., the same for clusters and the field. Furthermore, considering only cluster galaxies, we find that no differences can be detected in their mass functions either within the virialised regions, or when we compare galaxies inside and outside the virial radius. Finally, we find that red and blue galaxies have different mass functions. However, the shapes of the mass functions of blue and red galaxies do not seem to depend on their environment (clusters groups and the field).

show abstract

“…Some studies have attempted to measure the SMF as a function of local environment at 0.4 z 1.2 (e.g. Bundy et al 2006;Bolzonella et al 2010;Vulcani et al 2011Vulcani et al , 2012Giodini et al 2012). A measurement of the SMF at the highest densities has not yet been achieved in this redshift range.…”

Section: Introductionmentioning

confidence: 99%

The environmental dependence of the stellar mass function atz~ 1

Burg

Muzzin

Hoekstra

et al. 2013

A&A

112

View full text Add to dashboard Cite

Aims. We present the stellar mass functions (SMFs) of star-forming and quiescent galaxies from observations of ten rich, redsequence selected, clusters in the Gemini Cluster Astrophysics Spectroscopic Survey (GCLASS) in the redshift range 0.86 < z < 1.34. We compare our results with field measurements at similar redshifts using data from a K s -band selected catalogue of the COSMOS/UltraVISTA field. Methods. We construct a K s -band selected multi-colour catalogue for the clusters in eleven photometric bands covering u-8 μm, and estimate photometric redshifts and stellar masses using spectral energy distribution fitting techniques. To correct for interlopers in our cluster sample, we use the deep spectroscopic component of GCLASS, which contains spectra for 1282 identified cluster and field galaxies taken with Gemini/GMOS. This allowed us to correct cluster number counts from a photometric selection for false positive and false negative identifications. Both the photometric and spectroscopic samples are sufficiently deep that we can probe the SMF down to masses of 10 10 M . Results. We distinguish between star-forming and quiescent galaxies using the rest-frame U − V versus V − J diagram, and find that the best-fitting Schechter parameters α and M * are similar within the uncertainties for these galaxy types within the different environments. However, there is a significant difference in the shape and normalisation of the total SMF between the clusters and the field sample. This difference in the total SMF is primarily a reflection of the increased fraction of quiescent galaxies in high-density environments. We apply a simple quenching model that includes components of mass-and environment-driven quenching, and find that in this picture 45 +4 −3 % of the star-forming galaxies, which normally would be forming stars in the field, are quenched by the cluster. Conclusions. If galaxies in clusters and the field quench their star formation via different mechanisms, these processes have to conspire in such a way that the shapes of the quiescent and star-forming SMF remain similar in these different environments.

show abstract

The importance of the local density in shaping the galaxy stellar mass functions★

Cited by 53 publications

References 58 publications

Wings-Spe

Wings-Spe

The galaxy stellar mass function and its evolution with time show no dependence on global environment

The environmental dependence of the stellar mass function atz~ 1

Contact Info

Product

Resources

About