Galaxy groups in the 2dF Galaxy Redshift Survey: galaxy spectral type segregation in groups

Dominguez, M.; Zandivarez, Ariel; Martínez, H.; Merchán, Manuel; Muriel, H.; Lambas, D. García

doi:10.1046/j.1365-8711.2002.05669.x

Cited by 51 publications

(64 citation statements)

References 43 publications

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“…The observed morphology-density (e.g., Dressler 1980;Postman & Geller 1984;Dressler et al 1985;Goto et al 2003) and morphology-clustercentric radius (e.g., Whitmore & Gallagher 1991;Domínguez et al 2002;Goto et al 2003) relations for galaxies are in qualitative agreement with the trends obtained here for halos. The fraction of intermediate-type galaxies (mostly S0's) increases from the outskirts of clusters to intermediate cluster radii, while the fraction of late-type galaxies decreases.…”

Section: The Morphology-density Relation and Its Evolutionsupporting

confidence: 82%

“…The main observable dependencies with environment are seen for the morphological mix of elliptical and spiral galaxies (e.g., Dressler 1980;Postman & Geller 1984;Whitmore et al 1993;Domínguez et al 2002;Goto et al 2003), color and specific star formation rate (e.g., Balogh et al 1998Balogh et al , 2004Kodama et al 2001;Tran et al 2001;Pimbblet et al 2002;Lewis et al 2002;Blanton et al 2003;Gómez et al 2003;Kauffmann et al 2004;Hogg et al 2004;Tanaka et al 2004;Croton et al 2005). Besides, there is some evidence that these dependencies evolve, becoming weaker at higher redshifts (Treu et al 2003;Goto et al 2004;Bell et al 2004;Smith et al 2005;Postman et al 2005).…”

Section: M0mentioning

confidence: 99%

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The Dependence of the Mass Assembly History of Cold Dark Matter Halos on Environment

Maulbetsch

Avila-Reese

Colín

et al. 2007

ApJ

111

119

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We show by means of a high-resolution N-body simulation how the mass assembly histories of galaxy-size cold dark matter (CDM) halos depend on environment. Halos in high density environments form earlier and a higher fraction of their mass is assembled in major mergers, compared to low density environments. The distribution of the present-day specific mass aggregation rate is strongly dependent on environment. While in low density environments only ∼ 20% of the halos are not accreting mass at the present epoch, this fraction rises to ∼ 80% at high densities. At z = 1 the median of the specific aggregation rate is ∼ 4 times larger than at z = 0 and almost independent on environment. All the dependences on environment found here are critically enhanced by local processes associated to subhalos because the fraction of subhalos increases as the environment gets denser. The distribution of the halo specific mass aggregation rate as well as its dependence on environment resemble the relations for the specific star formation rate distribution of galaxies. An analogue of the morphology-density relation is also present at the level of CDM halos, being driven by the halo major merging history. Nevertheless, baryonic processes are necessary in order to explain further details and the evolution of the star formation rate-, color-and morphology-environment relations.

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Section: The Morphology-density Relation and Its Evolutionsupporting

confidence: 82%

Section: M0mentioning

confidence: 99%

The Dependence of the Mass Assembly History of Cold Dark Matter Halos on Environment

Maulbetsch

Avila-Reese

Colín

et al. 2007

ApJ

111

119

View full text Add to dashboard Cite

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“…In fact, Carlberg et al (2001b) found the presence of a color gradient only in groups with σ v > 150 km s −1 , and Domínguez et al (2002) detected spectral-type segregation only in groups with mass M ∼ > 10 13.5 h −1 M . Additional support to this idea is given by our analysis in Sect.…”

Section: Summary and Discussionmentioning

confidence: 99%

Morphology and luminosity segregation of galaxies in nearby loose groups

Girardi

Rigoni

Mardirossian

et al. 2003

A&A

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Abstract.We study morphology and luminosity segregation of galaxies in loose groups. We analyze the two catalogs of groups identified in the Nearby Optical Galaxy (NOG) sample, by means of hierarchical and percolation "friends-of-friends" methods (HG and PG catalogs, respectively). In the first part of our analysis we consider 387 and 436 groups of HG and PG and compare morphology-(luminosity-) weighted to unweighted group properties: velocity dispersion, mean pairwise distance, and mean groupcentric distance of member galaxies. The second part of our analysis is based on two ensemble systems, one for each catalog, built by suitably combining together galaxies of all groups (1584 and 1882 galaxies for HG and PG groups). We find that earlier-type (brighter) galaxies are more clustered and lie closer to the group centers, both in position and in velocity, than later-type (fainter) galaxies. Spatial segregations are stronger than kinematical segregations. These effects are generally detected at the ∼ >3-sigma level. Luminosity segregation is shown to be independent of morphology segregation. Our main conclusions are strengthened by the detection of segregation in both hierarchical and percolation catalogs. Our results agree with a continuum of segregation properties of galaxies in systems, from low-mass groups to massive clusters.

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“…This result suggests that galaxy transformation starts to occur in the infalling filaments, which consist of chains of groups in which field galaxies are affected by the group environment which changes their star-forming blue field-like properties into passive, red cluster-like galaxies. But even if groups seem to be the key environment to search for the nurture scenario, still the observational evidence for related segregation phenomena is quite scarce and holds mainly for the local Universe (Postman & Geller 1984;Mahdavi et al 1999;Tran et al 2001;Carlberg et al 2001a,b;Girardi et al 2003;Domínguez et al 2002;Wilman et al 2009;Bai et al 2010;Ribeiro et al 2010).…”

Section: Introductionmentioning

confidence: 99%

A journey from the outskirts to the cores of groups

Presotto

Iovino

Scodeggio

et al. 2012

A&A

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Context. Studying the evolution of galaxies located within groups may have important implications for our understanding of the global evolution of the galaxy population as a whole. The fraction of galaxies bound in groups at z ∼ 0 is as high as 60% and therefore any mechanism (among the many suggested) that could quench star formation when a galaxy enters group environment would be an important driver for galaxy evolution. Aims. Using the group catalog obtained from zCOSMOS spectroscopic data and the complementary photometric data from the COSMOS survey, we explore segregation effects occurring in groups of galaxies at intermediate/high redshifts. Our aim is to reveal if, and how significantly, group environment affects the evolution of infalling galaxies. Methods. We built two composite groups at intermediate (0.2 ≤ z ≤ 0.45) and high (0.45 < z ≤ 0.8) redshifts, and we divided the corresponding composite group galaxies into three samples according to their distance from the group center. The samples roughly correspond to galaxies located in a group's inner core, intermediate, and infall region. We explored how galaxy stellar masses and colors -working in narrow bins of stellar masses -vary as a function of the galaxy distance from the group center. Results. We found that the most massive galaxies in our sample (log(M gal /M ) ≥ 10.6) do not display any strong group-centric dependence of the fractions of red/blue objects. For galaxies of lower masses (9.8 ≤ log(M gal /M ) ≤ 10.6) there is a radial dependence in the changing mix of red and blue galaxies. This dependence is most evident in poor groups, whereas richer groups do not display any obvious trend of the blue fraction. Interestingly, mass segregation shows the opposite behavior: it is visible only in rich groups, while poorer groups have a a constant mix of galaxy stellar masses as a function of radius. Conclusions. These findings can be explained in a simple scenario where color-and mass-segregation originate from different physical processes. While dynamical friction is the obvious cause for establishing mass segregation, both starvation and galaxy-galaxy collisions are plausible mechanisms to quench star formation in groups at a faster rate than in the field. In poorer groups the environmental effects are caught in action superimposed to secular galaxy evolution. Their member galaxies display increasing blue fractions when moving from the group center to more external regions, presumably reflecting the recent accretion history of these groups.

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Galaxy groups in the 2dF Galaxy Redshift Survey: galaxy spectral type segregation in groups

Cited by 51 publications

References 43 publications

The Dependence of the Mass Assembly History of Cold Dark Matter Halos on Environment

The Dependence of the Mass Assembly History of Cold Dark Matter Halos on Environment

Morphology and luminosity segregation of galaxies in nearby loose groups

A journey from the outskirts to the cores of groups

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