The Padova-Millennium Galaxy and Group Catalogue (PM2GC): the group-finding method and the PM2GC catalogues of group, binary and single field galaxies

Calvi, Rosa; Poggianti, Bianca M.; Vulcani, Benedetta

doi:10.1111/j.1365-2966.2011.19088.x

Cited by 84 publications

(111 citation statements)

References 74 publications

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“…They claim that this difference can be due to the offset between stellar masses in their samples, drawn from different catalogues. On the other hand, Poggianti et al (2013) use a similar cluster sample for galaxies with masses M * < 3 × 10 11 M ⊙ and compare it with both a sample extracted from PM2GC (Calvi, Poggianti & Vulcani 2011) and the local relation by Shen et al (2003), also finding an offset of about 1−σ between both relations. Figure 11 shows the results obtained by Valentinuzzi et al (2010) and Poggianti et al (2013), rescaled to a Chabrier (2003) IMF, together with the stellar mass-size relation obtained in this work for cluster and field galaxies.…”

Section: Thementioning

confidence: 99%

The effect of the environment on the stellar mass–size relationship for present-day galaxies

Cebrián¹,

Trujillo²

2014

Monthly Notices of the Royal Astronomical Society

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To study how the environment can influence the relation between stellar mass and effective radius of nearby galaxies (z < 0.12), we use a mass-complete sample extracted from the NYU-Value Added Catalogue. This sample contains almost 232000 objects with masses up to 3 × 10 11 M ⊙ . For every galaxy in our sample, we explore the surrounding density within 2 Mpc using two different estimators of the environment. We find that galaxies are slightly larger in the field than in high-density regions. This effect is more pronounced for late-type morphologies (∼ 7.5 % larger) and especially at low masses (M * < 2 × 10 10 M ⊙ ), although it is also measurable in early-type galaxies (∼ 3.5 % larger). The environment also leaves a subtle imprint in the scatter of the stellar mass-size relation. This scatter is larger in low-density regions than in high-density regions for both morphologies, on average ∼ 3.5 % larger for early-type and ∼ 0.8 % for late-type galaxies. Late-type galaxies with low masses (M * < 2 × 10 10 M ⊙ ) show the largest differences in the scatter among environments. The scatter is ∼ 20 % larger in the field than in clusters for these low-mass objects. Our analysis suggest that galaxies in clusters form earlier than those in the field. In addition, cluster galaxies seem to be originated from a more homogeneous family of progenitors.

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Section: Thementioning

confidence: 99%

The effect of the environment on the stellar mass–size relationship for present-day galaxies

Cebrián¹,

Trujillo²

2014

Monthly Notices of the Royal Astronomical Society

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“…The percentages of field galaxies in each class have been estimated using the PadovaMillennium Galaxy and Group Catalogue (Calvi et al 2011(Calvi et al , 2012, PM2GC), consisting of a spectroscopically complete sample of galaxies at 0.03 z 0.11 brighter than MB = −18.7. This sample is sourced from the Millennium Galaxy Catalogue ( contiguous equatorial survey, complete down to B=20 and representative of the general field population in the local Universe.…”

Section: Removing the Field Galaxiesmentioning

confidence: 99%

Morphological fractions of galaxies in WINGS clusters: revisiting the morphology–density paradigm

Fasano¹,

Poggianti²,

Bettoni³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We present the Morphology-Density and Morphology-Radius relations (T -Σ and T -R, respectively) obtained from the WINGS database of galaxies in nearby clusters. Aiming to achieve the best statistics, we exploit the whole sample of galaxies brighter than M V = −19.5 (5,504 objects), stacking up the 76 clusters of the WINGS survey altogether.Using this global cluster sample, we find that the T -Σ relation holds only in the inner cluster regions (R < 1/3 × R 200 ), while the T -R relation keeps almost unchanged over the whole range of local density. A couple of tests and two sets of numerical simulations support the robustness of these results against the effects of the limited cluster area coverage of the WINGS imaging. The above mentioned results hold for all cluster masses (X-ray luminosity and velocity dispersion) and all galaxy stellar masses (M * ). The strength of the T -Σ relation (where present) increases with increasing M * , while this effect is not found for the T -R relation.Noticeably, the absence/presence of subclustering determines the presence/absence of the T -Σ relation outside the inner cluster regions, leading us to the general conclusion that the link between morphology and local density is preserved just in dynamically evolved regions. We hypothesize that some mechanism of morphological broadening/redistribution operates in the intermediate/outer regions of substructured ("non relaxed") clusters, producing a strong weakening of the T -Σ relation.

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“…We have carried out a complementary study in the local universe (Calvi et al, in prep.) using a mass-limited sample (M * ≥ 10 10.25 M ) of galaxies from the Padova Millennium Galaxy and Group Catalog (PM2GC) (Calvi et al 2011) and the WINGS survey. This work also shows that cluster, group and field galaxies at low-z have comparable mass functions 7 .…”

Section: The Evolution Of the Mass Functions Is Very Similar In Diffementioning

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

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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).

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The Padova-Millennium Galaxy and Group Catalogue (PM2GC): the group-finding method and the PM2GC catalogues of group, binary and single field galaxies

Cited by 84 publications

References 74 publications

The effect of the environment on the stellar mass–size relationship for present-day galaxies

The effect of the environment on the stellar mass–size relationship for present-day galaxies

Morphological fractions of galaxies in WINGS clusters: revisiting the morphology–density paradigm

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

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