A journey from the outskirts to the cores of groups

Presotto, V.; Iovino, A.; Scodeggio, M.; Cucciati, O.; Knobel, C.; Bolzonella, M.; Oesch, Pascal; Finoguenov, A.; Tanaka, Masayuki; Kovač, K.; Peng, Yingjie; Zamorani, G.; Bardelli, S.; Pozzetti, L.; Kampczyk, P.; López-Sanjuan, C.; Vergani, D.; Zucca, E.; Tasca, L.; Carollo, C. M.; Contini, T.; Kneib, Jean-Paul; Fèvre, O. Le; Lilly, S. J.; Mainieri, V.; Renzini, A.; Bongiorno, A.; Caputi, K.; Torre, S. de la; Ravel, L. de; Franzetti, P.; Garilli, B.; Lamareille, F.; Borgne, J. F. Le; Brun, V. Le; Maier, C.; Mignoli, M.; Pelló, R.; Pérez-Montero, E.; Ricciardelli, E.; Silverman, John D.; Tresse, L.; Barnes, Luke A.; Bordoloi, Rongmon; Cappi, A.; Cimatti, A.; Coppa, G.; Koekemoer, Anton M.; McCracken, H. J.; Moresco, M.; Nair, Preethi; Welikala, N.

doi:10.1051/0004-6361/201118293

Cited by 41 publications

(77 citation statements)

References 97 publications

(84 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The radial fraction of red dwarf galaxies is higher in the center than in the outskirts when we estimate the red dwarf fraction using the color-magnitude relation (equation (1)) by Weinmann et al (2011). This observation is consistent with the results of simulations (Wetzel et al 2012(Wetzel et al , 2013) and other observations (Popesso et al 2006;Presotto et al 2012;Lee et al 2016). The standard interpretation of this effect is that the central galaxies have lower star formation rates.…”

Section: The Ngc 2784 Galaxy Groupsupporting

confidence: 88%

“…We find with 99.1% confidence that the samples do not have the same radial distribution. The difference in central concentration may reflect mass segregation, with more massive galaxies in a cluster or group being more centrally concentrated (Presotto et al 2012;Roberts et al 2015). Plausible physical reasons for that apparent concentration range from environmentally dependent formation histories, differences in dynamical friction, or mass-dependent tidal stripping.…”

Section: The Ngc 2784 Galaxy Groupmentioning

confidence: 99%

See 1 more Smart Citation

Dwarf Galaxy Discoveries from the KMTNet Supernova Program. I. The NGC 2784 Galaxy Group^*

Park

Moon

Zaritsky

et al. 2017

ApJ

View full text Add to dashboard Cite

We present BV I surface photometry of 31 dwarf galaxy candidates discovered in a deep image stack from the KMTNet Supernova Program of ∼ 30 square degrees centered on the nearby NGC 2784 galaxy group. Our final images have a 3σ surface brightness detection limit of µ V ≈ 28.5 mag arcsec −2 . The faintest central surface brightness that we measure is µ 0,V = 26.1 mag arcsec −2 . If these candidates are at the distance of NGC 2784, then they have absolute magnitudes greater than M V = −9.5 mag and effective radii larger than 170 pc. Their radial number density decreases exponentially with distance from the center of NGC 2784 until it flattens beyond a radius of 0.5 Mpc. We interpret the baseline density level to represent the background contamination and so estimate that 22 of the 31 new candidates are dwarf members of the group. The candidate's average color, (B − V ) 0 ≈ 0.7, and Sérsic structural parameters are consistent with those parameters for the dwarf populations of other groups. We find that the central population of dwarfs is redder and brighter than the rest of the population. The measured faint end slope of the luminosity function, α ≈ −1.33, is steeper than that of the Local Group but consistent with published results for other groups. Such comparisons are complicated by systematic differences among different studies, but will be simpler when the KMTNet survey, which will provide homogenous data for 15 to 20 groups, is completed.

show abstract

Section: The Ngc 2784 Galaxy Groupsupporting

confidence: 88%

Section: The Ngc 2784 Galaxy Groupmentioning

confidence: 99%

Dwarf Galaxy Discoveries from the KMTNet Supernova Program. I. The NGC 2784 Galaxy Group^*

Park

Moon

Zaritsky

et al. 2017

ApJ

View full text Add to dashboard Cite

show abstract

“…In addition, Fig. 5 shows that the red fraction of principal galaxies outside groups is lower than in groups (e.g., Gerke et al 2007;Balogh et al 2009;Iovino et al 2010;Cucciati et al 2010b;Presotto et al 2012). These trends are also present in the companion sample, but f red is a factor of two lower than for principal galaxies (Fig.…”

Section: Measuring the Group Richnessmentioning

confidence: 97%

“…We checked that our conclusions are the same if the parameters for blue galaxies in Faber et al (2007) are used. Then, we added our sources into the group environment, as an "infall", starting the quenching process (e.g., Presotto et al 2012). Quenched galaxies become less luminous in the B-band and eventually reach the red sequence after a quenching time T Q .…”

Section: The Assembly Of Passive and Star-forming L B L * B Galaxies mentioning

confidence: 99%

The VIMOS VLT Deep Survey

López-Sanjuan

Cucciati

Fèvre

et al. 2013

A&A

Self Cite

View full text Add to dashboard Cite

Aims. Understanding the role of environment in galaxy evolution is an important but still open issue. In the present work we study the close environment of red and blue L B L * B galaxies hosted by VVDS-Deep groups. Methods. We use the VIMOS VLT Deep Survey to study the close environment of galaxies in groups at 0.2 ≤ z < 0. .25 galaxies belonging to that group. We split our principal sample into red, passive galaxies with NUV − r ≥ 4.25 and blue, star-forming galaxies with NUV − r < 4.25. We study how the number of close neighbours per L B L * B galaxy depends on N, colour, and redshift. Results. Blue galaxies with a close neighbour are primarily located in poor groups, while the red ones are in rich groups. The number of close neighbours per red galaxy increases with N, n red ∝ 0.11N, while that of blue galaxies does not depend on N and is roughly constant. In addition, these trends are found to be independent of redshift, and only the average n blue evolves, decreasing with cosmic time. Conclusions. Our results support the following assembly history of L B L * B galaxies in the group environment: red, massive (M ∼ 10 10.8 M ) galaxies were formed in/accreted by the dark matter halo of the group at early times (z 1), therefore their number of neighbours provides a fossil record of the stellar mass assembly of groups, traced by their richness N. On the other hand, blue, less massive (M ∼ 10 10.2 M ) galaxies have recently been accreted by the group potential and are still in their parent dark matter halo, having the same number of neighbours irrespective of N. As time goes by, these blue galaxies settle in the group potential and turn red and/or fainter, thus becoming satellite galaxies in the group. With a toy quenching model, we estimate an infall rate of field galaxies into the group environment of infall = 0.9 − 1.5 × 10 −4 Mpc −3 Gyr −1 at z ∼ 0.7.

show abstract

“…Presotto et al 2012) will result in using a redder color to split blue and red galaxies, hence in increasing f blue .…”

Section: Remark On Taking Into Account Secular Evolution When Estimatmentioning

confidence: 99%

Galaxy mass, cluster-centric distance and secular evolution: their role in the evolution of galaxies in clusters in the last 10 Gyr

Raichoor

Andreon

2012

A&A

View full text Add to dashboard Cite

Context. Galaxy mass and environment are known to play a key role in galaxy evolution: studying galaxy colors as a function of redshift, galaxy mass, and environment offers a powerful diagnosis to disentangle the role of each. Aims. We study the simultaneous dependence of the fraction of blue galaxies f blue on secular evolution, environment, and galaxy mass with a well-controlled cluster sample. We are thus able to study the evolution and respective role of the cessation of star formation history (SFH) in clusters caused by galaxy mass ("mass quenching") or by environment ("environmental quenching"). Methods. We defined an homogenous X-ray selected cluster sample (25 clusters with 0 < z < 1 and one cluster at z ∼ 2.2), having similar masses and well-defined sizes. Using multicolor photometry and a large spectroscopic sample to calibrate photometric redshifts, we carefully estimated f blue for each cluster at different galaxy mass and cluster-centric distance bins. We then fitted the dependence of f blue on redshift (z), environment (r/r 200 ) and galaxy mass (M) with a simple model. Results. f blue increases with cluster-centric distance with a slope α = 1.2 +0.4 −0.3 , decreases with galaxy mass with a slope β = −3.8 +0.6 −0.5 , and increases with redshift with a slope γ = 3.3 +0.7 −0.6 . The data also require for the first time a differential evolution with galaxy mass of f blue with redshift, with lower mass galaxies evolving slower by a factor ζ = −3.9 +0.9 −1.1 . Conclusions. Our study shows that the processes responsible for the cessation of star formation in clusters are effective at all epochs (z < ∼ 2.2), and more effective in denser environments and for more massive galaxies. We found that the mass and environmental quenchings are separable, that environmental quenching does not change with epoch, and that mass quenching is a dynamical process, i.e. its evolutionary rate is mass-dependent. Our study extends the downsizing-like scenario, where the most massive galaxies have their properties set at a very high redshift, to the cluster environment and all galaxies. It illustrates the need to disentangle galaxy mass and cluster-centric distance to properly estimate the behavior of f blue in clusters.

show abstract

A journey from the outskirts to the cores of groups

Cited by 41 publications

References 97 publications

Dwarf Galaxy Discoveries from the KMTNet Supernova Program. I. The NGC 2784 Galaxy Group^*

Dwarf Galaxy Discoveries from the KMTNet Supernova Program. I. The NGC 2784 Galaxy Group^*

The VIMOS VLT Deep Survey

Galaxy mass, cluster-centric distance and secular evolution: their role in the evolution of galaxies in clusters in the last 10 Gyr

Contact Info

Product

Resources

About

A journey from the outskirts to the cores of groups

Cited by 41 publications

References 97 publications

Dwarf Galaxy Discoveries from the KMTNet Supernova Program. I. The NGC 2784 Galaxy Group*

Dwarf Galaxy Discoveries from the KMTNet Supernova Program. I. The NGC 2784 Galaxy Group*

The VIMOS VLT Deep Survey

Galaxy mass, cluster-centric distance and secular evolution: their role in the evolution of galaxies in clusters in the last 10 Gyr

Contact Info

Product

Resources

About

Dwarf Galaxy Discoveries from the KMTNet Supernova Program. I. The NGC 2784 Galaxy Group^*

Dwarf Galaxy Discoveries from the KMTNet Supernova Program. I. The NGC 2784 Galaxy Group^*