Star-formation rates of cluster galaxies: nature versus nurture

Laganá, T. F.; Ulmer, M. P.

doi:10.1093/mnras/stx3210

Cited by 18 publications

(24 citation statements)

References 66 publications

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“…As for the SFR, the SSFR at fixed stellar mass is independent of environment, for both star forming and quiescent galaxies (although again, the very massive quiescent galaxies seem to show some dependence). Our results agree well with former studies (e.g., Muzzin et al 2012;Laganá & Ulmer 2018). Muzzin et al (2012) studied the effects of stellar mass and envi- Muzzin et al (2013).…”

Section: Environmental Quenchingsupporting

confidence: 93%

“…Their conclusion is supported by other works, such as Wetzel et al (2012); Darvish et al (2016); Laganá & Ulmer (2018). Darvish et al (2016) used a sample of star forming and quiescent galaxies in the COSMOS field at z < 3, and studied the role of environment and stellar mass on galaxy properties, in particular the evolution of the SFR and SSFR with overdensity (as a proxy of the environment) as a function of redshift.…”

Section: Discussionsupporting

confidence: 61%

“…Our results are consistent with a scenario where the enviromental processes play a marginal effect in galaxy quenching, at any time, or they are very rapid in such a way that the net environmental quenching is not seen. This scenario is supported by a number of observational achievements (e.g., Peng et al 2010;Sobral et al 2011;Muzzin et al 2012;Koyama et al 2013;Laganá & Ulmer 2018).…”

Section: Discussionmentioning

confidence: 75%

“…This is in good agreement with our results, and in general with a picture where the environment does not influence the star formation activity of star forming galaxies, but it can increase the probability of a given galaxy to become quiescent. Indeed, it has been pointed out by many authors (Patel et al 2009;Peng et al 2010;Darvish et al 2016;Pintos-Castro et al 2019) that the fraction of quiescent galaxies strongly depends on the environment, but the SFR and SSFR of star forming galaxies are independent of environment (Muzzin et al 2012;Wetzel et al 2012;Koyama et al 2013;Darvish et al 2016;Laganá & Ulmer 2018;this work).…”

Section: Discussionmentioning

confidence: 92%

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The Roles of Mass and Environment in the Quenching of Galaxies

Contini

Kang

et al. 2019

ApJ

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We study the roles of stellar mass and environment in quenching the star formation activity of a large set of simulated galaxies by taking advantage of an analytic model coupled to the merger tree extracted from an N-body simulation. The analytic model has been set to match the evolution of the global stellar mass function since redshift z ∼ 2.3 and give reasonable predictions of the star formation history of galaxies at the same time. We find that stellar mass and environment play different roles: the star formation rate/specific star formation rate-M * relations are independent of the environment (defined as the halo mass) at any redshift probed, 0 < z < 1.5, for both star forming and quiescent galaxies, while the star formation rate-M halo relation strongly depends on stellar mass in the same redshift range, for both star forming and quiescent galaxies. Moreover, the star formation rate and the specific star formation rate are strongly dependent on stellar mass even when the distance from the cluster core is used as a proxy for the environment, rather than the halo mass. We then conclude that stellar mass is the main driver of galaxy quenching at any redshift probed in this study, not just at z > 1 as generally claimed, while the environment has a minimal role. All the physical processes linked to the environment must act on very short timescales, such that they do not influence the star formation of active galaxies, but increase the probability of a given galaxy to become quiescent.

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Section: Environmental Quenchingsupporting

confidence: 93%

Section: Discussionsupporting

confidence: 61%

Section: Discussionmentioning

confidence: 75%

Section: Discussionmentioning

confidence: 92%

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The Roles of Mass and Environment in the Quenching of Galaxies

Contini

Kang

et al. 2019

ApJ

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“…The galaxy cluster RXJ1347.5-1145 (hereafter RXJ1347) at z∼0.45 is one of the most massive and most X-ray luminous clusters known (Schindler et al 1995). In recent years, RXJ1347 has been the subject of intense research, through spectroscopic (Laganá & Ulmer 2018, Jørgensen et al 2017, Fogarty et al 2017), X-ray (Ghirardini et al 2017, Ueda et al 2018, lensing (Chiu et al 2018, and Sunyaev-Zel'dovich effect (Kitayama et al 2016, Adam et al 2018 analyses. However, most previous works were focused on the determination of the cluster internal substructures.…”

Section: Sample Selection and Observationsmentioning

confidence: 99%

Galaxy kinematics across different environments in the RXJ1347−1145 cluster complex

Pérez-Martínez

Ziegler

Böhm

et al. 2020

A&A

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Aims. In order to understand the role of the different processes that drive galaxy evolution in clusters, we need comprehensive studies that simultaneously examine several of the most important physical properties of galaxies. In this work we study the interplay between the kinematic state and star formation activity of galaxies in the RXJ1347-1145 cluster complex at z∼0.45. Methods. We used VLT/VIMOS to obtain slit spectra for 95 galaxies across the 40 x40 area where the RXJ1347-1145 cluster complex resides. We determined the cluster membership of our targets by identifying one or more of the available emission lines within the wavelength range. Our spectroscopy is complemented with archival SUBARU/Suprime-Cam deep photometric observations in five optical bands (B, V, Rc, Ic, z'). We examined the kinematic properties of our sample attending to the degree of distortion of the extracted rotation curves. Regular rotating galaxies were included in our Tully-Fisher analysis while the distorted ones were used to study the role of cluster-specific interactions with respect to star formation and AGN activity. Results. Our analysis confirmed the cluster membership for approximately half of our targets. We report a higher fraction of galaxies with irregular gas kinematics in the cluster environment than in the field. Cluster galaxies with regular rotation display a moderate brightening in the B-band Tully-Fisher relation compatible with the gradual evolution of the stellar populations with lookback time, and no significant evolution in the stellar-mass Tully-Fisher relation, in line with previous studies at similar redshift. Average specific star formation rate (sSFR) values are slightly lower in our cluster sample (-0.15 dex) with respect to the main sequence of starforming galaxies, confirming the role of the environment in the early quenching of star formation in clusters. Finally, we carried out an exploratory observational study on the stellar-to-halo mass relation finding that cluster galaxies tend to have slightly lower stellar mass values for a fixed halo mass compared to their field counterparts.

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Galaxy evolution studies in clusters: the case of Cl0024 + 1652 cluster galaxies at z ∼ 0.4

et al. 2019

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Studying the transformation of cluster galaxies contributes a lot to have a clear picture of evolution of the universe. Towards that we are studying different properties (morphology, star formation, AGN contribution and metallicity) of galaxies in clusters up to z ∼ 1.0 taking three different clusters: ZwCl0024 + 1652 at z ∼ 0.4, RXJ1257 + 4738 at z ∼ 0.9 and Virgo at z ∼ 0.0038. For ZwCl0024 + 1652 and RXJ1257 + 4738 clusters we used tunable filters data from GLACE survey taken with GTC 10.4 m telescope and other public data, while for Virgo we used public data. We did the morphological classification of 180 galaxies in ZwCl0024 + 1652 using galSVM, where 54 % and 46 % of galaxies were classified as early-type (ET) and late-type (LT) respectively. We did a comparison between the three clusters within the clustercentric distance of 1 Mpc and found that ET proportion (decreasing with redshift) dominates over the LT (increasing with redshift) throughout. We finalized the data reduction for ZwCl0024 + 1652 cluster and identified 46 [OIII] and 73 Hβ emission lines. For this cluster we have classified 22 emission line galaxies (ELGs) using BPT-NII diagnostic diagram resulting with 14 composite, 1 AGN and 7 star forming (SF) galaxies. We are using these results, together with the public data, for further analysis of the variations of properties in relation to redshift within z < 1.0.

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Star-formation rates of cluster galaxies: nature versus nurture

Cited by 18 publications

References 66 publications

The Roles of Mass and Environment in the Quenching of Galaxies

The Roles of Mass and Environment in the Quenching of Galaxies

Galaxy kinematics across different environments in the RXJ1347−1145 cluster complex

Galaxy evolution studies in clusters: the case of Cl0024 + 1652 cluster galaxies at z ∼ 0.4

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