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(Reference retrieved automatically from Web of Science through information on FAPESP grant and its corresponding number as mentioned in the publication by the authors.)

From blue cloud to red sequence: evidence of morphological transition prior to star formation quenching

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Author(s):
Sampaio, V. M. [1] ; de Carvalho, R. R. [1] ; Ferreras, I [2, 3, 4] ; Aragon-Salamanca, A. [5] ; Parker, L. C. [6]
Total Authors: 5
Affiliation:
[1] Univ Cidade Sao Paulo, NAT Univ Cruzeiro do Sul, BR-01506000 Sao Paulo, SP - Brazil
[2] Univ La Laguna, Dept Astrofis, E-38206 Tenerife - Spain
[3] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT - England
[4] Inst Astrofis Canarias, Calle Via Lactea S-N, E-38205 Tenerife - Spain
[5] Univ Nottingham, Sch Phys & Astron, Univ Pk, Nottingham NG7 2RD - England
[6] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1 - Canada
Total Affiliations: 6
Document type: Journal article
Source: Monthly Notices of the Royal Astronomical Society; v. 509, n. 1, p. 567-585, JAN 2022.
Web of Science Citations: 0
Abstract

We present a study of a sample of 254 clusters from the SDSS-DR7 Yang Catalogue and an auxiliary sample of field galaxies to perform a detailed investigation on how galaxy quenching depends on both environment and galaxy stellar mass. Our samples are restricted to 0.03 <= z <= 0.1 and we only consider clusters with log (M-halo/M-circle dot) >= 14. Comparing properties of field and cluster galaxies in the blue cloud, green valley, and red sequence, we find evidence that field galaxies in the red sequence hosted star formation events 2.1 +/- 0.7 Gyr ago, on average, more recently than galaxies in cluster environments. Dissecting the star formation rate versus stellar mass diagram we show how morphology rapidly changes after reaching the green valley region, while the star formation rate keeps decreasing. In addition, we use the relation between location in the projected phase space and infall time to explore the time delay between morphological and specific star formation rate variations. We estimate that the transition from late- to early-type morphology happens in Delta t(inf )similar to 1 Gyr, whereas the quenching of star formation takes similar to 3 Gyr. The time-scale we estimate for morphological transitions is similar to the expected for the delayed-then-rapid quenching model. Therefore, we suggest that the delay phase is characterized mostly by morphological transition, which then contributes morphological quenching as an additional ingredient in galaxy evolution. (AU)

FAPESP's process: 14/11156-4 - What drives the stellar mass growth of Early-Type galaxies? Born or made: the saga continues
Grantee:Reinaldo Ramos de Carvalho
Support Opportunities: Research Projects - Thematic Grants
FAPESP's process: 20/16243-3 - Investigating environmental effects in galaxy evolution: from cosmological simulations to observations
Grantee:Vitor Medeiros Sampaio
Support Opportunities: Scholarships in Brazil - Doctorate