scholarly journals STAR FORMATION HISTORIES IN A CLUSTER ENVIRONMENT ATz∼ 0.84

2010 ◽  
Vol 725 (1) ◽  
pp. 1252-1276 ◽  
Author(s):  
R. Demarco ◽  
R. Gobat ◽  
P. Rosati ◽  
C. Lidman ◽  
A. Rettura ◽  
...  
Keyword(s):  
Star Formation ◽  
Cluster Environment ◽  
Star Formation Histories

scholarly journals The time delay between star formation quenching and morphological transformation of galaxies in clusters: a phase–space view of EDisCS

2019 ◽  
Vol 486 (1) ◽  
pp. 868-884 ◽  
Author(s):  
Kshitija Kelkar ◽  
Meghan E Gray ◽  
Alfonso Aragón-Salamanca ◽  
Gregory Rudnick ◽  
Yara L Jaffé ◽  
...  
Keyword(s):  
Star Formation ◽  
Phase Space ◽  
Structural Parameters ◽  
Imaging Data ◽  
Morphological Transformation ◽  
Star Forming ◽  
Cluster Environment ◽  
Cluster Cores ◽  
Two Parameters ◽  
Star Formation Histories

Abstract We explore the possible effect of cluster environments on the structure and star formation histories of galaxies by analysing the projected phase–space (PPS) of intermediate-redshift clusters (0.4 ≤ z ≤ 0.8). HST I−band imaging data from the ESO Distant Cluster Survey (EDisCS) allow us to measure deviations of the galaxies’ light distributions from symmetric and smooth profiles using two parameters, Ares (‘asymmetry’) and RFF (residual flux fraction or ‘roughness’). Combining these structural parameters with age-sensitive spectral indicators ($H_{\delta \rm {A}}$, $H_{\gamma \rm {A}}$, and Dn4000), we establish that in all environments younger star-forming galaxies of all morphologies are ‘rougher’ and more asymmetric than older, more quiescent ones. Combining a subset of the EDisCS clusters, we construct a stacked PPS diagram and find a significant correlation between the position of the galaxies on the PPS and their stellar ages, irrespective of their morphology. We also observe an increasing fraction of galaxies with older stellar populations towards the cluster core, while the galaxies’ structural parameters (Ares and RFF) do not seem to segregate strongly with PPS. These results may imply that, under the possible influence of their immediate cluster environment, galaxies have their star formation suppressed earlier, while their structural transformation happens on a longer time-scale as they accumulate and age in the cluster cores.

scholarly journals The Relation Between Galactic Properties and Cluster Structure

2005 ◽  
Vol 216 ◽  
pp. 239-248
Author(s):  
Bianca M. Poggianti ◽  
Terry J. Bridges ◽  
M. Yagi ◽  
N. Kashikawa ◽  
Y. Komiyama ◽  
...  
Keyword(s):  
Star Formation ◽  
Abrupt Change ◽  
Cluster Structure ◽  
Clusters Of Galaxies ◽  
Coma Cluster ◽  
Theoretical Progress ◽  
Star Formation Activity ◽  
Cluster Environment ◽  
History Of ◽  
Star Formation Histories

A satisfactory understanding of the origin of the dependence of galaxy properties on their environment has remained, so far, out of reach. In the light of numerous observational results and substantial theoretical progress obtained for clusters of galaxies in the last few years, a primary goal is to understand how the star formation activity depends on cluster substructure, i.e. on the merging/accretion history of a cluster. In this contribution we present a case in which it is possible to identify the cluster environment, and in particular the intracluster medium and the recent infall history of galaxies onto the cluster, as the cause for an abrupt change in the star formation histories of a subset of galaxies in the Coma cluster.

scholarly journals The effects of star formation history in the SFR–M* relation of H ii galaxies

2020 ◽  
Vol 500 (3) ◽  
pp. 3240-3253
Author(s):  
Amanda R Lopes ◽  
Eduardo Telles ◽  
Jorge Melnick
Keyword(s):  
Star Formation ◽  
Spectral Energy Distribution ◽  
Formation Rate ◽  
Star Formation History ◽  
Spectral Energy ◽  
Distribution Fitting ◽  
Good Tool ◽  
Star Forming ◽  
Additional Information ◽  
Star Formation Histories

ABSTRACT We discuss the implications of assuming different star formation histories (SFH) in the relation between star formation rate (SFR) and mass derived by the spectral energy distribution fitting (SED). Our analysis focuses on a sample of H ii galaxies, dwarf starburst galaxies spectroscopically selected through their strong narrow emission lines in SDSS DR13 at z < 0.4, cross-matched with photometric catalogues from GALEX, SDSS, UKIDSS, and WISE. We modelled and fitted the SEDs with the code CIGALE adopting different descriptions of SFH. By adding information from different independent studies, we find that H ii galaxies are best described by episodic SFHs including an old (10 Gyr), an intermediate age (100−1000 Myr) and a recent population with ages < 10 Myr. H ii galaxies agree with the SFR−M* relation from local star-forming galaxies, and only lie above such relation when the current SFR is adopted as opposed to the average over the entire SFH. The SFR−M* demonstrated not to be a good tool to provide additional information about the SFH of H ii galaxies, as different SFH present a similar behaviour with a spread of <0.1 dex.

scholarly journals Galaxy and mass assembly (GAMA): the inferred mass–metallicity relation from z = 0 to 3.5 via forensic SED fitting

2021 ◽  
Vol 503 (3) ◽  
pp. 3309-3325
Author(s):  
Sabine Bellstedt ◽  
Aaron S G Robotham ◽  
Simon P Driver ◽  
Jessica E Thorne ◽  
Luke J M Davies ◽  
...  
Keyword(s):  
Star Formation ◽  
Gas Phase ◽  
Large Range ◽  
Three Dimensional ◽  
Cosmic Time ◽  
Slowing Down ◽  
History Of ◽  
Mass Assembly ◽  
Star Formation Histories ◽  
Cosmic History

ABSTRACT We analyse the metallicity histories of ∼4500 galaxies from the GAMA survey at z < 0.06 modelled by the SED-fitting code ProSpect using an evolving metallicity implementation. These metallicity histories, in combination with the associated star formation histories, allow us to analyse the inferred gas-phase mass–metallicity relation. Furthermore, we extract the mass–metallicity relation at a sequence of epochs in cosmic history, to track the evolving mass–metallicity relation with time. Through comparison with observations of gas-phase metallicity over a large range of redshifts, we show that, remarkably, our forensic SED analysis has produced an evolving mass–metallicity relationship that is consistent with observations at all epochs. We additionally analyse the three-dimensional mass–metallicity–SFR space, showing that galaxies occupy a clearly defined plane. This plane is shown to be subtly evolving, displaying an increased tilt with time caused by general enrichment, and also the slowing down of star formation with cosmic time. This evolution is most apparent at lookback times greater than 7 Gyr. The trends in metallicity recovered in this work highlight that the evolving metallicity implementation used within the SED-fitting code ProSpect produces reasonable metallicity results over the history of a galaxy. This is expected to provide a significant improvement to the accuracy of the SED-fitting outputs.

scholarly journals The nature and origin of substructure in the outskirts of M31 – II. Detailed star formation histories★

2014 ◽  
Vol 446 (3) ◽  
pp. 2789-2801 ◽  
Author(s):  
Edouard J. Bernard ◽  
Annette M. N. Ferguson ◽  
Jenny C. Richardson ◽  
Mike J. Irwin ◽  
Michael K. Barker ◽  
...  
Keyword(s):  
Star Formation ◽  
Star Formation Histories

scholarly journals Constraints on the star formation histories of galaxies fromz∼ 1 to 0

2009 ◽  
Vol 393 (2) ◽  
pp. 406-418 ◽  
Author(s):  
Yan-Mei Chen ◽  
Vivienne Wild ◽  
Guinevere Kauffmann ◽  
Jérémy Blaizot ◽  
Marc Davis ◽  
...  
Keyword(s):  
Star Formation ◽  
Star Formation Histories

scholarly journals Star formation histories of resolved galaxies

2008 ◽  
Vol 4 (S258) ◽  
pp. 61-72
Author(s):  
Monica Tosi
Keyword(s):  
Star Formation ◽  
Observational Data ◽  
Stellar Populations ◽  
Morphological Type ◽  
The Other ◽  
Early Type ◽  
Significant Rate ◽  
Star Formation Histories

AbstractThe colour-magnitude diagrams of resolved stellar populations are the best tool to study the star formation histories of the host galactic regions. In this review the method to derive star formation histories by means of synthetic colour-magnitude diagrams is briefly outlined, and the results of its application to resolved galaxies of various morphological types are summarized. It is shown that all the galaxies studied so far were already forming stars at the lookback time reached by the observational data, independently of morphological type and metallicity. Early-type galaxies have formed stars predominantly, but in several cases not exclusively, at the earliest epochs. All the other galaxies appear to have experienced rather continuous star formation activities throughout their lifetimes, although with significant rate variations and, sometimes, short quiescent phases.

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