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  4. The relation between star formation, morphology, and local density in high-redshift clusters and groups
 
research article

The relation between star formation, morphology, and local density in high-redshift clusters and groups

Poggianti, Bianca M.
•
Desai, Vandana
•
Finn, Rose
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2008
The Astrophysical Journal

We investigate how the [O II] properties and the morphologies of galaxies in clusters and groups at z = 0.4-0.8 depend on projected local galaxy density, and compare with the field at similar redshifts and clusters at low z. In both nearby and distant clusters, higher density regions contain proportionally fewer star-forming galaxies, and the average [O II] equivalent width of star-forming galaxies is independent of local density. However, in distant clusters the average current star formation rate (SFR) in star-forming galaxies seems to peak at densities similar to 15-40 galaxies Mpc(-2). At odds with low-z results, at high z the relation between star-forming fraction and local density varies from high- to low-mass clusters. Overall, our results suggest that at high z the current star formation ( SF) activity in star-forming galaxies does not depend strongly on global or local environment, though the possible SFR peak seems at odds with this conclusion. We find that the cluster SFR normalized by cluster mass anticorrelates with mass and correlates with the star-forming fraction. These trends can be understood given (1) that the average star-forming galaxy forms about 1M(circle dot) yr(-1) (uncorrected for dust) in all clusters; (2) that the total number of galaxies scales with cluster mass; and (3) the dependence of star-forming fraction on cluster mass. We present the morphology-density ( MD) relation for our z 0.4 - 0.8 clusters, and uncover that the decline of the spiral fraction with density is entirely driven by galaxies of type Sc or later. For galaxies of a given Hubble type, we see no evidence that SF properties depend on local environment. In contrast with recent findings at low z, in our distant clusters the SF-density relation and the MD relation are equivalent, suggesting that neither of the two is more fundamental than the other.

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Type
research article
DOI
10.1086/589936
Web of Science ID

WOS:000258889000013

Author(s)
Poggianti, Bianca M.
Desai, Vandana
Finn, Rose
Bamford, Steven
De Lucia, Gabriella
Varela, Jesus
Aragon-Salamanca, Alfonso
Halliday, Claire
Noll, Stefan
Saglia, Roberto
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Date Issued

2008

Published in
The Astrophysical Journal
Volume

684

Start page

888

End page

904

Subjects

galaxies : clusters : general

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galaxies : evolution

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galaxies : stellar content

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Digital Sky Survey

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Tully-Fisher Relation

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Color-Magnitude Relation

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Hubble-Space-Telescope

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Wide-Field Survey

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Stellar Mass

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Galaxy Clusters

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Environmental Dependence

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Formation Rates

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Red-Sequence

Editorial or Peer reviewed

REVIEWED

Written at

EPFL

EPFL units
LASTRO  
Available on Infoscience
November 30, 2010
Use this identifier to reference this record
https://infoscience.epfl.ch/handle/20.500.14299/61074
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