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Disc colours in field and cluster spiral galaxies at 0.5 ≲ z ≲ 0.8

Cantale, Nicolas and Jablonka, Pascale and Courbin, Frédéric and Rudnick, Gregory and Zaritsky, Dennis and Meylan, Georges and Desai, Vandana and De Lucia, Gabriella and Aragón-Salamanca, Alfonso and Poggianti, Bianca M. and Finn, Rose and Simard, Luc (2016) Disc colours in field and cluster spiral galaxies at 0.5 ≲ z ≲ 0.8. Astronomy and Astrophysics, 589 . Art. No. A82. ISSN 0004-6361. https://resolver.caltech.edu/CaltechAUTHORS:20160620-144453871

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Abstract

We present a detailed study of the colours of late-type galaxy discs for ten of the EDisCS galaxy clusters with 0.5 ≲ z ≲ 0.8. Our cluster sample contains 172 spiral galaxies, and our control sample is composed of 96 field disc galaxies. We deconvolved their ground-based V and I images obtained with FORS2 at the VLT with initial spatial resolutions between 0.4 and 0.8 arcsec to achieve a final resolution of 0.1 arcsec with 0.05 arcsec pixels, which is close to the resolution of the ACS at the HST. After removing the central region of each galaxy to avoid pollution by the bulges, we measured the V−I colours of the discs. We find that 50% of cluster spiral galaxies have disc V−I colours redder by more than 1σ of the mean colours of their field counterparts. This is well above the 16% expected for a normal distribution centred on the field disc properties. The prominence of galaxies with red discs depends neither on the mass of their parent cluster nor on the distance of the galaxies to the cluster cores. Passive spiral galaxies constitute 20% of our sample. These systems are not abnormally dusty. They are are made of old stars and are located on the cluster red sequences. Another 24% of our sample is composed of galaxies that are still active and star forming, but less so than galaxies with similar morphologies in the field. These galaxies are naturally located in the blue sequence of their parent cluster colour–magnitude diagrams. The reddest of the discs in clusters must have stopped forming stars more than ~5 Gyr ago. Some of them are found among infalling galaxies, suggesting preprocessing. Our results confirm that galaxies are able to continue forming stars for some significant period of time after being accreted into clusters, and suggest that star formation can decline on seemingly long (1 to 5 Gyr) timescales.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1051/0004-6361/201525801DOIArticle
http://www.aanda.org/articles/aa/abs/2016/05/aa25801-15/aa25801-15.htmlPublisherArticle
http://arxiv.org/abs/1601.05192arXivDiscussion Paper
ORCID:
AuthorORCID
Rudnick, Gregory0000-0001-5851-1856
Zaritsky, Dennis0000-0002-5177-727X
Desai, Vandana0000-0002-1340-0543
Aragón-Salamanca, Alfonso0000-0001-8215-1256
Poggianti, Bianca M.0000-0001-8751-8360
Finn, Rose0000-0001-8518-4862
Additional Information:© 2016 ESO. Article published by EDP Sciences. Received 4 February 2015; Accepted 5 January 2016; Published online 18 April 2016. This work was supported by the Swiss National Science Foundation (SNSF). We warmly thank Yara Jaffe for timely and informative discussions.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
Swiss National Science Foundation (SNSF)UNSPECIFIED
Subject Keywords:methods: data analysis / galaxies: clusters: general / galaxies: evolution
Record Number:CaltechAUTHORS:20160620-144453871
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20160620-144453871
Official Citation:Disc colours in field and cluster spiral galaxies at 0.5 ≲z ≲ 0.8 Nicolas Cantale, Pascale Jablonka, Frédéric Courbin, Gregory Rudnick, Dennis Zaritsky, Georges Meylan, Vandana Desai, Gabriella De Lucia, Alfonso Aragón-Salamanca, Bianca M. Poggianti, Rose Finn and Luc Simard A&A, 589 (2016) A82 DOI: http://dx.doi.org/10.1051/0004-6361/201525801
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:68541
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:21 Jun 2016 23:35
Last Modified:28 Oct 2019 18:35

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