Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Quick Search
My eDoc
Session History
Support Wiki
Direct access to
document ID:

          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 276753.0, MPI für Astronomie / Publikationen_mpia
The fundamental plane of cluster elliptical galaxies at z=1.25
Authors:Holden, B. P.; van der Wel, A.; Franx, M.; Illingworth, G. D.; Blakeslee, J. P.; van Dokkum, P.; Ford, H.; Magee, D.; Postman, M.; Rix, H.-W.; Rosati, P.
Date of Publication (YYYY-MM-DD):2005
Title of Journal:The Astrophysical Journal
Journal Abbrev.:The Astrophysical Journal
Start Page:L83
End Page:L86
Review Status:not specified
Audience:Experts Only
Abstract / Description:Using deep Hubble Space Telescope Advanced Camera for Surveys imaging and Very Large Telescope FOcal Reducer/low dispersion Spectrograph 2 spectra, we determined the velocity dispersions, effective radii, and surface brightnesses for four early-type galaxies in the z=1.237 cluster RDCS 1252.9-2927. All four galaxies are massive, greater than 1011 Msolar. These four galaxies, combined with three from RDCS 0848+4453 at z=1.276, establish the fundamental plane of massive early-type cluster galaxies at z=1.25. The offset of the fundamental plane shows that the luminosity evolution in rest-frame B is Deltaln(M/LB)=(-0.98+/-0.06)z for galaxies with M>1011.5 Msolar. To reproduce the observed mass-to- light ratio (M/L) evolution, we determine the characteristic age of the stars in these M>1011.5 Msolar galaxies to be 3.0+0.3-0.3 Gyr; i.e., z*=3.4+0.5-0.4. Including selection effects caused by morphological bias (the ``progenitor bias''), we estimate an age of 2.1+0.2-0.2 Gyr, or z*=2.3+0.2-0.2 for the elliptical galaxy population. Massive cluster early-type galaxies appear to have a large fraction of stars that formed early in the history of the universe. However, there is a large scatter in the derived M/L values, which is confirmed by the spread in the galaxies' colors. Two lower mass galaxies in our z=1.25 sample have much lower M/L values, implying significant star formation close to the epoch of observation. Thus, even in the centers of massive clusters, there appears to have been significant star formation in some massive, M~=1011 Msolar, galaxies at z~=1.5.
Free Keywords:Galaxies: Clusters: General; Galaxies: Clusters: Individual: Alphanumeric: RDCS 1252.9-2927; Galaxies: Elliptical and Lenticular; cD; Galaxies: Evolution; Galaxies: Fundamental Parameters; Galaxies: Photometry
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:URL:http://adsabs.harvard.edu/cgi-bin/nph- bib_query?b... [ID No:1]
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.