The VIMOS-VLT Deep Survey. Galaxy luminosity function per morphological type up to z = 1.2

Details The VIMOS-VLT Deep Survey. Galaxy luminosity function per morphological type up to z = 1.2 The VIMOS-VLT Deep Survey. Galaxy luminosity function per morphological type up to z = 1.2

Jul 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006a%26a...453..809i&link_type=abstract

Astronomy and Astrophysics, Volume 453, Issue 3, July III 2006, pp.809-815

Astronomy and Astrophysics

Astrophysics

54

Surveys, Galaxy: Evolution, Galaxies: Luminosity Function, Mass Function, Galaxies: Fundamental Parameters

Scientific paper

Aims.We have computed the evolution of the rest-frame B-band luminosity function (LF) for bulge and disk-dominated galaxies since z=1.2. Methods: .We use a sample of 605 spectroscopic redshifts with IAB≤ 24 in the Chandra Deep Field South from the VIMOS-VLT Deep Survey, 3555 galaxies with photometric redshifts from the COMBO-17 multi-color data, coupled with multi-color HST/ACS images from the Great Observatories Origin Deep Survey. We split the sample in bulge- and disk-dominated populations on the basis of asymmetry and concentration parameters measured in the rest-frame B-band. Results: .We find that at z=0.4-0.8, the LF slope is significantly steeper for the disk-dominated population (α=-1.19 ± 0.07) compared to the bulge-dominated population (α=-0.53 ± 0.13). The LF of the bulge-dominated population is composed of two distinct populations separated in rest-frame color: 68% of red (B-I)AB>0.9 and bright galaxies showing a strongly decreasing LF slope α=+0.55 ± 0.21, and 32% of blue (B-I)AB<0.9 and more compact galaxies which populate the LF faint-end. We observe that red bulge-dominated galaxies are already well in place at z≃1, but the volume density of this population is increasing by a factor 2.7 between z˜ 1 and z˜ 0.6. It may be related to the building-up of massive elliptical galaxies in the hierarchical scenario. In addition, we observe that the blue bulge-dominated population is dimming by 0.7 mag between z˜ 1 and z˜ 0.6. Galaxies in this faint and more compact population could possibly be the progenitors of the local dwarf spheroidal galaxies.

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