EDP Sciences
Free Access
Volume 422, Number 3, August II 2004
Page(s) 841 - 863
Section Cosmology (including clusters of galaxies)
DOI https://doi.org/10.1051/0004-6361:20047140
Published online 16 July 2004

A&A 422, 841-863 (2004)
DOI: 10.1051/0004-6361:20047140

The ESO-Sculptor Survey: Evolution of late-type galaxies at redshifts 0.1-0.5

V. de Lapparent1, S. Arnouts2, G. Galaz3 and S. Bardelli4

1  Institut d'Astrophysique de Paris, CNRS, Univ. Pierre et Marie Curie, 98 bis boulevard Arago, 75014 Paris, France
    e-mail: lapparen@iap.fr
2  Laboratoire d'Astrophysique de Marseille, BP8, Traverse du Siphon, 13376 Marseille Cedex 12, France
    e-mail: stephane.arnouts@oamp.fr
3  Depto. de Astronomía et Astrofísica, Pontificia Universidad Católica de Chile, Casilla 306, Santiago 22, Chile
    e-mail: ggalaz@astro.puc.cl
4  INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy
    e-mail: bardelli@excalibur.bo.astro.it

(Received 26 January 2004 / Accepted 1 April 2004)

Using the Gaussian+Schechter composite luminosity functions measured from the ESO-Sculptor Survey (de Lapparent et al. 2003, A&A, 404, 831) and assuming that these functions do not evolve with redshift out to $z\sim1$, we obtain evidence for evolution in the late spectral class containing late-type Spiral (Sc+Sd) and dwarf Irregular (dI) galaxies. There are indications that the Sc+Sd galaxies are the evolving population, but we cannot exclude that the dI galaxies also undergo some evolution. This evolution is detected as an increase of the Sc+Sd+dI galaxy density which can be modeled as either $n(z)\propto1+3(z-0.15)$ or $n(z)\propto(1+z)^2$ using the currently favored cosmological parameters $\Omega_{\rm m}=0.3$ and $\Omega_\Lambda=0.7$; the uncertainty in the linear and power-law evolution rates is of the order of unity. For $\Omega_{\rm m}=1.0$ and $\Omega_\Lambda=0.0$, the linear and power-law evolution rates are ~ $4\pm1$ and ~ $2.5\pm1$ respectively. Both models yield a good match to the ESS ${\it BVR}_{\rm c}$ redshift distributions to 21-22 $^{\rm mag}$ and to the number-counts to 23-23.5 $^{\rm mag}$, which probe the galaxy distribution to redshifts $z\sim0.5$ and $z\sim1.0$ respectively.

The present analysis shows the usefulness of the joint use of the magnitude and redshift distributions for studying galaxy evolution. It also illustrates how Gaussian+Schechter composite luminosity functions provide more robust constraints on the evolution rate than pure Schechter luminosity functions, thus emphasizing the importance of performing realistic parameterizations of the luminosity functions for studying galaxy evolution.

The detected density evolution indicates that mergers could play a significant role in the evolution of late-type Spiral and dwarf Irregular galaxies. However, the ESO-Sculptor density increase with redshift could also be caused by a ~1 $^{\rm mag}$ brightening of the Sc+Sd+dI galaxies at  $z\sim0.5$ and  $a \sim 1.5{-}2.0$ $^{\rm mag}$ brightening at  $z\sim1$, which is compatible with the expected passive brightening of Sc galaxies at these redshifts. Distinguishing between luminosity and density evolution is a major difficulty as these produce the same effect on the redshift and magnitude distributions. The detected evolution rate of the ESO-Sculptor Sc+Sd+dI galaxies is nevertheless within the range of measured values from the other existing analyses, whether they provide evidence for density or luminosity evolution.

Key words: galaxies: luminosity function, mass function -- galaxies: evolution -- galaxies: distances and redshifts -- galaxies: spiral -- galaxies: irregular -- galaxies: dwarf

© ESO 2004

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.