Volume 420, Number 1, June II 2004
|Page(s)||125 - 133|
|Published online||14 May 2004|
High-z massive galaxies in the Hubble Deep Field South
INAF – Osservatorio Astronomico di Brera, via Brera 28, 20121 Milano, Italy e-mail: firstname.lastname@example.org
2 INAF – Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monte Porzio Catone, Italy e-mail: [giallo, fontana]@coma.mporzio.astro.it
3 Laboratoire d'Astronomie de Marseille, Traverse du Siphon, BP 8, 13376 Marseille, France e-mail: email@example.com
4 INAF – Osservatorio Astronomico di Trieste, via G. B. Tiepolo 11, 40131 Trieste, Italy e-mail: [cristiani, nonino]@ts.astro.it
5 European Southern Observatory, Karl-Schwarzschildstr. 2, 85748 Garching, Germany e-mail: [sdodoric, evanzell]@eso.org
6 Dipartimento di Astronomia dell'Università di Padova, Vicolo dell'Osservatorio 2, 35122 Padova, Italy
Corresponding author: P. Saracco, firstname.lastname@example.org
Accepted: 25 February 2004
A census of massive galaxies at redshift increasingly higher than may provide strong constraints for the history of mass assembly and star formation. Here we report the analysis of three galaxies selected in the Hubble Deep Field South at on the basis of their unusually red near-IR color . We have used population synthesis models to constrain their redshifts and their stellar masses. One galaxy (HDFS-1269) is at redshift while the other two (HDFS-822 and HDFS-850) are at . All three galaxies have already assembled a stellar mass of about 1011 at the observed redshift, placing the possible merging event of their formation at . The inferred mass weighted age of their stellar populations implies that the bulk of the stars formed at . The resulting co-moving density of galaxies at is Mpc-3, about a factor two higher than the predictions of hierarchical models. The comparison with the local density of galaxies implies that the three galaxies must have already formed most of their stellar mass and that they cannot follow an evolution significantly different from a passive aging. The comparison with the density of local early types (passively evolved galaxies) suggests that their co-moving density cannot decrease by more than a factor 2.5–3 from to suggesting that up to 40% of the stellar mass content of bright () local early type galaxies was already in place at .
Key words: galaxies: evolution / galaxies: elliptical and lenticular, cD / galaxies: formation
© ESO, 2004
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