In the last couple of years a population of very massive (M(*) > 10(11) M(circle dot)), high-redshift (z >= 2) galaxies has been identified, but its role in galaxy evolution has not yet been fully understood. Aims. It is necessary to perform a systematic study of high- redshift massive galaxies, in order to determine the shape of the very massive tail of the stellar mass function and determine the epoch of their assembly. Methods. We selected high- z massive galaxies at 5.8 mu m, in the SWIRE ELAIS-S1 field (1 deg(2)). Galaxies with the 1.6 mu m stellar peak redshifted into the IRAC bands (z similar or equal to 1-3, called "IR-peakers") were identified. Stellar masses were derived by means of spectrophotometric fitting and used to compute the stellar mass function (MF) at z = 1-2 and 2-3. A parametric fit to the MF was performed, based on a Bayesian formalism, and the stellar mass density of massive galaxies above z = 2 determined. Results. We present the first systematic study of the very-massive tail of the galaxy stellar mass function at high redshift. A total of 326 sources were selected. The majority of these galaxies have stellar masses in excess of 10(11) M(circle dot) and lie at z > 1.5. The availability of mid-IR data turned out to be a valuable tool to constrain the contribution of young stars to galaxy SEDs, and thus their M(*)/L ratio. The influence of near-IR data and of the chosen stellar library on the SED fitting are also discussed. The z = 2-3 stellar mass function between 10(11) and similar to 10(12) M(circle dot) is probed with unprecedented detail. A significant evolution is found not only for galaxies with M similar to 10(11) M(circle dot), but also in the highest mass bins considered. The comoving number density of these galaxies was lower by more than a factor of 10 at z = 2-3, with respect to the local estimate. SWIRE 5.8 mu m peakers more massive than 1.6 x 10(11) M(circle dot) provide 30-50% of the total stellar mass density in galaxies at z = 2-3.
Berta, S., Lonsdale, C.j., Polletta, M., Savage, R.s., Franceschini, A., Buttery, H., et al. (2007). The contribution of very massive high-redshift SWIRE galaxies to the stellar mass function RID C-5880-2009. ASTRONOMY & ASTROPHYSICS, 476(1), 151-175 [10.1051/0004-6361:20077491].
The contribution of very massive high-redshift SWIRE galaxies to the stellar mass function RID C-5880-2009
LA FRANCA, Fabio;
2007-01-01
Abstract
In the last couple of years a population of very massive (M(*) > 10(11) M(circle dot)), high-redshift (z >= 2) galaxies has been identified, but its role in galaxy evolution has not yet been fully understood. Aims. It is necessary to perform a systematic study of high- redshift massive galaxies, in order to determine the shape of the very massive tail of the stellar mass function and determine the epoch of their assembly. Methods. We selected high- z massive galaxies at 5.8 mu m, in the SWIRE ELAIS-S1 field (1 deg(2)). Galaxies with the 1.6 mu m stellar peak redshifted into the IRAC bands (z similar or equal to 1-3, called "IR-peakers") were identified. Stellar masses were derived by means of spectrophotometric fitting and used to compute the stellar mass function (MF) at z = 1-2 and 2-3. A parametric fit to the MF was performed, based on a Bayesian formalism, and the stellar mass density of massive galaxies above z = 2 determined. Results. We present the first systematic study of the very-massive tail of the galaxy stellar mass function at high redshift. A total of 326 sources were selected. The majority of these galaxies have stellar masses in excess of 10(11) M(circle dot) and lie at z > 1.5. The availability of mid-IR data turned out to be a valuable tool to constrain the contribution of young stars to galaxy SEDs, and thus their M(*)/L ratio. The influence of near-IR data and of the chosen stellar library on the SED fitting are also discussed. The z = 2-3 stellar mass function between 10(11) and similar to 10(12) M(circle dot) is probed with unprecedented detail. A significant evolution is found not only for galaxies with M similar to 10(11) M(circle dot), but also in the highest mass bins considered. The comoving number density of these galaxies was lower by more than a factor of 10 at z = 2-3, with respect to the local estimate. SWIRE 5.8 mu m peakers more massive than 1.6 x 10(11) M(circle dot) provide 30-50% of the total stellar mass density in galaxies at z = 2-3.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
