Aims.We study the luminosity function of the high-redshift galaxy population with redshifts 3≤ z ≤ 4 using a purely I-band magnitude-selected spectroscopic sample obtained in the framework of the VIMOS VLT Deep Survey (VVDS). Methods: We determine the luminosity function from the VVDS taking care to add as few assumptions and as simple corrections as possible and compare our results with those obtained from photometric studies based on Lyman-break selections or photometric-redshift measurements. Results: We find that in the redshift range 3≤ z ≤ 4 the VVDS luminosity function is parameterized by φ^*=1.24+0.48-0.50×10-3 mag-1 Mpc-3 and M^*=-21.49+0.19-0.19 assuming a slope α=-1.4 consistent with most previous studies. While φ* is comparable to previously found values M* is significantly brighter by about 0.5 mag at least. Using the conservative slope α=-1.4 we find a luminosity density at 1700 Å L1700(M
Paltani S., Le Fèvre O., Ilbert O., Arnouts S., Bardelli S., Tresse L., et al. (2007). The VIMOS VLT deep survey. The ultraviolet galaxy luminosity function and luminosity density at 3 ≤ z ≤ 4. ASTRONOMY & ASTROPHYSICS, 463, 873-882 [10.1051/0004-6361:20066213].
The VIMOS VLT deep survey. The ultraviolet galaxy luminosity function and luminosity density at 3 ≤ z ≤ 4
MARANO, BRUNO;BONGIORNO, ANGELA;CUCCIATI, OLGA;
2007
Abstract
Aims.We study the luminosity function of the high-redshift galaxy population with redshifts 3≤ z ≤ 4 using a purely I-band magnitude-selected spectroscopic sample obtained in the framework of the VIMOS VLT Deep Survey (VVDS). Methods: We determine the luminosity function from the VVDS taking care to add as few assumptions and as simple corrections as possible and compare our results with those obtained from photometric studies based on Lyman-break selections or photometric-redshift measurements. Results: We find that in the redshift range 3≤ z ≤ 4 the VVDS luminosity function is parameterized by φ^*=1.24+0.48-0.50×10-3 mag-1 Mpc-3 and M^*=-21.49+0.19-0.19 assuming a slope α=-1.4 consistent with most previous studies. While φ* is comparable to previously found values M* is significantly brighter by about 0.5 mag at least. Using the conservative slope α=-1.4 we find a luminosity density at 1700 Å L1700(MI documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
