A multi-wavelength view of the star formation activity at z ∼ 3

G. E. Magdis, D. Elbaz, E. Daddi, G. E. Morrison, M. Dickinson, D. Rigopoulou, R. Gobat, H. S. Hwang

Producción científica: Contribución a una revistaArtículorevisión exhaustiva

63 Citas (Scopus)


We present a multi-wavelength, UV-to-radio analysis for a sample of massive (M * ∼ 1010 M ) IRAC- and MIPS 24 μm detected Lyman break galaxies (LBGs) with spectroscopic redshifts z 3 in the GOODS-North field. For LBGs without individual 24 μm detections, we employ stacking techniques at 24 μm, 1.1mm, and 1.4GHz to construct the average UV-to-radio spectral energy distribution and find it to be consistent with that of a luminous infrared galaxy with L IR = 4.5 +1.1 -2.3 × 1011 L and a specific star formation rate of 4.3 Gyr-1 that corresponds to a mass doubling time 230 Myr. On the other hand, when considering the 24 μm detected LBGs we find among them galaxies with L IR>10 12 L , indicating that the space density of z 3 UV-selected ultra-luminous infrared galaxies (ULIRGs) is (1.5 0.5) × 10-5 Mpc-3. We compare measurements of star formation rates from data at different wavelengths and find that there is tight correlation (Kendall's τ>99.7%) and excellent agreement between the values derived from dust-corrected UV, mid-IR, millimeter, and radio data for the whole range of L IR up to L IR 1013 L . This range is greater than that for which the correlation is known to hold at z ∼ 2, possibly due to the lack of significant contribution from polycyclic aromatic hydrocarbons to the 24 μm flux at z ∼ 3. The fact that this agreement is observed for galaxies with L IR> 1012 L suggests that star formation in UV-selected ULIRGs, as well as the bulk of star formation activity at this redshift, is not embedded in optically thick regions as seen in local ULIRGs and submillimeter-selected galaxies at z = 2.

Idioma originalInglés
Páginas (desde-hasta)1740-1745
Número de páginas6
PublicaciónAstrophysical Journal
EstadoPublicada - 2010
Publicado de forma externa


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