The Ha luminosity function and star formation rate up to z~1

dc.creatorTresse, L.
dc.creatorMaddox, S. J.
dc.creatorFevre, O. Le
dc.creatorCuby, J. -G.
dc.date2001-11-20
dc.date2002-08-21
dc.date.accessioned2026-07-07T11:28:50Z
dc.date.available2026-07-07T11:28:50Z
dc.descriptionWe describe ISAAC/ESO-VLT observations of the Ha(6563) Balmer line of 33 field galaxies from the Canada-France Redshift Survey (CFRS) with redshifts selected between 0.5 and 1.1. We detect Ha in emission in 30 galaxies and compare the properties of this sample with the low-redshift sample of CFRS galaxies at z~0.2 (Tresse & Maddox 1998). We find that the Ha luminosity, L(Ha), is tightly correlated to M(B(AB)) in the same way for both the low- and high-redshift samples. L(Ha) is also correlated to L([OII]3727), and again the relation appears to be similar at low and high redshifts. The ratio L([OII])/L(Ha) decreases for brighter galaxies by as much as a factor 2 on average. Derived from the Ha luminosity function, the comoving Ha luminosity density increases by a factor 12 from <z>=0.2 to <z>=1.3. Our results confirm a strong rise of the star formation rate (SFR) at z<1.3, proportional to (1+z)^{4.1+/-0.3} (with H_0=50 km/s/Mpc, q_0=0.5). We find an average SFR(2800 Ang)/SFR(Ha) ratio of 3.2 using the Kennicutt (1998) SFR transformations. This corresponds to the dust correction that is required to make the near UV data consistent with the reddening-corrected Ha data within the self-contained, I-selected CFRS sample.
dc.description16 pages, 16 figures and 3 tables included, figures and text updated, same results as in the 1st version, accepted in MNRAS
dc.identifierhttps://arxiv.org/abs/astro-ph/0111390
dc.identifierhttp://arxiv.org/abs/astro-ph/0111390
dc.identifierMon.Not.Roy.Astron.Soc.337:369,2002
dc.identifierdoi:10.1046/j.1365-8711.2002.05919.x
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/196526
dc.subjectAstrophysics
dc.titleThe Ha luminosity function and star formation rate up to z~1
dc.typetext

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