The Luminosity Function and Star Formation Rate between Redshifts of 0.07 and 1.47 for Narrow-band Emitters in the Subaru Deep Field

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dc.creatorLy, Chun
dc.creatorMalkan, Matt A.
dc.creatorKashikawa, Nobunari
dc.creatorShimasaku, Kazuhiro
dc.creatorDoi, Mamoru
dc.creatorNagao, Tohru
dc.creatorIye, Masanori
dc.creatorKodama, Tadayuki
dc.creatorMorokuma, Tomoki
dc.creatorMotohara, Kentaro
dc.date2006-10-27
dc.date.accessioned2026-07-07T10:24:02Z
dc.date.available2026-07-07T10:24:02Z
dc.descriptionAbridged: Subaru Deep Field line-emitting galaxies in four narrow-band filters at low and intermediate redshifts are presented. Broad-band colors, follow-up optical spectroscopy, and multiple NB filters are used to distinguish Ha, [O II], and [O III] emitters between redshifts of 0.07 and 1.47 to construct their luminosity functions (LFs). These LFs are derived down to faint magnitudes, which allows for a more accurate determination of the faint end slope. With a large (N~200-900) sample for each redshift interval, a Schechter profile is fitted to each LF. Prior to dust extinction corrections, the [O III] and [O II] LFs reported in this paper agree reasonably well with those of Hippelein et al. The z=0.08 Ha LF, which reaches two orders of magnitude fainter than Gallego et al., is steeper by 25%. This indicates that there are more low luminosity star-forming galaxies for z<0.1. The faint end slope αand ϕ_{\star} show a strong evolution with redshift while L_{\star} show little evolution. The evolution in αindicates that low-luminosity galaxies have a stronger evolution compared to brighter ones. Integrated star formation rate densities are derived via Ha, [O III], and [O II] for 0.07<z<1.47. A steep increase in the star-formation rate density, as a function of redshift, is seen for 0.4<z<0.9. For z>1, the star-formation rate densities are more or less constant. The latter is consistent with previous UV and [O II] measurements. Below z<0.4, the SFR densities are consistent with several Ha, [O II], and UV measurements, but other measurements are a factor of two higher. For example, the z=0.066-0.092 Ha LF agrees with those of Jones & Bland-Hawthorn, but at z=0.24 and 0.40, their number density is higher by a factor of two. This discrepancy can be explained by cosmic variance.
dc.description26 pages, 15 figures, 36 figure files (25 color; 11 B/W), emulateapj, accepted for publication in ApJ
dc.identifierhttps://arxiv.org/abs/astro-ph/0610846
dc.identifierhttp://arxiv.org/abs/astro-ph/0610846
dc.identifierAstrophys.J.657:738-759,2007
dc.identifierdoi:10.1086/510828
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/176047
dc.subjectAstrophysics
dc.titleThe Luminosity Function and Star Formation Rate between Redshifts of 0.07 and 1.47 for Narrow-band Emitters in the Subaru Deep Field
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