Details

Autor(en) / Beteiligte

• Ly, Chun
• Malkan, Matt A
• Kashikawa, Nobunari
• Shimasaku, Kazuhiro
• Doi, Mamoru
• Nagao, Tohru
• Iye, Masanori
• Kodama, Tadayuki
• Morokuma, Tomoki
• Motohara, Kentaro

Titel

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

Ist Teil von

• The Astrophysical journal, 2007-03, Vol.657 (2), p.738-759

Ort / Verlag

Chicago, IL: IOP Publishing

Erscheinungsjahr

2007

Link zum Volltext

Quelle

Electronic Journals Library

Beschreibungen/Notizen

• SDF line-emitting galaxies in four narrowband filters at low and intermediate redshifts are presented. Broadband colors, follow-up optical spectroscopy, and multiple NB filters are used to distinguish Ha, [O II], and [O III] emitters at z = 0.07-1.47 to construct their LFs. These LFs are derived down to faint magnitudes, allowing for an accurate determination of the faint-end slope. With a large (N 6200-900) 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 agree reasonably well with those of Hippelein et al. The z = 0.08 H a LF, which reaches 2 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 a and h sub(*) show a strong redshift evolution, while L sub(*) shows little evolution. The evolution in a indicates that low-luminosity galaxies have a stronger evolution compared to brighter ones. Integrated SFR densities are derived via Ha, [O III], and [O II] for 0.07 < z < 1.47. A steep increase in the SFR density, as a function of redshift, is seen for 0.4 < z < 0.9. For z > 1, the SFR densities are similar. 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 others are a factor of 2 higher. For example, the z = 0.066-0.092 LF agrees with Jones & Bland-Hawthorn, but at z = 0.24 and 0.40, their number densities are twice as high. This discrepancy can be explained by cosmic variance.