The evolution of the luminosity functions in the FORS deep field from low to high redshift II. The red bands

被引：0

作者：

Gabasch, A. ^{[1
,2
]}

Hopp, U. ^{[1
,2
]}

Feulner, G. ^{[1
,2
]}

Bender, R. ^{[1
,2
]}

Seitz, S. ^{[1
]}

Saglia, R.P. ^{[2
]}

Snigula, J. ^{[1
,2
]}

Drory, N. ^{[3
]}

Appenzeller, I. ^{[4
]}

Heidt, J. ^{[4
]}

Mehlert, D. ^{[4
]}

Noll, S. ^{[2
,4
]}

Böhm, A. ^{[5
]}

Jäger, K. ^{[5
]}

Ziegler, B. ^{[5
]}

机构：

[1] Universitäts-Sternwarte München, Scheinerstr. 1, 81679 München, Germany

[2] Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstraße, 85748 Garching, Germany

[3] McDonald Observatory, University of Texas at Austin, Austin, TX 78712, United States

[4] Landessternwarte Heidelberg, Königstuhl, 69117 Heidelberg, Germany

[5] Institut für Astrophysik, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany

来源：

Astronomy and Astrophysics | 2006年 / 448卷 / 01期

关键词：

We present the redshift evolution of the restframe galaxy luminosity function (LF) in the red r′; i′; and z′ bands; as derived from the FORS Deep Field (FDF); thus extending our earlier results to longer wavelengths. Using the deep and homogeneous I-band selected dataset of the FDF; we were able to follow the red LFs over the redshift range 0.5 spec + 1) &le 0.03 with only ∼ 1% outliers. A comparison with results from the literature shows the reliability of the derived LFs. Because of the depth of the FDF; we can give relatively tight constraints on the faint-end slope α of the LF; the faint-end of the red LFs does not show a large redshift evolution and is compatible within 1σ to 2σ with a constant slope over the redshift range 0.5 z 2.0. Moreover; the slopes in r′; and z′ are very similar to a best-fitting value of α = - 1.33 ± 0.03 for the combined bands. There is a clear trend of α to steepen with increasing wavelength: α UV&u′ = - 1.07 ± 0.04 &rarr α g′&B = - 1.25 ± 0.03 &rarr α r′&i′&z′ = - 1.33 ± 0.03. We subdivided our galaxy sample into four SED types and determined the contribution of a typical SED type to the overall LF. We show that the wavelength dependence of the LF slope can be explained by the relative contribution of different SED-type LFs to the overall LF; as different SED types dominate the LF in the blue and red bands. Furthermore we also derived and analyzed the luminosity density evolution of the different SED types up to z ∼ 2. We investigated the evolution of M* and Φ* by means of the redshift parametrization M*(z) = M0* + a ln (1 + z) and Φ*(z) = Φ0*(1 + z)b. Based on the FDF data; we found only a mild brightening of M* (ar′ ∼ -0.8; and ai′; z′ ∼ -0.4) and a decreasing Φ* (br′; z′ ∼ -0.6) with increasing redshift. Therefore; from (z) ∼ 0.5 to (z) ∼ 3 the characteristic luminosity increases by ∼0.8; ∼0.4; and ∼0.4 mag in the r′; respectively. Simultaneously the characteristic density decreases by about 40% in all analyzed wavebands. A comparison of the LFs with semianalytical galaxy formation models by Kauffmann et al. (1999) shows a similar result to the blue bands: the semi-analytical models predict LFs that describe the data at low redshift very well; but show growing disagreement with increasing redshifts. © ESO 2006;

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页码：101 / 121

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