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

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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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