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Title:
The nature of the red disk-like galaxies at high redshift: dust attenuation vs. intrinsically red stellar populations
Authors:
Pierini, D.; Maraston, C.; Gordon, K. D.; Witt, A. N.
Affiliation:
AA(Max-Planck-Institut für extraterrestrische Physik, Giessenbachstr., Postfach 1312, 85741 Garching, Germany), AB(Max-Planck-Institut für extraterrestrische Physik, Giessenbachstr., Postfach 1312, 85741 Garching, Germany), AC(Steward Observatory, The University of Arizona, 933 N Cherry Ave., Tucson, AZ 85721), AD(Ritter Astrophysical Research Centre, The University of Toledo, 2801 W Bancroft, Toledo, OH 43606)
Publication:
THE SPECTRAL ENERGY DISTRIBUTIONS OF GAS-RICH GALAXIES: Confronting Models with Data; International Workshop. AIP Conference Proceedings, Volume 761, pp. 313-319 (2005). (AIPC Homepage)
Publication Date:
04/2005
Origin:
AIP
PACS Keywords:
Distances, redshifts, radial velocities; spatial distribution of galaxies, Interstellar dust grains; diffuse emission; infrared cirrus, Stellar content and populations; radii; morphology and overall structure
DOI:
10.1063/1.1913945
Bibliographic Code:
2005AIPC..761..313P

Abstract

We investigate the nature of the disk-like galaxies with ``red'' colours (i.e. Ic - K > 4 or J - K > 2.3), discovered at redshift 0.7 < z < 3.2, by combining models of radiative transfer of the stellar and scattered radiation through different dusty interstellar media with stellar population evolutionary synthesis models. Reproducing the observed optical/near-infrared colours suggests that high-z, red disk-like galaxies have declining star-formation rates with e-folding times as short as ~ 3 Gyr. Being ``red'' does not necessarily imply having luminosity-weighted old (i.e. > 1 Gyr) ages and/or being very dusty, since the contribution to the bolometric luminosity of the intermediate-age (i.e. between 0.2 and 1-2 Gyr) stellar populations is relevant. In particular, this is due to the thermally pulsating Asymptotic-Giant-Branch stars, with intrinsically red rest-frame V - K colours. The winds of these intermediate-age stars are expected to contribute substantially to the enrichment of the interstellar medium of their host disk-like galaxy with carbonaceous dust (e.g. the Policyclic Aromatic Hydrocarbons). Finally, our models of dusty, star-forming disks barely show Rc - K > 5.3, and only for an extremely limited region of the explored parameter space, whatever their redshift. Hence, Rc - K-selected galaxies at 0.7 < z < 3.2 most probably are either systems with a bulge (and, thus, potential hosts of an active galactic nucleus), maybe old and passively evolving, or starbursts/mergers.
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