Extending pure luminosity evolution models into the mid-infrared, far-infrared and submillimetre

Details Extending pure luminosity evolution models into the mid-infrared, far-infrared and submillimetre Extending pure luminosity evolution models into the mid-infrared, far-infrared and submillimetre

Jul 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011mnras.414.1875h&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 414, Issue 3, pp. 1875-1886.

Astronomy and Astrophysics

Astronomy

3

Dust, Extinction, Galaxies: Evolution, Infrared: Galaxies, Submillimetre: Galaxies

Scientific paper

Simple pure luminosity evolution (PLE) models, in which galaxies brighten at high redshift due to increased star formation rates (SFRs), are known to provide a good fit to the colours and number counts of galaxies throughout the optical and near-infrared. We show that optically defined PLE models, where dust reradiates absorbed optical light into infrared spectra composed of local galaxy templates, fit galaxy counts and colours out to 8 μm and to at least z≈ 2.5. At 24-70 μm, the model is able to reproduce the observed source counts with reasonable success if 16 per cent of spiral galaxies show an excess in mid-IR flux due to a warmer dust component and a higher SFR, in line with observations of local starburst galaxies. There remains an underprediction of the number of faint-flux, high-z sources at 24 μm, so we explore how the evolution may be altered to correct this. At 160 μm and longer wavelengths, the model fails, with our model of normal galaxies accounting for only a few percent of sources in these bands. However, we show that a PLE model of obscured AGN, which we have previously shown to give a good fit to observations at 850 μm, also provides a reasonable fit to the Herschel/BLAST number counts and redshift distributions at 250-500 μm. In the context of a ΛCDM cosmology, an AGN contribution at 250-870 μm would remove the need to invoke a top-heavy IMF for high-redshift starburst galaxies.

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