The Contribution of Faint Blue Galaxies to the Sub-mm Counts and Background

Abstract

Observations in the submillimetre waveband have recently revealed a new population of luminous, sub-mm sources. These are proposed to lie at high redshift and to be optically faint due to their high intrinsic dust obscuration. The presence of dust has been previously invoked in optical galaxy count models which assume $τ=9$ Gyr Bruzual & Charlot evolution for spirals and these fit the count data well from U to K. We now show that by using either a 1/$λ$ or Calzetti absorption law for the dust and re-distributing the evolved spiral galaxy UV radiation into the far infra-red(FIR), these models can account for all of the `faint&#39;($\leq1$mJy) $850μ$m galaxy counts, but fail to fit &#39;bright&#39;($\ge2$mJy) sources, indicating that another explanation for the sub-mm counts may apply at brighter fluxes(e.g. QSOs, ULIRGs). We find that the main contribution to the faint, sub-mm number counts is in the redshift range $0.5 < z < 3$, peaking at $z\approx 1.8$. The above model, using either dust law, can also explain a significant proportion of the extra-galactic background at $850μ$m as well as producing a reasonable fit to the bright $60μm$ IRAS counts.