Are z>2 Herschel galaxies proto-spheroids?

TL;DR

This paper models the evolution of proto-spheroids and late-type galaxies across redshifts 0 to 3, showing that z>2 Herschel galaxies can be progenitors of local spheroids, with a focus on the redshift z_0.5 parameter.

Contribution

It introduces a combined phenomenological and physically motivated backward model to interpret galaxy luminosity functions across redshifts, emphasizing the role of proto-spheroids at z>2.

Findings

Proto-spheroids form predominantly between z=1.5 and z=3.

z_0.5~2 accurately reproduces observed source counts and redshift distributions.

Most z>2 Herschel galaxies are progenitors of local spheroids.

Abstract

We present a backward approach for the interpretation of the evolution of the near-infrared and the far-infrared luminosity functions across the redshift range 0<z<3. In our method, late-type galaxies are treated by means of a parametric phenomenological method based on PEP/HerMES data up to z~4, whereas spheroids are described by means of a physically motivated backward model. The spectral evolution of spheroids is modelled by means of a single-mass model, associated to a present-day elliptical with K-band luminosity comparable to the break of the local early-type luminosity function. The formation of proto-spheroids is assumed to occurr across the redshift range 1< z < 5. The key parameter is represented by the redshift z_0.5 at which half proto-spheroids are already formed. A statistical study indicates for this parameter values between z_0.5=1.5 and z_0.5=3. We assume as fiducial value z_0.5~2, and show that this assumption allows us to describe accourately the redshift distributions and the source counts. By assuming z_0.5 ~ 2 at the far-IR flux limit of the PEP-COSMOS survey, the PEP-selected sources observed at z>2 can be explained as progenitors of local spheroids caught during their formation. We also test the effects of mass downsizing by dividing the spheroids into three populations of different present-day stellar masses. The results obtained in this case confirm the validity of our approach, i.e. that the bulk of proto-spheroids can be modelled by means of a single model which describes the evolution of galaxies at the break of the present-day early type K-band LF.