The trace of a substantial assembly of massive E-S0 galaxies at 0.8<z<1.5 in galaxy number counts

TL;DR

This study reveals that the slope change in K-band galaxy number counts at 17.5 mag is due to a shift from quiescent E-S0 galaxies to star-forming discs, indicating significant assembly of massive E-S0s at 0.8<z<1.5.

Contribution

It demonstrates that the slope change is linked to the late assembly of massive E-S0 galaxies, supporting models with galaxy formation occurring mainly at z<1.5.

Findings

The slope change is caused by a population shift from E-S0 to star-forming discs.

Models with passive evolution since z>2 cannot predict the slope change.

Major mergers are necessary to explain the assembly of massive E-S0 galaxies at 0.8<z<1.5.

Abstract

K-band galaxy number counts (GNCs) exhibit a slope change at K~17.5 mag not present in optical bands. To unveil the nature of this feature, we have derived the contribution of different galaxy types to the total K-band GNCs at 0.3<z<1.5 by redshift bins and compared the results with expectations from several galaxy evolutionary models. We show that the slope change is caused by a sudden swap of the galaxy population that numerically dominates the total GNCs (from quiescent E-S0's at K<17.5 mag to blue star-forming discs at fainter magnitudes), and that it is associated with a flattening of the contribution of the E-S0's at 0.6<z<1 to the total GNCs. We confirm previous studies showing that models in which the bulk of massive E-S0's have evolved passively since z>2 cannot predict the slope change, whereas those imposing a relatively late assembly on them (z<1.5) can reproduce it. The K-band GNCs by redshift bins and morphological types point to a progressively definitive build-up of ~50% of this galaxy population at 0.8<z<1.5, which can be explained only through the major mergers reported by observations. We conclude that the slope change in total K-band GNCs is a vestige of the definitive assembly of a substantial fraction of present-day massive E-S0's at 0.8<z<1.5.