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We use ZENS data at low redshift to study the dependence of the quenchedsatellite fraction and of the morphological mix of these quenched satellites,on three different environmental parameters: group halo mass, halo-centricdistance and large-scale structure over-density. The fraction of quenchedsatellites is independent of halo mass and the surrounding large-scaleoverdensity, but increases towards the centres of the haloes, as previouslyfound. The morphological mix is, however, constant with radial position,indicating that the well-known morphology-density relation results from theincreasing fraction of quenched galaxies towards the centres of haloes. Theconstancy of the morphological outcome suggests that mass-quenching andsatellite quenching have the same effect on the morphologies of the galaxies.The quenched satellites have larger B/T and smaller half-light radii than thestar-forming satellites. These are mostly due to differences in the disks. Thebulges in quenched satellites have very similar luminosities and surfacebrightness profiles, and any mass growth of the bulges associated withquenching cannot greatly change these quantities. The quenched disks arefainter and have smaller scale lengths than in star-forming satellites. Thiscan be explained either by a differential fading of the disks or if disks weregenerally smaller in the past, both of which are expected in an inside-outgrowth of disks. At least at low redshifts, the structure of massive quenchedsatellites is produced by processes that operate before quenching takes place.A comparison with semi-analytic models argues for a reduction in the efficiencyof group halos in quenching their disk satellites and for mechanisms toincrease the B/T of low mass quenched satellites. [abridged]

astrophysical journal/the astrophysical journal

ZENS IV. Similar Morphological Changes associated with Mass- and  Environment-Quenching, and the Relative importance of Bulge Growth versus the  Fading of Disks