Speaker
Description
Conditional Luminosity Function (CLF) means the Luminosity Function (LF) of a similar dark halo mass. It is more meaningful from the perspective of the galaxy-halo connection. CLFs of halo mass $M_h > 10^{12} 𝑀_\odot$ at z~0 have been measured down to rather faint luminosity reliably. In this work, we combined the DESI SV3 spectroscopic group central galaxies and the HSC photometric galaxies, and measured CLFs of central and satellite galaxies, red and blue populations separately, for groups with halo mass $\sim 10^{12}𝑀_\odot$ to $\sim 10^{15}𝑀_\odot$ , from redshift z∼0 to z∼1, towards an unprecedentedly faint magnitude limit. We found that the red satellite CLFs show a significant faint-end upturn in all halo mass and redshift bins, with a hardly evolved faint-end slope, implying that the red dwarf satellites have already been in place by z ∼ 1. We also found the evolution of bright end of CLFs is consistent with the passive evolution. The fraction of red (old) satellites as a function of stellar mass minimizes at a characteristic mass scale, $𝑀_* \sim 10^9𝑀_\odot$, from z∼0 to z∼1, indicating a dichotomy of quenching mechanisms for the satellite population. Besides higher redshift, we also expanded the CLF measurements to the unprecedented scale of low-mass halos $\sim 10^{10}𝑀_\odot$ at z < 0.2, by using spectroscopic dwarf galaxies combined with HSC deep layer and CLAUDS survey. We found that the faint-end slopes of the satellite CLFs of both blue and red populations, and the fraction of red (old) satellites in low-mass halos show a similar performance as their higher-mass halo counterparts.
