Near-infrared luminosity function of galaxies in distant clusters
Near-infrared luminosity function of galaxies in distant clusters
Near-infrared luminosity function of galaxies in distant clusters
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The near-<strong><strong>in</strong>frared</strong> <strong>lum<strong>in</strong>osity</strong> <strong>function</strong><br />
as a tool to study galaxy evolution<br />
● well established at redshift zero, provid<strong>in</strong>g a zeropo<strong>in</strong>t<br />
for evolutionary studies at higher redshift<br />
● less affected by dust ext<strong>in</strong>ction (compared to bluer<br />
wavelengths)<br />
● small dependence <strong>of</strong> k-correction on galaxy type<br />
● provides a proxy to the stellar mass <strong>function</strong>, s<strong>in</strong>ce<br />
observed K-band light reasonably traces stellar mass<br />
even at redshift ~ 1<br />
● observed over a wide look-back time range sets<br />
constra<strong>in</strong>ts on when the bulk <strong>of</strong> the stars formed and<br />
when the bulk <strong>of</strong> the galaxy mass was assembled
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