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UV & U-band luminosity functions from CLAUDS and HSC-SSP -- I. Using four million galaxies to simultaneously constrain the very faint and bright regimes to $z sim 3$ | | Thibaud Moutard
; Marcin Sawicki
; Stéphane Arnouts
; Anneya Golob
; Jean Coupon
; Olivier Ilbert
; Xiaohu Yang
; Stephen Gwyn
; | | Date: |
19 Jan 2020 | | Abstract: | We constrain the rest-frame FUV (1546AA), NUV (2345AA) and U-band (3690AA)
luminosity functions (LFs) and luminosity densities (LDs) with unprecedented
precision from $z sim 0.2$ up to $z sim 3$ (FUV, NUV) and $z sim 2$ (U
band). Our sample of more than 4.3 million galaxies, selected from the CFHT
Large Area $U$-band Deep Survey (CLAUDS) and HyperSuprime-Cam Subaru Strategic
Program (HSC-SSP) data lets us probe the very faint regime (down to
$M_mathrm{FUV}$, $M_mathrm{NUV}$, $M_mathrm{U} simeq -15$) while
simultaneously detecting very rare galaxies at the bright end down to comoving
densities $<10^{-5}$ Mpc$^{-3}$. Our FUV and NUV LFs are well fitted by a
single Schechter function, with faint-end slopes that are very stable up to
$zsim 2$. We confirm, but self-consistently and with much better precision
than previous findings that the LDs at all three wavelengths increase rapidly
with lookback time to $zsim1$, and then much more slowly at $1<z<2$-$3$.
Evolution of the FUV and NUV LFs and LDs at $z<1$ is driven almost entirely by
the fading of the characteristic magnitude, $M^star_{UV}$, while at $z>1$ it
is due to the evolution of both $M^star_{UV}$ and the characteristic number
density $phi^star_{UV}$. In contrast, the U-band LF has an excess of faint
galaxies and is fitted with a double-Schechter form; $M^star_mathrm{U}$ and
both $phi^star_mathrm{U}$ components, as well as the bright-end slope evolve
throughout $0.2<z<2$, while the faint-end slope appears to be constant over
$0.05 < z < 0.6$ (where the double-Schechter profile of the U-band LF is
undeniable), at least. We present tables of our Schechter parameters and LD
measurements that can be used for testing theoretical galaxy evolution models
and forecasting future observations. | | Source: | arXiv, 2001.6904 | | Services: | Forum | Review | PDF | Favorites | |
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