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We constrain the rest-frame FUV (1546\AA), NUV (2345\AA) and U-band (3690\AA)luminosity functions (LFs) and luminosity densities (LDs) with unprecedentedprecision from $z\sim0.2$ to $z\sim3$ (FUV, NUV) and $z\sim2$ (U-band). Oursample of over 4.3 million galaxies, selected from the CFHT Large Area $U$-bandDeep Survey (CLAUDS) and HyperSuprime-Cam Subaru Strategic Program (HSC-SSP)data lets us probe the very faint regime (down to$M_\mathrm{FUV},M_\mathrm{NUV},M_\mathrm{U} \simeq -15$ at low redshift) whilesimultaneously detecting very rare galaxies at the bright end down to comovingdensities $<10^{-5}$ Mpc$^{-3}$. Our FUV and NUV LFs are well fitted by singleSchechter functions, with faint-end slopes that are very stable up to $z\sim2$.We confirm, but self-consistently and with much better precision than previousstudies, that the LDs at all three wavelengths increase rapidly with lookbacktime to $z\sim1$, and then much more slowly at $1<z<2$--$3$. Evolution of theFUV and NUV LFs and LDs at $z<1$ is driven almost entirely by the fading of thecharacteristic magnitude, $M^\star_{UV}$, while at $z>1$ it is due to theevolution of both $M^\star_{UV}$ and the characteristic number density$\phi^\star_{UV}$. In contrast, the U-band LF has an excess of faint galaxiesand is fitted with a double-Schechter form; $M^\star_\mathrm{U}$, both$\phi^\star_\mathrm{U}$ components, and the bright-end slope evolve throughout$0.2<z<2$, while the faint-end slope is constant over at least the measurable$0.05<z<0.6$. We present tables of our Schechter parameters and LD measurementsthat can be used for testing theoretical galaxy evolution models andforecasting future observations.

monthly notices of the royal astronomical society

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 $z \sim 3$