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 $z \sim 3$

We constrain the rest-frame FUV (1546A), NUV (2345A) and U-band (3690A) 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 $ 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

Keywords:

• Characteristic number
• Physics
• Galaxy formation and evolution
• Astronomy
• Galaxy
• Astrophysics
• Luminosity
• Redshift

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