The galaxy UV luminosity function at z ~ 2 - 4; new results on faint-end slope and the evolution of luminosity density

TL;DR

This study provides new measurements of the UV galaxy luminosity function at redshifts 2-4, revealing a flatter faint-end slope and detailed evolution of luminosity density, based on extensive multi-survey data and improved photometric redshift techniques.

Contribution

It offers the first robust, deep UV luminosity function measurements at z ~ 2-4 with a focus on faint galaxies, refining the faint-end slope and luminosity density evolution.

Findings

Faint-end slope at z~2-3 is shallower (~-1.32) than previous estimates.

Luminosity density peaks at z~2.5-3, indicating the epoch of maximum unobscured star formation.

Characteristic luminosity (M*) brightens by about 1 mag from z~2 to 4.

Abstract

We present a new, robust measurement of the evolving rest-frame UV galaxy luminosity function (LF) over the key redshift range z = 2 - 4. Our results are based on the high dynamic range provided by combining the HUDF, CANDELS/GOODS-South, and UltraVISTA/COSMOS surveys. We utilise the unparalleled multi-frequency photometry available in this survey `wedding cake' to compile complete galaxy samples at z ~ 2,3,4 via photometric redshifts (calibrated against the latest spectroscopy) rather than colour-colour selection, and to determine accurate rest-frame UV absolute magnitudes from SED fitting. Our new determinations of the UV LF extend from M_{1500} ~ -22 down to M_{1500} = -14.5, -15.5 and -16 at z ~ 2, 3 and 4 respectively (thus reaching ~ 3 - 4 magnitudes fainter than previous blank-field studies at z ~ 2 - 3). At z ~ 2 - 3 we find a much shallower faint-end slope (alpha = -1.32 +- 0.03) than the steeper values (alpha ~ -1.7) reported by Reddy & Steidel (2009) or by Alavi et al. (2014), and show that this new measurement is robust. By z ~ 4 the faint-end slope has steepened slightly, to alpha = -1.43 +- 0.04, and we show that these measurements are consistent with the overall evolutionary trend from z = 0 to z = 8. Finally, we find that while characteristic number density (phi*) drops from z ~ 2 to z ~ 4, characteristic luminosity (M*) brightens by ~ 1 mag over this redshift range. This, combined with the new flatter faint-end slopes, has the consequence that UV luminosity density (and hence unobscured star-formation density) peaks at z ~ 2.5 - 3, when the Universe was ~ 2.5 Gyr old.