UV SEDs of early-type cluster galaxies: A new look at the UV upturn

TL;DR

This study investigates the UV upturn phenomenon in early-type cluster galaxies using multi-wavelength photometry, revealing its prevalence across galaxy types and linking it to stellar populations and galaxy mass.

Contribution

It provides detailed UV SEDs for cluster galaxies, identifies UV upturns in fainter galaxies, and suggests a helium-rich horizontal branch star origin, expanding understanding of galaxy evolution.

Findings

UV upturn present in all galaxy types studied

UV upturn strength correlates with galaxy mass

Helium-rich stars likely cause the UV upturn

Abstract

Using GALEX, UVOT and optical photometry, we explore the prevalence and strength of the UV-upturn in the spectra of quiescent early type galaxies in several nearby clusters. Even for galaxies with completely passive optical colours, there is a large spread in vacuum UV colour consistent with almost all having some UV upturn component. Combining GALEX and UVOT data below 3000\AA, we generate for the first time comparatively detailed UV SEDs for Coma cluster galaxies. Fitting the UV upturn component with a blackbody, twenty six of these show a range of characteristic temperatures (10000--21000K) for the UV upturn population. Assuming a single temperature to explain GALEX-optical colours could underestimate the fraction of galaxies with UV upturns and mis-classify some as systems with residual star formation. The UV upturn phenomenon is not an exclusive feature found only in giant galaxies; we identify galaxies with similar (or even bluer) $FUV-V$ colours to the giants with upturns over a range of fainter luminosities. The temperature and strength of the UV upturn are correlated with galaxy mass. Under the plausible hypothesis that the sources of the UV upturn are blue horizontal branch stars, the most likely mechanism for this is the presence of a substantial (between 4\% and 20\%) Helium rich ($Y > 0.3$) population of stars in these galaxies, potentially formed at $z\sim 4$ and certainly at $z>2$; this plausibly sets a lower limit of $\sim {\rm 0.3 - 0.8} \times 10^{10}$ $M_{\odot}$ to the {\it in situ} stellar mass of $\sim L^*$ galaxies at this redshift.