# A Catalog of GALEX Ultraviolet Emission from Asymptotic Giant Branch Stars

## TL;DR

This study analyzes GALEX ultraviolet observations of AGB stars, revealing correlations with optical/infrared emission, variability in UV light, and suggesting UV emission originates from the stars themselves rather than binary companions.

## Contribution

It provides the first comprehensive catalog of UV emission from AGB stars and investigates the origins and variability of this emission using GALEX data.

## Key findings

- UV emission correlates with optical/infrared brightness.
- UV emission varies in phase with visible light in some stars.
- UV emission is anti-correlated with circumstellar envelope density.

## Abstract

We have performed a comprehensive study of the UV emission detected from AGB stars by the Galaxy Evolution Explorer (GALEX). Of the 468 AGB stars in our sample, 316 were observed by GALEX. In the NUV bandpass ($\lambda_{\rm eff} \sim 2310$z A), 179 AGB stars were detected and 137 were not detected. Only 38 AGB stars were detected in the FUV bandpass ($\lambda_{\rm eff} \sim1528$ A). We find that NUV emission is correlated with optical to near infrared emission leading to higher detection fractions among the brightest, hence closest, AGB stars. Comparing the AGB time-variable visible phased light curves to corresponding GALEX NUV phased light curves we find evidence that for some AGB stars the NUV emission varies in phase with the visible light curves. We also find evidence that the NUV emission, and possibly, the FUV emission are anti-correlated with the circumstellar envelope density. These results suggest that the origin of the GALEX-detected UV emission is an inherent characteristic of the AGB stars that can most likely be traced to a combination of photospheric and chromospheric emission. In most cases, UV detections of AGB stars are not likely to be indicative of the presence of binary companions.