Variation of the ultraviolet extinction law across the Taurus-Auriga star forming complex. A GALEX based study

TL;DR

This study uses GALEX and IR data to analyze how the ultraviolet extinction law varies across the Taurus-Auriga star-forming complex, revealing dust grain evolution and environmental effects.

Contribution

It introduces a novel UV-IR photometric technique to map the 2175 Å bump variations across the TMC, linking dust properties to star formation environments.

Findings

We identified regions with weaker 2175 Å bump indicating dust grain evolution.

Dust grains begin to decouple from magnetic fields in the cloud envelope.

The results support previous findings on dust evolution from Spitzer data.

Abstract

The Taurus-Auriga molecular complex (TMC) is the main laboratory for the study of low mass star formation. The density and properties of interstellar dust are expected to vary across the TMC. These variations trace important processes such as dust nucleation or the magnetic field coupling with the cloud. In this article, we show how the combination of near ultraviolet (NUV) and infrared (IR) photometry can be used to derive the strength of the 2175 \AA\ bump and thus any enhancement in the abundance of small dust grains and PAHs in the dust grains size distribution. This technique is applied to the envelope of the TMC, mapped by the GALEX All Sky Survey (AIS). UV and IR photometric data have been retrieved from the GALEX-AIS and the 2MASS catalogues. NUV and K-band star counts have been used to identify the areas in the cloud envelope where the 2175 \AA\ bump is weaker than in the diffuse ISM namely, the low column density extensions of L1495, L1498 and L1524 in Taurus, L1545, L1548, L1519, L1513 in Auriga and L1482-83 in the California region. This finding agrees with previous results on dust evolution derived from Spitzer data and suggests that dust grains begin to decouple from the environmental galactic magnetic field already in the envelope.