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The Taurus-Auriga molecular complex (TMC) is the main laboratory for thestudy of low mass star formation. The density and properties of interstellardust are expected to vary across the TMC. These variations trace importantprocesses such as dust nucleation or the magnetic field coupling with thecloud. 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 andPAHs in the dust grains size distribution. This technique is applied to theenvelope of the TMC, mapped by the GALEX All Sky Survey (AIS). UV and IRphotometric data have been retrieved from the GALEX-AIS and the 2MASScatalogues. NUV and K-band star counts have been used to identify the areas inthe cloud envelope where the 2175 \AA\ bump is weaker than in the diffuse ISMnamely, 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 fromSpitzer data and suggests that dust grains begin to decouple from theenvironmental galactic magnetic field already in the envelope.

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