Title: ALMA  studies of the Magellanic Bridge

Abstract:
The Magellanic Bridge is a filamentary structure of about 15 to 21 kpc seen in neutral hydrogen 
(HI) lying between the LMC and the SMC. It represent the nearest tidally interaction between 
these two galaxies some 200 Myr ago. It has a lower metallicity than the SMC and therefore 
allow to study the ISM in extreme conditions. Recent studies have revealed the presence of 
young (< 200Myr) massive stars and CO molecular clouds. The latter were barely resolved 
in single-dish observations and are spatially related to warm dust emission sources, as recently 
established by the Spitzer SMC-SAGE and Herschel HERITAGE studies Surprisingly, one of 
this source shows  a large 870 mu submillimeter excess, as determine from our 870 mu studies 
and thus  indicative of either very cold dust or a dramatically different submillimeter emissivity. 
We will present results of ALMA C1 CO observations of Magellanic Bridge A and their physical 
properties at arc second resolution.