Molecules in the Large Magellanic Cloud

M. E. ORTEGA; P. A. JONES; C. FARIÑA; M. RUBIO; S. PARON; M. CUNNINGHAM

Campinas (San Pablo)

Simposio; International Symposium and Workshop on Astrochemistry; 2016

The Large Magellanic Cloud (LMC) is a gas rich environment with reduced metallicity (Z about half of the Galactic value) that allow us to study star formation in an interstellar medium (ISM) that may be comparable, to certain degree, to those conditions of some star-forming sites in our Galaxy in the early stages (see for example Yamada et al. 2013).Most of the molecular line observations towards the LMC do not cover the 345 GHz window, which contains several molecular lines that provide substantial information about the physical and chemical conditions. Thus, we performed observations in this spectral window towards several regions in the LMC (see Paron et al. 2014 and 2016).