The Origin of the Diffuse X-ray Emission from the Carina Nebula

Details The Origin of the Diffuse X-ray Emission from the Carina Nebula The Origin of the Diffuse X-ray Emission from the Carina Nebula

Feb 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002noao.prop..329g&link_type=abstract

NOAO Proposal ID #2002A-0329

Physics

Scientific paper

The Carina Nebula is a nearby, relatively unobscured giant H II region. It hosts the highest concentration of O3 stars in the Galaxy as well as the most massive luminous blue variable, η Car. Thus it is an excellent site to study stellar energy feedback into the interstellar medium. The stellar energy feedback produces shock-heated, X-ray-emitting gas, which has indeed been detected in the Carina Nebula. It has been debated whether the X-ray-emitting gas in the Carina Nebula is powered by stellar winds only or by recent supernovae. We propose to use the CTIO 4m echelle spectrograph to study the kinematic structure of the Carina Nebula in regions with bright diffuse X-ray emission and in regions around OB associations. The spatial distribution and kinematic signatures of the high-velocity shocked gas allow us to (1) diagnose the presence of supernova remnants, and (2) assess the relative roles of stellar winds and supernovae in the stellar energy feedback in a starburst environment.

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