The Missing Baryons in the Local Group

Details The Missing Baryons in the Local Group The Missing Baryons in the Local Group

Sep 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003cxo..prop.1586b&link_type=abstract

Chandra Proposal ID #05910578

Mathematics

Logic

Chandra Proposal Id #05910578

Scientific paper

The detection of X-ray absorption and emission lines at z = 0 has been interpreted as an extensive isothermal Local Group medium with a gaseous mass exceeding the baryonic mass of all Local Group galaxies. A large gaseous mass helps to solve the "missing baryon problem", a leading cosmological issue. However, the gas mass is highly model dependent, and in an alternative model, the gas lies in a Galactic halo of size 50 kpc and with a gas mass orders of magnitude lower. We can discriminate between the Galactic Halo and Local Group models by determining whether most of the diffuse X-ray emission (0.5-1 keV) lies in front or behind a Magellanic Stream cloud at a distance of 50 kpc. For the Local Group model, the MS cloud will absorb the emission beyond it, casting an X-ray "shadow".

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