Stellar Mass Loss Versus External Accretion in X-Ray Bright Ellipticals

Details Stellar Mass Loss Versus External Accretion in X-Ray Bright Ellipticals Stellar Mass Loss Versus External Accretion in X-Ray Bright Ellipticals

Sep 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999cxo..prop...15s&link_type=abstract

Chandra Proposal ID #01600222

Computer Science

Chandra Proposal Id #01600222

Scientific paper

Observations of NGC 5846 and NGC 4649, two X-ray-bright elliptical galaxies with extended emission line filaments and dust, will be used to study the interaction between the hot, X-ray emitting gas and cooler interstellar material. We will determine whether heat conduction into the cooler gas or energy losses to grains affect the thermal state of the gas. The elemental abundances and gradients in the hot gas will be derived and compared to the stellar values. If the gas results from local stellar mass loss, the abundances should be similar. If there is a cooling flow, the abundances at each radius should reflect those of stars at larger radii. In these very bright galaxies, inflow of intergalactic gas may also be important; this would produce low abundances with only weak gradients.

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