Stellar Mass Loss Versus External Accretion in the X-ray Bright Elliptical NGC 5813

Details Stellar Mass Loss Versus External Accretion in the X-ray Bright Elliptical NGC 5813 Stellar Mass Loss Versus External Accretion in the X-ray Bright Elliptical NGC 5813

Sep 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004cxo..prop.1811s&link_type=abstract

Chandra Proposal ID #06610190

Computer Science

Chandra Proposal Id #06610190

Scientific paper

A Chandra image of NGC5813, an X-ray-bright elliptical with extended emission line filaments and dust, will be used to study the interaction between the hot, X-ray gas and cooler (merger related?) interstellar material. A previous ROSAT HRI image suggests a correlation with cooler 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. Inflow of intergalactic gas would produce low abundances with only weak gradients.

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