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Hot Gaseous Halos in Early Type Galaxies

Smithsonian Astrophysical Observatory, Cambridge, MA 02138, USA
Academic Editors: Duncan A. Forbes and Ericson D. Lopez
Galaxies 2017, 5(4), 60; https://doi.org/10.3390/galaxies5040060
Received: 31 July 2017 / Revised: 26 September 2017 / Accepted: 27 September 2017 / Published: 4 October 2017
(This article belongs to the Special Issue On the Origin (and Evolution) of Baryonic Galaxy Halos)
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Abstract

The hot gas in early type galaxies (ETGs) plays a crucial role in their formation and evolution. As the hot gas is often extended to the outskirts beyond the optical size, the large scale structural features identified by Chandra (including cavities, cold fronts, filaments, and tails) point to key evolutionary mechanisms, e.g., AGN feedback, merging history, accretion/stripping, as well as star formation and quenching. We systematically analyze the archival Chandra data of ETGs to study the hot ISM. Using uniformly derived data products with spatially resolved spectral information, we revisit the X-ray scaling relations of ETGs and address their implications by comparing them with those of groups/clusters and simulations. View Full-Text
Keywords: galaxies: elliptical and lenticular; cD–X-rays: galaxies galaxies: elliptical and lenticular; cD–X-rays: galaxies
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This is an open access article distributed under the Creative Commons Attribution License which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited (CC BY 4.0).
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Kim, D.-W. Hot Gaseous Halos in Early Type Galaxies. Galaxies 2017, 5, 60.

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