X-ray observations of hot gas in early-type galaxies and groups of galaxies

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dc.contributor Keel, W. C.
dc.contributor Townsley, Dean M.
dc.contributor Okada, Nobuchika
dc.contributor Dupke, Renato A.
dc.contributor.advisor White, Raymond E.
dc.contributor.advisor Irwin, Jimmy A.
dc.contributor.author Su, Yuanyuan
dc.date.accessioned 2017-03-01T16:52:15Z
dc.date.available 2017-03-01T16:52:15Z
dc.date.issued 2013
dc.identifier.other u0015_0000001_0001396
dc.identifier.other Su_alatus_0004D_11689
dc.identifier.uri https://ir.ua.edu/handle/123456789/1862
dc.description Electronic Thesis or Dissertation
dc.description.abstract Most of the baryonic matter in the Universe is not locked in stars. Instead, groups and clusters of galaxies as well as early-type galaxies contain a large mass of baryons in X-ray emitting hot gas. The study of such hot gas provides us a better understanding not only about the evolution of hierarchical structure formation and metal enrichment processes but also about baryon physics such as radiative cooling, ram pressure stripping, heating from active galactic nucleus (AGNs) and galactic winds. Moreover, such knowledge is invaluable for us to probe cosmology through galaxy clusters. In this dissertation I investigated the hot gas properties of galaxies and galaxy groups in three major scientific projects: (1) The measured metal abundance of the hot gas in early-type galaxies has been known to be lower than theoretical expectations. This may be related to the dilution of hot gas by mixing with cold gas. We studied the hot gas metal abundance with a sample of 32 early-type galaxies observed by <italic>Chandra<italic> and <italic>XMM-Newton<italic>. We find that there is virtually no correlation between hot gas Fe abundances and their atomic gas content. In contrast, we demonstrate a negative correlation between the measured hot gas Fe abundance and the ratio of molecular gas mass to hot gas mass. (2) We studied the X-ray brightest fossil group (poor cluster) ESO~3060170 out to its virial radius with <italic>Suzaku<italic>. The entropy and pressure profiles in the outer regions are flatter than in simulated clusters, similar to what is seen in observations of massive clusters. This may indicate that the gas is clumpy and/or the gas has been redistributed. (3) The nearby group centered on its bright central galaxy NGC~1407 has been thought to be an unusually dark system from previous kinematic studies. It is also known for hosting a bright galaxy NGC~1400 with a huge radial velocity difference (1200 km s$^{-1}$) with respect to the group center. We investigated the NGC~1407/1400 complex with <italic>XMM-Newton<italic> and <italic>Chandra<italic> observations. We show that a region of enhanced surface brightness between NGC~1407 and NGC~1400 is likely to be hot gas stripped from NGC~1400's ISM. We inferred that NGC~1407 system has a normal mass-to-light ratio from an X-ray--determined hydrostatic mass estimate.
dc.format.extent 197 p.
dc.format.medium electronic
dc.format.mimetype application/pdf
dc.language English
dc.language.iso en_US
dc.publisher University of Alabama Libraries
dc.relation.ispartof The University of Alabama Electronic Theses and Dissertations
dc.relation.ispartof The University of Alabama Libraries Digital Collections
dc.relation.hasversion born digital
dc.rights All rights reserved by the author unless otherwise indicated.
dc.subject.other Astrophysics
dc.subject.other Astronomy
dc.subject.other Physics
dc.title X-ray observations of hot gas in early-type galaxies and groups of galaxies
dc.type thesis
dc.type text
etdms.degree.department University of Alabama. Dept. of Physics and Astronomy
etdms.degree.discipline Physics
etdms.degree.grantor The University of Alabama
etdms.degree.level doctoral
etdms.degree.name Ph.D.

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