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          Institute: MPI für Radioastronomie     Collection: Publikationen des MPI für Radioastronomie     Display Documents



ID: 11192.0, MPI für Radioastronomie / Publikationen des MPI für Radioastronomie
Chandra observations of the disruption of the cool core in A133
Authors:Fujita, Y.; Sarazin, C. L.; Kempner, J. C.; Rudnick, L.; Slee, O. B.; Roy, A. L.; Andernach, H.; Ehle, M.
Language:English
Date of Publication (YYYY-MM-DD):2002-08-20
Title of Journal:Astrophysical Journal
Journal Abbrev.:Astrophys. J.
Volume:575
Issue / Number:2
Start Page:764
End Page:778
Review Status:Peer-review
Audience:Experts Only
Abstract / Description:We present the analysis of a Chandra observation of the galaxy cluster A133, which has a cooling flow core, a central radio source, and a diffuse, filamentary radio source that has been classified as a radio relic. The X-ray image shows that the core has a complex structure. The most prominent feature is a tongue of emission that extends from the central cD galaxy to the northwest and partly overlaps the radio relic. Spectral analysis shows that the emission from the tongue is thermal emission from relatively cool gas at a temperature of similar to1.3 keV. One possibility is that this tongue is produced by Kelvin-Helmholtz (KH) instabilities through the interaction between the cold gas around the cD galaxy and hot intracluster medium. We estimate the critical velocity and timescale for the KH instability to be effective for the cold core around the cD galaxy. We find that the KH instability can disrupt the cold core if the relative velocity is greater than or similar to400 km s(-1). We compare the results with those of clusters in which sharp, undisrupted cold fronts have been observed; in these clusters, the low-temperature gas in their central regions has a more regular distribution. In contrast to A133, these cluster cores have longer timescales for the disruption of the core by the KH instability when they are normalized to the timescale of the cD galaxy motion. Thus, the other cores are less vulnerable to KH instability. Another possible origin of the tongue is that it is gas that has been uplifted by a buoyant bubble of non-thermal plasma that we identify with the observed radio relic. From the position of the bubble and the radio estimate of the age of the relic source, we estimate a velocity of 700 km s(-1) for the bubble. The structure of the bubble and this velocity are consistent with numerical models for such buoyant bubbles. The energy dissipated by the moving bubble may affect the cooling flow in A133. The combination of the radio and X-ray observations of the radio relic suggest that it is a relic radio lobe formerly energized by the central cD rather than a merger shock generated cluster radio relic. The lobe may have been displaced from the central cD galaxy by the motion of the cD galaxy or by the buoyancy of the lobe.
Free Keywords:cooling flows; galaxies : clusters : general; galaxies : clusters : individual (A133); intergalactic medium; radio continuum : galaxies; X-rays : galaxies : clusters
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Radioastronomie
External Affiliations:Natl Astron Observ, Osawa 2-21-1, Tokyo 1818588, Japan; Natl Astron Observ, Tokyo 1818588, Japan; Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA; Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA; CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia; Max Planck Inst Radioastron, D-53121 Bonn, Germany; Univ Guanajuato, Dept Astron, Guanajuato 36000, Mexico; XMM Newton Sci Operat Ctr, E-28080 Madrid, Spain; ESA, ESTEC, Res & Sci Support Dept, Sci Operat & Data Syst Div, NL-2200 AG Noordwijk, Netherlands
Identifiers:ISI:000177430600014
ISSN:0004-637X
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