Buoyant AGN Bubbles in the Quasi-isothermal Potential of NGC 1399

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dc.contributor.author Su, Yuanyuan
dc.contributor.author Nulsen, Paul E. J.
dc.contributor.author Kraft, Ralph P.
dc.contributor.author Forman, William R.
dc.contributor.author Jones, Christine
dc.contributor.author Irwin, Jimmy A.
dc.contributor.author Randall, Scott W.
dc.contributor.author Churazov, Eugene
dc.date.accessioned 2018-12-05T14:21:22Z
dc.date.available 2018-12-05T14:21:22Z
dc.date.issued 2017-10-01
dc.identifier.citation Su, Y. et al. (2017): Buoyant AGN Bubbles in the Quasi-isothermal Potential of NGC 1399. The Astrophysical Journal, 847(2). DOI: 10.3847/1538-4357/aa8954 en_US
dc.identifier.uri http://ir.ua.edu/handle/123456789/5143
dc.description.abstract The Fornax Cluster is a low-mass cool-core galaxy cluster. We present a deep Chandra study of NGC 1399, the central dominant elliptical galaxy of Fornax. The cluster center harbors two symmetric X-ray cavities coincident with a pair of radio lobes fed by two collimated jets along a north–south axis. A temperature map reveals that the active galactic nucleus (AGN) outburst has created a channel filled with cooler gas out to a radius of 10 kpc. The cavities are surrounded by cool bright rims and filaments that may have been lifted from smaller radii by the buoyant bubbles. X-ray imaging suggests a potential ghost bubble of ≳5 kpc diameter to the northwest. We find that the amount of gas lifted by AGN bubbles is comparable to that which would otherwise cool, demonstrating that AGN-driven outflow is effective in offsetting cooling in low-mass clusters. The cluster cooling timescale is >30 times longer than the dynamical timescale, which is consistent with the lack of cold molecular gas at the cluster center. The X-ray hydrostatic mass is consistent within 10%, with the total mass derived from the optical data. The observed entropy profile rises linearly, following a steeper slope than that observed at the centers of massive clusters; gas shed by stars in NGC 1399 may be incorporated in the hot phase. However, it is far-fetched for supernova-driven outflow to produce and maintain the thermal distribution in NGC 1399, and it is in tension with the metal content in the hot gas. en_US
dc.format.mimetype application/pdf en_US
dc.subject galaxies: clusters: intracluster medium en_US
dc.subject ISM: bubbles en_US
dc.subject X-rays: galaxies: clusters en_US
dc.title Buoyant AGN Bubbles in the Quasi-isothermal Potential of NGC 1399 en_US
dc.type text en_US


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