[ITAL]Chandra[/ITAL] X-Ray Observations of the Hydra A Cluster: An Interaction between the Radio Source and the X-Ray–emitting Gas

McNamara, B. R.; Wise, Michael; Nulsen, P. E. J.; David, L. P.; Sarazin, Craig L.; Bautz, Marshall W.; Markevitch, M.; Vikhlinin, A.; Forman, W.; Jones, C.; Harris, D. E.

doi:10.1086/312662

Cited by 595 publications

(523 citation statements)

References 13 publications

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“…In contrast, the radio morphology does not appear correlated with the X-ray emission. An anticorrelation between X-ray and radio morphology has been seen in some nearby clusters of galaxies (McNamara et al 2000), but these data do not clearly show this effect.…”

Section: Optical and Radio Comparisonsmentioning

confidence: 73%

ChandraX‐Ray Spectroscopy and Imaging of the Galaxy Cluster PKS 0745−191

Hicks

Wise

Houck

et al. 2002

ApJ

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We present a detailed spectral and spatial analysis of the galaxy cluster PKS 0745À191, using recent observations from the Chandra X-Ray Observatory. The data provide information on the temperature and metallicity of the intracluster medium, the distribution of emission throughout the cluster, morphology of the cluster core, and an independent mass estimate that can be compared to that from gravitational lensing. X-ray spectra extracted from the central 300 kpc ($2 0 ) are well described by a two-temperature plasma, and the mean cluster temperature is consistent with previously determined values. The distribution of both temperature and metallicity within the inner 360 kpc (2<3) of PKS 0745À191 is probed on scales of 8 00 ($20 kpc), yielding a relatively constant abundance throughout the region and a strong temperature gradient (down to $4-5 keV) within the central 215 kpc. -model fits to the surface brightness profile of PKS 0745À191 indicate that a second -model component is required to fit the inner $10 kpc. Imaging analysis of the cluster core reveals an irregular morphology within the inner 50 kpc and confirms that the X-ray emission peak lies within 0>5 (the spatial resolution of Chandra) of both the optical and radio central cD positions. The cluster mass, based on both two-temperature and multiphase fits to the X-ray spectrum, is in close agreement with lensing mass estimates of PKS 0745À191.

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Section: Optical and Radio Comparisonsmentioning

confidence: 73%

ChandraX‐Ray Spectroscopy and Imaging of the Galaxy Cluster PKS 0745−191

Hicks

Wise

Houck

et al. 2002

ApJ

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“…The X-ray filament coincides with an emission line filament observed in Hα+NII (Cowie et al 1983). In Hydra A McNamara et al (2000) observed a flattened excess X-ray emission structure which is coincident with a gaseous star-forming disk with an estimated star formation rate between 1 and 15 M yr −1 (depending on the duration of the assumed star burst ∼10 9 or 10 8 yr, respectively, McNamara et al 2000). Also in A1835 an excess emission region close to the center and inhomogeneities are observed.…”

Section: Evidence For Inhomogeneities and Mass Deposition In X-ray Immentioning

confidence: 95%

The new emerging model for the structure of cooling cores in clusters of galaxies

Böhringer

Matsushita

Churazov

et al. 2002

A&A

173

171

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Abstract. New X-ray observations with XMM-Newton show a lack of spectral evidence for large amounts of cooling and condensing gas in the centers of galaxy clusters believed to harbour strong cooling flows. This paper re-explores the cooling flow scenario in the light of the new observations. We explore the diagnostics of the temperature structure of cooling cores with XMM-spectroscopy, tests for intracluster X-ray absorption towards central AGN, the effect of metal abundance inhomogeneities, and the implications of high resolution images in the centers of clusters. We find no evidence of intrinsic absorption in the center of the cooling flows of M 87 and the Perseus cluster. We further consider the effect of cluster rotation in cooling flow regions in the frame of cosmic structure evolution models. Also, the heating of the core regions of clusters by jets from a central AGN is reconsidered. We find that the power of the AGN jets as estimated by their interaction effects with the intracluster medium in several examples is more then sufficient to heat the cooling flows and to reduce the mass deposition rates. We explore in more detail which requirements such a heating model has to fulfill to be consistent with all observations, point out the way such a model could be constructed, and argue that such model building seems to be successful. In summary, it is argued that most observational evidence points towards much lower mass deposition rates than previously inferred in the central region of clusters thought to contain strong cooling flows.

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“…Therefore, this activity can have a repeated impact on the AGN host galaxy and its environment, starting from the initial phase of the radio source's life (O'Dea 2002) on to its later stages (McNamara et al 2000). The morphology of a (recurrent) radio source can vary significantly (see e.g.…”

Section: Introductionmentioning

confidence: 99%

The peculiar radio galaxy 4C 35.06: a case for recurrent AGN activity?

Shulevski

Morganti

Barthel

et al. 2015

A&A

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Using observations obtained with the LOw Fequency ARray (LOFAR), the Westerbork Synthesis Radio Telescope (WSRT) and archival Very Large Array (VLA) data, we have traced the radio emission to large scales in the complex source 4C 35.06 located in the core of the galaxy cluster Abell 407. At higher spatial resolution (∼4 ), the source was known to have two inner radio lobes spanning 31 kpc and a diffuse, low-brightness extension running parallel to them, offset by about 11 kpc (in projection). At 62 MHz, we detect the radio emission of this structure extending out to 210 kpc. At 1.4 GHz and intermediate spatial resolution (∼30 ), the structure appears to have a helical morphology. We have derived the characteristics of the radio spectral index across the source. We show that the source morphology is most likely the result of at least two episodes of AGN activity separated by a dormant period of around 35 Myr. The outermost regions of radio emission have a steep spectral index (α < −1), indicative of old plasma. We connect the spectral index properties of the resolved source structure with the integrated flux density spectral index of 4C 35.06 and suggest an explanation for its unusual integrated flux density spectral shape (a moderately steep power law with no discernible spectral break), possibly providing a proxy for future studies of more distant radio sources through inferring their detailed spectral index properties and activity history from their integrated spectral indices. The AGN is hosted by one of the galaxies located in the cluster core of Abell 407. We propose that it is intermittently active as it moves in the dense environment in the cluster core. In this scenario, the AGN turned on sometime in the past, and has produced the helical pattern of emission, possibly a sign of jet precession/merger during that episode of activity. Using LOFAR, we can trace the relic plasma from that episode of activity out to greater distances from the core than ever before. Using the the WSRT, we detect H I in absorption against the center of the radio source. The absorption profile is relatively broad (FWHM of 288 km s −1 ), similar to what is found in other clusters. The derived column density is N HI ∼ 4 × 10 20 cm −2 for a T spin = 100 K. This detection supports the connection -already suggested for other restarted radio sources -between the presence of cold gas and restarting activity. The cold gas appears to be dominated by a blue-shifted component although the broad H I profile could also include gas with different kinematics. Understanding the duty cycle of the radio emission as well as the triggering mechanism for starting (or restarting) the radio-loud activity can provide important constraints to quantify the impact of AGN feedback on galaxy evolution. The study of these mechanisms at low frequencies using morphological and spectral information promises to bring new important insights in this field.

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[ITAL]Chandra[/ITAL] X-Ray Observations of the Hydra A Cluster: An Interaction between the Radio Source and the X-Ray–emitting Gas

Cited by 595 publications

References 13 publications

ChandraX‐Ray Spectroscopy and Imaging of the Galaxy Cluster PKS 0745−191

ChandraX‐Ray Spectroscopy and Imaging of the Galaxy Cluster PKS 0745−191

The new emerging model for the structure of cooling cores in clusters of galaxies

The peculiar radio galaxy 4C 35.06: a case for recurrent AGN activity?

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