XMM-Newton observations of M 87 and its X-ray halo

Böhringer, H.; Belsole, E.; Kennea, J. A.; Matsushita, Kyoko; Molendi, S.; Worrall, D. M.; Mushotzky, R. F.; Ehle, M.; Guainazzi, M.; Sakelliou, I.; Stewart, G. C.; Vestrand, W. T.; Santos, S. Dos

doi:10.1051/0004-6361:20000092

Cited by 158 publications

(194 citation statements)

References 27 publications

Supporting

Mentioning

174

Contrasting

Unclassified

Order By: Relevance

“…Moreover, the new estimated mass deposition rates are significantly smaller than those evaluated by using previous X-ray satellite data (McNamara et al 2001;Peterson et al 2001). Finally, the new data show that cluster spectra are better represented by a single (or double) temperature model rather than the standard multiphase (multitemperature) cooling flow model (Molendi & Pizzolato 2001;Böhringer et al 2001;Fabian et al 2001;Matsushita et al 2002).…”

Section: Introductionmentioning

confidence: 69%

Radiative Cooling and Heating and Thermal Conduction in M87

Ghizzardi

Molendi

Pizzolato

et al. 2004

ApJ

View full text Add to dashboard Cite

The crisis of the standard cooling flow model brought about by Chandra and XMM-Newton observations of galaxy clusters has led to the development of several models that explore different heating processes in order to assess whether they can quench the cooling flow. Among the most appealing mechanisms are thermal conduction and heating through buoyant gas deposited in the intracluster medium (ICM) by active galactic nuclei (AGNs). We combine Virgo/M87 observations of three satellites (Chandra, XMM-Newton, and BeppoSAX ) to inspect the dynamics of the ICM in the center of the cluster. Using the spectral deprojection technique, we derive the physical quantities describing the ICM and determine the extra heating needed to balance the cooling flow, assuming that thermal conduction operates at a fixed fraction of the Spitzer value. We assume that the extra heating is due to buoyant gas, and we fit the data using the model developed by Ruszkowski and Begelman. We derive a scale radius for the model of $5 kpc, which is comparable with the M87 AGN jet extension, and a required luminosity of the AGN of a few ; 10 42 ergs s À1 , which is comparable to the observed AGN luminosity. We discuss a scenario in which the buoyant bubbles are filled with relativistic particles and magnetic field, which are responsible for the radio emission in M87. The AGN is supposed to be intermittent and to inject populations of buoyant bubbles through a succession of outbursts. We also study the X-ray-cool component detected in the radio lobes and suggest that it is structured in blobs that are tied to the radio buoyant bubbles.

show abstract

Section: Introductionmentioning

confidence: 69%

Radiative Cooling and Heating and Thermal Conduction in M87

Ghizzardi

Molendi

Pizzolato

et al. 2004

ApJ

View full text Add to dashboard Cite

show abstract

“…One of the most striking results presented is a very marked drop in the abundance profiles of Si and Fe within 1 arcmin of the center of M 87. Böhringer et al (2001) suggest that resonant scattering may be responsible for this drop. Mathews…”

Section: Introductionmentioning

confidence: 91%

“…Details on the observation, as well as results from a first analysis of this object, have already been published in Böhringer et al (2001) and Belsole et al (2001).…”

Section: Observations and Data Preparationmentioning

confidence: 99%

See 1 more Smart Citation

On the metal abundance in the core of M 87

Molendi

Gastaldello

2001

A&A

Self Cite

View full text Add to dashboard Cite

Abstract. We revisit the XMM-Newton observation of M 87 to make a new and more detailed measurement of the metal abundance profile. After having verified that spectral fits with single temperature models show a dramatic abundance drop within 1 arcmin of the cluster core, we show that more appropriate models, which include a multi-temperature component to account for the strong temperature gradient observed in M 87, and a power-law component to account for the emission of the nucleus and knot A, give a substantially flat abundance profile. The drastic abundance decrement found by fitting a single temperature component to the data is an artifact known as "Fe-bias" (Buote 2000a,b) following from the application of an oversimplified spectral model to the data.

show abstract

“…The spectral index interpolated between the radio (18 GHz) and X-ray is αrx = 0.95, typical of jet cores and knots (e.g., Balmaverde, Capetti & Grandi 2006;Harwood & Hardcastle 2012). If the X-ray is interpreted as dominated by emission from a small-scale jet and arising from the electron population responsible for the radio core, the combination of αx and αrx requires the synchrotron spectrum to steepen somewhere between the radio and X-ray, and a spectral break of ∆α = 0.5 is the simple prediction for energy losses (although observations of resolved jet knots often find somewhat larger breaks (e.g., Böhringer et al 2001;Birkinshaw, Worrall & Hardcastle 2002). The data for PKS B1416−493 can be accommodated by a break at the relatively high frequency of about 10 16 Hz if ∆α = 0.5 between a presumed index of αr = 0.86 in the radio and αx = 1.36 (Fig.…”

Section: Corementioning

confidence: 99%

A non cool-core 4.6-keV cluster around the bright nearby radio galaxy PKS B1416−493

Worrall¹,

Birkinshaw²

2017

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

We present new X-ray (Chandra) and radio (ATCA) observations of the z = 0.09 radio galaxy PKS B1416−493, a member of the southern equivalent of the 3CRR sample. We find the source to be embedded in a previously unrecognized bright kT = 4.6-keV non cool-core cluster. The discovery of new clusters of such high temperature and luminosity within z = 0.1 is rare. The radio source was chosen for observation based on its intermediate FR I/II morphology. We identify a cavity coincident with the northeast lobe, and excess counts associated with the southwest lobe that we interpret as inverse Compton X-ray emission. The jet power, at 5.3 × 10 44 erg s −1 , when weighted by radio source density, supports suggestions that radio sources of intermediate morphology and radio power may dominate radio-galaxy heating in the local Universe.

show abstract

XMM-Newton observations of M 87 and its X-ray halo

Cited by 158 publications

References 27 publications

Radiative Cooling and Heating and Thermal Conduction in M87

Radiative Cooling and Heating and Thermal Conduction in M87

On the metal abundance in the core of M 87

A non cool-core 4.6-keV cluster around the bright nearby radio galaxy PKS B1416−493

Contact Info

Product

Resources

About