In‐Depth<i>Chandra</i>Study of the AGN Feedback in Virgo Elliptical Galaxy M84

Finoguenov, A.; Ruszkowski, Mateusz; Jones, Christine; Brüggen, M.; Vikhlinin, A.; Mandel, Eric

doi:10.1086/591662

Cited by 61 publications

(62 citation statements)

References 27 publications

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“…The implication of the presence of cavities in the X‐ray gas distribution coincident with the radio lobes is that the sources are interacting strongly with the thermal gas, displacing rather than mixing with it (see McNamara & Nulsen 2007 for a review). For the sources in the present paper, the X‐ray observations of M 84 (Finoguenov et al 2008, Fig. 1b) and 3C 270 (Croston et al 2008, Fig.…”

Section: Rotation‐measure Bands From Compressionmentioning

confidence: 92%

Ordered magnetic fields around radio galaxies: evidence for interaction with the environment

Guidetti

Laing

Bridle

et al. 2011

Monthly Notices of the Royal Astronomical Society

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We present detailed imaging of Faraday rotation and depolarization for the radio galaxies 0206+35, 3C 270, 3C 353 and M 84, based on Very Large Array observations at multiple frequencies in the range 1365 to 8440 MHz. All of the sources show highly anisotropic banded rotation measure (RM) structures with contours of constant RM perpendicular to the major axes of their radio lobes. All except M84 also have regions in which the RM fluctuations have lower amplitude and appear isotropic. We give a comprehensive description of the banded RM phenomenon and present an initial attempt to interpret it as a consequence of interactions between the sources and their surroundings. We show that the material responsible for the Faraday rotation is in front of the radio emission and that the bands are likely to be caused by magnetized plasma which has been compressed by the expanding radio lobes. We present a simple model for the compression of a uniformly magnetized external medium and show that RM bands of approximately the right amplitude can be produced, but only for special initial conditions. A two‐dimensional magnetic structure in which the field lines are a family of ellipses draped around the leading edge of the lobe can produce RM bands in the correct orientation for any source orientation. We also report the first detections of rims of high depolarization at the edges of the inner radio lobes of M 84 and 3C 270. These are spatially coincident with shells of enhanced X‐ray surface brightness, in which both the field strength and the thermal gas density are likely to be increased by compression. The fields must be tangled on small scales.

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Section: Rotation‐measure Bands From Compressionmentioning

confidence: 92%

Ordered magnetic fields around radio galaxies: evidence for interaction with the environment

Guidetti

Laing

Bridle

et al. 2011

Monthly Notices of the Royal Astronomical Society

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“…Moreover, they also attribute the presence of small-scale metallicity gradients to relatively weak levels of small-scale turbulence, which could be consistent with viscous damping of gas motions. AGNs are known to generate intermittent outflows, causing weak shocks and sound waves (e.g., Fabian et al 2003;Forman et al 2005;Finoguenov et al 2008). The dissipation of the energy contained in these waves may be sufficient to offset radiative cooling of the gas.…”

Section: Introductionmentioning

confidence: 99%

Cosmological Magnetohydrodynamic Simulations of Cluster Formation With Anisotropic Thermal Conduction

Ruszkowski¹,

Lee²,

Brüggen³

et al. 2011

ApJ

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The intracluster medium (ICM) has been suggested to be buoyantly unstable in the presence of magnetic field and anisotropic thermal conduction. We perform first cosmological simulations of galaxy cluster formation that simultaneously include magnetic fields, radiative cooling, and anisotropic thermal conduction. In isolated and idealized cluster models, the magnetothermal instability (MTI) tends to reorient the magnetic fields radially whenever the temperature gradient points in the direction opposite to gravitational acceleration. Using cosmological simulations of cluster formation we detect radial bias in the velocity and magnetic fields. Such radial bias is consistent with either the inhomogeneous radial gas flows due to substructures or residual MTI-driven field rearrangements that are expected even in the presence of turbulence. Although disentangling the two scenarios is challenging, we do not detect excess bias in the runs that include anisotropic thermal conduction. The anisotropy effect is potentially detectable via radio polarization measurements with LOFAR and the Square Kilometer Array and future X-ray spectroscopic studies with the International X-ray Observatory. We demonstrate that radiative cooling boosts the amplification of the magnetic field by about two orders of magnitude beyond what is expected in the non-radiative cases. This effect is caused by the compression of the gas and frozen-in magnetic field as it accumulates in the cluster center. At z = 0 the field is amplified by a factor of about 10 6 compared to the uniform magnetic field that evolved due to the universal expansion alone. Interestingly, the runs that include both radiative cooling and thermal conduction exhibit stronger magnetic field amplification than purely radiative runs. In these cases, buoyant restoring forces depend on the temperature gradients rather than the steeper entropy gradients. Thus, the ICM is more easily mixed and the winding up of the frozen-in magnetic field is more efficient, resulting in stronger magnetic field amplification. We also demonstrate that thermal conduction partially reduces the gas accretion driven by overcooling despite the fact that the effective conductivity is suppressed below the Spitzer-Braginskii value.

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“…The radio morphology of early type galaxies can range from radio lobes which fill the X-ray cavities, as found for M84 (Finoguenov et al 2008), NGC5813 (Randall et al 2011), and UGC408 (Bogdan et al 2014), to X-ray cavities which show little or no associated radio emission, such as the two cavities in NGC4477 (see Fig. 2), and several of the X-ray cavities in NGC5044 (David et al 2009).…”

Section: Overviewmentioning

confidence: 93%

“…The size and number of cavities in the hot gas varies from one galaxy to another. As examples, NGC4636 and NGC4552 each show two primary cavities (Jones et al 2002, Baldi et al 2009, Machacek et al 2006, while M84 and the NGC5813 group show multiple cavities aligned along a single axis through the nucleus (Finoguenov et al 2008, Randall et al 2011. The cavity morphology of the group NGC5044 exhibits multiple cavities throughout its hot gas (David et al 2009).…”

Section: Overviewmentioning

confidence: 97%

X-ray jets and nuclear emission in low redshift early-type galaxies

Jones¹,

Forman²,

Churazov

et al. 2014

Proc. IAU

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Abstract. Due to its high angular resolution, the Chandra Observatory has allowed the discovery and detailed study of extragalactic X-ray jets. Although supermassive black holes are regularly found in the cores of massive galaxies and X-ray emission is detected from ∼80% of these, X-ray and radio jets are only detected in a small fraction of "normal" galaxies. X-ray jets are either single-sided or double-sided and, with only one possible exception, are found to have radio emission. However many radio jets are not detected in current X-ray observations. The expanding jets produce cavities in the surrounding hot gas in the galaxy halos. By determining how much gas has been pushed out of these cavities, we can determine the mechanical energy and power of the jet.

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In‐DepthChandraStudy of the AGN Feedback in Virgo Elliptical Galaxy M84

Cited by 61 publications

References 27 publications

Ordered magnetic fields around radio galaxies: evidence for interaction with the environment

Ordered magnetic fields around radio galaxies: evidence for interaction with the environment

Cosmological Magnetohydrodynamic Simulations of Cluster Formation With Anisotropic Thermal Conduction

X-ray jets and nuclear emission in low redshift early-type galaxies

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