Active Galactic Nucleus Feedback in the Hot Halo of NGC 4649

Paggi, A.; Fabbiano, G.; Kim, Dong Woo; Pellegrini, Silvia; Civano, F.; Strader, Jay

doi:10.1088/0004-637x/787/2/134

Cited by 17 publications

(29 citation statements)

References 82 publications

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“…The coadded images show there are a pair of wings in both the northeast and south directions. These wings align with the direction of the outburst of the AGN at the core of M60 (Paggi et al 2014).…”

Section: Wings and Tail Structures Of M60supporting

confidence: 55%

The Infall of the Virgo Elliptical Galaxy M60 toward M87 and the Gaseous Structures Produced by Kelvin–Helmholtz Instabilities

Wood

Jones

Macháček

et al. 2017

ApJ

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We present Chandra observations of hot gas structures, characteristic of gas stripping during infall, in the Virgo cluster elliptical galaxy M60 (NGC4649) located 1 Mpc east of M87. 0.5 − 2 keV Chandra X-ray images show a sharp leading edge in the surface brightness 12.4 ± 0.1 kpc north and west of the galaxy center in the direction of M87 characteristic of a merger cold front due to M60's motion through the Virgo ICM. We measured a temperature of 1.00 ± 0.02 keV for abundance 0.5Z inside the edge and 1.37 +0.35 −0.19 keV for abundance 0.1Z in the Virgo ICM free stream region. We find that the observed jump in surface brightness yields a density ratio n in /n out = 6.44 +1.04 −0.67 between gas inside the edge and in the cluster free stream region. If the edge is a cold front due solely to the infall of M60 in the direction of M87, we find a pressure ratio of 4.7 +1.7 −1.4 and Mach number 1.7 +0.3 −0.3 . For 1.37 keV Virgo gas, we find a total infall velocity for M60 of v M60 = 1030 ± 180 km s −1 . We calculate the motion in the plane of the sky to be v tran = 1012 +183 −192 km s −1 implying an inclination angle ξ = 11 +3 −3 degrees. Surface brightness profiles also show the presence of a faint, diffuse gaseous tail. We identify filamentary gaseous wing structures caused by the galaxy's motion through the ICM. The structure and dimensions of these wings are consistent with simulations of Kelvin-Helmholtz instabilities as expected if the gas stripping is close to inviscid.

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Section: Wings and Tail Structures Of M60supporting

confidence: 55%

The Infall of the Virgo Elliptical Galaxy M60 toward M87 and the Gaseous Structures Produced by Kelvin–Helmholtz Instabilities

Wood

Jones

Macháček

et al. 2017

ApJ

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“…The sizes for all these cavities (except for NGC 4649) were taken from a single source, Shin et al (2016). For NGC 4649, we used the X-ray cavity size given in Paggi et al (2014). The cavity volumes and the associated uncertainties were calculated No.…”

Section: Feedback Cyclesmentioning

confidence: 99%

Thermodynamic properties, multiphase gas, and AGN feedback in a large sample of giant ellipticals

Lakhchaura

Werner

Sun

et al. 2018

Monthly Notices of the Royal Astronomical Society

100

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We present a study of the thermal structure of the hot X-ray emitting atmospheres for a sample of 49 nearby X-ray and optically bright elliptical galaxies using Chandra X-ray data. We focus on the connection between the properties of the hot X-ray emitting gas and the cooler Hα+[NII] emitting phase, and the possible role of the latter in the AGN (Active Galactic Nuclei) feedback cycle. We do not find evident correlations between the Hα+[NII] emission and global properties such as X-ray luminosity, mass of hot gas, and gas mass fraction. We find that the presence of Hα+[NII] emission is more likely in systems with higher densities, lower entropies, shorter cooling times, shallower entropy profiles, lower values of min(t cool /t ff ), and disturbed X-ray morphologies (linked to turbulent motions). However, we see no clear separations in the observables obtained for galaxies with and without optical emission line nebulae. The AGN jet powers of the galaxies with X-ray cavities show hint of a possible weak positive correlation with their Hα+ [NII] luminosities. This correlation and the observed trends in the thermodynamic properties may result from chaotic cold accretion (CCA) powering AGN jets, as seen in some high-resolution hydrodynamic simulations.

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“…For the early-type galaxy NGC 1332, which also has a centrally peaked temperature profile, Humphrey et al (2009a) showed that adding an SMBH with a plausible mass did little to alter the central temperature over that established by the stellar potential. Only for the massive elliptical galaxy NGC 4649, for which the sphere of influence is largely resolved by Chandra, is there a strong case for a central X-ray temperature peak generated by the potential of the SMBH Brighenti et al 2009;Paggi et al 2014).…”

Section: Super-massive Black Holementioning

confidence: 99%

The Unusually High Halo Concentration of the Fossil Group NGC 6482: Evidence for Weak Adiabatic Contraction

Buote

2017

ApJ

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Although fossil galaxy systems are thought to be very old, and thus should possess above-average halo concentrations, typically fossils have unexceptional concentrations for their masses. We revisit the massive isolated elliptical galaxy / fossil group NGC 6482 for which previous X-ray studies of a modest Chandra observation obtained a very uncertain, but also possibly very high, halo concentration. We present new measurements of the hot gas surface brightness, temperature, and iron abundance using the modest Chandra observation and a previously unpublished Suzaku observation, the latter of which allows the measurements of the gas properties to be extended out to ∼ r 2500 . By constructing hydrostatic equilibrium models of the gas with separate components for the gas, BCG stellar mass, and the dark matter (DM), we measure c 200 = 32.2 ± 7.1 and M 200 = (4.5 ± 0.6) × 10 12 M ⊙ using an NFW DM profile. For a halo of this mass, the measured concentration c 200 exceeds the mean value (7.1) expected for relaxed ΛCDM halos by 3.5σ in terms of the observational error, and by 6σ considering the intrinsic scatter in the ΛCDM c − M relation, which situates NGC 6482 as the most extreme outlier known for a fossil system. We explored several variants of adiabatic contraction (AC) models and, while the AC models provide fits of the same quality as the un-contracted models, they do have the following advantages: (1) smaller c 200 that is less of an outlier in the ΛCDM c − M relation, and (2) baryon fractions ( f b,200 ) that agree better with the mean cosmic value. While the standard AC prescriptions yield a BCG stellar mass that is uncomfortably small compared to results from stellar population synthesis (SPS) models, a weaker AC variant that artificially shuts off cooling and star formation at z = 2 yields the same stellar mass as the un-contracted models. For these reasons, we believe our X-ray analysis prefers this weaker AC variant applied to either an NFW or Einasto DM halo. Finally, the stellar mass we measure for the BCG from the hydrostatic analysis strongly favors results from SPS models with a Chabrier or Kroupa IMF over a Salpeter IMF.

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Active Galactic Nucleus Feedback in the Hot Halo of NGC 4649

Cited by 17 publications

References 82 publications

The Infall of the Virgo Elliptical Galaxy M60 toward M87 and the Gaseous Structures Produced by Kelvin–Helmholtz Instabilities

The Infall of the Virgo Elliptical Galaxy M60 toward M87 and the Gaseous Structures Produced by Kelvin–Helmholtz Instabilities

Thermodynamic properties, multiphase gas, and AGN feedback in a large sample of giant ellipticals

The Unusually High Halo Concentration of the Fossil Group NGC 6482: Evidence for Weak Adiabatic Contraction

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