Cold molecular gas in the Perseus cluster core

Salomé, P.; Combes, F.; Edge, A. C.; Crawford, C. S.; Erlund, Mary; Fabian, A. C.; Hatch, N. A.; Johnstone, R. M.; Sanders, J. S.; Wilman, R. J.

doi:10.1051/0004-6361:20054745

Cited by 218 publications

(294 citation statements)

References 39 publications

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“…This triggers AGN jets that heat the ICM above the threshold for clump formation before the cluster cools down again, thus closing the loop of AGN feedback. This scenario is supported by observations of atomic (Crawford et al 1999;McDonald et al 2011;Werner et al 2014) and molecular (Donahue et al 2000;Edge 2001;Salomé et al 2006;Hamer et al 2014;Russell et al 2014) gas at the center of many CC clusters. Entropy profiles of observed CC clusters also appear to follow a baseline profile predicted by the precipitationregulated feedback model .…”

Section: Smbh Accretion and Feedback Prescriptionsmentioning

confidence: 60%

Interplay Among Cooling, Agn Feedback, and Anisotropic Conduction in the Cool Cores of Galaxy Clusters

Yang

Reynolds

2016

ApJ

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Feedback from the active galactic nuclei (AGNs) is one of the most promising heating mechanisms to circumvent the cooling-flow problem in galaxy clusters. However, the role of thermal conduction remains unclear. Previous studies have shown that anisotropic thermal conduction in cluster cool cores (CCs) could drive the heat-flux-driven buoyancy instabilities (HBIs) that reorient the field lines in the azimuthal directions and isolate the cores from conductive heating from the outskirts. However, how the AGN interacts with the HBI is still unknown. To understand these interwined processes, we perform the first 3D magnetohydrodynamic simulations of isolated CC clusters that include anisotropic conduction, radiative cooling, and AGN feedback. We find the following: (1) For realistic magnetic field strengths in clusters, magnetic tension can suppress a significant portion of HBI-unstable modes, and thus the HBI is either completely inhibited or significantly impaired, depending on the unknown magnetic field coherence length. (2) Turbulence driven by AGN jets can effectively randomize magnetic field lines and sustain conductivity at ∼1/3 of the Spitzer value; however, the AGN-driven turbulence is not volumefilling. (3) Conductive heating within the cores could contribute to ∼10% of the radiative losses in Perseus-like clusters and up to ∼50% for clusters twice the mass of Perseus. (4) Thermal conduction has various impacts on the AGN activity and intracluster medium properties for the hottest clusters, which may be searched by future observations to constrain the level of conductivity in clusters. The distribution of cold gas and the implications are also discussed.

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Section: Smbh Accretion and Feedback Prescriptionsmentioning

confidence: 60%

Interplay Among Cooling, Agn Feedback, and Anisotropic Conduction in the Cool Cores of Galaxy Clusters

Yang

Reynolds

2016

ApJ

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“…bipolar molecular flow in similarly extended filaments that may be accelerated outward by the mechanical energy associated with rising radio bubbles (McNamara et al 2014). Single dish detections of molecular gas coincident with Hα filaments beneath buoyant radio bubbles in the Perseus cluster are consistent with this scenario (Salomé et al 2006(Salomé et al , 2011. Radio jet-driven outflows of molecular gas have also been detected in nearby galaxies (eg.…”

Section: Molecular Gas Clouds Lifted By Radio Bubbles?mentioning

confidence: 78%

“…The Perseus cluster hosts 4 × 10 10 M of extended molecular gas filaments coincident with the coolest X-ray gas (Salomé et al 2006). The simplest interpretation of their velocity structure is an inflow of gas cooling from the ICM, free-falling toward the BCG Lim, Ao & Dinh-V-Trung 2008).…”

Section: Origin Of the Molecular Gasmentioning

confidence: 99%

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ALMA observations of cold molecular gas filaments trailing rising radio bubbles in PKS 0745−191

Russell

McNamara

Fabian

et al. 2016

Mon. Not. R. Astron. Soc.

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105

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We present ALMA observations of the CO(1-0) and CO(3-2) line emission tracing filaments of cold molecular gas in the central galaxy of the cluster PKS 0745-191. The total molecular gas mass of 4.6±0.3×10 9 M , assuming a Galactic X CO factor, is divided roughly equally between three filaments each extending radially 3 − 5 kpc from the galaxy centre. The emission peak is located in the SE filament ∼ 1 arcsec (2 kpc) from the nucleus. The velocities of the molecular clouds in the filaments are low, lying within ±100 km s −1 of the galaxy's systemic velocity. Their FWHMs are less than 150 km s −1 , which is significantly below the stellar velocity dispersion. Although the molecular mass of each filament is comparable to a rich spiral galaxy, such low velocities show that the filaments are transient and the clouds would disperse on < 10 7 yr timescales unless supported, likely by the indirect effect of magnetic fields. The velocity structure is inconsistent with a merger origin or gravitational free-fall of cooling gas in this massive central galaxy. If the molecular clouds originated in gas cooling even a few kpc from their current locations their velocities would exceed those observed. Instead, the projection of the N and SE filaments underneath X-ray cavities suggests they formed in the updraft behind bubbles buoyantly rising through the cluster atmosphere. Direct uplift of the dense gas by the radio bubbles appears to require an implausibly high coupling efficiency. The filaments are coincident with low temperature X-ray gas, bright optical line emission and dust lanes indicating that the molecular gas could have formed from lifted warmer gas that cooled in situ.

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“…O'Dea et al 2010;Tremblay 2011). Relative to field galaxies or those in non-CC clusters, BCGs in CCs preferentially harbour radio sources and kpc-scale filamentary forbidden and Balmer emission line nebulae amid 10 9 -10 11 M repositories of vibrationally excited and cold molecular gas (Heckman 1981;Hu, Cowie & Wang 1985;Baum 1987;Heckman et al 1989;Burns 1990;Jaffe & Bremer 1997;Donahue et al 2000;Edge 2001;Edge & Frayer 2003;Salomé & Combes 2003;Egami et al 2006;Salomé et al 2006;Edwards et al 2007; von der Wilman, Edge & Swinbank 2009;Edge et al 2010a,b;Salomé et al 2011;McNamara et al 2014;Russell et al 2014). Low to moderate levels (∼1 to 10 M yr −1 ) of star formation appear to be ongoing amid these mysteriously dusty (O'Dea et al 2008;Quillen et al 2008;Edge et al 2010a,b;Mittal et al 2011;Rawle et al 2012;Tremblay et al 2012b), polycyclic aromatic hydrocarbon (PAH)-rich (Donahue et al 2011) cold reservoirs on 50 kpc scales in clumpy and filamentary distributions (e.g.…”

mentioning

confidence: 99%

Far-ultraviolet morphology of star-forming filaments in cool core brightest cluster galaxies

Tremblay

O’Dea

Baum

et al. 2015

Mon. Not. R. Astron. Soc.

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We present a multiwavelength morphological analysis of star forming clouds and filaments in the central (< ∼ 50 kpc) regions of 16 low redshift (z < 0.3) cool core brightest cluster galaxies (BCGs). The sample spans decades-wide ranges of X-ray mass deposition and star formation rates as well as active galactic nucleus (AGN) mechanical power, encompassing both high and low extremes of the supposed intracluster medium (ICM) cooling and AGN heating feedback cycle. New Hubble Space Telescope (HST) imaging of far ultraviolet continuum emission from young (< ∼ 10 Myr), massive (> ∼ 5 M ) stars reveals filamentary and clumpy morphologies, which we quantify by means of structural indices. The FUV data are compared with X-ray, Lyα, narrowband Hα, broadband optical/IR, and radio maps, providing a high spatial resolution atlas of star formation locales relative to the ambient hot (∼ 10 7−8 K) and warm ionised (∼ 10 4 K) gas phases, as well as the old stellar population and radio-bright AGN outflows. Nearly half of the sample possesses kpc-scale filaments that, in projection, extend toward and around radio lobes and/or X-ray cavities. These filaments may have been uplifted by the propagating jet or buoyant X-ray bubble, or may have formed in situ by cloud collapse at the interface of a radio lobe or rapid cooling in a cavity's compressed shell. Many other extended filaments, however, show no such spatial correlation, and the dominant driver of their morphology remains unclear. We nevertheless show that the morphological diversity of nearly the entire FUV sample is reproduced by recent hydrodynamical simulations in which the AGN powers a self-regulating rain of thermally unstable star forming clouds that precipitate from the hot atmosphere. In this model, precipitation triggers where the cooling-to-freefall time ratio is t cool /t ff ∼ 10. This condition is roughly met at the maxmial projected FUV radius for more than half of our sample, and clustering about this ratio is stronger for sources with higher star formation rates.

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Cold molecular gas in the Perseus cluster core

Cited by 218 publications

References 39 publications

Interplay Among Cooling, Agn Feedback, and Anisotropic Conduction in the Cool Cores of Galaxy Clusters

Interplay Among Cooling, Agn Feedback, and Anisotropic Conduction in the Cool Cores of Galaxy Clusters

ALMA observations of cold molecular gas filaments trailing rising radio bubbles in PKS 0745−191

Far-ultraviolet morphology of star-forming filaments in cool core brightest cluster galaxies

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