Mapping the cold molecular gas in a cooling  flow cluster:
Abell 1795

Salomé, P.; Combes, F.

doi:10.1051/0004-6361:20031744

Cited by 51 publications

(59 citation statements)

References 25 publications

(29 reference statements)

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“…Cold molecular gas mass as a function of Hα luminosity for the regions in the filaments detected at both wavelengths (see Table 3). Circles are CO detections from Edge et al (2001), squares are CO detections from Salomé & Combes (2004a) and triangles are present results. Overlaid in dashed line is the linear relation fitted by Salomé & Combes (2003).…”

Section: Intermittent Cooling Flow Scenariomentioning

confidence: 99%

Cold molecular gas in the Perseus cluster core

Salomé¹,

Combes²,

Edge³

et al. 2006

A&A

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Cold molecular gas has recently been detected in several cooling flow clusters of galaxies containing huge optical nebula. These optical filaments are tightly linked to cooling flows and related phenomena, such as rising bubbles of relativistic plasma fed by radio jets. We present here a map, in the CO(2-1) rotational line, of the cold molecular gas associated with some of the Hα filaments surrounding the central galaxy of the Perseus cluster: NGC 1275. The map, extending to about 50 kpc (135 arcsec) from the center of the galaxy, has been made with the 18-receiver array HERA at the focus of the IRAM 30 m telescope. Although most of the cold gas is concentrated to the center of the galaxy, the CO emission is also clearly associated with the extended filaments conspicuous in ionised gas, and could trace a possible reservoir fueling the star formation there. Some of the CO emission is also found where the X-ray gas could cool down more efficiently at the rims of the central X-ray cavities (where the hot gas is thought to have been pushed out and compressed by the expanding radio lobes of the central AGN). The CO global kinematics do not show any rotation in NGC 1275. The cold gas is probably a mixture of gas falling down on the central galaxy and of uplifted gas dragged out by a rising bubble in the intracluster medium. As recently suggested in other cluster cores, the cold gas peculiar morphology and kinematics argue for the picture of an intermittent cooling flow scenario where the central AGN plays an important role.

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Section: Intermittent Cooling Flow Scenariomentioning

confidence: 99%

Cold molecular gas in the Perseus cluster core

Salomé¹,

Combes²,

Edge³

et al. 2006

A&A

Self Cite

219

266

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“…To improve our statistics, we performed a search of the literature and archive data for VLBI data of BCGs in Abell clusters that have detailed information about the cluster dynamics (X-ray emission) and radio emission at mas and arcsec resolution. To obtain an extended BCG list, we added to our complete sample the following sources: Giovannini et al 2005); -Hydra A in A780 (Taylor 1996;Wise et al 2007); -4C 26.42 in A1795 (Liuzzo et al 2009a;Salomé & Combes 2004); -3C317 in A2052 (Venturi et al 2004); -B2151+174 in A2390 (Augusto et al 2006); -PKS 2322-123 in A2597 (Morris & Fabian 2005;Taylor et al 1999): -PKS 1246-410 (NGC4696) in A3526 (Taylor et al 2006b). …”

Section: The Extended Samplementioning

confidence: 99%

Parsec-scale properties of brightest cluster galaxies

Liuzzo

Giovannini

Giroletti³

et al. 2010

A&A

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We present new VLBI observations at 5 GHz of a complete sample of brightest cluster galaxies (BCGs) in nearby Abell clusters (distance class <3). Combined with data from the literature, we provide parsec-scale information for 34 BCGs. Our analysis of the parsec-scale radio emission of BCGs and the cluster X-ray properties finds a possible dichotomy between BCGs in cool-core clusters and those in non-cool-core clusters. Among resolved sources, those in cool-core clusters tend to have two-sided parsec-scale jets, while those in less relaxed clusters have predominantly one-sided parsec-scale jets. We suggest that this difference is caused by the interplay between the jets and the surrounding medium. The one-sided structure in non-cool-core clusters may be due to Doppler boosting effects in relativistic, intrinsically symmetric jets whereas two-sided morphology in cool core clusters is probably related to the presence of heavy and mildly relativistic jets that have been decelerated on the parsec-scale. Evidence of recurrent activity is also found in BCGs in cool-core clusters.

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“…Despite the large CO luminosity, no significant 1-0 S series of H 2 has been detected. Observations of the CO(1-0) and CO(2-1) lines showed that the molecular gas traces the Hα emission, but is not centered on the galaxy (Salomé & Combes 2004 Quillen et al 2008). The BCG also hosts significant quantities of dust, with a dust mass of 2.2´10 7  M assuming a dust temperature of 40 K (Edge 2001).…”

Section: Introductionmentioning

confidence: 99%

A ¹³CO Detection in a Brightest Cluster Galaxy

Vantyghem

McNamara

Edge

et al. 2017

ApJ

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We present ALMA Cycle 4 observations of CO(1-0), CO(3-2), and 13 CO(3-2) line emission in the brightest cluster galaxy (BCG) of RXJ0821+0752. This is one of the first detections of 13 CO line emission in a galaxy cluster. Half of the CO(3-2) line emission originates from two clumps of molecular gas that are spatially offset from the galactic center. These clumps are surrounded by diffuse emission that extends 8kpc in length. The detected 13 CO emission is confined entirely to the two bright clumps, with any emission outside of this region lying below our detection threshold. Two distinct velocity components with similar integrated fluxes are detected in the 12 CO spectra. The narrower component (60 km s −1 FWHM) is consistent in both velocity centroid and linewidth with 13 CO(3-2) emission, while the broader (130-160 km s −1 ), slightly blueshifted wing has no associated 13 CO(3-2) emission. A simple local thermodynamic model indicates that the 13 CO emission traces 2.1×10 9 M e of molecular gas. Isolating the 12 CO velocity component that accompanies the 13 CO emission yields a CO-to-H 2 conversion factor of α CO =2.3M e (K km s −1 ) −1 , which is a factor of two lower than the Galactic value. Adopting the Galactic CO-to-H 2 conversion factor in BCGs may therefore overestimate their molecular gas masses by a factor of two. This is within the object-to-object scatter from extragalactic sources, so calibrations in a larger sample of clusters are necessary in order to confirm a sub-Galactic conversion factor.

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Mapping the cold molecular gas in a cooling flow cluster: Abell 1795

Cited by 51 publications

References 25 publications

Cold molecular gas in the Perseus cluster core

Cold molecular gas in the Perseus cluster core

Parsec-scale properties of brightest cluster galaxies

A ¹³CO Detection in a Brightest Cluster Galaxy

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Mapping the cold molecular gas in a cooling flow cluster: Abell 1795

Cited by 51 publications

References 25 publications

Cold molecular gas in the Perseus cluster core

Cold molecular gas in the Perseus cluster core

Parsec-scale properties of brightest cluster galaxies

A 13CO Detection in a Brightest Cluster Galaxy

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A ¹³CO Detection in a Brightest Cluster Galaxy