Two-dimensional spectrophotometry of the cores of X-ray luminous clusters

Cowie, L. L.; Hu, E. M.; Jenkins, Edward B.; York, D. G.

doi:10.1086/161259

Cited by 140 publications

(117 citation statements)

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“…Tamura et al 2001). discovered with the Chandra satellite a 40 long (∼60 kpc, with an adopted Hubble constant of H 0 = 75 km s −1 Mpc −1 ) X-ray filament in its core, coinciding with an H α +NII filament previously found by Cowie et al (1983). This filament is also conspicuous in the U-band (McNamara et al 1996a), and the site of star formation: the blue continuum along the edges of the radio lobes are resolved into bright knots with the Hubble Space Telescope (HST).…”

Section: Abell 1795supporting

confidence: 68%

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

Salomé

Combes

2004

A&A

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Abstract. Cold molecular gas is found in several clusters of galaxies (Edge 2001;Salomé & Combes 2003): single dish telescope observations in CO(1-0) and CO(2-1) emission lines have revealed the existence of large amounts of cold gas (up to ∼10 11 M ) in the central region of cooling flow clusters. We present here interferometric observations performed with the IRAM Plateau de Bure interferometer in Abell 1795. Comparison with IRAM 30 m data shows the cold gas detected is extended suggesting a cooling flow origin. The CO features identified are very similar to the structures observed in H α and with the star forming regions observed through UV continuum excess. A large fraction of the cold gas is not centered on the central cD, but located near brightest X-ray emitting regions along the North-West orientated radio lobe. The cold gas kinematics is consistent with the optical nebulosity behaviour in the very central region. It is not in rotation around the central cD: a velocity gradient shows the cold gas might be cooled gas from the intra-cluster medium being accreted by the central galaxy. The optical filaments, aligned with the cD orbit, are intimately related to the radio jets and lobes. The material fueling the star formation certainly comes from the deposited gas, cooling more efficiently along the edge of the radio lobes. Even if some heating mechanisms are present, these millimetric observations show that an effective cooling to very low temperatures indeed occurs and is probably accelerated by the presence of the radio source.

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Section: Abell 1795supporting

confidence: 68%

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

Salomé

Combes

2004

A&A

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“…Molecular gas in the cD galaxy has been detected through molecular hydrogen emission (Falcke et al 1998). Fabian et al (1994) observed in the core an X-ray filament that coincides with an H α emission Article published by EDP Sciences feature discovered by Cowie et al (1983). This filament is produced by cooling gas from the ICM, and could be significant in improving our understanding of the energy and ionization source of the optical nebulosity, so frequently found in cooling core clusters.…”

Section: Introductionmentioning

confidence: 91%

The parsec-scale properties of the radio galaxy 4C 26.42 in the dense cooling core cluster A1795

Liuzzo

Taylor

Giovannini

et al. 2009

A&A

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Aims. The aim of the present work is to study the radio emission on the parsec scale of 4C 26.42, the Brightest cluster galaxy in Abell 1795, in the framework of radiosources in a dense cool core cluster. Methods. We present Very Long Baseline Array (VLBA) observations at 1.6, 5, 8.4 and 22 GHz. We performed a spectral index and multiepoch analysis. Results. The source appears two-sided with a well defined and symmetric Z-structure at ∼5 mas from the core. The kiloparsec-scale morphology is similar to the parsec-scale structure, but reversed in PA, with symmetric 90 • bends at about 2 arcsec from the nuclear region. Comparing data obtained at 3 different epochs we derive a 3σ limit to the apparent proper motion of β a < 0.04. We suggest that the parsec-scale jets are sub-relativistic, in contrast with the high velocities found for most low-power radio galaxies. The origin of the unusual radio morphology remains a puzzle. We suggest that the identification of the parent galaxy with the central cD in a cooling cluster plays an important role in the properties and structure of the jets.

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“…Overall, the [O ii] emission has a very similar morphology to the blue continuum, suggesting that this gas may be photoionized by young stars. The presence of extended, filamentary [O ii] extending >30 kpc from the center of Phoenix A is reminiscent of the complex Hα filaments in nearby systems such as NGC 1275 (e.g., Conselice et al 2001;Fabian et al 2003;Hatch et al 2006) and Abell 1795 (Cowie et al 1983;McDonald & Veilleux 2009). Luminous, extended [O iii] emission is not, however, typically found in the central galaxies of cool core clusters.…”

Section: Optical Emission-line Mapsmentioning

confidence: 99%

The State of the Warm and Cold Gas in the Extreme Starburst at the Core of the Phoenix Galaxy Cluster (Spt-Clj2344-4243)

McDonald

Swinbank

Edge

et al. 2014

ApJ

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We present new optical integral field spectroscopy (Gemini South) and submillimeter spectroscopy (Submillimeter Array) of the central galaxy in the Phoenix cluster (SPT-CLJ2344-4243). This cluster was previously reported to have a massive starburst (∼800 M yr −1 ) in the central, brightest cluster galaxy, most likely fueled by the rapidly cooling intracluster medium. These new data reveal a complex emission-line nebula, extending for >30 kpc from the central galaxy, detected at [O ii]λλ3726, 3729, [O iii]λλ4959, 5007, Hβ, Hγ , Hδ, [Ne iii]λ3869, and He ii λ4686. The total Hα luminosity, assuming Hα/Hβ = 2.85, is L Hα = 7.6 ± 0.4 ×10 43 erg s −1 , making this the most luminous emission-line nebula detected in the center of a cool core cluster. Overall, the relative fluxes of the low-ionization lines (e.g., [O ii], Hβ) to the UV continuum are consistent with photoionization by young stars. In both the center of the galaxy and in a newly discovered highly ionized plume to the north of the galaxy, the ionization ratios are consistent with both shocks and active galactic nucleus (AGN) photoionization. We speculate that this extended plume may be a galactic wind, driven and partially photoionized by both the starburst and central AGN. Throughout the cluster we measure elevated high-ionization line ratios (e.g., He ii/Hβ, [O iii]/Hβ), coupled with an overall high-velocity width (FWHM 500 km s −1 ), suggesting that shocks are likely important throughout the interstellar medium of the central galaxy. These shocks are most likely driven by a combination of stellar winds from massive young stars, core-collapse supernovae, and the central AGN. In addition to the warm, ionized gas, we detect a substantial amount of cold, molecular gas via the CO(3-2) transition, coincident in position with the galaxy center. We infer a molecular gas mass of M H 2 = 2.2 ± 0.6 × 10 10 M , which implies that the starburst will consume its fuel in ∼30 Myr if it is not replenished. The L IR /M H 2 that we measure for this cluster is consistent with the starburst limit of 500 L /M , above which radiation pressure is able to disperse the cold reservoir. The combination of the high level of turbulence in the warm phase and the high L IR /M H 2 ratio suggests that this violent starburst may be in the process of quenching itself. We propose that phases of rapid star formation may be common in the cores of galaxy clusters, but so short-lived that their signatures are quickly erased and appear only in a subsample of the most strongly cooling clusters.

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Two-dimensional spectrophotometry of the cores of X-ray luminous clusters

Cited by 140 publications

References 0 publications

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

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

The parsec-scale properties of the radio galaxy 4C 26.42 in the dense cooling core cluster A1795

The State of the Warm and Cold Gas in the Extreme Starburst at the Core of the Phoenix Galaxy Cluster (Spt-Clj2344-4243)

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