An Enormous Molecular Gas Flow in the RX J0821+0752 Galaxy Cluster

Vantyghem, A. N.; McNamara, B. R.; Russell, H. R.; Edge, A. C.; Nulsen, P. E. J.; Combes, F.; Fabian, A. C.; McDonald, Michael; Salomé, P.

doi:10.3847/1538-4357/aaf1b4

Cited by 31 publications

(36 citation statements)

References 105 publications

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“…For all central galaxies in our sample (except RXJ 0821, see Vantyghem et al 2019), the continuum emission is unresolved and consistent with a nuclear point source. The measured sub-mm continuum fluxes are given in Table 4.…”

Section: Continuummentioning

confidence: 67%

“…Self-calibration was also employed to produce modest increases in continuum sensitivity for targets with continuum peaks greater than a few mJy. The continuum emission was due to nuclear point sources coincident with the AGN in all targets, except RXJ0821+0752 where the submm continuum is spatially extended and offset from the AGN ( Vantyghem et al 2019).…”

Section: Data Reductionmentioning

confidence: 96%

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Driving massive molecular gas flows in central cluster galaxies with AGN feedback

Russell

McNamara

Fabian

et al. 2019

Monthly Notices of the Royal Astronomical Society

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119

111

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We present an analysis of new and archival ALMA observations of molecular gas in twelve central cluster galaxies. We examine emerging trends in molecular filament morphology and gas velocities to understand their origins. Molecular gas masses in these systems span 10 9 − 10 11 M , far more than most gas-rich galaxies. ALMA images reveal a distribution of morphologies from filamentary to disk-dominated structures. Circumnuclear disks on kiloparsec scales appear rare. In most systems, half to nearly all of the molecular gas lies in filamentary structures with masses of a few ×10 8−10 M that extend radially several to several tens of kpc. In nearly all cases the molecular gas velocities lie far below stellar velocity dispersions, indicating youth, transience or both. Filament bulk velocities lie far below the galaxy's escape and free-fall speeds indicating they are bound and being decelerated. Most extended molecular filaments surround or lie beneath radio bubbles inflated by the central AGN. Smooth velocity gradients found along the filaments are consistent with gas flowing along streamlines surrounding these bubbles. Evidence suggests most of the molecular clouds formed from low entropy X-ray gas that became thermally unstable and cooled when lifted by the buoyant bubbles. Uplifted gas will stall and fall back to the galaxy in a circulating flow. The distribution in morphologies from filament to disk-dominated sources therefore implies slowly evolving molecular structures driven by the episodic activity of the AGN.

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Section: Continuummentioning

confidence: 67%

Section: Data Reductionmentioning

confidence: 96%

Driving massive molecular gas flows in central cluster galaxies with AGN feedback

Russell

McNamara

Fabian

et al. 2019

Monthly Notices of the Royal Astronomical Society

Self Cite

119

111

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“…Central cluster galaxies are known to have reservoirs of molecular gas that are detected through their CO line emission at low redshifts (e.g. Edge 2001;McNamara et al 2014;Temi et al 2018;Vantyghem et al 2019;Rose et al 2019) and at redshifts as high as z = 1.7 (Webb et al 2017). These molecular gas clouds are observed to have line of sight velocities of the order of ∼ 200 to 300 km s −1 , which would support a chaotic cold accretion type model in BCGs (e.g., David et al 2014;Tremblay et al 2016).…”

Section: Mergers Of Infalling Gas Rich Galaxies With Bcgmentioning

confidence: 90%

Constraining radio mode feedback in galaxy clusters with the cluster radio AGNs properties to z ∼ 1

Gupta

Pannella

Mohr

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We study the properties of the Sydney University Molonglo Sky Survey (SUMSS) 843 MHz radio active galactic nuclei (AGNs) population in galaxy clusters from two large catalogues created using the Dark Energy Survey (DES): ∼11 800 optically selected RM-Y3 and ∼1000 X-ray selected MARD-Y3 clusters. We show that cluster radio loud AGNs are highly concentrated around cluster centres to $z$ ∼ 1. We measure the halo occupation number for cluster radio AGNs above a threshold luminosity, finding that the number of radio AGNs per cluster increases with cluster halo mass as N ∝ M1.2 ± 0.1 (N ∝ M0.68 ± 0.34) for the RM-Y3 (MARD-Y3) sample. Together, these results indicate that radio mode feedback is favoured in more massive galaxy clusters. Using optical counterparts for these sources, we demonstrate weak redshift evolution in the host broad-band colours and the radio luminosity at fixed host galaxy stellar mass. We use the redshift evolution in radio luminosity to break the degeneracy between density and luminosity evolution scenarios in the redshift trend of the radio AGNs luminosity function (LF). The LF exhibits a redshift trend of the form (1 + $z$)γ in density and luminosity, respectively, of γD = 3.0 ± 0.4 and γP = 0.21 ± 0.15 in the RM-Y3 sample, and γD = 2.6 ± 0.7 and γP = 0.31 ± 0.15 in MARD-Y3. We discuss the physical drivers of radio mode feedback in cluster AGNs, and we use the cluster radio galaxy LF to estimate the average radio-mode feedback energy as a function of cluster mass and redshift and compare it to the core (<0.1R500) X-ray radiative losses for clusters at $z$ < 1.

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“…This was done by adding a number of clusters found recently to have cavities that are not present in the B08 sample, e.g. 4C+55.16 (Rafferty et al 2006), ZwCl 8276 (Ettori et al 2013), A2390 (Savini et al 2019), RX J0820.9+0752 (Vantyghem et al 2019), A1361, ZwCl 0235, RX J0352.9+1941, MS 0839.9+2938 (Shin et al 2016). We also included some cooling flow clusters that might harbor cavities and where significant H α emission is present (e.g.…”

Section: The Samplementioning

confidence: 99%

LOFAR observations of X-ray cavity systems

Bîrzan

Rafferty

Brüggen

et al. 2020

Monthly Notices of the Royal Astronomical Society

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ABSTRACT We present LOFAR observations at 120–168 MHz of 42 systems with possible X-ray cavities in their hot atmosphere, of which 17 are groups or ellipticals, 19 are nearby clusters (z < 0.3), and six are higher redshift clusters (z > 0.3). The X-ray cavities, formed by the radio lobes of the central active galactic nucleus (AGN), are evidence of radio-mode AGN feedback. In the groups and ellipticals sample, half of the systems have X-ray cavities for which no associated lobe emission was detected. Conversely, we report the discovery of large radio lobes in NGC 6338, extending far beyond the emission reported previously in the literature. In the case of the nearby clusters, our observations show that there is little low-frequency radio emission that extends beyond the cavities (e.g. MS 0735.6+7421, A2052). For the first time, we report secure cavity-radio associations in 2A 0335+096, ZwCl 2701, and ZwCl 8276 that strengthens their interpretation as AGN-created cavities. However, in some known cavity systems (e.g. A1795 and ZwCl 3146) we report the lack of detectable low-frequency radio emission associated with the cavities. Our sample of higher redshifts systems is small, and unfortunately the present LOFAR observations are not able to resolve the lobes in many of them. Nevertheless, our sample represents one of the best available for investigating the connection between radio and jet power in radio-mode AGN feedback.

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An Enormous Molecular Gas Flow in the RX J0821+0752 Galaxy Cluster

Cited by 31 publications

References 105 publications

Driving massive molecular gas flows in central cluster galaxies with AGN feedback

Driving massive molecular gas flows in central cluster galaxies with AGN feedback

Constraining radio mode feedback in galaxy clusters with the cluster radio AGNs properties to z ∼ 1

LOFAR observations of X-ray cavity systems

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