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

Russell, H. R.; McNamara, B. R.; Fabian, A. C.; Nulsen, P. E. J.; Edge, A. C.; Combes, F.; Murray, Norman; Parrish, Ian J.; Salomé, P.; Sanders, J. S.; Baum, Stefi A.; Donahue, M.; Main, Robert; O’Connell, R. W.; O’Dea, C. P.; Oonk, J. B. R.; Tremblay, G. R.; Vantyghem, A. N.; Voit, G. Mark

doi:10.1093/mnras/stw409

Cited by 85 publications

(123 citation statements)

References 114 publications

(199 reference statements)

Supporting

Mentioning

107

Contrasting

Order By: Relevance

“…In the Perseus cluster, the velocity structure of the Hα-emitting filaments, which are coincident with detections of CO emission from the IRAM 30 m telescope, traces streamlines underneath a buoyantly rising radio bubble (Salomé et al 2006(Salomé et al , 2011. ALMA observations of molecular gas at the centers of clusters (David et al 2014;McNamara et al 2014;Russell et al 2014Russell et al , 2016Tremblay et al 2016;Vantyghem et al 2016) have shown cold gas filaments extending along the trajectories of radio bubbles. The molecular clouds have either been lifted directly by the bubbles or cooled in situ from warmer, thermally unstable gas lifted in their wakes.…”

Section: Introductionsupporting

confidence: 62%

“…These observations now clearly demonstrate that the structure of the largest molecular gas reservoirs located in the most massive galaxies is shaped by the expansion and trajectory of the radio bubbles. Previous sub-mm observations of brightest cluster galaxies have indicated tentative correlations between X-ray cavity axes and the orientations of molecular gas filaments, including ALMA observations of Abell 1835 and PKS 0745-191 (McNamara et al 2014;Russell et al 2016). IRAM observations of the nearby Perseus cluster detected molecular gas coincident with regions of the complex optical emission line nebula, including several filaments of ionized gas that extend toward radio bubbles (Salomé et al 2006(Salomé et al , 2011Lim et al 2008).…”

Section: Discussionmentioning

confidence: 94%

See 1 more Smart Citation

Alma Observations of Massive Molecular Gas Filaments Encasing Radio Bubbles in the Phoenix Cluster

Russell

McDonald

McNamara

et al. 2017

ApJ

Self Cite

102

View full text Add to dashboard Cite

We report new ALMA observations of the CO(3-2) line emission from the  ´M 2.1 0.3 10 10 molecular gas reservoir in the central galaxy of the Phoenix cluster. The cold molecular gas is fueling a vigorous starburst at a rate of - -M 500 800 yr 1 and powerful black hole activity in the forms of both intense quasar radiation and radio jets. The radio jets have inflated huge bubbles filled with relativistic plasma into the hot, X-ray atmospheres surrounding the host galaxy. The ALMA observations show that extended filaments of molecular gas, each -10 20 kpc long with a mass of several billion solar masses, are located along the peripheries of the radio bubbles. The smooth velocity gradients and narrow line widths along each filament reveal massive, ordered molecular gas flows around each bubble, which are inconsistent with gravitational free-fall. The molecular clouds have been lifted directly by the radio bubbles, or formed via thermal instabilities induced in low-entropy gas lifted in the updraft of the bubbles. These new data provide compelling evidence for close coupling between the radio bubbles and the cold gas, which is essential to explain the self-regulation of feedback. The very feedback mechanism that heats hot atmospheres and suppresses star formation may also paradoxically stimulate production of the cold gas required to sustain feedback in massive galaxies.

show abstract

Section: Introductionsupporting

confidence: 62%

Section: Discussionmentioning

confidence: 94%

Alma Observations of Massive Molecular Gas Filaments Encasing Radio Bubbles in the Phoenix Cluster

Russell

McDonald

McNamara

et al. 2017

ApJ

Self Cite

102

View full text Add to dashboard Cite

show abstract

“…It is interesting to compare our results with a study of the molecular gas in PKS 0745-191 by Russell et al (2016). Even though NGC 5044 is a group and PKS 0745-191 is a massive cluster, the central dominant galaxies in these two systems have very similar gravitating masses of ∼ 2×10 14 M within 30 kpc (David et al 2009;Sanders et al 2014).…”

Section: Multiphase Gas In the X-ray And Hα Filamentsmentioning

confidence: 78%

The Presence of Thermally Unstable X-Ray Filaments and the Production of Cold Gas in the NGC 5044 Group

David

Vrtilek

O’Sullivan

et al. 2017

ApJ

View full text Add to dashboard Cite

We present the results of a deep Chandra observation of the X-ray bright, moderate cooling flow group NGC 5044 along with the observed correlations between the ionized, atomic, and molecular gas in this system. The Chandra observation shows that the central AGN has undergone two outbursts in the past 10 8 years, based on the presence of two pairs of nearly bipolar X-ray cavities. The molecular gas and dust within the central 2 kpc is aligned with the orientation of the inner pair of bipolar X-ray cavities, suggesting that the most recent AGN outburst had a dynamical impact on the molecular gas. NGC 5044 also hosts many X-ray filaments within the central 8 kpc, but there are no obvious connections between the X-ray and Hα filaments and the more extended X-ray cavities that were inflated during the prior AGN outburst. Using the linewidth of the blended Fe-L line complex as a diagnostic for multiphase gas, we find that the majority of the multiphase, thermally unstable gas in NGC 5044 is confined within the X-ray filaments. While the cooling time and entropy of the gas within the X-ray filaments are very similar, not all filaments show evidence of gas cooling or an association with Hα emission. We suggest that the various observed properties of the X-ray filaments are suggestive of an evolutionary sequence where thermally unstable gas begins to cool, becomes multiphased, develops Hα emitting plasma, and finally produces cold gas.

show abstract

“…The single phase ICM Molecular cold gas has been detected in a growing number of cool-core clusters (David et al 2014;Russell et al, 2014Russell et al, , 2016McNamara et al 2014;Edge & Frayer 2003). This is generally believed to be the product of thermally unstable cooling from the hot ICM (McCourt et al 2012;, although other sources, such as merger debris from gas-rich galaxies cannot be ruled out.…”

Section: Uplift Of Cluster Gas By Radio Lobesmentioning

confidence: 99%

Buoyant AGN Bubbles in the Quasi-isothermal Potential of NGC 1399

Nulsen

Kraft

et al. 2017

ApJ

View full text Add to dashboard Cite

The Fornax Cluster is a low-mass cool-core galaxy cluster. We present a deep Chandra study of NGC 1399, the central dominant elliptical galaxy of Fornax. The cluster center harbors two symmetric X-ray cavities coincident with a pair of radio lobes fed by two collimated jets along a north-south axis. A temperature map reveals that the AGN outburst has created a channel filled with cooler gas out to a radius of 10 kpc. The cavities are surrounded by cool bright rims and filaments that may have been lifted from smaller radii by the buoyant bubbles. X-ray imaging suggests a potential ghost bubble of 5 kpc diameter to the northwest. We find that the amount of gas lifted by AGN bubbles is comparable to that which would otherwise cool, demonstrating that AGN driven outflow is effective in offsetting cooling in low-mass clusters. The cluster cooling time scale is > 30 times longer than the dynamical time scale, which is consistent with the lack of cold molecular gas at the cluster center. The X-ray hydrostatic mass is consistent within 10% with the total mass derived from the optical data. The observed entropy profile rises linearly, following a steeper slope than that observed at the centers of massive clusters; gas shed by stars in NGC 1399 may be incorporated in the hot phase. However, it is far-fetched for supernova-driven outflow to produce and maintain the thermal distribution in NGC 1399 and it is in tension with the metal content in the hot gas.

show abstract

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

Cited by 85 publications

References 114 publications

Alma Observations of Massive Molecular Gas Filaments Encasing Radio Bubbles in the Phoenix Cluster

Alma Observations of Massive Molecular Gas Filaments Encasing Radio Bubbles in the Phoenix Cluster

The Presence of Thermally Unstable X-Ray Filaments and the Production of Cold Gas in the NGC 5044 Group

Buoyant AGN Bubbles in the Quasi-isothermal Potential of NGC 1399

Contact Info

Product

Resources

About