Radio Jets Clearing the Way Through a Galaxy: Watching Feedback in Action

Morganti, Raffaella; Fogasy, Judit; Paragi, Z.; Oosterloo, Thomas; Orienti, M.

doi:10.1126/science.1240436

Cited by 205 publications

(239 citation statements)

References 28 publications

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“…The molecular gas filaments could therefore have formed from warmer gas that was uplifted by the radio bubble and cooled locally (Churazov et al 2001;Li & Bryan 2014). Rapid cooling of shock-heated outflowing gas to form molecules on short timescales has been suggested to explain the molecular gas kinematics in IC 5063 and 4C 12.50 (Morganti et al 2013;Tadhunter et al 2014;Zubovas & King 2014;Morganti et al 2015). Fig.…”

Section: Forming Molecular Gas In Extended Filamentsmentioning

confidence: 98%

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.

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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Section: Forming Molecular Gas In Extended Filamentsmentioning

confidence: 98%

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.

105

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“…This theoretical picture has been supported by numerous observations. The strongest evidence comes from the brightest cluster galaxies (BCGs) of cool core clusters, whose powerful radio jets have swept out cavities in the intracluster medium (ICM; Rosner & Tucker 1989;Allen et al 2001;McNamara & Nulsen 2007), while in some individual galaxies, energy transportation into the ISM via AGN-driven outflows is observed to remove gas from the central regions of the galaxy (Crenshaw et al 2003;Nesvadba et al 2007;Alexander et al 2010;Morganti et al 2013). All these show the negative effect of AGN feedback by removing/heating up the gas and eventually suppressing the star formation and regulating the galaxy growth.…”

Section: Introductionmentioning

confidence: 99%

Constraints on Feedback in the Local Universe: The Relation Between Star Formation and Agn Activity in Early-Type Galaxies

Vaddi

O’Dea

Baum

et al. 2016

ApJ

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We address the relation between star formation and active galactic nucleus (AGN) activity in a sample of 231 nearby (0.0002 < z < 0.0358) early-type galaxies by carrying out a multi-wavelength study using archival observations in the UV, IR, and radio. Our results indicate that early-type galaxies in the current epoch are rarely powerful AGNs, with P 10 WHz 22 1 < -for a majority of the galaxies. Only massive galaxies are capable of hosting powerful radio sources while less massive galaxies are hosts to lower radio power sources. Evidence of ongoing star formation is seen in approximately 7% of the sample. The star formation rate (SFR) of these galaxies is less than 0.1 M e yr −1 . They also tend to be radio faint (P 10 WHzThere is a nearly equal fraction of star-forming galaxies in radio faint (P 10 WHz 22 1 < -) and radio bright galaxies (P 10 WHz 22 1  -) suggesting that both star formation and radio mode feedback are constrained to be very low in our sample. We notice that our galaxy sample and the Brightest Cluster Galaxies follow similar trends in radio power versus SFR. This may be produced if both radio power and SFR are related to stellar mass.

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“…Nesvadba et al 2008Nesvadba et al , 2011Alexander et al 2010;Rupke & Veilleux 2011;Sturm et al 2011;Morganti et al 2013;Nyland et al 2013). Perhaps the strongest evidence for AGN feedback comes from the central galaxies of clusters, which are surrounded by hot gas with short cooling times (Fabian 1994).…”

Section: Introductionmentioning

confidence: 99%

The triggering of local AGN and their role in regulating star formation

Kaviraj

Shabala

Deller

et al. 2015

Mon. Not. R. Astron. Soc.

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We explore the processes that trigger local AGN and the role of these AGN in regulating star formation, using ∼550 nearby galaxies observed by the mJy Imaging VLBA Exploration at 20 cm (mJIVE) survey. The 10 7 K brightness temperature required for an mJIVE detection cannot be achieved via star formation alone, allowing us to unambiguously detect nearby radio AGN and study their role in galaxy evolution. Radio AGN are an order of magnitude more common in early-type galaxies (ETGs) than in their late-type counterparts. The VLBI-detected ETGs in this study have a similar stellar mass distribution to their undetected counterparts, are typically not the central galaxies of clusters and exhibit merger fractions that are significantly higher than in the average ETG. This suggests that these radio AGN (which have VLBI luminosities >10 22 W Hz −1 ) are primarily fuelled by mergers, and not by internal stellar mass-loss or cooling flows. Our radio AGN are a factor of ∼3 times more likely to reside in the UV-optical red sequence than the average ETG. Furthermore, typical AGN lifetimes (a few 10 7 yr) are much shorter than the transit times from blue cloud to red sequence (∼1.5 Gyr). This indicates that nearby (merger-triggered) AGN appear several dynamical time-scales into the associated star formation episode. This implies that such AGN typically couple only to residual gas, at a point where star formation has already declined significantly, and are, therefore, unlikely to play a significant role in regulating the star formation episode.

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Radio Jets Clearing the Way Through a Galaxy: Watching Feedback in Action

Cited by 205 publications

References 28 publications

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

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

Constraints on Feedback in the Local Universe: The Relation Between Star Formation and Agn Activity in Early-Type Galaxies

The triggering of local AGN and their role in regulating star formation

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