Massive molecular gas flows and AGN feedback in galaxy...
Transcript of Massive molecular gas flows and AGN feedback in galaxy...
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Helen Russell (Cambridge)Brian McNamara (Waterloo), Andy Fabian (Cambridge), Paul Nulsen (CfA),
Michael McDonald (MIT), Alastair Edge (Durham), Francoise Combes (Paris), Philippe Salomé (Paris), the SPT collaboration et al.
Massive molecular gas flows and AGN feedback in galaxy clusters
Image credit: ALMA (ESO/NAOJ/NRAO) H.Russell, et al.; NASA/ESA Hubble; NASA/CXC/MIT/M.McDonald et al.; B. Saxton (NRAO/AUI/NSF)
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• Introduction
• Radiative cooling in galaxy clusters
• AGN feedback
• Results
• ALMA observations of molecular gas in central cluster galaxies
• Massive filaments drawn up around radio bubbles
• Direct uplift of molecular clouds or cooling in situ?
• Closely coupled feedback
• Prospects for Lynx
• Conclusions
Outline
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X-ray surface brightness peaks in cluster cores
Lewis et al. 2003, Allen et al. 2004
• 100 – 1000 M⊙ per year gas cooling?
X-ray radiative cooling time
Voigt & Fabian 2004
Optical
Coolin
g t
ime (
Gyr)
Chandra X-ray
100 kpc 100 kpc
Radius (kpc)
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• Searches for vast reservoir of molecular gas find less than 10% of that expected
(Edge '01, Salomé + Combes '03) → residual cooling
• AGN heating replaces radiative losses → feedback loop
• Truncates galaxy growth, keeps ellipticals ‘red and dead’, M-σ relation
MS0735, McNamara et al. 2005
200 kpc
Optical, X-ray, Radio
Radio jets heat cluster gas
LX(<rcool) (1042 ergs-1)
Pcav
(10
42
erg
s-1
)
Rafferty et al. 2006; Birzan et al. 2004; Fabian 2012
He
atin
g
Cooling
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• Origin of molecular gas in BCGs?
• Is molecular gas fuelling feedback?
• Does radio-jet feedback operate on molecular clouds?
• BCGs in cool core clusters are rich in molecular gas(Edge 2001, Salomé & Combes 2003)
What is the role of molecular gas in feedback?
CO detections on Hα image
Perseus: Hα
Fabian et al. 2003; Conselice et al. 2001;Lim et al. 2008; Salome et al. 2011
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• Origin of molecular gas in BCGs?
• Is molecular gas fuelling feedback?
• Does radio-jet feedback operate on molecular clouds?
• BCGs in cool core clusters are rich in molecular gas(Edge 2001, Salomé & Combes 2003)
What is the role of molecular gas in feedback?
Chandra/Lynx: hot gas, energy output ALMA: cold gas, fuelling?
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ALMA capabilities
Credit: ESO
• 50 x 12m antennas in the 12m Array plus 12 x 7m and 4 x 12m antennas in the ACA
• Range of configurations with baselines up to 16km (0.013” at 300GHz)
• Receiver bands cover 84 to 950GHz in atmospheric windows
• ALMA will image CO in MW-like galaxies out to
z=3 and [CII] or dust continuum in moderate
starburst galaxies to epoch of reionization
• Dynamical black hole masses eg. NGC1332
6.6±0.6 x 108 M⊙Barth et al. 2016
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0.3”
0.5 kpc
• Massive filaments each ~ a few x 109
– 1010
M⊙ and 3 – 15 kpc long
Russell et al. 2016, 2017, submitted
PKS0745
Extended filaments of molecular gas
CO(2-1)
Phoenix
CO(3-2)
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Low velocities and low dispersions
• Modest velocities ±100 km/s, narrow FWHM ~100 km/s
• Gas not settled in gravitational potential
• Merger origin unlikely
Russell et al. 2016
Velocity map Velocity dispersion
PKS0745
PKS0745:
Beam: 0.3”, 0.5 kpc
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Smooth velocity gradients along filaments
A1795:
Velocity map Velocity dispersion
Beam size: 0.7 arcsec, 0.8 kpc
• Smooth gradient 0km/s to -370km/s
• Low FWHM ~100km/s
Russell et al. submitted
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• A1795: molecular gas 2.5 x 109
M⊙ around N radio lobe
• Smooth velocity gradient from 0 to -370 km/s
Integrated CO(2-1) intensity Jy.km/s Line of sight velocity (km/s)
Russell et al. submitted
Radio lobes
Molecular gas
Molecular gas filaments encase radio bubbles
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Molecular gas filaments encase radio bubbles
• Phoenix: filaments encase lower half of radio bubbles
• 3 x 1010M⊙ of molecular gas total with half in filaments around radio
bubbles
30 kpc
CO(3-2)
Russell et al. 2017
HST
McDonald + SPT collaboration 2012
cavitypositions
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Molecular gas filaments extend toward radio bubbles
Sanders et al. 2014Russell et al. 2016
• PKS0745 + A1835: filaments drawn up underneath X-ray cavities and
radio lobes
2kpc
X-ray cavities
PKS0745
A1835
McNamara et al. 2014
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Direct uplift of molecular gas clouds or cooling in situ?
Integrated CO(2-1) intensity Jy.km/s
A1795
Phoenix
PKS0745• Direct uplift of molecular gas clouds?
• Pmech ~ 1043-45
erg/s
• High coupling efficiency required
• Rapid cooling of uplifted thermally unstable
low entropy gas?
• Molecular gas coincident with soft X-ray
• Dust lanes
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Direct uplift of molecular gas clouds or cooling in situ?
Integrated CO(2-1) intensity Jy.km/s
A1795
Phoenix
PKS0745• Direct uplift of molecular gas clouds?
• Pmech ~ 1043-45
erg/s
• High coupling efficiency required
• Rapid cooling of uplifted thermally unstable
low entropy gas?
• Molecular gas coincident with soft X-ray
• Dust lanes
• But molecular gas mass divided by buoyancy time exceeds XMM-RGS limits
• XCO factor too large? Factor of two possible (Vantyghem et al. submitted)
• Gas cools over multiple AGN outbursts
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A closely coupled feedback loop
log(temperature/K)Revaz et al. 2008
Sanders et al. 2014
PKS0745
• Rising bubbles that heat X-ray atmospheres simultaneously promote
cooling in their wakes (stimulated feedback, McNamara et al. 2016)
• Inflows fuelling subsequent AGN outbursts?
Bubble simulation
Russell et al. 2016
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Phoenix cluster: ordered gas flow to centre
• Smooth velocity gradients and low FWHM in filaments
• Velocity gradient across nucleus with much higher FWHM
• Velocities too low for free fall in gravitational potential
Russell et al. 2017
CO(3-2)
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Molecular gas disks on few kpc scales
• Additional velocity component close to the BCG systemic velocity with smooth
gradient across the nucleus
3 kpc
Integrated CO(1-0)
Nucle
us
Phoenix
A1664
Russell et al. 2014, 2017
HST
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• CO(2-1) absorption features with ~5km/s linewidth typical of GMC and
infalling velocity 250-350 km/s
David et al. 2014
NGC5044 + A2597: absorption features
NGC5044
Flu
x (
mJy)
Velocity (km/s)
Tremblay et al. 2016
A2597
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Lynx science
• Hitomi results for Perseus: X-ray velocity gradient matches that along
Hα/CO filaments
• Dissipation and distribution of jet energy over large scales
• Regulation of gas cooling and AGN fuelling
• Detection of cavities, soft X-ray filaments, complex structure
• Jet power, gas velocities, X-ray cooling rates
Abell 1795
100ks observation
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Lynx science
• Hitomi results for Perseus: X-ray velocity gradient matches that along
Hα/CO filaments
• Dissipation and distribution of jet energy over large scales
• Regulation of gas cooling and AGN fuelling
• Detection of cavities, soft X-ray filaments, complex structure
• Jet power, gas velocities, X-ray cooling rates
Abell 1795
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• Molecular gas structure shaped by radio bubble expansion
• Massive 109-1010M⊙ filaments drawn up around and beneath radio bubbles
Conclusions
• Molecular emission lines are narrow
• Extended filaments, ordered velocity structure
• Gas not settled in gravitational potential
• Circulation flow
• Radio bubbles supply large-scale heating to stabilise cluster atmospheres and lift gas in their wakes
• Long-lived feedback loop
Phoenix
PKS0745
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Highest velocities at largest radii
McNamara et al. 2014
A1835
●1010
M molecular flow at 200-400 km/s extending to 10kpc
A1835:
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A1835 CO(3-2)
2kpc
●Gas filaments drawn up around radio bubble
●Interaction with cold gas in radio-mode feedback
A1835: gas flow drawn up around the X-ray cavities
McNamara et al. 2014
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●CO(2-1) absorption features with ~ 5 km/s linewidth typical of GMC and
infalling velocity 250-350 km/s
David et al. 2014
Filaments consist of many GMCs
NGC5044
Flu
x (m
Jy)
Velocity (km/s)Tremblay et al. 2016
A2597