Massive molecular gas flows and AGN feedback in galaxy ... · Molecular gas structure shaped by...
Transcript of Massive molecular gas flows and AGN feedback in galaxy ... · Molecular gas structure shaped by...
Massive molecular gas flows and AGN feedback in galaxy clusters
CO(3-2)
Helen Russell (Cambridge)Brian McNamara (Waterloo), Andy Fabian (Cambridge), Paul Nulsen (CfA),
Michael McDonald (MIT), Alastair Edge (Durham), Francoise Combes (Paris), Philippe Salomé (Paris), Jeremy Sanders (MPE) and the SPT collaboration
● Introduction
– Radiative cooling in galaxy clusters
– AGN feedback
● Results
– ALMA observations of molecular gas in central cluster galaxies
– Massive extended filaments, smooth velocity gradients
– AGN-driven gas outflows
– Direct uplift of molecular clouds or cooling in situ?
● Conclusions
Outline
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
Coo
ling
time
(Gyr
)
Chandra X-ray
100 kpc 100 kpc
Radius (kpc)
● 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(<r
cool) (1042 ergs-1)
Pca
v (10
42 e
rgs-1
)
Rafferty et al. 2006; Birzan et al. 2004; Fabian 2012
He
atin
g
Cooling
Chandra: energy output ALMA: fuelling?
● 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?
0.3”
0.5 kpc
● Massive filaments each ~ a few x 109 – 1010 M and 3 – 15 kpc long
Russell et al. 2016, submitted
PKS0745
Extended filaments of molecular gas
Phoenix
CO(3-2)
● 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
Low velocities and low dispersions
● Modest velocities ±100 km/s, narrow FWHM ~100 km/s
● Gas not settled in gravitational potential
Beam size: 0.3 arcsec, 0.5 kpc Russell et al. 2016
Velocity map Velocity dispersion
PKS0745:
PKS0745
Smooth velocity gradients along filaments
● Low velocities at small radii
● Highest velocities at largest radii
● Outflow?
A1795:
Highest velocities at largest radii
McNamara et al. 2014
A1835
● 1010 M molecular flow at 200-400 km/s extending to 10kpc
A1835:
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
CO(3-2)
Russell et al. submitted
Molecular gas not settled in the gravitational potential
● Massive filaments, low velocities → merger origin is unlikely
● Low velocities compared to stars → filaments not supported by rotation
● Highest velocities at large radii → outflow?
Fabian et al. 2003; Conselice et al. 2001; Lim et al. 2008; Salome et al. 2011
CO detections on Hα image
Perseus: Hα
Molecular gas filaments extend toward radio bubbles
0.3 arcsec
0.5 kpc
Sanders et al. 2014
Russell et al. 2016
● PKS0745: massive filaments drawn up underneath X-ray cavities and radio lobes
A1835 CO(1-0)
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
6.7 kpc
1.7 arcsec
X-ray cavities
McNamara et al. 2014
Phoenix cluster: filaments encase cavities
● Phoenix hosts a ~600 M /yr starburst and a 'transition' AGN bright in both X-ray/optical and radio
● 3 x 1010M of molecular gas total with half in filaments around radio bubbles
30 kpc
CO(3-2)
Russell et al. submitted
HST
McDonald + SPT collaboration 2012
cavitypositions
● Molecular gas structure shaped by radio bubble expansion
● Direct uplift of molecular gas clouds?
– Pcav ~ 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
Direct uplift of molecular gas clouds or cooling in situ?
Phoenix
PKS0745
Phoenix
● 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
Phoenix
PKS0745