Molecular gas & AGN feedback in brightest cluster galaxies

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1 Molecular gas & AGN feedback in brightest cluster galaxies Helen Russell Brian McNamara Alastair Edge Robert Main Adrian Vantyghem Francoise Combes Andy Fabian Philippe Salomé

2 Outline Introduction Radiative cooling in galaxy clusters AGN feedback Results ALMA Early Science observations of molecular gas in central cluster galaxies AGN-driven gas outflows, ordered motion, extended filaments,... Future work

3 Radiative cooling in cluster cores X-ray surface brightness: Optical Chandra X-ray BCG 100 kpc 100 kpc Lewis et al. 2003, Allen et al Credit: S. Allen + A. Fabian M per year cooling?

4 Cavity heating Searches for vast reservoir of molecular gas find less than 10% of that expected (Edge '01, Salome + Combes '03) AGN heating replaces radiative losses Optical, X-ray, Radio 200 kpc 20 kpc MS0735, McNamara et al Hydra A, Kirkpatrick et al. 2009

5 Radio bubble heating is sufficient to offset radiative cooling Heating appears coupled to the cooling rate Heating Pcav (1042 ergs-1) Heating + cooling balance feedback LX(<rcool) (1042 ergs-1) Cooling Rafferty et al. 2006; Birzan et al. 2004; Fabian 2012

6 How is AGN feedback fuelled? Chandra: energy output ALMA: fuel input? Origin of molecular gas in BCGs? Is molecular gas fuelling feedback? Does radio/mechanical feedback operate on molecular 6 clouds?

7 AGN-driven gas outflows Radiation and jet-driven ionised and molecular gas winds Mrk231: molecular outflow 5 x 108 M with velocities up to 750 km/s extending to a few kpc NGC1433: radio jets Mrk231: quasar CO(1-0) Outflow 7 Morganti et al. 2005; Feruglio et al. 2010; Rupke & Veilleux 2011; Maiolino et al. 2012; Combes et al. 2013

8 ALMA Early Science Extreme X-ray cooling rates, radiative cooling times < 1Gyr Single dish observations: molecular gas ~1010M Mergers unlikely gas cooling from X-ray atmosphere A1664 z = 0.13 A1835 z = 0.25 HST observations: O'Dea et al. 2010, CO observations: Edge 2001, Salomé & Combes 2003

9 A1835, 70 min Intensity (mk) 30m IRAM CO(1-0) total spectra A1664, 60 min Edge 2001 Intensity (mk) Velocity (km/s) Velocity (km/s)

10 ALMA CO(1-0) total spectra A1835: 60 min, 20 antennas M(H2) = 5 x 1010 M A1664: 50 min, 16 antennas M(H2) = x 109 M

11 A1664 CO(1-0) Component at BCG systemic (red) + high velocity filament at -600km/s (blue) 3 kpc 3kpc Integrated CO(1-0) intensity Nucleus

12 A1664 CO(1-0): Ordered Motion Nucleus Rotating disk of molecular gas around AGN?

13 A1835 CO(1-0): Molecular flow Lack of high velocity gas towards nucleus

14 A1835 X-ray Cavities Molecular outflow directed toward the X-ray cavities Gas velocity similar to buoyant bubble velocity CO(1-0) 6kpc

15 A1835 X-ray Cavities Gas filaments drawn up around radio bubble Interaction with cold gas in radio-mode feedback A1835 CO(3-2) 2kpc

16 A1835 CO(1-0): Molecular flow Mmol = 1010M outflow of gas to 10 kpc at km/s Energy requirements of outflow PK = 1043erg/s What can drive the gas out?

17 A1835 CO(1-0): Molecular flow Mmol = 1010M outflow of gas at km/s Energy requirements of outflow PK = 1043erg/s What can drive the gas out? Radiation pressure from young stars Luminosity too low by 3 orders of magnitude Supernovae 1043 erg/s, would need 100% coupling Radio bubbles 1045 erg/s!

18 Radio jet-driven outflows Molecular gas lifted with hot gas in updraft Hα emission (104 K) But how can radio bubbles lift dense molecular gas? X-ray image Fabian et al. 2003, 2011; Hatch et al. 2006

19 Radio jet-driven outflows Molecular gas lifted with hot gas in updraft Hα emission (104 K) But how can radio bubbles lift dense molecular gas? AGN heating couples to both volume-filling X-ray gas and cold, dense molecular gas clouds Radio jet outbursts drive molecular gas out of galaxies 'red and dead' ellipticals X-ray image Fabian et al. 2003, 2011; Hatch et al. 2006

20 Conclusions X-ray cavities provide a measure of the mechanical power of radio jets launched by a SMBH Radio jet heating is energetically sufficient to balance radiative cooling in cluster cores Preliminary ALMA results very exciting: Molecular gas strongly centrally condensed Ordered motion about nucleus fuelling? High velocity filament outflows Radio bubble interaction in A1835 dragging molecular gas outward Much more to follow!

21

22 ALMA Cycle 1 2A0335 (z=0.03) and PKS0745 (z=0.1) X-ray X-ray Hα R, Hα Similar molecular gas masses Jet power and Hα luminosity very different

23 Radiative cooling in cluster cores X-ray + optical images of Abell 2029 Lewis et al. 2003, Allen et al M per year cooling? Voigt & Fabian 2004

24 Quasar mode outflows Radiation-driven ionised and molecular gas winds Archetype Mrk231: molecular outflow 5 x 108 M with velocities up to 750 km/s extending to a few kpc Mrk231 J z=6.4 CO(1-0) [CII] 158µm Wind 24 Morganti et al. 2005; Feruglio et al. 2010; Rupke & Veilleux 2011 Maiolino et al. 2012

25 Massive molecular gas flows Two more BCG pathfinder observations in Cycle 1! Priority for future cycles is to build up a sample of BCGs: Do inflows of molecular gas fuel SMBH activity? Can radio jet outbursts sweep the galaxy of the remaining gas to suppress cooling and star formation? Atacama Large Millimeter Array (ALMA)

26 Cavity heating Hydra A, Kirkpatrick et al MS0735, McNamara et al Perseus Fabian et al. 2008

27 A1664 CO(3-2): -600km/s filament Possible disk at BCG systemic (red) but also high velocity component at -600km/s (blue) 1.3kpc

28 Cold gas flows in central galaxies How is the SMBH coupled to the cluster atmosphere? Where does the molecular gas originate? Is molecular gas fuelling the SMBH? Does radio/mechanical feedback operate on molecular clouds? Role of star formation in regulating the SMBH growth? Atacama Large Millimeter Array (ALMA)

29 A1664 CO(3-2): -600km/s outflow High velocity clouds in front of galaxy Optical Buried star formation dusty disk

30 Massive molecular gas flows Commissioning will be complete by December 2013 (Cycle 2) Two more BCG pathfinder observations in Cycle 1! Sixty 12m radio dishes Baselines up to 16km ALMA compact array Frequencies in the range 84 to 720GHz

31 A1664 CO(3-2): -600km/s filament Broad velocity dispersion for each clump No clear velocity gradient

32 Alma a feedback loop? Abell 1664 Hα Lyα Abell 1835 Rband Lyα

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