AGN fueling and feedback Franoise Combes Observatoire de Paris 1 - PowerPoint PPT Presentation

Star formation, AGN fueling and feedback Françoise Combes Observatoire de Paris 1 M82 Seoul, October 2013 N1433

Outline 1- Gas distribution and Star Formation Star formation law is a molecular gas law 2- Star formation modes; main sequence, Starburst, mergers? 3- Modes of Quenching: SF and AGN feedback M51, CO IRAM-PdB 2 Schinnerer et al 2013

Atomic hydrogen HI-21cm 3

Molecular gas from CO(2-1) 4 Leroy et al 2013

Molecular gas and Star formation Bigiel et al 2009 H 2 forms stars at a constant efficiency (n=1) Time-scale for SF 2 10 9 yrs At sub-kpc scale S SFR SFR not strongly Correlated with HI H 2 when > 9 Mopc -2 S gas 5

Essential role of H2 S SFR S SFR S HI S H2 Bigiel et al 2008 Average over 7 galaxies Confirmed with 38 galaxies, Heracles, Things Leroy et al 2013 6

Even in low surface density Schruba et al 2011 7

Disk simulations with H2/HI a fb energy fraction for SN feedback c UV radiation field 100 Myr -- a fb= 40% c x 500 UV factor H2 formation enhances the SFR Then the feedback expels gas  Thicker gas disk 8 Halle & Combes 2013

Disk simulations with H2/HI 9 Halle & Combes 2013

Star formation with H2 Without H2 With H2, a fb=1% 10 Halle & Combes 2013

Evidence of molecular thick disk ? 50% of diffuse gas, M51, Pety et al 2013 11 More direct in edge-on galaxies, like NGC891 , Garcia-Burillo et al 1992

Depletion time lower towards the center The star formation efficiency is larger in the galaxy centers Leroy et al 2013 12

The depletion time is lower at high redshift Galaxy centers are more starbursting Even in main-sequence galaxies SF time-scale shorter  not only in starburst Daddi et al 2010, Genzel et al 2010 13

2- Star formation modes: main sequence, starburst ? sSFR Specific SFR/M Inverse of growth time Change of the SSFR? Bouwens et al 2012 HUDF + CLASH 14

Main sequence, Major mergers Wuyts et al 2011 80 Galaxies, z=2 M*> 10 10 Mo During mergers, still gas accretion May be 15% due to mergers? Kaviraj et al 2013 15

PHIBSS: 52 galaxies Molecular gas at IRAM, at z~2.3 and at z~1.2 High detection rate >85%, in these « normal » massive Star Forming Galaxies (SFG) Quiescent SF, in the main sequence Gas content ~34% and 44% in average at z=1.2 and 2.3 resp. 0.8 (1+z) 2.7 SFR proportional to M * 16 Tacconi et al 2010, 2013

EGS13003805 z=1.23 CO: v c =250 km/s (i~57 0 ), R 1/2 =3.3 kpc (R d (I)= 6.3), f gas =0.46 1” (8.46 kpc) CO 3-2 - log I – log V log I - CO red – CO blue log I – log V 4 EGS13003805 300 km/s 3 CO 3-2 line intensity (mJy) 2 1 0 0.5” -1 -1000 -500 0 500 1000 velocity offset (km/s)

Evolution of specific SFR tdep=1.5/(1+z) Gyr Comparison with COLDGASS at z=0 Green: optical surveys 18

Starbursts 0.2 < z < 1 SFR/Mgas Mgas/M* Star formation efficiency and gas fraction sSFR=SFExMg/M * <z=1>/<z=0> 2.1 and 3.8 (with upper limits) 3.2 and 2.5 Both contribute, factor 3+1 increase between z=0 and 1 SF efficiency should also be increased due to more violent dynamics 19 Combes et al 2013

Perseus A 3- SF & AGN feedback Mrk 231, SF and AGN AGN and also nuclear starburst, 700 Mo/yr, >> ionised gas Cooling flow clusters: Inflow and outflow coexist The cooled gas fuels the AGN The molecular gas coming from previous cooling is dragged out by the AGN feedback 20 Ferruglio et al 2010 Salome et al 2008

Feedback in nuclei: H2 & CO 6 out of 300 systems searched show H 2 outflows 4C12.50 SFR ~400-1000 Mo/yr Outflow ~130 Mo/yr 21 Dasyra & Combes 2011, 2012

Molecular outflows are massive Aalto et al 2012 Some outflows are more massive then N1377 their dense nuclear disk, e.g. N1377 200pc extent with modest 140km/s M out = 1-5 10 7 M o , disk mass ~2 10 7 M o Outflows due to SN: M82, Mout ~ 510 7 M o V~200km/s (Nakai et al 1987) N3256 merger, Mout ~ 10 7 M o 10 Mo/yr, V~420km/s (Sakamoto et al 2006) Arp220, Pcygni profiles 100pc, HCO+, Mout ~ 10 8 M o (Sakamoto et al 2009) More violent outflows due to AGN: V> 1000km/s, up to 1200 Mo/yr OH, H 2 O abs Herschel, Sturm et al (2011), ULIRG+AGN Mrk231 (Feruglio+ 2010) 700 Mo/yr, depleted in 10 7 yrs, Mout ~ 10 8 M o N1266 (Alatalo et al 2011) Mout ~ 2 10 7 M o , depleted in ~10 8 yrs 22

Fueling in low-luminosity AGN NGC 1433: barred spiral, the « Lord of the Rings » Buta et al 2001 Atomic gas only in the inner and outer ring (Ryder et al 1996) CO in the nuclear ring and disk (Bajaja et al 1995) CO(3-2) with ALMA (Cycle 0)  CO does not follow the nuclear bar 23

The Seyfert 2 NGC 1433 CO(3-2) map with ALMA, No HCN, HCO+(4-3) Beam = 0.5’’ = 24pc Discovery of an inner ILR at r=200pc + Molecular torus? 24pc size, dust cont. 24 Combes et al 2013

The smallest molecular outflow PV major axis Flow of 50pc size CO on HST PV minor axis 25 CO on unsharp masked HST image

Properties of the outflow Total MH2= 5.2 10 7 Mo in FOV=18’’ MH2= 1.8 10 8 Mo in beam 43’’ (Bajaja et al 1995) Blue and red-shifted outflows, with 100km/s (200km/s if in the plane) 2’’=50pc from the center, Total 7% of the mass = 3.6 10 6 Mo SFR = 0.2 Mo/yr dM/dt ∼ (Mv/d) tan α= 7 tan α M ⊙ /yr,  ~40 SFR α = angle of outflow/line of sight L kin =0.5 dM/dt v 2 =2.3 tan α (1+ tan2 α) 10 40 erg/s L bol (AGN)= 1.3 10 43 erg/s Flow momentum >> L AGN /c  Jet driven flow , P jet = 2 10 42 erg/s from radio 26

Other low-luminosity AGN flows Driven by both the starburst and the radio jets The LINER NGC 6764 : 4.310 6 M ⊙ Vout~100 km/s (Leon et al. 2007) Larger than in NGC 1433, but outflow rate ~1 M ⊙ /yr The LINER NGC 1266 highest flow rate of 13 M ⊙ /yr, with 2.4 10 7 M ⊙ of H2 and V=177 km/s (Alatalo et al. 2011) LINER NGC1377 , SFR of ∼ 1 M ⊙ /yr, outflow rate of 8 M ⊙ /yr, Mflow = 1.1 10 7 M ⊙ at V=140 km/s (Aalto et al. 2012) 27

CONCLUSION  Star formation law is a molecular gas law  Depletion time scale lower in galaxy centers, as at high z  Stars form essentially on the MS (starburst small contribution)  Evidence of inflow/outflow: quenching by SN, powerful AGN  Low-luminosity AGN can drive molecular gas outflows 28