1. (Cold) dust and gas in high-z AGNs: a prelude to Herschel and ALMA Roberto Maiolino Osservatorio Astronomico di Roma

2. The “cold” side of AGNs Molecular transitions (gas mass, dynamics...) Far-IR fine structure lines (PDR, HII, star formation, dynamics...) Thermal dust emission (star formation, dust mass,...) Cleaner view of the host galaxy (unaffected/little affected by AGN light) than at other wavelengths...

3. Two modes of star formation “starburst” high efficiency merger-interaction driven “secular” low efficiency disk instabilities (smooth gas inflow) Daddi+10 Genzel+10 In what mode does black hole accretion occur? Higher gas fraction at high-z Does this play a role into BH accretion and obscuration at high-z? Tacconi+10 gas fraction local QSOs high-z slope=1.3

4. Shao+10 Herschel: a tight connection between BH accretion and galaxy formation only seen in the luminous QSO regime (merging?) Low luminosity AGN hosts mostly undergoing secular evolution Walter+09 1.5 kpc z=6.4 L AGN ~L Edd  SFR ~ 1000 M o yr -1 kpc -2 (Eddington limited SF)  gas ~ 10 10 M o kpc -2 (~GMC cores) M BH /M bul L(SF) [erg/s] L(AGN) [erg/s]

5. CO velocity fields: AGN host galaxy dynamics at high z High z QSO hosts Low z galaxies M BH -M * Relation out to z>6 M * ~ M dyn -M gas CO Velocity (deprojected) Riechers+09 Wang+10 Lamastra+10 CO map (Einstein ring z~4.8) from CO rotation curve... yes, the molecular gas rotates... and traces the dynamical mass... really true?

6. If molecular gas in QSO hosts rotates and is dynamically settled... where’s the feedback?!... the bulk of the gas (~molecular) in the host galaxy seems unaffected by the presence of a QSO. Mrk231 the closest QSO However past CO observations plagued by narrow bandwidth -200 +200 0 Mrk231 re-observed with IRAM broad bandwidth Feruglio+10 Velocity (km/s) Downes & Solomon 1998 Broad wings

7. Massive molecular outflow in Mrk231 extended over ~1 kpc Inferred outflow rate ~ 2000 M  /yr ! Will expel the available molecular gas (hence stop star formation) in less than 10 7 yrs Same outflow component observed by Herschel through OH and H 2 O absorption Fisher+10

8. Herschel+ALMA powerful tools to probe dynamics and feedback in high-z AGN hosts! But are molecular tracers really the best ones in typical galaxies at high-z? “Low metallicity” (Z~0.3 Zsun) galaxy observed by Herschel [CII]/CO ~ 50000 !!! Far-IR fine structure lines (especially PDR tracers) more promising Cormier+10 [CII] CO

9. star forming galaxies ULIRGs Far-IR fine structure lines in high-z AGN hosts. Not only kinematics, but also galaxy physics. Iono+06 Walter+09 Maiolino+05,09 Ivison+10 z>4 QSOs AGN in z~2 SMG AGN in z~2 SMG local ULIRGs local SB and SF galaxies n=10 6 n=10 4 n=10 2 G 0 =10 2 G 0 =10 4 L CO(1-0) /L bol L [CII] /L bol [CII] @ z=4.4

10. Also NLR far-IR tracers at high-z, but not clear-cut in identifying AGNs Sturm+10 Ferkinhoff+10 However, the mm/submm spectral range host other powerful tracers of (obscured) AGNs...

11. X-ray Dominated Regions (XDR’s)  Photo Dissociated Regions (PDR’s) UV X-ray X-rays penetrate deep into the molecular cloud and keep the temperature high Maloney+96, Lepp & Dalgarno 96, Meijerink+05,07

12. Van den Werf+10 Herschel-SPIRE XDR Powerful tool to identify totally obscured and embedded AGNs

13. Weiss etal 2005/7 non - linear (slope 1.7) QSOs SMGs The high CO excitation observed in high-z QSOs is probably associated with XDR

14. X-ray Dominated Regions (XDR’s)  Photo Dissociated Regions (PDR’s) UV X-ray X-rays penetrate deep into the molecular cloud and keep the temperature high high-T favors chemical reactions ( e.g. formation of HCN) Maloney+96, Lepp & Dalgarno 96, Meijerink+05,07

15. XDR-enhanced species can identify the presence of hidden/elusive AGNs HCO+(1-0) Starbursts and Composite Sy’s Pure Sy’s HCN / HCO+ HCN / CO Khono+08 Krips+09

16. With ALMA the identification of XDR will be feasible not only in all local (obscured) AGNs, but also at high redshift HCN HCO+ CO CCH Example of QSO at z=6.4 Not only ~  S/N on CO line (  detailed dynamical studies, see discussion later on), but also several other molecular lines -> astrochemistry -> XDR tracers IRAM 14 hours Bertoldi+03