1. THE HERSCHEL VIEW OF AGN EVOLUTION AND CONNECTIONS WITH SF IN HOST GALAXIES C. Gruppioni INAF - OABo C. Gruppioni INAF - OABo AGN9: Ferrara 24-27 Maggio 2010

2. HERSCHEL IN A NUTSHELL Successfully launched on 14 May 2009, is currently in science operation, performing photometry and spectroscopy in the 55-672 µm range With its 3.5-m Cassegrain telescope, it is the largest space telescope ever launched Passively cooled Telescope with three focal-plane instruments onboard:  HIFI : high resolution spectrometer at 480-1910 GHz  PACS : photometer and spectrometer at 60 - 210 µm  SPIRE : photometer and FTS spectrometer at 200 - 670 µm Successfully launched on 14 May 2009, is currently in science operation, performing photometry and spectroscopy in the 55-672 µm range With its 3.5-m Cassegrain telescope, it is the largest space telescope ever launched Passively cooled Telescope with three focal-plane instruments onboard:  HIFI : high resolution spectrometer at 480-1910 GHz  PACS : photometer and spectrometer at 60 - 210 µm  SPIRE : photometer and FTS spectrometer at 200 - 670 µm

3. Herschel - one year into the mission

4. First images from Herschel PACS three bands

5. First Herschel results on the AGN side http://herschel.esac.esa.int/FirstResul tsSymposium.shtml http://herschel.esac.esa.int/FirstResul tsSymposium.shtmlESLAB2010 presentations available at http://herschel.esac.esa.int/FirstResul tsSymposium.shtml http://herschel.esac.esa.int/FirstResul tsSymposium.shtml First Results published as Letters in A&A Special Issue dedicated to Herschel Most papers already on astro/ph http://herschel.esac.esa.int/FirstResul tsSymposium.shtml http://herschel.esac.esa.int/FirstResul tsSymposium.shtmlESLAB2010 presentations available at http://herschel.esac.esa.int/FirstResul tsSymposium.shtml http://herschel.esac.esa.int/FirstResul tsSymposium.shtml First Results published as Letters in A&A Special Issue dedicated to Herschel Most papers already on astro/ph

6. Herschel Comprehensive ULIRG Emission Survey PI: P. van der Werf (Leiden Observatory) Inventory of gas cooling lines in 29 (U)LIRGs: — SPIRE: High resolution FTS — PACS: [CII] 158μm, [OI] 63 and 146 μm Low-z benchmark for ALMA Inventory of gas cooling lines in 29 (U)LIRGs: — SPIRE: High resolution FTS — PACS: [CII] 158μm, [OI] 63 and 146 μm Low-z benchmark for ALMA Only low-J lines (<6) observable from ground ž SPIRE: J=5-4 up to J=13-12 ž Differentiation between UV and X-ray excitation: Only low-J lines (<6) observable from ground ž SPIRE: J=5-4 up to J=13-12 ž Differentiation between UV and X-ray excitation: Meijerink, 2006 Markarian 231 2 PDRs + XDR 6.4:1:4.0 ž ISM components in Mrk 231: — Extended, low density PDR — Small scale, dense PDR — High excitation component ž PDR or XDR? — Both reproduce CO ladder — IR SED and chemistry rule out PDR  Third component is XDR

7. The Astrophysical Teraherz Large Area Survey - ATLAS PI: S. Eales (Cardiff) The Herschel ATLAS is a key legacy survey of 550 deg 2 covering 5 bands with PACS andSPIRE (110 – 500 microns) to 5 sigma ~132, 126, 33,36 and 45 mJy / beam from 110-500μm Particularly useful for studying the AGN over all redshifts. The large area ensures to : sample the rare AGN (most luminous QSOs, radio-loud quasars and the FRI/FRIIs) be able to undertake the first unbiased survey of Blazars in the FIR In the full area  ~7000 SDSS QSOs (+ a lot more fainter ones), ~3500 z>1 FRII radio galaxies, ~10000 FRIs and ~80 Blazars. The Herschel ATLAS is a key legacy survey of 550 deg 2 covering 5 bands with PACS andSPIRE (110 – 500 microns) to 5 sigma ~132, 126, 33,36 and 45 mJy / beam from 110-500μm Particularly useful for studying the AGN over all redshifts. The large area ensures to : sample the rare AGN (most luminous QSOs, radio-loud quasars and the FRI/FRIIs) be able to undertake the first unbiased survey of Blazars in the FIR In the full area  ~7000 SDSS QSOs (+ a lot more fainter ones), ~3500 z>1 FRII radio galaxies, ~10000 FRIs and ~80 Blazars.  Herschel-ATLAS QSOs PG QSOs  SDSS OSOs  850 m QSOs  1200 m QSOs Serjeant+10, A&A Special Issue Serjeant+10 A&A Special Issue -22>I AB >-24 -24>I AB >-26 -26>I AB >-28 -28>I AB >-30 Evidence for downsizing in the QSO host galaxies  Luminous QSOs have higher SFR at higher z

8. The Astrophysical Teraherz Large Area Survey - ATLAS PI: S. Eales (Cardiff)

11. Herschel Multi-Tiered Extragalactic Survey - HERMES PI: S. Oliver (Sussex) Mat Page: Active Galactic Nuclei and the Growth of Galaxy Bulges (in prep.) Star formation in QSOs. Obscured vs unobscured AGN. Star formation around lower luminosity AGN. Star formation in QSOs. Obscured vs unobscured AGN. Star formation around lower luminosity AGN. Hatzminouglou+’10 A&A Special Issue [only at z>2: L SB  L acc 0.35 ]

12. Herschel Multi-Tiered Extragalactic Survey - HERMES PI: S. Oliver (Sussex) Mat Page: Active Galactic Nuclei and the Growth of Galaxy Bulges Star formation in QSOs. Obscured vs unobscured AGN. Star formation around lower luminosity AGN. Star formation in QSOs. Obscured vs unobscured AGN. Star formation around lower luminosity AGN.

13. Herschel Multi-Tiered Extragalactic Survey - HERMES PI: S. Oliver (Sussex) Mat Page: Active Galactic Nuclei and the Growth of Galaxy Bulges Star formation in QSOs. Obscured vs unobscured AGN. Star formation around lower luminosity AGN. Star formation in QSOs. Obscured vs unobscured AGN. Star formation around lower luminosity AGN.

14. Herschel Multi-Tiered Extragalactic Survey - HERMES PI: S. Oliver (Sussex) Mat Page: Active Galactic Nuclei and the Growth of Galaxy Bulges Star formation in QSOs. Obscured vs unobscured AGN. Star formation around lower luminosity AGN. Star formation in QSOs. Obscured vs unobscured AGN. Star formation around lower luminosity AGN. Many AGN (  20% of optical/X ‐ ray/radio AGN) are detected at 250 µm at redshifts > 1. Detection rate doesn’t appear to depend on AGN luminosity. The far-IR emission appears to be star-formation powered. AGN lived in vigorously star ‐ forming galaxies in the past. Both optical obscuration (i.e. type 2 objects) and X-ray absorption appear to be associated with the bright sub-mm population and to be a common feature of star ‐ forming AGN. Support to the hypothesis that AGN have an obscured growth phase while their host spheroid is forming  Alternatively: the host galaxy ISM contributed to the obscuration

15. Herschel Multi-Tiered Extragalactic Survey - HERMES PI: S. Oliver (Sussex) Conclusions HerMES brings a huge range of AGN into view at far ‐ IR/submm wavelengths. Many AGN (  20% of optical/X ‐ ray/radio AGN) are detected at 250 µm at redshifts > 1. The far-IR emission appears to be star-formation powered. AGN lived in vigorously star ‐ forming galaxies in the past. Detection rate doesn’t appear to depend very strong trend on the AGN luminosity. Optical and X ‐ ray obscuration/absorption appears to be a common feature of star ‐ forming AGN. Conclusions HerMES brings a huge range of AGN into view at far ‐ IR/submm wavelengths. Many AGN (  20% of optical/X ‐ ray/radio AGN) are detected at 250 µm at redshifts > 1. The far-IR emission appears to be star-formation powered. AGN lived in vigorously star ‐ forming galaxies in the past. Detection rate doesn’t appear to depend very strong trend on the AGN luminosity. Optical and X ‐ ray obscuration/absorption appears to be a common feature of star ‐ forming AGN.

16. PACS Evolutionary Probe - PEP PI: D.Lutz (MPE) PEP is the major Herschel 100/160 μm extragalactic survey of key multiwavelength fields

17. PACS Evolutionary Probe - PEP PI: D.Lutz (MPE) Star-formation in AGN hosts in GOODS-N: 2 Msec Chandra X-ray catalogue (Alexander+’03)  324 X-ray AG N  21% detected by PACS Star-formation in AGN hosts in GOODS-N: 2 Msec Chandra X-ray catalogue (Alexander+’03)  324 X-ray AG N  21% detected by PACS z-distribution Large range of optical-to-FIR SEDs L FIR vs N H : no trend with obscuration SF (FIR) Luminosity vs. AGN Luminosity The host FIR L of AGN increases with z. There is little dependence of FIR L on AGN L No dependence of FIR L with X-ray obscuring column   two paths of AGN/host coevolution: hig-L : SF L and AGN L correlate (merging ?) low-L : SF L independent on AGN L (non-merger SF) (Shao+’10 A&A Special Issue)

18. Seyfert2/1.8: 25% X-ray detected; ~10 43 erg s -1 cm -2 Starburst: 12% X-ray detected; ~10 42.5 erg s -1 cm -2 Spirals: 4% X-ray detected; ~10 42 erg s -1 cm -2 For comparison: QSO: 50% X-ray detected; ~10 45 erg s -1 cm -2 composite: 50% X-ray detected; ~10 44 erg s -1 cm -2 PACS Evolutionary Probe - PEP PI: D.Lutz (MPE) (Gruppioni+’10 A&A Special Issue) First Herschel Probe of Dusty galaxy evolution up to z~3: FIR AGN and galaxy Luminosity Function First Herschel Probe of Dusty galaxy evolution up to z~3: FIR AGN and galaxy Luminosity Function 216 and 237 PEP sources with z detected at 100 and 160 µm respectively (S 100 (3  )>3 mJy, S 160 (3  )>5.7mJy) broad-band multi-wavelength characterisation and SED classification (using Polletta+’07 templates) large fraction of type 2 AGN (Seyfert2/Seyfert1.8) in ~10% (40% of type 2 AGN SEDs) FIR data were underestimated by the templates, fitting all other data  “FIR” templates constructed by averaging data  Spiral Starburst composite AGN2 AGN1  Spiral Starburst composite AGN2 AGN1 (µm) (%) 100 216 28 32 6 33 2 160 237 27 35 5 32 3 Polletta+’07 originall Sey2 template

19. PACS Evolutionary Probe - PEP PI: D.Lutz (MPE) (Gruppioni+’10 A&A Special Issue) First Herschel Probe of Dusty galaxy evolution up to z~3: FIR AGN and galaxy Luminosity Function First Herschel Probe of Dusty galaxy evolution up to z~3: FIR AGN and galaxy Luminosity Function Seyfert2/1.8 dominate the LF around L  ( 10 10.5 L  <L 90 <10 11.5 L  ) at 0.5<z<1.2 (then starburst galaxies prevail) The composite and quasar populations are never dominant in the FIR, contributing to the LF only at z > 2 Sey2/1.8 compositeQSO Rest-frame 60 and 90 µm LF (total and for the different populations separately) Compared to backward evolution model predictions of Gruppioni & Pozzi (in prep.), considering different evolutionary paths Good agreement between data and model Luminosity evolution Luminosity evolution green : spirals Density evolution Density evolution cyan : starbursts red : AGN2 magenta: composite blue : AGN1 Spiral Starburst

20. PACS Evolutionary Probe - PEP PI: D.Lutz (MPE) FIR emission in AGNs mostly powered by Star-Formation hints of two paths of AGN/host coevolution low-L (type 2) AGNs found in large fraction (~30%) in the GOODS- N: dominate from z~0.2-0.3 up to z~1.2-1.5 high-L AGN (both composite - AGN+starburst - and quasar) never dominant population: significant contribution at z > 1.5-2 Significant contribution to the comoving IR Luminosity Density also from objects containing an AGN  Future: all survey data becoming available (many are already): more statistics, larger fields => test existence of AGN by comparison with X-rays, decompose SED into accretion- and SF-powered  Evolution of AGN component Gruppioni+10 (A&A Special Issue)