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THE HERSCHEL VIEW OF AGN EVOLUTION AND CONNECTIONS WITH SF IN HOST GALAXIES

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

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THE HERSCHEL VIEW OF AGN EVOLUTION AND CONNECTIONS WITH SF IN HOST GALAXIES

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  1. THE HERSCHEL VIEW OF AGN EVOLUTION AND CONNECTIONS WITH SF IN HOST GALAXIES 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

  3. Herschel - one year into the mission

  4. First images from Herschel PACS three bands

  5. First Herschel results on the AGN side • ESLAB2010 presentations available at http://herschel.esac.esa.int/FirstResultsSymposium.shtml • First Results published as Letters in A&A Special Issue dedicated to Herschel • Most papers already on astro/ph

  6. The Astrophysical Teraherz Large Area Survey - ATLASPI: S. Eales (Cardiff) -22>IAB>-24 • The Herschel ATLAS is a key legacy survey of 550 deg2 covering 5 bands with PACS andSPIRE (110 – 500 microns) to 5 sigma ~132, 126, 33,36 and 45mJy / 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. -24>IAB>-26 -26>IAB>-28  Herschel-ATLAS QSOs  PG QSOs  SDSS OSOs 850 m QSOs  1200 m QSOs -28>IAB>-30 Serjeant+10, A&A Special Issue Serjeant+10 A&A Special Issue Evidence for downsizing in the QSO host galaxies  Luminous QSOs have higher SFR at higher z

  7. Herschel Multi-Tiered Extragalactic Survey - HERMESPI: 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. [only at z>2: LSBLacc0.35] Hatzminouglou+’10 A&A Special Issue

  8. Herschel Multi-Tiered Extragalactic Survey - HERMESPI: S. Oliver (Sussex) • Many AGN (20% of optical/X‐ray/radioAGN) 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 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.

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

  10. PACS Evolutionary Probe - PEPPI: 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 (Shao+’10 A&A Special Issue) z-distribution LFIR vs NH: no trend with obscuration Large range of optical-to-FIR SEDs 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)

  11. PACS Evolutionary Probe - PEPPI: D.Lutz (MPE) First Herschel Probe of Dusty galaxy evolution up to z~3: FIR AGN and galaxy Luminosity Function (Gruppioni+’10 A&A Special Issue) • 216 and 237 PEP sources with z detected at 100 and 160 µm respectively (S100(3)>3 mJy, S160(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 (µm) (%) 100 216 28 32 6 33 2 160 237 27 35 5 32 3 Seyfert2/1.8: 25% X-ray detected; <L(2-8keV)>~1043 erg s-1 cm-2 Starburst: 12% X-ray detected; <L(2-8keV)>~1042.5 erg s-1 cm-2 Spirals: 4% X-ray detected; <L(2-8keV)>~1042 erg s-1 cm-2 For comparison: QSO: 50% X-ray detected; <L(2-8keV)>~1045 erg s-1 cm-2 composite: 50% X-ray detected; <L(2-8keV)>~1044 erg s-1 cm-2 Polletta+’07 originall Sey2 template

  12. PACS Evolutionary Probe - PEPPI: D.Lutz (MPE) First Herschel Probe of Dusty galaxy evolution up to z~3: FIR AGN and galaxy Luminosity Function (Gruppioni+’10 A&A Special Issue) • 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 Spiral Sey2/1.8 Starburst composite QSO • Seyfert2/1.8 dominate the LF around L ( 1010.5L<L90<1011.5L) 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 Luminosity evolution green : spirals Density evolution cyan : starbursts red : AGN2 magenta: composite blue : AGN1

  13. PACS Evolutionary Probe - PEPPI: 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)

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