Revealing powerful outflows in z~1.5 obscured QSOs

Transcription

1 Revealing powerful outflows in z~1.5 obscured QSOs Marcella Brusa 1) Dipartimento di Fisica e Astronomia / Universita di Bologna 2) Max-Planck Institut für Extraterrestrische Physik / Garching, Germany (major) credits: A. Bongiorno, G. Cresci, F. La Franca, R. Maiolino, M. Mignoli Black Hole (g)astronomy - Brindisi September 2013

2 AGN-galaxy coevolution paths MERGERS SCENARIO: (last decade paradigm) Major mergers can trigger SF and BH activity (e.g. Silk & Rees 1998, Granato et al. 2004, Di Matteo et al. 2005, Croton et al. 2006, Fontanot et al. 2006, De Lucia et al. 2006, Sijacki et al. 2007, Menci et al. 2008, Hopkins et al. 2008, Marulli et al. 2009) strong correlation between M BH and bulge properties (e.g. Ferrarese & Merritt 2000, Gebhardt et al. 2000, Gultekin et al. 2009) Alexander & Hickox 2012 SECULAR SCENARIO: (this decade novelty) (weak) activity driven stochastically by local processes (inflow, disks/bars instabilities; Croton+2006, Ciotti&Ostriker 2007, Cen 2011, Dekel+2008, Bournaud+2011, Di Matteo+2011) no correlation between M BH and disk or pseudobulge properties (Kormendy et al. 2011; see also Graham et al. 2010) QSO-ULIRGS-mergers connection (e.g. Sanders et al. 1988) (see also Bellovary talk) A population of galaxies evolved without mergers does clearly exist (disks are observed at z~2; e.g. Genzel +2006, 2008) also in AGN hosts (Cisternas+2011, Kocevski +2012)

3 AGN-galaxy coevolution paths MERGERS SCENARIO: (last decade paradigm) Major mergers can trigger SF and BH activity (e.g. Silk & Rees 1998, Granato et al. 2004, Di Matteo et al. 2005, Croton et al. 2006, Fontanot et al. 2006, De Lucia et al. 2006, Sijacki et al. 2007, Menci et al. 2008, Hopkins et al. 2008, Marulli et al. 2009) High luminosity strong correlation between M BH and bulge minority properties (e.g. Ferrarese & Merritt 2000, Gebhardt et al. 2000, Gultekin et al. 2009) Alexander & Hickox 2012 SECULAR SCENARIO: (this decade novelty) (weak) activity driven stochastically by local processes (inflow, disks/bars instabilities; Croton+2006, Ciotti&Ostriker 2007, Cen 2011, Dekel+2008, Bournaud+2011, Di Matteo+2011) Low luminosity no correlation between M BH and disk majority pseudobulge properties (Kormendy et al. 2011; see also Graham et al. 2010) QSO-ULIRGS-mergers connection (e.g. Sanders et al. 1988) Feedback! Feedback? (see also Bellovary talk) A population of galaxies evolved without mergers does clearly exist (disks are observed at z~2; e.g. Genzel +2006, 2008) also in AGN hosts (Cisternas+2011, Kocevski +2012)

4 evidences for (AGN) feedback at z>1 INDIRECT Harrison+2012a SFR vs. Lx CDFN/CDFS/COSMOS (see also Page+2012, Rosario+2012) (see Maiolino review) DIRECT Harrison+2012b ionized outflows / integrated NIR spectra ([OIII] broad and shifted wings) see also molecular outflows (e.g. Feruglio+10) MORE DIRECT Cano-DIaz+2012, Alexander+2010, Maiolino+2012 spatially resolved IR spectroscopy estimate spatial scale (distance!) to get energy

5 [OIII] FWHM as tracers of outflows/gas broad distribution of [OIII] width vs. total luminosity in SDSS Syeferts (Mullaney+2013) - Gas is kinematically disturbed - SDSS broadest profile in highest L/LEdd sources dynamics

6 [OIII] FWHM as tracers of outflows/gas broad distribution of [OIII] width vs. total luminosity in SDSS Syeferts (Mullaney+2013) - Gas is kinematically disturbed - SDSS broadest profile in highest L/LEdd sources dynamics Higher incidence of broad components in Sey-ULIRGs wrt non-sey ULIRGs (Rodriguez-Zaurin et al. 2013)

7 [OIII] FWHM as tracers of outflows/gas broad distribution of [OIII] width vs. total luminosity in SDSS Syeferts (Mullaney+2013) - Gas is kinematically disturbed - SDSS broadest profile in highest L/LEdd sources dynamics Higher incidence of broad components in Sey-ULIRGs wrt non-sey ULIRGs (Rodriguez-Zaurin et al. 2013) Large [OIII] FWHM in high-z luminous and very luminous ULIRGs/QSO (Harrison et al compilation)

8 High-z: biases on the selection? most of previous studies are on preselected radio and/or SMG - ULIRGs systems and/or serendipitous, generally z>2 Kinetic vs. radiative feedback vs. SN feedback Alexander et al. 2010, Harrison et al (SMG / ULIRGS) Nesvadba et al. 2006, 2008, 2011 (radio galaxies) Cano-Diaz et al (ULIRG)

9 Finding the sweet spot for feedback Hopkins et al (see also Lamastra+2013) Narayanan et al Lbol=45.5 MERGERS MODEL PREDICTIONS/IMPLICATIONS: 1) blow-out/feedback phase very short (<~ 100 Myr) - RARE! 2) BH growth and SF almost simultaneous 3) blow-out/feedback phase X-ray obscured (torus+host ISM) 4) blow-out/feedback phase IR bright

10 Finding the sweet spot for feedback Hopkins et al (see also Lamastra+2013) Narayanan et al AGN in FEEDBACK: X-ray luminous, obscured and dusty Lbol=45.5 MERGERS MODEL PREDICTIONS/IMPLICATIONS: 1) blow-out/feedback phase very short (<~ 100 Myr) - RARE! 2) BH growth and SF almost simultaneous 3) blow-out/feedback phase X-ray obscured (torus+host ISM) 4) blow-out/feedback phase IR bright

11 HOW to efficiently select QSO in feedback phase Use correlations between observables (X/O, R-K, HR, luminosities) for the identified samples to isolate obscured AGN XMM-COSMOS 2-10 kev (~1000 objects) FULL XMM-COSMOS sample (~1800 objects) Brusa et al. 2010

12 HOW to efficiently select QSO in feedback phase Use correlations between observables (X/O, R-K, HR, luminosities) for the identified samples to isolate obscured AGN Most efficient selection to pick up obscured QSO using only 3 bands! ~100 objects vs. ~1000 (~10%) XMM-COSMOS 2-10 kev (~1000 objects) FULL XMM-COSMOS sample (~1800 objects) Brusa et al. 2010

13 HOW to efficiently select QSO in feedback phase Use correlations between observables (X/O, R-K, HR, luminosities) for the identified samples to isolate obscured AGN Most efficient selection to pick up obscured QSO using only 3 bands! ~100 objects vs. ~1000 (~10%) XMM-COSMOS 2-10 kev (~1000 objects) FULL XMM-COSMOS sample (~1800 objects) Brusa et al. 2010

14 HOW to efficiently select QSO in feedback phase Use correlations between observables (X/O, R-K, HR, luminosities) for the identified samples to isolate obscured AGN Most efficient selection to pick up obscured QSO using only 3 bands! ~100 objects vs. ~1000 (~10%) XMM-COSMOS 2-10 kev (~1000 objects) FULL XMM-COSMOS sample (~1800 objects) Brusa et al. 2010

15 HOW to efficiently select QSO in feedback phase Use correlations between observables (X/O, R-K, HR, luminosities) for the identified samples to isolate obscured AGN Most efficient selection to pick up obscured QSO using only 3 bands! ~100 objects vs. ~1000 (~10%) XMM-COSMOS 2-10 kev (~1000 objects) FULL XMM-COSMOS sample (~1800 objects) Brusa et al X-ray and IR brightest objects observed with Xshooter

16 X-shooter NIR spectra Brusa et al, in prep 3 nights in February targets goals: 1) measure redshifts for only photoz (6/10) 2) measure BH mass from broad Halpha (>50%, Bongiorno et al. in prep) 3) search for outflows Common properties: Lx>10 44 NH>~10 22 red /dusty systems M*>10 11

17 X-shooter NIR spectra Brusa et al, in prep Spectro-z (from COSMOS optical campaigns: zcosmos, IMACS, Keck) Common properties: Lx>10 44 NH>~10 22 red /dusty systems M*>10 11

18 X-shooter NIR spectra Brusa et al, in prep PACS detected (PEP data) Common properties: Lx>10 44 NH>~10 22 red /dusty systems M*>10 11

19 Brusa et al, in prep X-shooter NIR spectra Radio detected (VLA data) none radio-loud Common properties: Lx>10 44 NH>~10 22 red /dusty systems M*>10 11

20 XID 2028 loglx~45 lognh~22 loglir>13 SFR~450 Msun/yr logmstar=11.7 FWHM([OIII])=810 km/s XID 5321 loglx=45 lognh=21.6 loglir=12.2 SFR>200 Msun/yr logmstar=12.1 FWHM([OIII])=1200 km/s outflow of ~300 km/s

21 X-ray obscured QSOs in a context Seyfert-ULIRG (Rodriguez-Zaurin +13) High-z ULIRGs (Harrison+2012 compilation) cluster around the z~2-4 SMG/ULIRGs SDSS AGN (Mullaney+13)

22 X-ray obscured QSOs in a context Seyfert-ULIRG (Rodriguez-Zaurin +13) High-z ULIRGs (Harrison+2012 compilation) cluster around the z~2-4 SMG/ULIRGs SDSS AGN (Mullaney+13)

23 Take home message feedback phase is luminous, X-ray bright, dusty: cheap selection: based on observed quantities vs. intrinsic properties large [OIII] widths are observed in X-ray selected, luminous, obscured and dusty QSOs: selection does work feedback phase is short (RARE objects): quest for very large area X-ray surveys (see also posters by Urry, Menzel)

24 erosita huge discovery space erosita(+4most) AGN science case expected ~3500 obscured QSO (Lx>45, NH>21, z=1-3) in the hard band can be easily identified by the combination of only 3 bands! see Merloni et al. 2012, arxiv: