Radio Quiet AGN: Black Hole & Host Galaxy Proper;es
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- Phoebe Lester
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1 Radio Quiet AGN: Black Hole & Host Galaxy Proper;es (ESO) Collaborators: V. Mainieri, P. Padovani, P. Rosa6, N. Miller, K. I. Kellermann, P. Tozzi, S. Va>akunnel, A. Bongiorno, + PEP Collaboration
2 Credit: ESO
3 In the RADIO! Credit: ESO
4 AGN-host galaxy coevolution M BH σ relation (Ferrarese & Merri> 2000; Gebhardt+00; Haering&Rix 2004; Greene+07, Gultekin et al., 2009) Gultekin et al., 2009 σ (km /s)
![galaxies form at higher redshi]](/docs-images/72/66544652/images/5-4.jpg "(La Franca+05) (Perez-")
5 AGN-host galaxy coevolution Downsizing: More luminous AGN had the peak of ac6vity at earlier redshi]s More massive galaxies form at higher redshi] (La Franca+05) (Perez- Gonzalez+08) Feedback
6 Why in the radio? Perseus Cluster X- ray cavi6es inflated by radio jets. (e.g Fabian & Sanders 2006) Not affected by DUST X- ray Chandra Image. Credit: NASA Obscured sources High z
7 Why deep in the radio? 1) Below 0.1 mjy: Star Forming Galaxies (SFG) Radio Loud (RL) AGN Star Forming galaxy M82 Credit: NRAO/AUI
8 Why deep in the radio? 1) Below 0.1 mjy: Star Forming Galaxies (SFG) 2) Most of the AGN are Radio Quiet (RQ) AGN RL AGN ~ 1,000 x RQ AGN
9 Why deep in the radio? 1) Below 0.1 mjy: Star Forming Galaxies (SFG) 2) Most of the AGN are Radio Quiet (RQ) AGN 3) Square Kilometer Array (SKA) & pathfinder ASKAP MeerKAT SKA
10 Extended Chandra Deep Field South 1.4 GHz / VLA ~ 900 sources 5σ flux density limit: ~30 µjy (Miller+,in prepara6on) 30 arcmin
11 Extended Chandra Deep Field South 1.4 GHz / VLA ~ 900 sources 5σ flux density limit: ~30 µjy (Miller+,in prepara6on) ~90% sub-mjy objects 30 arcmin
12 Extended Chandra Deep Field South GHz ks / VLA ~ 900 sources 5σ flux density limit: ~30 µjy (Miller+,in prepara6on) 4 Ms Chandra: 250 ks + 4 Ms GEMS/ACS, VLT/ FORS + ISAAC, Subaru, NTT/ SOFI, ESO2.2m/ WFI 30 arcmin GOODS/ACS Spitzer/IRAC +MIPS
![Optical and IR counterparts Sources with counterpart: 94% with redshi]: 78% (40%](/docs-images/72/66544652/images/13-1.jpg "spectroscopic), <z> 1 VLA 1.4 GHz images ACS z-band images MIPS 24 µm images (Bonzini+.")
13 Optical and IR counterparts Sources with counterpart: 94% with redshi]: 78% (40% spectroscopic), <z> 1 VLA 1.4 GHz images ACS z-band images MIPS 24 µm images (Bonzini , in press on ApJS)
14 AGN or SFG? q24 = S 24µm S 1.4GHz SFG locus +2σ M82-2σ (Sargent+10)
15 AGN or SFG? q24 = S 24µm S 1.4GHz RL AGN
16 AGN or SFG? SFG IRAC color- color diagram: QSO λ PAH dominated sources Elliptical (Lacy+04, Donley+12) λ Power law sources: AGN dominated λ Old stellar population galaxies (Templates from Polletta+07)
17 AGN or SFG? If NOT RL AGN L x >10 42 erg s - 1 Power law sources AGN (Lacy+04, Donley+12) YES = RQ AGN; NO = SFG
18 63% SFG - 20% RQ AGN - 17% RL AGN (Bonzini , in prepara6on)
19 Euclidean normalized number counts
20 M star & Morphology Stellar mass from SED fiung: (Bongiorno+12; Bruzual&Charlot03, Richards+06) TOTAL GALAXY AGN SFG RQ AGN RL AGN
21 M star & Morphology RL SFG RQ Blue band rest- frame morphology: higher frac6on of late type host galaxies for RQ AGN. SFG RQ AGN RL AGN (Sérsic index from GEMS catalog, Häußler et al. 2007)
22 Radio emission in RQ AGN The Luminosity Function (LF) of RQ AGN appears as an extension of the SFG LF + SFG and RQ AGN have the same evolution Padovani+11 Hypothesis: radio emission from star formation rather then from accretion
23 SFR from radio luminosity SFR = 5.9 ± L [ M yr GHz sun ] (Bell+03) RQ AGN, 0.8 < z <1.2 RQ AGN, 1.4 < z <2.5
24 SFR from radio luminosity SFR = 5.9 ± L [ M yr GHz sun ] (Bell+03) Z=2 Z=1 Radio flux density limits 0.8 < z <1.2 (Elbaz+07) 1.4 < z <2.5 (Daddi+ 2007)
25 SFR from Far-IR luminosity F ν Wavelength (micron) Herschel/PACS: PEP project, PI: D. Lutz
![8 10 10 L bol / L sun [M sun yr 1 ]](/docs-images/72/66544652/images/26-2.jpg "(Rodighiero+10b) Herschel/PACS PEP")
26 SFR from Far-IR luminosity F ν Wavelength (micron) SFR = L bol / L sun [M sun yr 1 ] (Rodighiero+10b) Herschel/PACS PEP project, PI: D. Lutz
27 SFR comparison for SFG SFG
28 SFR comparison for RQ AGN SFG RQ AGN
29 SFR comparison for RQ AGN SFG RQ AGN RL AGN
30 Summary & Outlook Deepest radio sources counterpart catalog Host galaxy proper6es vs radio loudness: from RQ AGN (late type, M star ~ M ) to RL AGN (early type, M star ~10 11 M ) Black hole proper6es: M BH & Eddington Ra6o Radio emission in RQ AGN due to SF Bonzini et al. 2012, in press 2 evolu6onary phases? Op6cal and NIR spectroscopy (FMOS KMOS) ALMA proposal submi>ed Luminosity func6on
31 Summary & Outlook ASKAP SKA MeerKAT
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