agn feedback in action: constraints on the scaling relations between bh and galaxy at high redshift...
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![Page 1: AGN feedback in action: constraints on the scaling relations between BH and galaxy at high redshift Andrea Merloni (EXC, MPE) A. Bongiorno (MPE), COSMOS](https://reader036.vdocuments.us/reader036/viewer/2022062322/5697bfeb1a28abf838cb8297/html5/thumbnails/1.jpg)
AGN feedback in action: constraints on the scaling relations between
BH and galaxy at high redshift
Andrea Merloni (EXC, MPE)
A. Bongiorno (MPE), COSMOS + zCOSMOS teams
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Outline
•Co-evolution of stellar and SMBH mass densities: integral constraints
•Scaling relations in high redshift AGN (COSMOS/zCOSMOS)
•Future prospects
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Simultaneous growth of BH and galaxies
Fabian and Iwasawa (1999) ~0.1; Elvis, Risaliti and Zamorani (2002) >0.15; Yu and Tremaine (2002) >0.1; Marconi et al. (2004) 0.16> >0.04;
Merloni, Rudnick, Di Matteo (2004) 0.12> >0.04; Shankar et al. (2007) ~0.07
BHAR(z) =1) AGN LF
2) Local BH mass density
3) Local scaling relationand their evolution
4) Link to the Hubble sequence evolution?
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Parallel lives
See Merloni, Rudnick, Di Matteo (2004)
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Parallel lives
Merloni, Rudnick, Di Matteo (2004); Hopkins et al. (2006)
Mild evolution <MBH/M*,bulge> ~ (1+z)0.4
BH/* = 0.0015
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Parallel lives
Merloni, Rudnick, Di Matteo (2004); Hopkins et al. (2006)
Very weak constraints on disk-spheroid ratio evolution
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AGN in the COSMOS
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COSMOS survey
HST/XMM/Chandra COSMOS [Scoville, Hasinger, Elvis]
●2 deg2 equatorial ●HST treasury project●Deep: ACS iAB < 27●Similar volume as SDSS, but fainter and higher z
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Type-1 AGN in the zCOSMOS surveyMeasure BH mass using
“virial” relation applied to MgII (1<z<2.2) 89 AGN
Merloni, Bongiorno et al. 2010
Log MBH=6.8 Log[FWHM10002 L3000
0.47]
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The REAL problem:How to obtain reliable host galaxy masses in
Type I AGN?
Credit: Dr. John Hutchings,Dominion Astrophysical Observatory, NASA
HST image of PG 1229+204 (z=0.064)
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Unveiling AGN hosts through SED fitting
AGN templates: - Richards et al. (2006) - E(b-v)=0 - 0.3Galaxy templates: - 14 phenomenological Polletta (2007) - Libr. of synthetic sp. (Bruzual & Charlot) a) 10 declining SFH SFR µe-t/t t=[0.1-30] Gyr tage=[50Myr-5 Gyr] tage<tuniv(z) 0 < E(B-V) <0.5 b) 1 constant SF
14 Bands Used6 SUBARU bandsI + K band (CFHT)
4 Spitzer/IRAC24mm Spitzer/MIPS
Merloni, Bongiorno et al. 2010
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Host Galaxy properties I
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Host Galaxy Properties II
Cumulative probability distribution for SFR and total stellar mass of the HG
SFR= 50 M*/yr M* ~1010.8
Our Host Galaxies are likely actively Star Forming objectsKauffmann et al. (2003); Brammer et al. (2009); Silverman et al. (2009)
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Scaling relations at 1<z<2
Solid line (+scatter): MBH-bulge relations, z=0
(Graham et al. 2007; Haring & Rix 2004)
Merloni, Bongiorno et al. 2010
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Redshift evolution of the MBH-M* relation
Evolution in the Normalization?
MBH/M* (1+z)0.70.1+0.6-0.3
Merloni, Bongiorno et al. 2010
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Redshift evolution of the MBH-M* relation
Evolution in the normalization?
cyan lines: Luminosity Bias (Lauer+07)
0.7 dex
0.3 dex
Evolution in the scatter?
Significant mismatch between the typical growth times of BH and
host galaxiesMerloni, Bongiorno et al. 2010
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Future tests of “Luminosity bias”
for MBH<108
Expected bias minimal
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A consistent picture?
<M
BH>
>
Bennert et al. 2009
Decarli et al. 2009
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Selection, selection, selection
Lamastra et al. (2010)
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Flow patterns in the MBH-M* plane Solid line (+scatter): MBH-bulge mass relation, z=0
(Haring & Rix 2004)
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Flow patterns in the MBH-M* plane Solid line (+scatter): MBH-bulge mass relation, z=0
(Haring & Rix 2004)
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Solid line (+scatter): MBH-bulge mass relation, z=0 (Haring & Rix 2004)
Flow patterns in the MBH-M* plane
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Future prospects
Thanks to P. Rosati (ESO)
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• AGN-galaxy co-evolution is evident in integrated quantities (masses and SFR/BHAR densities)
• No strong evolution of <MBH/M*> from integral constraints
• The most rapidly growing black holes (QSOs at 1<z<4) show an offset from the local scaling relation: for a given host BHs appear to be bigger than at z=0
• This could be due to (moderate) evolution in either normalization and/or scatter in the Magorrian relation
• Strong Co-evolution and Simplest “Explosive” feedback models fail to reproduce the data.
• Predictions about evolution of scatter are crucial
• Need BH mass estimators in (mildly) obscured AGN!!
Conclusions