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The MBH-Mstar relation in obscured AGNs at high z: New clues on the Black Holes-Galaxy co-evolution Julian Enrique Sarria Chavez Terza Università di Roma With: R. Maiolino, F. La Franca, F. Pozzi, S. Berta, F. Cocchia, G. Melini et al. How did the local MBH - Mbul relation come into place? Various theoretical models have been proposed. Each of them predict a different evolution of the MBH-Mbul relation at high-z (see e.g. Lamastra’s talk) Locally: MBH/Mbulge ~0.002 Marconi & Hunt 2003 Jian Hu 2009 Lamastra+10 Redshift evolution of (MBH/Mstar)(z)/(MBH/Mstar)(z=0)=G(z) type 1 AGN: G(z>1) > G(z=0) but bias due to AGN luminosity selection? (“Lauer’s bias”) models type 2 AGN in SMGs: G(z>1) < G(z=0) but bias due to SF selected host? (SF~Mstar) New near-IR (1-2.4mm) integral field spectroscopy (SINFONI+VLT) of high-z obscured AGNs Selection criteria 14 objects: - X-ray selected (F2-10keV>10-14 erg cm-2 s-1) - High X-ray/Optical ratio (X/O>10) - Very red colors: R-K>5 (EROs) - K~18 (dominated by the host galaxy) Results: -Spectroscopic identification of 7 objects - 1.3 < z < 2.1 - 1044 < L2-10keV < 1045 erg s-1 type 2 QSOs - 1022.3<NH<1023 cm-2 Example of spectra H maps XMM172 nord, H z= 1,6679 XMM172, H z= 1,71 Weighing Black Holes with the broad line H Although obscured, three of the targets show broad H -> can be used to infer the black hole mass through the virial estimators (Greene et al. 2005) Issue of broad H broad flux being suppressed by dust extinction -> we inferred the “intrinsic” AGN luminosity from X-rays The inferred black hole masses are in the range 107<MBH<109 M The inferred accretion rates are close to the Eddington limit M BH M Edd Lbol LEdd 1 The optical and near-IR light is dominated by the host galaxy, hence the optical/near-IR SED can be used to constrain the stellar mass in the host galaxy (Pozzi et al. 2010) Resulting MBH-Mstar relation at z~2 unobscured obscured X-ray selected obscured in SMGs Resulting MBH-Mstar relation at z~2 unobscured • z~2 X-ray selected obscured QSOs have black hole UNDERMASSIVE relative to the local relation • Their galaxies form faster than their black hole; obscured • The AGN selection bias X-ray (“Lauer’s bias”) would go in selected the opposite direction the effect is real obscured in SMGs • Obscured AGNs show the opposite evolution of MBH/Mstar w.r.t. unobscured AGNs • Either most unobscured AGNs are affected by strong selection effects (“Lauer’s bias”) • Or obscured and unobscured AGNs follow different evolutionary paths Resulting MBH-Mstar relation at z~2 By measuring the SFR (from the SED) and the BH accretion rate (from LX) it is possible to define the expected evolution on the MBH-Mstar diagram unobscured 108 yr obscured X-ray selected obscured in SMGs They are rapidly moving towards the local relation Conclusions - We have measured the redshift for 7 sources (1.3<z<2.1) - We detected broad Hα in three of these targets, which allowed us to estimate their black hole masses. - The galaxy masses have been estimated from their SED - z~2 obscured AGNs have MBH/Mstar lower than the local relation, in contrast with unobscured AGNs • Either most unobscured AGNs are affected by strong selection effects • Or obscured and unobscured AGNs follow different evolutionary paths