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Red QSOs in the MBH-M∗ plane

Published online by Cambridge University Press:  25 July 2014

Angela Bongiorno
Angela Bongiorno*
Affiliation:
INAF, Osservatorio Astronomico di Roma, via di frascati 33, Monteporzio Catone - Rome, Italy email: [email protected]
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Abstract

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We present new results on the the MBH-M∗ relation of X-ray obscured, red QSOs at high redshift (1.2<z<2.6). The sample is made of 21 red QSOs, nine of them are new sources for which near-infrared spectra have been obtained with SINFONI and XShooter observations at ESO VLT, and show a broad Hα component. The rest of the sample (12 sources) is made of sources taken from the literature with similar properties. From the broad Hα line we have computed the BH masses through the virial formula while stellar masses have been obtained through multi-component SED fitting.

We find that red QSOs preferentially lie on the local relation up to z ~ 2.6 with the most massive objects mainly located above it. We also studied the evolution of these sources on the MBH-M∗ plane compared to a sample of optically blue type–1 QSOs and we find that obscured red QSOs show a constant MBH/M∗ ratio consistent/slightly higher than the local one but lower than what has been found for blue QSOs. These sources may represent the intermediate phase (blow-out phase) between the major-merger induced starbursts which appear as ULIRGs and SMGs and the optical type–1 blue QSOs which are revealed once the dust and nuclear gas is cleared up.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S304: Multiwavelength AGN Surveys and Studies , October 2013 , pp. 195 - 198
Copyright
Copyright © International Astronomical Union 2014 

References

Hopkins, P. F.et al. 2008, ApJS, 175, 356Google Scholar
Magorrian, J.et al. 1998, AJ, 115, 2285CrossRefGoogle Scholar
Maiolino, R.et al. 2007, A&A, 472, L33Google Scholar
Marconi, A. & Hunt, L. K. 2003, ApJ (Letters), 589, L21CrossRefGoogle Scholar
Menci, N., et al. 2008, ApJ, 686, 219Google Scholar
Merloni, A.et al. 2010, ApJ, 708, 137Google Scholar
Peng, C. Y.et al. 2006, ApJ, 640, 114CrossRefGoogle Scholar
Salviander, S. & Shields, G. A. 2013, ApJ, 764, 80CrossRefGoogle Scholar
Salviander, S.et al. 2007, ApJ, 662, 131Google Scholar
Sani, E.et al. 2011, MNRAS, 413, 1479Google Scholar
Shields, G. A.et al. 2003, ApJ, 583, 124CrossRefGoogle Scholar
Woo, J.et al. 2008, ApJ, 681, 925Google Scholar