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A low-luminosity type-1 QSO sample: Insight from integral-field spectroscopy

Published online by Cambridge University Press:  09 February 2015

Gerold Busch
Affiliation:
I. Physikalisches Institut, Universität zu Köln, Cologne, Germany email: busch@ph1.uni-koeln.de
Semir Smajić
Affiliation:
I. Physikalisches Institut, Universität zu Köln, Cologne, Germany email: busch@ph1.uni-koeln.de Max Planck Institut für Radioastronomie, Bonn, Germany
Lydia Moser
Affiliation:
I. Physikalisches Institut, Universität zu Köln, Cologne, Germany email: busch@ph1.uni-koeln.de
Mónica Valencia-S.
Affiliation:
I. Physikalisches Institut, Universität zu Köln, Cologne, Germany email: busch@ph1.uni-koeln.de
Jens Zuther
Affiliation:
I. Physikalisches Institut, Universität zu Köln, Cologne, Germany email: busch@ph1.uni-koeln.de
Julia Scharwächter
Affiliation:
LERMA, Observatoire de Paris, Paris, France
Andreas Eckart
Affiliation:
I. Physikalisches Institut, Universität zu Köln, Cologne, Germany email: busch@ph1.uni-koeln.de Max Planck Institut für Radioastronomie, Bonn, Germany
Corresponding
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Abstract

The properties of the host galaxies of quasi-stellar objects (QSOs) are essential for the understanding of the suspected coevolution of central supermassive black holes (BHs) and their host galaxies. In Busch et al. (2014), we present a study of 20 low-luminosity type-1 QSOs (LLQSO; Busch et al.2012) that have been selected from the Hamburg/ESO survey for bright UV-excess QSOs (z ≤ 0.06). Performing careful decomposition of deep near-infrared J,H,K images, we found that the observed sources do not follow published MBHLbulge relations for inactive galaxies, supporting similar results found for type-1 AGN in the optical. This can be explained by overluminous bulges with very young stellar populations or undermassive black holes that are observed in a phase of growth. We use 3d-spectroscopy in the optical and near-infrared as a powerful tool to analyze gas and stellar kinematics, determine gas masses, star formation rate, trace underlying stellar continuum, etc. (e.g., Smajić et al.2014) and thereby constrain possible evolution scenarios. The results will be interpreted in the context of galaxy evolution and particularly the still unknown role of the AGN in this process. Here, we show first results for HE 1029-1831.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2015 

References

Busch, G., Zuther, J., Valencia-S., M., et al., 2014, A&A, 561, A140Google Scholar
Busch, G., Zuther, J., Valencia-S., M., et al., 2012, PoS(Seyfert2012)060, arXiv:1307.1049Google Scholar
Fischer, S., Iserlohe, C., Zuther, J., et al., 2006, A&A, 452, 827Google Scholar
Kormendy, J. & Ho, L., 2013, ARA&A, 51, 511CrossRefGoogle Scholar
Smajić, S., Moser, L., Eckart, A., et al., 2014, A&A, 567, A119Google Scholar

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