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Feii strength in NLS1s – dependence on the viewing angle and FWHM(Hβ)

Published online by Cambridge University Press:  29 January 2021

Swayamtrupta Panda ,
Paola Marziani  and
Bożena Czerny
Swayamtrupta Panda
Affiliation:
Center For Theoretical Physics, Polish Academy of Sciences, Al. Lotników 32/46, 02-668 Warsaw, Poland email: panda@cft.edu.pl Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, Poland
Paola Marziani
Affiliation:
INAF-Astronomical Observatory of Padova, Vicolo dell’Osservatorio, 5, 35122PadovaPD, Italy
Bożena Czerny
Affiliation:
Center For Theoretical Physics, Polish Academy of Sciences, Al. Lotników 32/46, 02-668 Warsaw, Poland email: panda@cft.edu.pl
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Abstract

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We address the effect of orientation of the accretion disk plane and the geometry of the broad line region (BLR) in the context of understanding the distribution of quasars along their Main Sequence. We utilize the photoionization code CLOUDY to model the BLR, incorporating the ‘un-constant’ virial factor. We show the preliminary results of the analysis to highlight the co-dependence of the Eigenvector 1 parameter, RFeII on the broad HβFWHM (i.e. the line dispersion) and the inclination angle (θ), assuming fixed values for the Eddington ratio (Lbol/ LEdd), black hole mass (MBH), spectral energy distribution (SED) shape, cloud density (nH) and composition.†

Keywords

accretionaccretion disksradiation mechanisms: thermalradiative transfergalaxies: active(galaxies:) quasars: emission linesgalaxies: Seyfert
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S356: Nuclear Activity in Galaxies Across Cosmic Time , October 2019 , pp. 332 - 334
Copyright
© The Author(s), 2021. Published by Cambridge University Press on behalf of International Astronomical Union

Footnotes

†

The project was partially supported by NCN grant no. 2017/26/A/ST9/00756 (MAESTRO 9) and MNiSW grant DIR/WK/2018/12. PM acknowledges the INAF PRIN-SKA 2017 program 1.05.01.88.04.

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