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Strong FeII emission in NLS1s: An unsolved mystery

Published online by Cambridge University Press:  10 June 2020

Swayamtrupta Panda Open the ORCID record for Swayamtrupta Panda [Opens in a new window] ,
Katarzyna Małek ,
Marzena Śniegowska  and
Bożena Czerny
Swayamtrupta Panda
Affiliation:
Center for Theoretical Physics — PAS, Al. Lotników 32/46, Warsaw, Poland 02—668 Nicolaus Copernicus Astronomical Center, ul. Bartycka 18, Warsaw, Poland 00—716
Katarzyna Małek
Affiliation:
National Center for Nuclear Research, ul. Hoża 69, Warsaw, Poland 00—681 Aix Marseille Univ. CNRS, CNES, LAM Marseille13388, France
Marzena Śniegowska
Affiliation:
Nicolaus Copernicus Astronomical Center, ul. Bartycka 18, Warsaw, Poland 00—716
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Abstract

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In Panda et al.2018a, we constructed a refined sample from the original Shen et al.(2011) QSO catalog. Based on our hypothesis — the main driver of the Quasar Main Sequence is the maximum of the accretion disk temperature (TBBB) defined by the Big Blue Bump on the Spectral Energy Distribution (Panda et al.2017; Panda et al.2018b). We select the four extreme sources that have RFeII ⩾ 4.0 and use {CIGALE (Boquien et al.2018) to fit their multi—band photometric data. We also perform detailed spectral fitting including the Fe II pseudo—continuum (based on Śniegowska et al.2018)) to estimate and compare the value of RFEII. We show the dependence of FeII strength on changing metallicity.

Keywords

galaxies: active(galaxies:) quasars: emission linesaccretion disksradiative transfertechniques: photometric
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S341: Challenges in Panchromatic Modelling with Next Generation Facilities , November 2019 , pp. 297 - 298
Copyright
© International Astronomical Union 2020

References

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