Are Narrow Line Seyfert 1s a special class of Active Galactic Nuclei?

Дата и время публикации : 2013-05-14T20:00:02Z

Авторы публикации и институты :
M. Valencia-S. (I. Physikalisches Institut, University of Cologne, Max-Planck-Institut fuer Radioastronomie)
J. Zuther (I. Physikalisches Institut, University of Cologne)
A. Eckart (I. Physikalisches Institut, University of Cologne, Max-Planck-Institut fuer Radioastronomie)
S. Smajic (I. Physikalisches Institut, University of Cologne, Max-Planck-Institut fuer Radioastronomie)
C. Iserlohe (I. Physikalisches Institut, University of Cologne)
M. Garcia-Marin (I. Physikalisches Institut, University of Cologne)
G. Busch (I. Physikalisches Institut, University of Cologne)
M. Vitale (I. Physikalisches Institut, University of Cologne, Max-Planck-Institut fuer Radioastronomie)
M. Bremer (I. Physikalisches Institut, University of Cologne)
S. Fischer (I. Physikalisches Institut, University of Cologne)
M. Horrobin (I. Physikalisches Institut, University of Cologne)
L. Moser (I. Physikalisches Institut, University of Cologne)
Y. E. Rashed (I. Physikalisches Institut, University of Cologne)
C. Straubmeier (I. Physikalisches Institut, University of Cologne)
. (I. Physikalisches Institut, University of Cologne, Max-Planck-Institut fuer Radioastronomie)

Ссылка на журнал-издание: Ссылка на журнал-издание не найдена
Коментарии к cтатье: New version includes a Figure and extra references. Proceedings of the Conference “Nuclei of Seyfert galaxies and QSOs – Central engine & conditions of star formation” (Bonn, Germany, 6-8 November 2012)
Первичная категория: astro-ph.CO

Все категории : astro-ph.CO

Краткий обзор статьи: No. Due to their apparently extreme optical to X-ray properties, Narrow Line Seyfert 1s (NLSy1s) have been considered a special class of active galactic nuclei (AGN). Here, we summarize observational results from different groups to conclude that none of the characteristics that are typically used to define the NLSy1s as a distinct group – from the, nowadays called, Broad Line Seyfert 1s (BLSy1s) – is unique, nor ubiquitous of these particular sources, but shared by the whole Type 1 AGN. Historically, the NLSy1s have been distinguished from the BLSy1s by the narrow width of the broad Hbeta emission line. The upper limit on the full width at half maximum of this line is 2000 km/s for NLSy1s, while in BLSy1s it can be of several thousands of km/s. However, this border has been arbitrarily set and does not correspond to the change of any physical property. All observed parameters in Type 1 AGN cover continues ranges of values, which does not allow to infer the existence of two different kind of populations with FWHM(Hbeta,broad) = 2000 km/s as dividing point. We argue that the usage of this velocity limit to define samples of NLSy1s galaxies – as it is usually done in comparative studies -, together with the well known observational biases, naturally favors the selection of sources with low black hole masses and high Eddington ratios that are hosted by blue spiral galaxies. Therefore selection biases might be responsible for the reported differences between NLSy1 and BLSy1 sources.

Category: Physics