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Revisiting the Geometry of the BLR in AKN120: Preliminary Results from UV Data and Line Profile Analysis

Published online by Cambridge University Press:  07 August 2017

D. Alloin ,
T. Baribaud ,
C. Boisson  and
D. Pelat
D. Alloin
Affiliation:
Observatoire de Paris, 92195, Meudon, France
T. Baribaud
Affiliation:
Observatoire de Paris, 92195, Meudon, France
C. Boisson
Affiliation:
Observatoire de Paris, 92195, Meudon, France
D. Pelat
Affiliation:
Observatoire de Paris, 92195, Meudon, France

Abstract

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From continuum and line intensity light-curves in the ultraviolet range, we find that the CIV peak-emission lies at about 2 ± 0.5 light-month from the centre. Line profile variations in the Ha and CIV emission suggest that the BLR is made of two regions with distinct kinematical properties:

  1. • a spherically distributed set of clouds, responsible for the broad HIL emission and responding to ionizing flux variations with a time-lag of 2 light-months at most

  2. • a disc-like structure from which most of the LIL emission arises, with a slow response to ionizing flux changes: hence larger is size.

Type
Part 4: Black Holes, Accretion Disks and Gravitational Lenses
Information
Symposium - International Astronomical Union , Volume 134: Active Galactic Nuclei , 1989 , pp. 259 - 261
Copyright
Copyright © Kluwer 1989 

References

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