SIMBAD references

2012MNRAS.426..317D - Mon. Not. R. Astron. Soc., 426, 317-329 (2012/October-2)

SBS 0846+513: a new γ-ray-emitting narrow-line Seyfert 1 galaxy.

D'AMMANDO F., ORIENTI M., FINKE J., RAITERI C.M., ANGELAKIS E., FUHRMANN L., GIROLETTI M., HOVATTA T., MAX-MOERBECK W., PERKINS J.S., READHEAD A.C.S., RICHARDS J.L., STAWARZ L. and DONATO D.

Abstract (from CDS):

We report Fermi Large Area Telescope (LAT) observations of the radio-loud active galactic nucleus SBS 0846+513 (z = 0.5835), optically classified as a narrow-line Seyfert 1 galaxy, together with new and archival radio-to-X-ray data. The source was not active at γ-ray energies during the first two years of Fermi operation. A significant increase in activity was observed during 2010 October–2011 August. In particular, a strong γ-ray flare was observed in 2011 June reaching an isotropic γ-ray luminosity (0.1–300GeV) of 1.0 x 1048erg/s, comparable to that of the brightest flat spectrum radio quasars, and showing spectral evolution in γ rays. An apparent superluminal velocity of (8.2±1.5)c in the jet was inferred from 2011 to 2012 Very Long Baseline Array (VLBA) images, suggesting the presence of a highly relativistic jet.

Both the power released by this object during the flaring activity and the apparent superluminal velocity are strong indications of the presence of a relativistic jet as powerful as those of blazars. In addition, variability and spectral properties in radio and γ-ray bands indicate blazar-like behaviour, suggesting that, except for some distinct optical characteristics, SBS 0846+513 could be considered as a young blazar at the low end of the blazar's black hole mass distribution. Comparison of star formation rates from Hα and infrared luminosity as seen by Herschel*


Abstract Copyright: © 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS

Journal keyword(s): galaxies: active - galaxies: individual: SBS 0846+513 - galaxies: nuclei - galaxies: Seyfert - gamma-rays: general

Simbad objects: 11

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2019.10.17-13:52:21

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