Details

Autor(en) / Beteiligte

• Orienti, M.
• Koyama, S.
• D'Ammando, F.
• Giroletti, M.
• Kino, M.
• Nagai, H.
• Venturi, T.
• Dallacasa, D.
• Giovannini, G.
• Angelakis, E.
• Fuhrmann, L.
• Hovatta, T.
• Max-Moerbeck, W.
• Schinzel, F. K.
• Akiyama, K.
• Hada, K.
• Honma, M.
• Niinuma, K.
• Gasparrini, D.
• Krichbaum, T. P.
• Nestoras, I.
• Readhead, A. C. S.
• Richards, J. L.
• Riquelme, D.
• Sievers, A.
• Ungerechts, H.
• Zensus, J. A.

Titel

Radio and γ-ray follow-up of the exceptionally high-activity state of PKS 1510−089 in 2011

Ist Teil von

• Monthly notices of the Royal Astronomical Society, 2013-01, Vol.428 (3), p.2418-2429

Ort / Verlag

Oxford University Press

Erscheinungsjahr

2013

Quelle

Alma/SFX Local Collection

Beschreibungen/Notizen

• We investigate the radio and γ-ray variability of the flat spectrum radio quasar PKS 1510−089 in the time range between 2010 November and 2012 January. In this period the source showed an intense activity, with two major γ-ray flares detected in 2011 July and October. During the latter episode both the γ-ray and the radio flux density reached their historical peak. Multiwavelength analysis shows a rotation of about 380° of the optical polarization angle close in time with the rapid and strong γ-ray flare in 2011 July. An enhancement of the optical emission and an increase of the fractional polarization both in the optical and in radio bands are observed about three weeks later, close in time with another γ-ray outburst. On the other hand, after 2011 September a huge radio outburst has been detected, first in the millimetre regime followed with some time delay at centimetre down to decimetre wavelengths. This radio flare is characterized by a rising and a decaying stage, in agreement with the formation of a shock and its evolution, as a consequence of expansion and radiative cooling. If the γ-ray flare observed in 2011 October is related to this radio outburst, then this strongly indicates that the region responsible for the γ-ray variability is not within the broad line, but a few parsecs downstream along the jet.