Broad-band radio activity of gamma-ray flaring FSRQ B3 0650+453

ATel #3596; R. Schmidt, L. Fuhrmann, E. Angelakis, I. Nestoras, T. P. Krichbaum, J. A. Zensus (F-GAMMA team, MPIfR, Bonn, Germany), H. Ungerechts, A. Sievers, D. Riquelme (IRAM, Granada, Spain)
on 26 Aug 2011; 13:09 UT
Credential Certification: Emmanouil Angelakis (angelaki@mpifr-bonn.mpg.de)

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Responding to ATel #3580 reporting the recent Fermi/GST flaring activity of B3 0650+453 at gamma-rays late August 2011, we here report its behavior at radio bands as observed by the F-GAMMA program.

Long-term activity:
The source has been observed with the Effelsberg 100-m and the IRAM 30-m telescope since January and late July 2009, respectively. Since then, it showed a pronounced activity period chiefly at high frequencies starting in November 2009 until October 2010. After a brief minimum, the source switches to a raising trend at all frequencies in early 2011 (see e.g. 32 GHz).

Recent activity:
Recently, this long-term increasing trend turned into a rapid increase starting early May 2011 (see e.g. frequencies 10.45 GHz and above). For instsance, the flux density increased from 0.51+/-0.01 Jy to 1.11+/-0.04 Jy at 10.45 GHz, from 0.54+/-0.01 Jy to 1.24+/-0.06 Jy at 14.6 GHz and from 0.61+/-0.06 Jy to 1.71+/-0.19 Jy at 32 GHz on August 6, 2011. This radio activity is most likely related to the flaring event reported at gamma-rays. The radio light curves can be accessed separately at low, intermediate and high frequencies. Alternatively, also the evolution of its spectrum as a function of time can be accessed.

The source will be continuously monitored and possible future activity will be reported through the current platform.

F-GAMMA program:
F-GAMMA (Fermi-GST AGN Multi-frequency Monitoring Alliance) program is the coordinated effort of several observatories and research teams to probe AGN physics through the multi-frequency monitoring approach. The core program relies on monthly observations with the Effelsberg 100-m radio telescope (operating at 8 frequencies between 2.6 and 43 GHz), the IRAM 30-m telescope (observing at 86 and 142 GHz) and additional measurements with the APEX 12-m telescope (operating at 345 GHz). The core sample consists of roughly 60 Fermi-GST/LAT monitored blazars. The data are taken quasi-simultaneously within 40 minutes for Effelsberg and truly simultaneous at the IRAM telescope while the cross-station coherency is of order of 10 days. Data products are publicly accessible here.