Space VLBI Polarimetry of IDV Sources: Lessons from VSOP and Prospects for VSOP-2


Paper:	Space VLBI Polarimetry of IDV Sources: Lessons from VSOP and Prospects for VSOP-2
Volume:	402, Approaching Micro-Arcsecond Resolution with VSOP-2: Astrophysics and Technologies
Page:	252
Authors:	Bach, U.; Krichbaum, T.P.; Bernhart, S.; Impellizzeri, C.M.V.; Kraus, A.; Fuhrmann, L.; Witzel, A.; Zensus, J.A.
Abstract:	To locate and image the compact emission regions in quasars, which are closely connected to the phenomenon of IntraDay Variability (IDV), space VLBI observations are of prime importance. Here we report on VSOP observations of a prominent IDV source, the BL Lac objects S5 0716+714. To monitor their short term variability, these sources were observed with VSOP at 5GHz in several polarisation sensitive experiments, separated in time by one day to six days, in autumn 2000. Contemporaneous flux density measurements with the Effelsberg 100m radio telescope were used to directly compare the single dish IDV with changes of the VLBI images. A clear IDV behaviour in total intensity and linear polarization was observed in 0716+714. Analysis of the VLBI data shows that the variations are located inside the VLBI core component of 0716+714. In good agreement with the single-dish measurements, the VLBI ground array images and the VSOP images, both show a decrease in the total flux density of ∼ 20mJy and a drop of ∼ 5mJy in the linear polarization of the VLBI core. No variability was found in the jet. These findings are supported by VLBA observations of five IDV sources, including 0716+714, in December 2000, that show a similar behaviour. From the variability timescales we estimate a source size of a few micro-arcseconds and brightness temperatures exceeding 10¹⁵ K. Independent of whether the interpretation of the IDV seen in the VLBI core is source intrinsic or extrinsic a lower limit of T_B > 2×10¹² K is obtained by model fitting of the VLBI-core. Our results show that future VSOP2 observations should be accompanied by a single dish monitoring not only to discriminate between source-extrinsic (interstellar scintillation) and source-intrinsic effects but to allow also a proper calibration and interpretation of ultra-high resolution VSOP2 images.