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|Title:||Short timescale photometric and polarimetric behavior of two BL Lacertae type objects||Authors:||COVINO, Stefano
Baglio, M. C.
Barres de Almeida, U.
di Fabrizio, L.
MOLINARI, Emilio Carlo
RAITERI, Claudia Maria
|Issue Date:||2015||Journal:||ASTRONOMY & ASTROPHYSICS||Number:||578||First Page:||A68||Abstract:||Context. Blazars are astrophysical sources whose emission is dominated by non-thermal processes, i.e. synchrotron and inverse Compton emission. Although the general picture is rather robust and consistent with observations, many aspects are still unexplored. Aims: Polarimetric monitoring can offer a wealth of information about the physical processes in blazars. Models with largely different physical ingredients can provide almost indistinguishable predictions for the total flux, but usually are characterized by different polarization properties. We explore the possibility to derive structural information about the emitting regions of blazars by means of a joint analysis of rapid variability of the total and polarized flux at optical wavelengths. Methods: Short timescale (from tens of seconds to a couple of minutes) optical linear polarimetry and photometry for two blazars, <ASTROBJ>BL Lacertae</ASTROBJ> and <ASTROBJ>PKS 1424+240</ASTROBJ>, was carried out with the PAOLO polarimeter at the 3.6 m Telescopio Nazionale Galileo. Several hours of almost continuous observations were obtained for both sources. Results: Our intense monitoring allowed us to draw different scenarios for <ASTROBJ>BL Lacertae</ASTROBJ> and <ASTROBJ>PKS 1424+240</ASTROBJ>, with the former characterized by intense variability and the latter practically constant in total flux. Essentially the same behavior is observed for the polarized flux and the position angle. The variability time-scales turned out to be as short as a few minutes, although involving only a few percent variation of the flux. The polarization variability time-scale is generally consistent with the total flux variability. Total and polarized flux appear to be essentially uncorrelated. However, even during our relatively short monitoring, different regimes can be singled out. Conclusions: No simple scenario is able to satisfactorily model the very rich phenomenology exhibited in our data. Detailed numerical simulations show that the emitting region should be characterized by some symmetry, and the inclusion of turbulence for the magnetic field may constitute the missing ingredient for a more complete interpretation of the data. Partly based on data obtained at the INAF/Telescopio Nazionale Galileo at the Canary Island of La Palma under program Id: A29TAC_21 (PI: S. Covino).||Acknowledgments:||This work has been supported by ASI grant I/004/11/0. H.Z. is supported by the LANL/LDRD program and by DoE/Office of Fusion Energy Science through CMSO. Simulations were conducted on LANL’s Institutional Computing machines. The work of M.B. is supported by the Department and Technology and the National Research Foundation of South Africa through the South African Research Chair Initiative (SARChI). We also thank the anonymous referee for her/his competent comments that greatly enhanced the quality of the paper.||URI:||http://hdl.handle.net/20.500.12386/23677||URL:||https://www.aanda.org/articles/aa/abs/2015/06/aa25674-15/aa25674-15.html||ISSN:||0004-6361||DOI:||10.1051/0004-6361/201525674||Bibcode ADS:||2015A&A...578A..68C||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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