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Very Long Baseline polarimetry and the γ-ray connection in Markarian 421 during the broadband campaign in 2011. / Lico, R.; Giroletti, M.; Orienti, M.; Gómez, J.L.; Casadio, C.; D'Ammando, F.; Blasi, M.G.; Cotton, W.; Edwards, P.G.; Fuhrmann, L.; Jorstad, S.; Kino, M.; Kovalev, Y.Y.; Krichbaum, T.P.; Marscher, A.P.; Paneque, D.; Piner, B.G.; Sokolovsky, K.V.

In: Astronomy and Astrophysics, Vol. 571, No. А54, 2014, p. 1-13.

Research output: Contribution to journal › Article

Harvard

Lico, R, Giroletti, M, Orienti, M, Gómez, JL, Casadio, C, D'Ammando, F, Blasi, MG, Cotton, W, Edwards, PG, Fuhrmann, L, Jorstad, S, Kino, M, Kovalev, YY, Krichbaum, TP, Marscher, AP, Paneque, D, Piner, BG & Sokolovsky, KV 2014, 'Very Long Baseline polarimetry and the γ-ray connection in Markarian 421 during the broadband campaign in 2011', Astronomy and Astrophysics, vol. 571, no. А54, pp. 1-13. https://doi.org/10.1051/0004-6361/201424341

APA

Lico, R., Giroletti, M., Orienti, M., Gómez, J. L., Casadio, C., D'Ammando, F., Blasi, M. G., Cotton, W., Edwards, P. G., Fuhrmann, L., Jorstad, S., Kino, M., Kovalev, Y. Y., Krichbaum, T. P., Marscher, A. P., Paneque, D., Piner, B. G., & Sokolovsky, K. V. (2014). Very Long Baseline polarimetry and the γ-ray connection in Markarian 421 during the broadband campaign in 2011. Astronomy and Astrophysics, 571(А54), 1-13. https://doi.org/10.1051/0004-6361/201424341

Vancouver

Lico R, Giroletti M, Orienti M, Gómez JL, Casadio C, D'Ammando F et al. Very Long Baseline polarimetry and the γ-ray connection in Markarian 421 during the broadband campaign in 2011. Astronomy and Astrophysics. 2014;571(А54):1-13. https://doi.org/10.1051/0004-6361/201424341

Author

Lico, R. ; Giroletti, M. ; Orienti, M. ; Gómez, J.L. ; Casadio, C. ; D'Ammando, F. ; Blasi, M.G. ; Cotton, W. ; Edwards, P.G. ; Fuhrmann, L. ; Jorstad, S. ; Kino, M. ; Kovalev, Y.Y. ; Krichbaum, T.P. ; Marscher, A.P. ; Paneque, D. ; Piner, B.G. ; Sokolovsky, K.V. / Very Long Baseline polarimetry and the γ-ray connection in Markarian 421 during the broadband campaign in 2011. In: Astronomy and Astrophysics. 2014 ; Vol. 571, No. А54. pp. 1-13.

BibTeX

@article{4a7ad14f4965400bb0f6145745d9fa40,
title = "Very Long Baseline polarimetry and the γ-ray connection in Markarian 421 during the broadband campaign in 2011",
abstract = "{\textcopyright} 2014 ESO. Aims. We investigate the structure of the high angular resolution polarization, the magnetic topology, the total intensity light curve, the γ-ray flux, and the photon index. We describe how they evolve and how they are connected. Methods. We analyzed data in polarized intensity obtained with the Very Long Baseline Array (VLBA) at twelve epochs (one observation per month from January to December 2011) at 15, 24, and 43 GHz. For the absolute orientation of the electric vector position angles (EVPA) we used the D-terms method; we also confirm its accuracy. We also used γ-ray data from the Fermi Large Area Telescope on weekly time bins throughout 2011. Results. The source shows polarized emission, and its properties vary with time, frequency, and location along the jet. The core mean polarization fraction is generally between 1% and 2%, with a 4% peak at 43 GHz in March; the polarization angle is variable, mainly at 15 GHz, where it changes frequently, and less so at 43 GHz, where it oscillates in the",
author = "R. Lico and M. Giroletti and M. Orienti and J.L. G{\'o}mez and C. Casadio and F. D'Ammando and M.G. Blasi and W. Cotton and P.G. Edwards and L. Fuhrmann and S. Jorstad and M. Kino and Y.Y. Kovalev and T.P. Krichbaum and A.P. Marscher and D. Paneque and B.G. Piner and K.V. Sokolovsky",
year = "2014",
doi = "10.1051/0004-6361/201424341",
language = "English",
volume = "571",
pages = "1--13",
journal = "ASTRONOMY & ASTROPHYSICS",
issn = "0004-6361",
publisher = "EDP Sciences",
number = "А54",

}

RIS

TY - JOUR

T1 - Very Long Baseline polarimetry and the γ-ray connection in Markarian 421 during the broadband campaign in 2011

AU - Lico, R.

AU - Giroletti, M.

AU - Orienti, M.

AU - Gómez, J.L.

AU - Casadio, C.

AU - D'Ammando, F.

AU - Blasi, M.G.

AU - Cotton, W.

AU - Edwards, P.G.

AU - Fuhrmann, L.

AU - Jorstad, S.

AU - Kino, M.

AU - Kovalev, Y.Y.

AU - Krichbaum, T.P.

AU - Marscher, A.P.

AU - Paneque, D.

AU - Piner, B.G.

AU - Sokolovsky, K.V.

PY - 2014

Y1 - 2014

N2 - © 2014 ESO. Aims. We investigate the structure of the high angular resolution polarization, the magnetic topology, the total intensity light curve, the γ-ray flux, and the photon index. We describe how they evolve and how they are connected. Methods. We analyzed data in polarized intensity obtained with the Very Long Baseline Array (VLBA) at twelve epochs (one observation per month from January to December 2011) at 15, 24, and 43 GHz. For the absolute orientation of the electric vector position angles (EVPA) we used the D-terms method; we also confirm its accuracy. We also used γ-ray data from the Fermi Large Area Telescope on weekly time bins throughout 2011. Results. The source shows polarized emission, and its properties vary with time, frequency, and location along the jet. The core mean polarization fraction is generally between 1% and 2%, with a 4% peak at 43 GHz in March; the polarization angle is variable, mainly at 15 GHz, where it changes frequently, and less so at 43 GHz, where it oscillates in the

AB - © 2014 ESO. Aims. We investigate the structure of the high angular resolution polarization, the magnetic topology, the total intensity light curve, the γ-ray flux, and the photon index. We describe how they evolve and how they are connected. Methods. We analyzed data in polarized intensity obtained with the Very Long Baseline Array (VLBA) at twelve epochs (one observation per month from January to December 2011) at 15, 24, and 43 GHz. For the absolute orientation of the electric vector position angles (EVPA) we used the D-terms method; we also confirm its accuracy. We also used γ-ray data from the Fermi Large Area Telescope on weekly time bins throughout 2011. Results. The source shows polarized emission, and its properties vary with time, frequency, and location along the jet. The core mean polarization fraction is generally between 1% and 2%, with a 4% peak at 43 GHz in March; the polarization angle is variable, mainly at 15 GHz, where it changes frequently, and less so at 43 GHz, where it oscillates in the

U2 - 10.1051/0004-6361/201424341

DO - 10.1051/0004-6361/201424341

M3 - Article

VL - 571

SP - 1

EP - 13

JO - ASTRONOMY & ASTROPHYSICS

JF - ASTRONOMY & ASTROPHYSICS

SN - 0004-6361

IS - А54

ER -

ID: 7036217