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DOI

  • Pouya M. Kouch
  • Ioannis Liodakis
  • Riccardo Middei
  • Dawoon E. Kim
  • Fabrizio Tavecchio
  • Alan P. Marscher
  • Herman L. Marshall
  • Steven R. Ehlert
  • Laura Di Gesu
  • Iván Agudo
  • Grzegorz M. Madejski
  • Roger W. Romani
  • Manel Errando
  • Elina Lindfors
  • Kari Nilsson
  • Ella Toppari
  • Stephen B. Potter
  • Ryo Imazawa
  • Mahito Sasada
  • Yasushi Fukazawa
  • Koji S. Kawabata
  • Makoto Uemura
  • Tsunefumi Mizuno
  • Tatsuya Nakaoka
  • Hiroshi Akitaya
  • Callum McCall
  • Helen E. Jermak
  • Iain A. Steele
  • Ioannis Myserlis
  • Mark Gurwell
  • Garrett K. Keating
  • Ramprasad Rao
  • Sincheol Kang
  • Sang-Sung Lee
  • Sang-Hyun Kim
  • Whee Yeon Cheong
  • Hyeon-Woo Jeong
  • Emmanouil Angelakis
  • Alexander Kraus
  • Francisco José Aceituno
  • Giacomo Bonnoli
  • Víctor Casanova
  • Juan Escudero
  • Beatriz Agís-González
  • César Husillos
  • Daniel Morcuende
  • Jorge Otero-Santos
  • Alfredo Sota
  • Rumen Bachev
  • Lucio Angelo Antonelli
  • Matteo Bachetti
  • Luca Baldini
  • Wayne H. Baumgartner
  • Ronaldo Bellazzini
  • Stefano Bianchi
  • Stephen D. Bongiorno
  • Raffaella Bonino
  • Alessandro Brez
  • Niccolò Bucciantini
  • Fiamma Capitanio
  • Simone Castellano
  • Elisabetta Cavazzuti
  • Chien-Ting Chen
  • Stefano Ciprini
  • Enrico Costa
  • Alessandra De Rosa
  • Ettore Del Monte
  • Niccolò Di Lalla
  • Alessandro Di Marco
  • Immacolata Donnarumma
  • Victor Doroshenko
  • Michal Dovčiak
  • Teruaki Enoto
  • Yuri Evangelista
  • Sergio Fabiani
  • Riccardo Ferrazzoli
  • Javier A. Garcia
  • Shuichi Gunji
  • Kiyoshi Hayashida
  • Jeremy Heyl
  • Wataru Iwakiri
  • Philip Kaaret
  • Vladimir Karas
  • Fabian Kislat
  • Takao Kitaguchi
  • Jeffery J. Kolodziejczak
  • Henric Krawczynski
  • Fabio La Monaca
  • Luca Latronico
  • Simone Maldera
  • Alberto Manfreda
  • Frédéric Marin
  • Andrea Marinucci
  • Francesco Massaro
  • Giorgio Matt
  • Ikuyuki Mitsuishi
  • Fabio Muleri
  • Michela Negro
  • Chi-Yung Ng
  • Stephen L. O'Dell
  • Nicola Omodei
  • Chiara Oppedisano
  • Alessandro Papitto
  • George G. Pavlov
  • Abel Lawrence Peirson
  • Matteo Perri
  • Melissa Pesce-Rollins
  • Pierre-Olivier Petrucci
  • Maura Pilia
  • Andrea Possenti
  • Juri Poutanen
  • Simonetta Puccetti
  • Brian D. Ramsey
  • John Rankin
  • Ajay Ratheesh
  • Oliver J. Roberts
  • Carmelo Sgrò
  • Patrick Slane
  • Paolo Soffitta
  • Gloria Spandre
  • Douglas A. Swartz
  • Toru Tamagawa
  • Roberto Taverna
  • Yuzuru Tawara
  • Allyn F. Tennant
  • Nicholas E. Thomas
  • Francesco Tombesi
  • Alessio Trois
  • Sergey S. Tsygankov
  • Roberto Turolla
  • Jacco Vink
  • Martin C. Weisskopf
  • Kinwah Wu
  • Fei Xie
  • Silvia Zane
We report the X-ray polarization properties of the high-synchrotron-peaked (HSP) blazar PKS 2155‑304 based on observations with the Imaging X-ray Polarimetry Explorer (IXPE). We observed the source between Oct 27 and Nov 7, 2023. We also conducted an extensive contemporaneous multiwavelength (MW) campaign. We find that during the first half (T1) of the IXPE pointing, the source exhibited the highest X-ray polarization degree detected for an HSP blazar thus far, (30.7 ± 2.0)%; this dropped to (15.3 ± 2.1)% during the second half (T2). The X-ray polarization angle remained stable during the IXPE pointing at 129.4° ±1.8° and 125.4° ±3.9° during T1 and T2, respectively. Meanwhile, the optical polarization degree remained stable during the IXPE pointing, with average host-galaxy-corrected values of (4.3 ± 0.7)% and (3.8 ± 0.9)% during the T1 and T2, respectively. During the IXPE pointing, the optical polarization angle changed achromatically from ∼140° to ∼90° and back to ∼130°. Despite several attempts, we only detected (99.7% conf.) the radio polarization once (during T2, at 225.5 GHz): with degree (1.7 ± 0.4)% and angle 112.5° ±5.5°. The direction of the broad pc-scale jet is rather ambiguous and has been found to point to the east and south at different epochs; however, on larger scales (> 1.5 pc) the jet points toward the southeast (∼135°), similarly to all of the MW polarization angles. Moreover, the X-ray-to-optical polarization degree ratios of ∼7 and ∼4 during T1 and T2, respectively, are similar to previous IXPE results for several HSP blazars. These findings, combined with the lack of correlation of temporal variability between the MW polarization properties, agree with an energy-stratified shock-acceleration scenario in HSP blazars.
Язык оригиналаанглийский
Номер статьиA119
ЖурналAstronomy and Astrophysics
Том689
DOI
СостояниеОпубликовано - 1 сен 2024

    Области исследований

  • magnetic fields, polarization, relativistic processes, BL Lacertae objects: individual: HSP, galaxies: jets, Astrophysics - High Energy Astrophysical Phenomena

ID: 125281778