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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.18152">arXiv:2412.18152</a> <span> [<a href="https://arxiv.org/pdf/2412.18152">pdf</a>, <a href="https://arxiv.org/format/2412.18152">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Extremely luminous optical afterglow of a distant and energetic gamma-ray burst GRB 230204B </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gupta%2C+R">Rahul Gupta</a>, <a href="/search/astro-ph?searchtype=author&query=Racusin%2C+J">Judith Racusin</a>, <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V">Vladimir Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+Y+-">Y. -D. Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Gulati%2C+A">Ashna Gulati</a>, <a href="/search/astro-ph?searchtype=author&query=Castro-Tirado%2C+A+J">Alberto J. Castro-Tirado</a>, <a href="/search/astro-ph?searchtype=author&query=Murphy%2C+T">Tara Murphy</a>, <a href="/search/astro-ph?searchtype=author&query=Serino%2C+M">Motoko Serino</a>, <a href="/search/astro-ph?searchtype=author&query=Zhirkov%2C+K">Kirill Zhirkov</a>, <a href="/search/astro-ph?searchtype=author&query=Shilling%2C+S">S. Shilling</a>, <a href="/search/astro-ph?searchtype=author&query=Oates%2C+S+R">Samantha R. Oates</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+J+K">James K. Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Parsotan%2C+T">T. Parsotan</a>, <a href="/search/astro-ph?searchtype=author&query=Ror%2C+A+K">Amit K. Ror</a>, <a href="/search/astro-ph?searchtype=author&query=Pandey%2C+S+B">Shashi B. Pandey</a>, <a href="/search/astro-ph?searchtype=author&query=Iyyani%2C+S">S. Iyyani</a>, <a href="/search/astro-ph?searchtype=author&query=Sharma%2C+V">V. Sharma</a>, <a href="/search/astro-ph?searchtype=author&query=Aryan%2C+A">A. Aryan</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+J">Jin-Ming Bai</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P">Pavel Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+D">David Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Caballero-Garc%C3%ADa%2C+M+D">Mar铆a D. Caballero-Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Carrasco-Garc%C3%ADa%2C+I+M">I. M. Carrasco-Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Castell%C3%B3n%2C+A">A. Castell贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Castillo%2C+S">Sebasti谩n Castillo</a> , et al. (25 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.18152v1-abstract-short" style="display: inline;"> Robotic telescope networks play an important role in capturing early and bright optical afterglows, providing critical insights into the energetics and emission mechanisms of GRBs. In this study, we analyze GRB 230204B, an exceptionally energetic and multi-pulsed long GRB, detected by the Fermi GBM and MAXI detectors, with an isotropic equivalent gamma-ray energy exceeding 10$^{54}$ erg. Time-reso… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.18152v1-abstract-full').style.display = 'inline'; document.getElementById('2412.18152v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.18152v1-abstract-full" style="display: none;"> Robotic telescope networks play an important role in capturing early and bright optical afterglows, providing critical insights into the energetics and emission mechanisms of GRBs. In this study, we analyze GRB 230204B, an exceptionally energetic and multi-pulsed long GRB, detected by the Fermi GBM and MAXI detectors, with an isotropic equivalent gamma-ray energy exceeding 10$^{54}$ erg. Time-resolved spectral analysis reveals a transition in the prompt emission from hard (sub-photospheric dominated) spectra during early pulses to softer (synchrotron radiation dominated) spectra in later pulses, indicative of a hybrid jet composition. We report the discovery and characterization of the optical afterglow using the MASTER and BOOTES robotic telescope networks, alongside long-term radio observations extending to 335 days post-burst with the ATCA. At ~1.3 ks post-burst, the optical luminosity was exceptionally high, surpassing even other bright GRBs, such as GRB 221009A (the ``BOAT"). Multi-wavelength modeling, incorporating data from MASTER, BOOTES, DOT, Swift/XRT, and radio observations, was conducted using an external ISM forward-shock top-hat jet model with afterglowpy. The results reveal a narrow and highly collimated jet with a circumburst density of n$_{0}$ ~ 28.12 cm$^{-3}$, kinetic energy E$_{K}$ ~ 4.18 x 10$^{55}$ erg, and a relatively low value of $蔚_{B}$ = 2.14 x 10$^{-6}$, indicating shock-compression of the magnetic field in the surrounding interstellar medium. We constrained a low radiative efficiency of ~ 4.3 %. This study highlights the indispensable contribution of robotic networks to early afterglow observations and advances our understanding of GRB 230204B unique characteristics and underlying jet physics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.18152v1-abstract-full').style.display = 'none'; document.getElementById('2412.18152v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27 pages, 12 figures, 8 tables, submitted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.04068">arXiv:2412.04068</a> <span> [<a href="https://arxiv.org/pdf/2412.04068">pdf</a>, <a href="https://arxiv.org/format/2412.04068">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Multi-wavelength picture of the misaligned BL Lac object 3C 371 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Otero-Santos%2C+J">J. Otero-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Raiteri%2C+C+M">C. M. Raiteri</a>, <a href="/search/astro-ph?searchtype=author&query=Tramacere%2C+A">A. Tramacere</a>, <a href="/search/astro-ph?searchtype=author&query=Pedrosa%2C+J+E">J. Escudero Pedrosa</a>, <a href="/search/astro-ph?searchtype=author&query=Acosta-Pulido%2C+J+A">J. A. Acosta-Pulido</a>, <a href="/search/astro-ph?searchtype=author&query=Carnerero%2C+M+I">M. I. Carnerero</a>, <a href="/search/astro-ph?searchtype=author&query=Villata%2C+M">M. Villata</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Rahimov%2C+I+A">I. A. Rahimov</a>, <a href="/search/astro-ph?searchtype=author&query=Andreeva%2C+T+S">T. S. Andreeva</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+D+V">D. V. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Marchili%2C+N">N. Marchili</a>, <a href="/search/astro-ph?searchtype=author&query=Righini%2C+S">S. Righini</a>, <a href="/search/astro-ph?searchtype=author&query=Giroletti%2C+M">M. Giroletti</a>, <a href="/search/astro-ph?searchtype=author&query=Gurwell%2C+M+A">M. A. Gurwell</a>, <a href="/search/astro-ph?searchtype=author&query=Savchenko%2C+S+S">S. S. Savchenko</a>, <a href="/search/astro-ph?searchtype=author&query=Carosati%2C+D">D. Carosati</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W+P">W. P. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtanidze%2C+S+O">S. O. Kurtanidze</a>, <a href="/search/astro-ph?searchtype=author&query=Joner%2C+M+D">M. D. Joner</a>, <a href="/search/astro-ph?searchtype=author&query=Semkov%2C+E">E. Semkov</a>, <a href="/search/astro-ph?searchtype=author&query=Pursimo%2C+T">T. Pursimo</a>, <a href="/search/astro-ph?searchtype=author&query=Ben%C3%ADtez%2C+E">E. Ben铆tez</a>, <a href="/search/astro-ph?searchtype=author&query=Damljanovic%2C+G">G. Damljanovic</a>, <a href="/search/astro-ph?searchtype=author&query=Andreuzzi%2C+G">G. Andreuzzi</a> , et al. (30 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.04068v2-abstract-short" style="display: inline;"> The BL Lac object 3C 371 is one of the targets that are regularly monitored by the Whole Earth Blazar Telescope (WEBT) Collaboration to study blazar variability on both short and long timescales. We aim to evaluate the long-term multiwavelength (MWL) behaviour of 3C 371, comparing it with the results derived for its optical emission in our previous study. For this, we make use of the multi-band ca… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.04068v2-abstract-full').style.display = 'inline'; document.getElementById('2412.04068v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.04068v2-abstract-full" style="display: none;"> The BL Lac object 3C 371 is one of the targets that are regularly monitored by the Whole Earth Blazar Telescope (WEBT) Collaboration to study blazar variability on both short and long timescales. We aim to evaluate the long-term multiwavelength (MWL) behaviour of 3C 371, comparing it with the results derived for its optical emission in our previous study. For this, we make use of the multi-band campaigns organized by the WEBT Collaboration in optical and radio between January 2018 and December 2020, and of public data from Swift and Fermi satellites and the MOJAVE Very Large Interferometry programme. We evaluate the variability shown by the source in each band with the amplitude variability quantification, as well as possible interband correlation using the z-Discrete Correlation Function. We also present a deep analysis of the optical-UV, X-ray and $纬$-ray spectral variability. With the MOJAVE data we perform a kinematics analysis, looking for components propagating along the jet, calculating its kinematics parameters. This set of parameters is later used for the interpretation of the source MWL behaviour, modelling the broadband spectral energy distribution (SED) of the source with theoretical blazar emission scenarios. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.04068v2-abstract-full').style.display = 'none'; document.getElementById('2412.04068v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in A&A, 23 pages, 15 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.22319">arXiv:2410.22319</a> <span> [<a href="https://arxiv.org/pdf/2410.22319">pdf</a>, <a href="https://arxiv.org/format/2410.22319">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202452311">10.1051/0004-6361/202452311 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A wiggling filamentary jet at the origin of the blazar multi-wavelength behaviour </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Raiteri%2C+C+M">C. M. Raiteri</a>, <a href="/search/astro-ph?searchtype=author&query=Villata%2C+M">M. Villata</a>, <a href="/search/astro-ph?searchtype=author&query=Carnerero%2C+M+I">M. I. Carnerero</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtanidze%2C+S+O">S. O. Kurtanidze</a>, <a href="/search/astro-ph?searchtype=author&query=Mirzaqulov%2C+D+O">D. O. Mirzaqulov</a>, <a href="/search/astro-ph?searchtype=author&query=Ben%C3%ADtez%2C+E">E. Ben铆tez</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnoli%2C+G">G. Bonnoli</a>, <a href="/search/astro-ph?searchtype=author&query=Carosati%2C+D">D. Carosati</a>, <a href="/search/astro-ph?searchtype=author&query=Acosta-Pulido%2C+J+A">J. A. Acosta-Pulido</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Andreeva%2C+T+S">T. S. Andreeva</a>, <a href="/search/astro-ph?searchtype=author&query=Apolonio%2C+G">G. Apolonio</a>, <a href="/search/astro-ph?searchtype=author&query=Bachev%2C+R">R. Bachev</a>, <a href="/search/astro-ph?searchtype=author&query=Borman%2C+G+A">G. A. Borman</a>, <a href="/search/astro-ph?searchtype=author&query=Bozhilov%2C+V">V. Bozhilov</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+L+F">L. F. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Carbonell%2C+W">W. Carbonell</a>, <a href="/search/astro-ph?searchtype=author&query=Casadio%2C+C">C. Casadio</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W+P">W. P. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Damljanovic%2C+G">G. Damljanovic</a>, <a href="/search/astro-ph?searchtype=author&query=Ehgamberdiev%2C+S+A">S. A. Ehgamberdiev</a>, <a href="/search/astro-ph?searchtype=author&query=Elsaesser%2C+D">D. Elsaesser</a>, <a href="/search/astro-ph?searchtype=author&query=Escudero%2C+J">J. Escudero</a>, <a href="/search/astro-ph?searchtype=author&query=Feige%2C+M">M. Feige</a>, <a href="/search/astro-ph?searchtype=author&query=Fuentes%2C+A">A. Fuentes</a> , et al. (74 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.22319v1-abstract-short" style="display: inline;"> Blazars are beamed active galactic nuclei known for their strong multi-wavelength variability on timescales from years down to minutes. We aim to investigate the suitability of the twisting jet model presented in previous works to explain the multi-wavelength behaviour of BL Lacertae, the prototype of one of the blazar classes. According to this model, the jet is inhomogeneous, curved, and twistin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.22319v1-abstract-full').style.display = 'inline'; document.getElementById('2410.22319v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.22319v1-abstract-full" style="display: none;"> Blazars are beamed active galactic nuclei known for their strong multi-wavelength variability on timescales from years down to minutes. We aim to investigate the suitability of the twisting jet model presented in previous works to explain the multi-wavelength behaviour of BL Lacertae, the prototype of one of the blazar classes. According to this model, the jet is inhomogeneous, curved, and twisting, and the long-term variability is due to changes in the Doppler factor due to variations in the orientation of the jet-emitting regions. We analysed optical data of the source obtained during monitoring campaigns organised by the Whole Earth Blazar Telescope (WEBT) in 2019-2022, together with radio data from the WEBT and other teams, and gamma-ray data from the Fermi satellite. In this period, BL Lacertae underwent an extraordinary activity phase, reaching its historical optical and gamma-ray brightness maxima. The application of the twisting jet model to the source light curves allows us to infer the wiggling motion of the optical, radio, and gamma-ray jet-emitting regions. The optical-radio correlation shows that the changes in the radio viewing angle follow those in the optical viewing angle by about 120 days, and it suggests that the jet is composed of plasma filaments, which is in agreement with some radio high-resolution observations of other sources. The gamma-ray emitting region is found to be co-spatial with the optical one, and the analysis of the gamma-optical correlation is consistent with both the geometric interpretation and a synchrotron self-Compton (SSC) origin of the high-energy photons. We propose a geometric scenario where the jet is made up of a pair of emitting plasma filaments in a sort of double-helix curved rotating structure, whose wiggling motion produces changes in the Doppler beaming and can thus explain the observed multi-wavelength long-term variability. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.22319v1-abstract-full').style.display = 'none'; document.getElementById('2410.22319v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">In press for A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 692 (2024) A48 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.17983">arXiv:2409.17983</a> <span> [<a href="https://arxiv.org/pdf/2409.17983">pdf</a>, <a href="https://arxiv.org/format/2409.17983">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> GRB 240529A: A Tale of Two Shocks </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sun%2C+T">Tian-Rui Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Geng%2C+J">Jin-Jun Geng</a>, <a href="/search/astro-ph?searchtype=author&query=Yan%2C+J">Jing-Zhi Yan</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+Y">You-Dong Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+X">Xue-Feng Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Castro-Tirado%2C+A+J">Alberto J. Castro-Tirado</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+C">Chao Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Ping%2C+Y">Yi-Ding Ping</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+C">Chen-Ran Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+F">Fan Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+H">Hao-Xuan Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Jiang%2C+J">Ji-An Jiang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+Y">Yan-Tian Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Xue%2C+Y">Yongquan Xue</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Garc%C3%ADa%2C+I">Ignacio P茅rez-Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+S">Si-Yu Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Garc%C3%ADa%2C+E">Emilio Fern谩ndez-Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Caballero-Garc%C3%ADa%2C+M+D">Mar铆a D. Caballero-Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Ram%C3%ADrez%2C+R">Rub茅n S谩nchez-Ram铆rez</a>, <a href="/search/astro-ph?searchtype=author&query=Guziy%2C+S">Sergiy Guziy</a>, <a href="/search/astro-ph?searchtype=author&query=Olivares%2C+I">Ignacio Olivares</a>, <a href="/search/astro-ph?searchtype=author&query=del+Pulgar%2C+C+J+P">Carlos Jesus P茅rez del Pulgar</a>, <a href="/search/astro-ph?searchtype=author&query=Castell%C3%B3n%2C+A">A. Castell贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Castillo%2C+S">Sebasti谩n Castillo</a>, <a href="/search/astro-ph?searchtype=author&query=Xiong%2C+D">Ding-Rong Xiong</a> , et al. (44 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.17983v1-abstract-short" style="display: inline;"> Thanks to the rapidly increasing time-domain facilities, we are entering a golden era of research on gamma-ray bursts (GRBs). In this Letter, we report our observations of GRB 240529A with the Burst Optical Observer and Transient Exploring System, the 1.5-meter telescope at Observatorio Sierra Nevada, the 2.5-meter Wide Field Survey Telescope of China, the Large Binocular Telescope, and the Telesc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.17983v1-abstract-full').style.display = 'inline'; document.getElementById('2409.17983v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.17983v1-abstract-full" style="display: none;"> Thanks to the rapidly increasing time-domain facilities, we are entering a golden era of research on gamma-ray bursts (GRBs). In this Letter, we report our observations of GRB 240529A with the Burst Optical Observer and Transient Exploring System, the 1.5-meter telescope at Observatorio Sierra Nevada, the 2.5-meter Wide Field Survey Telescope of China, the Large Binocular Telescope, and the Telescopio Nazionale Galileo. The prompt emission of GRB 240529A shows two comparable energetic episodes separated by a quiescence time of roughly 400 s. Combining all available data on the GRB Coordinates Network, we reveal the simultaneous apparent X-ray plateau and optical re-brightening around $10^3-10^4$ s after the burst. Rather than the energy injection from the magnetar as widely invoked for similar GRBs, the multi-wavelength emissions could be better explained as two shocks launched from the central engine separately. The optical peak time and our numerical modeling suggest that the initial bulk Lorentz factor of the later shock is roughly 50, which indicates that the later jet should be accretion-driven and have a higher mass loading than a typical one. The quiescence time between the two prompt emission episodes may be caused by the transition between different accretion states of a central magnetar or black hole, or the fall-back accretion process. A sample of similar bursts with multiple emission episodes in the prompt phase and sufficient follow-up could help to probe the underlying physics of GRB central engines. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.17983v1-abstract-full').style.display = 'none'; document.getElementById('2409.17983v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Resubmitted to ApJL after addressing the referee's comments; comments are welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.15554">arXiv:2406.15554</a> <span> [<a href="https://arxiv.org/pdf/2406.15554">pdf</a>, <a href="https://arxiv.org/format/2406.15554">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202451037">10.1051/0004-6361/202451037 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Testing particle acceleration in blazar jets with continuous high-cadence optical polarization observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liodakis%2C+I">Ioannis Liodakis</a>, <a href="/search/astro-ph?searchtype=author&query=Kiehlmann%2C+S">Sebastian Kiehlmann</a>, <a href="/search/astro-ph?searchtype=author&query=Marscher%2C+A+P">Alan P. Marscher</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Haocheng Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Blinov%2C+D">Dmitry Blinov</a>, <a href="/search/astro-ph?searchtype=author&query=Jorstad%2C+S+G">Svetlana G. Jorstad</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">Iv谩n Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Ben%C3%ADtez%2C+E">Erika Ben铆tez</a>, <a href="/search/astro-ph?searchtype=author&query=Berdyugin%2C+A">Andrei Berdyugin</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnoli%2C+G">Giacomo Bonnoli</a>, <a href="/search/astro-ph?searchtype=author&query=Casadio%2C+C">Carolina Casadio</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+C">Chien-Ting Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">Wen-Ping Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Ehlert%2C+S+R">Steven R. Ehlert</a>, <a href="/search/astro-ph?searchtype=author&query=Escudero%2C+J">Juan Escudero</a>, <a href="/search/astro-ph?searchtype=author&query=Grishina%2C+T+S">Tatiana S. Grishina</a>, <a href="/search/astro-ph?searchtype=author&query=Hiriart%2C+D">David Hiriart</a>, <a href="/search/astro-ph?searchtype=author&query=Hsu%2C+A">Angela Hsu</a>, <a href="/search/astro-ph?searchtype=author&query=Imazawa%2C+R">Ryo Imazawa</a>, <a href="/search/astro-ph?searchtype=author&query=Jermak%2C+H+E">Helen E. Jermak</a>, <a href="/search/astro-ph?searchtype=author&query=Jose%2C+J">Jincen Jose</a>, <a href="/search/astro-ph?searchtype=author&query=Kaaret%2C+P">Philip Kaaret</a>, <a href="/search/astro-ph?searchtype=author&query=Kopatskaya%2C+E+N">Evgenia N. Kopatskaya</a>, <a href="/search/astro-ph?searchtype=author&query=Lalchand%2C+B">Bhavana Lalchand</a>, <a href="/search/astro-ph?searchtype=author&query=Larionova%2C+E+G">Elena G. Larionova</a> , et al. (22 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.15554v1-abstract-short" style="display: inline;"> Variability can be the pathway to understanding the physical processes in astrophysical jets, however, the high-cadence observations required to test particle acceleration models are still missing. Here we report on the first attempt to produce continuous, >24 hour polarization light curves of blazars using telescopes distributed across the globe and the rotation of the Earth to avoid the rising S… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.15554v1-abstract-full').style.display = 'inline'; document.getElementById('2406.15554v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.15554v1-abstract-full" style="display: none;"> Variability can be the pathway to understanding the physical processes in astrophysical jets, however, the high-cadence observations required to test particle acceleration models are still missing. Here we report on the first attempt to produce continuous, >24 hour polarization light curves of blazars using telescopes distributed across the globe and the rotation of the Earth to avoid the rising Sun. Our campaign involved 16 telescopes in Asia, Europe, and North America. We observed BL Lacertae and CGRaBS J0211+1051 for a combined 685 telescope hours. We find large variations in the polarization degree and angle for both sources in sub-hour timescales as well as a ~180 degree rotation of the polarization angle in CGRaBS J0211+1051 in less than two days. We compared our high-cadence observations to Particle-In-Cell magnetic reconnection and turbulent plasma simulations. We find that although the state of the art simulation frameworks can produce a large fraction of the polarization properties, they do not account for the entirety of the observed polarization behavior in blazar jets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.15554v1-abstract-full').style.display = 'none'; document.getElementById('2406.15554v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 15 figures, 2 tables, accepted for publication in A&A. The data used in the paper are available here: https://doi.org/10.7910/DVN/IETSXS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 689, A200 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.18045">arXiv:2403.18045</a> <span> [<a href="https://arxiv.org/pdf/2403.18045">pdf</a>, <a href="https://arxiv.org/format/2403.18045">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202449647">10.1051/0004-6361/202449647 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Optical variability of the blazar 3C 371: from minute to year timescales </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Otero-Santos%2C+J">J. Otero-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Raiteri%2C+C+M">C. M. Raiteri</a>, <a href="/search/astro-ph?searchtype=author&query=Acosta-Pulido%2C+J+A">J. A. Acosta-Pulido</a>, <a href="/search/astro-ph?searchtype=author&query=Carnerero%2C+M+I">M. I. Carnerero</a>, <a href="/search/astro-ph?searchtype=author&query=Villata%2C+M">M. Villata</a>, <a href="/search/astro-ph?searchtype=author&query=Savchenko%2C+S+S">S. S. Savchenko</a>, <a href="/search/astro-ph?searchtype=author&query=Carosati%2C+D">D. Carosati</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W+P">W. P. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtanidze%2C+S+O">S. O. Kurtanidze</a>, <a href="/search/astro-ph?searchtype=author&query=Joner%2C+M+D">M. D. Joner</a>, <a href="/search/astro-ph?searchtype=author&query=Semkov%2C+E">E. Semkov</a>, <a href="/search/astro-ph?searchtype=author&query=Pursimo%2C+T">T. Pursimo</a>, <a href="/search/astro-ph?searchtype=author&query=Ben%C3%ADtez%2C+E">E. Ben铆tez</a>, <a href="/search/astro-ph?searchtype=author&query=Damljanovic%2C+G">G. Damljanovic</a>, <a href="/search/astro-ph?searchtype=author&query=Apolonio%2C+G">G. Apolonio</a>, <a href="/search/astro-ph?searchtype=author&query=Borman%2C+G+A">G. A. Borman</a>, <a href="/search/astro-ph?searchtype=author&query=Bozhilov%2C+V">V. Bozhilov</a>, <a href="/search/astro-ph?searchtype=author&query=Galindo-Guil%2C+F+J">F. J. Galindo-Guil</a>, <a href="/search/astro-ph?searchtype=author&query=Grishina%2C+T+S">T. S. Grishina</a>, <a href="/search/astro-ph?searchtype=author&query=Hagen-Thorn%2C+V+A">V. A. Hagen-Thorn</a>, <a href="/search/astro-ph?searchtype=author&query=Hiriart%2C+D">D. Hiriart</a>, <a href="/search/astro-ph?searchtype=author&query=Hsiao%2C+H+Y">H. Y. Hsiao</a>, <a href="/search/astro-ph?searchtype=author&query=Ibryamov%2C+S">S. Ibryamov</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanidze%2C+R+Z">R. Z. Ivanidze</a>, <a href="/search/astro-ph?searchtype=author&query=Kimeridze%2C+G+N">G. N. Kimeridze</a> , et al. (19 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.18045v2-abstract-short" style="display: inline;"> The BL Lac object 3C 371 has been observed by the Transiting Exoplanet Survey Satellite (\textit{TESS}) for approximately a year, between July 2019 and July 2020, with an unmatched 2-minute observing cadence. In parallel, the Whole Earth Blazar Telescope (WEBT) Collaboration organized an extensive observing campaign, providing three years of continuous optical monitoring between 2018 and 2020. The… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.18045v2-abstract-full').style.display = 'inline'; document.getElementById('2403.18045v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.18045v2-abstract-full" style="display: none;"> The BL Lac object 3C 371 has been observed by the Transiting Exoplanet Survey Satellite (\textit{TESS}) for approximately a year, between July 2019 and July 2020, with an unmatched 2-minute observing cadence. In parallel, the Whole Earth Blazar Telescope (WEBT) Collaboration organized an extensive observing campaign, providing three years of continuous optical monitoring between 2018 and 2020. These datasets allow for a thorough investigation of the variability of the source. The goal of this study is evaluating the optical variability of 3C 371. Taking advantage of the remarkable cadence of \textit{TESS} data, we aim to characterize the intra-day variability (IDV) displayed by the source and identify its shortest variability timescale. With this estimate, constraints on the size of the emitting region and black hole mass can be calculated. Moreover, WEBT data is used to investigate long-term variability (LTV), including understanding spectral behaviour of the source and the polarization variability. Based on the derived characteristics, information on the origin of the variability on different timescales is extracted. We evaluated the variability applying the variability amplitude tool that quantifies how variable the emission is. Moreover, we employed common tools like ANOVA (ANalysis Of VAariance) tests, wavelet and power spectral density (PSD) analyses to characterize the shortest variability timescales present in the emission and the underlying noise affecting the data. Short- and long-term colour behaviours have been evaluated to understand the spectral behaviour of the source. The polarized emission was analyzed, studying its variability and possible rotation patterns of the electric vector position angle (EVPA). Flux distributions of IDV and LTV were also studied with the aim of linking the flux variations to turbulent and/or accretion disc related processes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.18045v2-abstract-full').style.display = 'none'; document.getElementById('2403.18045v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in A&A, 20 pages, 19 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 686, A228 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.11108">arXiv:2310.11108</a> <span> [<a href="https://arxiv.org/pdf/2310.11108">pdf</a>, <a href="https://arxiv.org/format/2310.11108">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Extreme photometric and polarimetric variability of blazar S4 0954+65 at its maximum optical and $纬$-ray brightness levels </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Raiteri%2C+C+M">C. M. Raiteri</a>, <a href="/search/astro-ph?searchtype=author&query=Villata%2C+M">M. Villata</a>, <a href="/search/astro-ph?searchtype=author&query=Carnerero%2C+M+I">M. I. Carnerero</a>, <a href="/search/astro-ph?searchtype=author&query=Savchenko%2C+S+S">S. S. Savchenko</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtanidze%2C+S+O">S. O. Kurtanidze</a>, <a href="/search/astro-ph?searchtype=author&query=Vlasyuk%2C+V+V">V. V. Vlasyuk</a>, <a href="/search/astro-ph?searchtype=author&query=Marchini%2C+A">A. Marchini</a>, <a href="/search/astro-ph?searchtype=author&query=Matsumoto%2C+K">K. Matsumoto</a>, <a href="/search/astro-ph?searchtype=author&query=Lorey%2C+C">C. Lorey</a>, <a href="/search/astro-ph?searchtype=author&query=Joner%2C+M+D">M. D. Joner</a>, <a href="/search/astro-ph?searchtype=author&query=Gazeas%2C+K">K. Gazeas</a>, <a href="/search/astro-ph?searchtype=author&query=Carosati%2C+D">D. Carosati</a>, <a href="/search/astro-ph?searchtype=author&query=Mirzaqulov%2C+D+O">D. O. Mirzaqulov</a>, <a href="/search/astro-ph?searchtype=author&query=Pulido%2C+J+A+A">J. A. Acosta Pulido</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Bachev%2C+R">R. Bachev</a>, <a href="/search/astro-ph?searchtype=author&query=Ben%C3%ADtez%2C+E">E. Ben铆tez</a>, <a href="/search/astro-ph?searchtype=author&query=Borman%2C+G+A">G. A. Borman</a>, <a href="/search/astro-ph?searchtype=author&query=Calcidese%2C+P">P. Calcidese</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W+P">W. P. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Damljanovic%2C+G">G. Damljanovic</a>, <a href="/search/astro-ph?searchtype=author&query=Ehgamberdiev%2C+S+A">S. A. Ehgamberdiev</a>, <a href="/search/astro-ph?searchtype=author&query=Els%C3%A4sser%2C+D">D. Els盲sser</a>, <a href="/search/astro-ph?searchtype=author&query=Feige%2C+M">M. Feige</a>, <a href="/search/astro-ph?searchtype=author&query=Frasca%2C+A">A. Frasca</a> , et al. (42 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.11108v1-abstract-short" style="display: inline;"> In 2022 the BL Lac object S4 0954+65 underwent a major variability phase, reaching its historical maximum brightness in the optical and $纬$-ray bands. We present optical photometric and polarimetric data acquired by the Whole Earth Blazar Telescope (WEBT) Collaboration from 2022 April 6 to July 6. Many episodes of unprecedented fast variability were detected, implying an upper limit to the size of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.11108v1-abstract-full').style.display = 'inline'; document.getElementById('2310.11108v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.11108v1-abstract-full" style="display: none;"> In 2022 the BL Lac object S4 0954+65 underwent a major variability phase, reaching its historical maximum brightness in the optical and $纬$-ray bands. We present optical photometric and polarimetric data acquired by the Whole Earth Blazar Telescope (WEBT) Collaboration from 2022 April 6 to July 6. Many episodes of unprecedented fast variability were detected, implying an upper limit to the size of the emitting region as low as $10^{-4}$ parsec. The WEBT data show rapid variability in both the degree and angle of polarization. We analyse different models to explain the polarization behaviour in the framework of a twisting jet model, which assumes that the long-term trend of the flux is produced by variations in the emitting region viewing angle. All the models can reproduce the average trend of the polarization degree, and can account for its general anticorrelation with the flux, but the dispersion of the data requires the presence of intrinsic mechanisms, such as turbulence, shocks, or magnetic reconnection. The WEBT optical data are compared to $纬$-ray data from the Fermi satellite. These are analysed with both fixed and adaptive binning procedures. We show that the strong correlation between optical and $纬$-ray data without measurable delay assumes different slopes in faint and high brightness states, and this is compatible with a scenario where in faint states we mainly see the imprint of the geometrical effects, while in bright states the synchrotron self-Compton process dominates. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.11108v1-abstract-full').style.display = 'none'; document.getElementById('2310.11108v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 13 figures, in press for MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.02547">arXiv:2210.02547</a> <span> [<a href="https://arxiv.org/pdf/2210.02547">pdf</a>, <a href="https://arxiv.org/format/2210.02547">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/acc181">10.3847/1538-4365/acc181 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multi-messenger characterization of Mrk 501 during historically low X-ray and $纬$-ray activity </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=MAGIC+collaboration"> MAGIC collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Aniello%2C+T">T. Aniello</a>, <a href="/search/astro-ph?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Engels%2C+A+A">A. Arbet Engels</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Baack%2C+D">D. Baack</a>, <a href="/search/astro-ph?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Baquero%2C+A">A. Baquero</a>, <a href="/search/astro-ph?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/astro-ph?searchtype=author&query=Batkovi%C4%87%2C+I">I. Batkovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Baxter%2C+J">J. Baxter</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Bednarek%2C+W">W. Bednarek</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardos%2C+M">M. Bernardos</a>, <a href="/search/astro-ph?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/astro-ph?searchtype=author&query=Besenrieder%2C+J">J. Besenrieder</a> , et al. (300 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.02547v3-abstract-short" style="display: inline;"> We study the broadband emission of Mrk 501 using multi-wavelength observations from 2017 to 2020 performed with a multitude of instruments, involving, among others, MAGIC, Fermi-LAT, NuSTAR, Swift, GASP-WEBT, and OVRO. Mrk 501 showed an extremely low broadband activity, which may help to unravel its baseline emission. Nonetheless, significant flux variations are detected at all wavebands, with the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.02547v3-abstract-full').style.display = 'inline'; document.getElementById('2210.02547v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.02547v3-abstract-full" style="display: none;"> We study the broadband emission of Mrk 501 using multi-wavelength observations from 2017 to 2020 performed with a multitude of instruments, involving, among others, MAGIC, Fermi-LAT, NuSTAR, Swift, GASP-WEBT, and OVRO. Mrk 501 showed an extremely low broadband activity, which may help to unravel its baseline emission. Nonetheless, significant flux variations are detected at all wavebands, with the highest occurring at X-rays and very-high-energy (VHE) $纬$-rays. A significant correlation ($>$3$蟽$) between X-rays and VHE $纬$-rays is measured, supporting leptonic scenarios to explain the variable parts of the emission, also during low activity. This is further supported when we extend our data from 2008 to 2020, and identify, for the first time, significant correlations between Swift-XRT and Fermi-LAT. We additionally find correlations between high-energy $纬$-rays and radio, with the radio lagging by more than 100 days, placing the $纬$-ray emission zone upstream of the radio-bright regions in the jet. Furthermore, Mrk 501 showed a historically low activity in X-rays and VHE $纬$-rays from mid-2017 to mid-2019 with a stable VHE flux ($>$0.2 TeV) of 5% the emission of the Crab Nebula. The broadband spectral energy distribution (SED) of this 2-year-long low-state, the potential baseline emission of Mrk 501, can be characterized with one-zone leptonic models, and with (lepto)-hadronic models fulfilling neutrino flux constraints from IceCube. We explore the time evolution of the SED towards the low-state, revealing that the stable baseline emission may be ascribed to a standing shock, and the variable emission to an additional expanding or traveling shock. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.02547v3-abstract-full').style.display = 'none'; document.getElementById('2210.02547v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">55 pages, 30 figures, 14 tables, accepted by APJS. Corresponding authors are L. Heckmann, D. Paneque, S. Gasparyan, M. Cerruti, and N. Sahakyan</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJS 266 37 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.03874">arXiv:2206.03874</a> <span> [<a href="https://arxiv.org/pdf/2206.03874">pdf</a>, <a href="https://arxiv.org/format/2206.03874">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac917">10.1093/mnras/stac917 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Rapid X-ray Variability in Mkn 421 during a Multiwavelength Campaign </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Markowitz%2C+A+G">Alex G. Markowitz</a>, <a href="/search/astro-ph?searchtype=author&query=Nalewajko%2C+K">Krzysztof Nalewajko</a>, <a href="/search/astro-ph?searchtype=author&query=Bhatta%2C+G">Gopal Bhatta</a>, <a href="/search/astro-ph?searchtype=author&query=Dewangan%2C+G+C">Gulab C. Dewangan</a>, <a href="/search/astro-ph?searchtype=author&query=Chandra%2C+S">Sunil Chandra</a>, <a href="/search/astro-ph?searchtype=author&query=Dorner%2C+D">Daniela Dorner</a>, <a href="/search/astro-ph?searchtype=author&query=Schleicher%2C+B">Bernd Schleicher</a>, <a href="/search/astro-ph?searchtype=author&query=Pajdosz-Smierciak%2C+U">Urszula Pajdosz-Smierciak</a>, <a href="/search/astro-ph?searchtype=author&query=Stawarz%2C+L">Lukasz Stawarz</a>, <a href="/search/astro-ph?searchtype=author&query=Zola%2C+S">Staszek Zola</a>, <a href="/search/astro-ph?searchtype=author&query=Ostrowski%2C+M">Michal Ostrowski</a>, <a href="/search/astro-ph?searchtype=author&query=Carosati%2C+D">Daniele Carosati</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+S">Saikruba Krishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Bachev%2C+R">Rumen Bachev</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+E">Erika Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Gazeas%2C+K">Kosmas Gazeas</a>, <a href="/search/astro-ph?searchtype=author&query=Hiriart%2C+D">David Hiriart</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+S">Shao-Ming Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Larionov%2C+V">Valeri Larionov</a>, <a href="/search/astro-ph?searchtype=author&query=Marchini%2C+A">Alessandro Marchini</a>, <a href="/search/astro-ph?searchtype=author&query=Matsumoto%2C+K">Katsura Matsumoto</a>, <a href="/search/astro-ph?searchtype=author&query=Nikiforova%2C+A+A">A. A. Nikiforova</a>, <a href="/search/astro-ph?searchtype=author&query=Pursimo%2C+T">Tapio Pursimo</a>, <a href="/search/astro-ph?searchtype=author&query=Raiteri%2C+C+M">Claudia M. Raiteri</a>, <a href="/search/astro-ph?searchtype=author&query=Reichart%2C+D+E">Daniel E. Reichart</a> , et al. (25 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.03874v1-abstract-short" style="display: inline;"> The study of short-term variability properties in AGN jets has the potential to shed light on their particle acceleration and emission mechanisms. We report results from a four-day coordinated multi-wavelength campaign on the highly-peaked blazar (HBL) Mkn 421 in 2019 January. We obtained X-ray data from AstroSAT, BVRI photometry with the Whole Earth Blazar Telescope (WEBT), and TeV data from FACT… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.03874v1-abstract-full').style.display = 'inline'; document.getElementById('2206.03874v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.03874v1-abstract-full" style="display: none;"> The study of short-term variability properties in AGN jets has the potential to shed light on their particle acceleration and emission mechanisms. We report results from a four-day coordinated multi-wavelength campaign on the highly-peaked blazar (HBL) Mkn 421 in 2019 January. We obtained X-ray data from AstroSAT, BVRI photometry with the Whole Earth Blazar Telescope (WEBT), and TeV data from FACT to explore short-term multi-wavelength variability in this HBL. The X-ray continuum is rapidly variable on time-scales of tens of ks. Fractional variability amplitude increases with energy across the synchrotron hump, consistent with previous studies; we interpret this observation in the context of a model with multiple cells whose emission spectra contain cutoffs that follow a power-law distribution. We also performed time-averaged and time-resolved (time-scales of 6 ks) spectral fits; a broken power-law model fits all spectra well; time-resolved spectral fitting reveals the usual hardening when brightening behaviour. Intra-X-ray cross correlations yield evidence for the 0.6-0.8 keV band to likely lead the other bands by an average of 4.6 +- 2.6 ks, but only during the first half of the observation. The source displayed minimal night-to-night variability at all wavebands thus precluding significant interband correlations during our campaign. The broadband SED is modeled well with a standard one-zone leptonic model, yielding jet parameters consistent with those obtained from previous SEDs of this source. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.03874v1-abstract-full').style.display = 'none'; document.getElementById('2206.03874v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">This article has been accepted for publication in The Monthly Notices of the Royal Astronomical Society (2022), and is published in Volume 513, Issue 2, pp.1662-1679. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. 19 pages; 12 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Monthly Notices of the Royal Astronomical Society, 2022, Volume 513, Issue 2, pp.1662-1679 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.11059">arXiv:2203.11059</a> <span> [<a href="https://arxiv.org/pdf/2203.11059">pdf</a>, <a href="https://arxiv.org/format/2203.11059">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202143010">10.1051/0004-6361/202143010 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GRB 190919B: Rapid optical rise explained as a flaring activity </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jel%C3%ADnek%2C+M">Martin Jel铆nek</a>, <a href="/search/astro-ph?searchtype=author&query=Topinka%2C+M">Martin Topinka</a>, <a href="/search/astro-ph?searchtype=author&query=Karpov%2C+S">Sergey Karpov</a>, <a href="/search/astro-ph?searchtype=author&query=Male%C5%88%C3%A1kov%C3%A1%2C+A">Al啪b臎ta Male艌谩kov谩</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+Y+-">Y. -D. Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Rigoselli%2C+M">Michela Rigoselli</a>, <a href="/search/astro-ph?searchtype=author&query=%C5%A0trobl%2C+J">Jan 艩trobl</a>, <a href="/search/astro-ph?searchtype=author&query=Ebr%2C+J">Jan Ebr</a>, <a href="/search/astro-ph?searchtype=author&query=Cunniffe%2C+R">Ronan Cunniffe</a>, <a href="/search/astro-ph?searchtype=author&query=Thoene%2C+C">Christina Thoene</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%C5%A1ek%2C+M">Martin Ma拧ek</a>, <a href="/search/astro-ph?searchtype=author&query=Jane%C4%8Dek%2C+P">Petr Jane膷ek</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandez-Garc%C3%ADa%2C+E">Emilio Fernandez-Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Hiriart%2C+D">David Hiriart</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+W+H">William H. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=V%C3%ADtek%2C+S">Stanislav V铆tek</a>, <a href="/search/astro-ph?searchtype=author&query=Hudec%2C+R">Ren茅 Hudec</a>, <a href="/search/astro-ph?searchtype=author&query=Tr%C3%A1vn%C3%AD%C4%8Dek%2C+P">Petr Tr谩vn铆膷ek</a>, <a href="/search/astro-ph?searchtype=author&query=Castro-Tirado%2C+A+J">Alberto J. Castro-Tirado</a>, <a href="/search/astro-ph?searchtype=author&query=Prouza%2C+M">Michael Prouza</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.11059v1-abstract-short" style="display: inline;"> Following the detection of a long GRB 190919B by INTEGRAL (INTErnational Gamma-Ray Astrophysics Laboratory), we obtained an optical photometric sequence of its optical counterpart. The light curve of the optical emission exhibits an unusually steep rise ~100 s after the initial trigger. This behaviour is not expected from a 'canonical' GRB optical afterglow. As an explanation, we propose a scenari… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.11059v1-abstract-full').style.display = 'inline'; document.getElementById('2203.11059v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.11059v1-abstract-full" style="display: none;"> Following the detection of a long GRB 190919B by INTEGRAL (INTErnational Gamma-Ray Astrophysics Laboratory), we obtained an optical photometric sequence of its optical counterpart. The light curve of the optical emission exhibits an unusually steep rise ~100 s after the initial trigger. This behaviour is not expected from a 'canonical' GRB optical afterglow. As an explanation, we propose a scenario consisting of two superimposed flares: an optical flare originating from the inner engine activity followed by the hydrodynamic peak of an external shock. The inner-engine nature of the first pulse is supported by a marginal detection of flux in hard X-rays. The second pulse eventually concludes in a slow constant decay, which, as we show, follows the closure relations for a slow cooling plasma expanding into the constant interstellar medium and can be seen as an optical afterglow sensu stricto. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.11059v1-abstract-full').style.display = 'none'; document.getElementById('2203.11059v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 8 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 662, A126 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.06493">arXiv:2011.06493</a> <span> [<a href="https://arxiv.org/pdf/2011.06493">pdf</a>, <a href="https://arxiv.org/format/2011.06493">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/staa3561">10.1093/mnras/staa3561 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The dual nature of blazar fast variability. Space and ground observations of S5 0716+714 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Raiteri%2C+C+M">C. M. Raiteri</a>, <a href="/search/astro-ph?searchtype=author&query=Villata%2C+M">M. Villata</a>, <a href="/search/astro-ph?searchtype=author&query=Carosati%2C+D">D. Carosati</a>, <a href="/search/astro-ph?searchtype=author&query=Ben%C3%ADtez%2C+E">E. Ben铆tez</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtanidze%2C+S+O">S. O. Kurtanidze</a>, <a href="/search/astro-ph?searchtype=author&query=Gupta%2C+A+C">A. C. Gupta</a>, <a href="/search/astro-ph?searchtype=author&query=Mirzaqulov%2C+D+O">D. O. Mirzaqulov</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ammando%2C+F">F. D'Ammando</a>, <a href="/search/astro-ph?searchtype=author&query=Larionov%2C+V+M">V. M. Larionov</a>, <a href="/search/astro-ph?searchtype=author&query=Pursimo%2C+T">T. Pursimo</a>, <a href="/search/astro-ph?searchtype=author&query=Acosta-Pulido%2C+J+A">J. A. Acosta-Pulido</a>, <a href="/search/astro-ph?searchtype=author&query=Baida%2C+G+V">G. V. Baida</a>, <a href="/search/astro-ph?searchtype=author&query=Balmaverde%2C+B">B. Balmaverde</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnoli%2C+G">G. Bonnoli</a>, <a href="/search/astro-ph?searchtype=author&query=Borman%2C+G+A">G. A. Borman</a>, <a href="/search/astro-ph?searchtype=author&query=Carnerero%2C+M+I">M. I. Carnerero</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W+-">W. -P. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Dhiman%2C+V">V. Dhiman</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Maggio%2C+A">A. Di Maggio</a>, <a href="/search/astro-ph?searchtype=author&query=Ehgamberdiev%2C+S+A">S. A. Ehgamberdiev</a>, <a href="/search/astro-ph?searchtype=author&query=Hiriart%2C+D">D. Hiriart</a>, <a href="/search/astro-ph?searchtype=author&query=Kimeridze%2C+G+N">G. N. Kimeridze</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtanidze%2C+O+M">O. M. Kurtanidze</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+C+S">C. S. Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+J+M">J. M. Lopez</a> , et al. (17 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2011.06493v1-abstract-short" style="display: inline;"> Blazar S5 0716+714 is well-known for its short-term variability, down to intra-day time-scales. We here present the 2-min cadence optical light curve obtained by the TESS space telescope in 2019 December - 2020 January and analyse the object fast variability with unprecedented sampling. Supporting observations by the Whole Earth Blazar Telescope Collaboration in B, V , R, and I bands allow us to i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.06493v1-abstract-full').style.display = 'inline'; document.getElementById('2011.06493v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.06493v1-abstract-full" style="display: none;"> Blazar S5 0716+714 is well-known for its short-term variability, down to intra-day time-scales. We here present the 2-min cadence optical light curve obtained by the TESS space telescope in 2019 December - 2020 January and analyse the object fast variability with unprecedented sampling. Supporting observations by the Whole Earth Blazar Telescope Collaboration in B, V , R, and I bands allow us to investigate the spectral variability during the TESS pointing. The spectral analysis is further extended in frequency to the UV and X-ray bands with data from the Neil Gehrels Swift Observatory. We develop a new method to unveil the shortest optical variability time-scales. This is based on progressive de-trending of the TESS light curve by means of cubic spline interpolations through the binned fluxes, with decreasing time bins. The de-trended light curves are then analysed with classical tools for time-series analysis (periodogram, auto-correlation and structure functions). The results show that below 3 d there are significant characteristic variability time-scales of about 1.7, 0.5, and 0.2 d. Variability on time-scales < 0.2 d is strongly chromatic and must be ascribed to intrinsic energetic processes involving emitting regions, likely jet sub-structures, with dimension less than about milliparsec. In contrast, flux changes on time-scales > 0.5 d are quasi-achromatic and are probably due to Doppler factor changes of geometric origin. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.06493v1-abstract-full').style.display = 'none'; document.getElementById('2011.06493v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 18 figures, accepted by MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.07999">arXiv:2007.07999</a> <span> [<a href="https://arxiv.org/pdf/2007.07999">pdf</a>, <a href="https://arxiv.org/format/2007.07999">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Multi-Wavelength Variability of BL Lacertae Measured with High Time Resolution </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Weaver%2C+Z+R">Zachary R. Weaver</a>, <a href="/search/astro-ph?searchtype=author&query=Williamson%2C+K+E">K. E. Williamson</a>, <a href="/search/astro-ph?searchtype=author&query=Jorstad%2C+S+G">S. G. Jorstad</a>, <a href="/search/astro-ph?searchtype=author&query=Marscher%2C+A+P">A. P. Marscher</a>, <a href="/search/astro-ph?searchtype=author&query=Larionov%2C+V+M">V. M. Larionov</a>, <a href="/search/astro-ph?searchtype=author&query=Raiteri%2C+C+M">C. M. Raiteri</a>, <a href="/search/astro-ph?searchtype=author&query=Villata%2C+M">M. Villata</a>, <a href="/search/astro-ph?searchtype=author&query=Acosta-Pulido%2C+J+A">J. A. Acosta-Pulido</a>, <a href="/search/astro-ph?searchtype=author&query=Bachev%2C+R">R. Bachev</a>, <a href="/search/astro-ph?searchtype=author&query=Baida%2C+G+V">G. V. Baida</a>, <a href="/search/astro-ph?searchtype=author&query=Balonek%2C+T+J">T. J. Balonek</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+E">E. Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Borman%2C+G+A">G. A. Borman</a>, <a href="/search/astro-ph?searchtype=author&query=Bozhilov%2C+V">V. Bozhilov</a>, <a href="/search/astro-ph?searchtype=author&query=Carnerero%2C+M+I">M. I. Carnerero</a>, <a href="/search/astro-ph?searchtype=author&query=Carosati%2C+D">D. Carosati</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W+P">W. P. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Damljanovic%2C+G">G. Damljanovic</a>, <a href="/search/astro-ph?searchtype=author&query=Dhiman%2C+V">V. Dhiman</a>, <a href="/search/astro-ph?searchtype=author&query=Dougherty%2C+D+J">D. J. Dougherty</a>, <a href="/search/astro-ph?searchtype=author&query=Ehgamberdiev%2C+S+A">S. A. Ehgamberdiev</a>, <a href="/search/astro-ph?searchtype=author&query=Grishina%2C+T+S">T. S. Grishina</a>, <a href="/search/astro-ph?searchtype=author&query=Gupta%2C+A+C">A. C. Gupta</a>, <a href="/search/astro-ph?searchtype=author&query=Hart%2C+M">M. Hart</a>, <a href="/search/astro-ph?searchtype=author&query=Hiriart%2C+D">D. Hiriart</a> , et al. (32 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2007.07999v1-abstract-short" style="display: inline;"> In an effort to locate the sites of emission at different frequencies and physical processes causing variability in blazar jets, we have obtained high time-resolution observations of BL Lacertae over a wide wavelength range: with the \emph{Transiting Exoplanet Survey Satellite} (TESS) at 6,000-10,000 脜 with 2-minute cadence; with the Neil Gehrels \emph{Swift} satellite at optical, UV, and X-ray ba… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.07999v1-abstract-full').style.display = 'inline'; document.getElementById('2007.07999v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.07999v1-abstract-full" style="display: none;"> In an effort to locate the sites of emission at different frequencies and physical processes causing variability in blazar jets, we have obtained high time-resolution observations of BL Lacertae over a wide wavelength range: with the \emph{Transiting Exoplanet Survey Satellite} (TESS) at 6,000-10,000 脜 with 2-minute cadence; with the Neil Gehrels \emph{Swift} satellite at optical, UV, and X-ray bands; with the Nuclear Spectroscopic Telescope Array at hard X-ray bands; with the \emph{Fermi} Large Area Telescope at $纬$-ray energies; and with the Whole Earth Blazar Telescope for measurement of the optical flux density and polarization. All light curves are correlated, with similar structure on timescales from hours to days. The shortest timescale of variability at optical frequencies observed with TESS is $\sim 0.5$ hr. The most common timescale is $13\pm1$~hr, comparable with the minimum timescale of X-ray variability, 14.5 hr. The multi-wavelength variability properties cannot be explained by a change solely in the Doppler factor of the emitting plasma. The polarization behavior implies that there are both ordered and turbulent components to the magnetic field in the jet. Correlation analysis indicates that the X-ray variations lag behind the $纬$-ray and optical light curves by up to $\sim 0.4$ days. The timescales of variability, cross-frequency lags, and polarization properties can be explained by turbulent plasma that is energized by a shock in the jet and subsequently loses energy to synchrotron and inverse Compton radiation in a magnetic field of strength $\sim3$ G <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.07999v1-abstract-full').style.display = 'none'; document.getElementById('2007.07999v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">33 pages, 25 figures, 14 tables. Accepted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1910.03609">arXiv:1910.03609</a> <span> [<a href="https://arxiv.org/pdf/1910.03609">pdf</a>, <a href="https://arxiv.org/ps/1910.03609">ps</a>, <a href="https://arxiv.org/format/1910.03609">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stz2792">10.1093/mnras/stz2792 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Investigating the multiwavelength behaviour of the flat spectrum radio quasar CTA 102 during 2013-2017 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=D%27Ammando%2C+F">F. D'Ammando</a>, <a href="/search/astro-ph?searchtype=author&query=Raiteri%2C+C+M">C. M. Raiteri</a>, <a href="/search/astro-ph?searchtype=author&query=Villata%2C+M">M. Villata</a>, <a href="/search/astro-ph?searchtype=author&query=Acosta-Pulido%2C+J+A">J. A. Acosta-Pulido</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Arkharov%2C+A+A">A. A. Arkharov</a>, <a href="/search/astro-ph?searchtype=author&query=Bachev%2C+R">R. Bachev</a>, <a href="/search/astro-ph?searchtype=author&query=Baida%2C+G+V">G. V. Baida</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+E">E. Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Borman%2C+G+A">G. A. Borman</a>, <a href="/search/astro-ph?searchtype=author&query=Boschin%2C+W">W. Boschin</a>, <a href="/search/astro-ph?searchtype=author&query=Bozhilov%2C+V">V. Bozhilov</a>, <a href="/search/astro-ph?searchtype=author&query=Butuzova%2C+M+S">M. S. Butuzova</a>, <a href="/search/astro-ph?searchtype=author&query=Calcidese%2C+P">P. Calcidese</a>, <a href="/search/astro-ph?searchtype=author&query=Carnerero%2C+M+I">M. I. Carnerero</a>, <a href="/search/astro-ph?searchtype=author&query=Carosati%2C+D">D. Carosati</a>, <a href="/search/astro-ph?searchtype=author&query=Casadio%2C+C">C. Casadio</a>, <a href="/search/astro-ph?searchtype=author&query=Castro-Segura%2C+N">N. Castro-Segura</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W+-">W. -P. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Damljanovic%2C+G">G. Damljanovic</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Paola%2C+A">A. Di Paola</a>, <a href="/search/astro-ph?searchtype=author&query=Echevarria%2C+J">J. Echevarria</a>, <a href="/search/astro-ph?searchtype=author&query=Efimova%2C+N+V">N. V. Efimova</a>, <a href="/search/astro-ph?searchtype=author&query=Ehgamberdiev%2C+S+A">Sh. A. Ehgamberdiev</a>, <a href="/search/astro-ph?searchtype=author&query=Espinosa%2C+C">C. Espinosa</a> , et al. (72 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1910.03609v2-abstract-short" style="display: inline;"> We present a multiwavelength study of the flat-spectrum radio quasar CTA 102 during 2013-2017. We use radio-to-optical data obtained by the Whole Earth Blazar Telescope, 15 GHz data from the Owens Valley Radio Observatory, 91 and 103 GHz data from the Atacama Large Millimeter Array, near-infrared data from the Rapid Eye Monitor telescope, as well as data from the Swift (optical-UV and X-rays) and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.03609v2-abstract-full').style.display = 'inline'; document.getElementById('1910.03609v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.03609v2-abstract-full" style="display: none;"> We present a multiwavelength study of the flat-spectrum radio quasar CTA 102 during 2013-2017. We use radio-to-optical data obtained by the Whole Earth Blazar Telescope, 15 GHz data from the Owens Valley Radio Observatory, 91 and 103 GHz data from the Atacama Large Millimeter Array, near-infrared data from the Rapid Eye Monitor telescope, as well as data from the Swift (optical-UV and X-rays) and Fermi ($纬$ rays) satellites to study flux and spectral variability and the correlation between flux changes at different wavelengths. Unprecedented $纬$-ray flaring activity was observed during 2016 November-2017 February, with four major outbursts. A peak flux of (2158 $\pm$ 63)$\times$10$^{-8}$ ph cm$^{-2}$ s$^{-1}$, corresponding to a luminosity of (2.2 $\pm$ 0.1)$\times$10$^{50}$ erg s$^{-1}$, was reached on 2016 December 28. These four $纬$-ray outbursts have corresponding events in the near-infrared, optical, and UV bands, with the peaks observed at the same time. A general agreement between X-ray and $纬$-ray activity is found. The $纬$-ray flux variations show a general, strong correlation with the optical ones with no time lag between the two bands and a comparable variability amplitude. This $纬$-ray/optical relationship is in agreement with the geometrical model that has successfully explained the low-energy flux and spectral behaviour, suggesting that the long-term flux variations are mainly due to changes in the Doppler factor produced by variations of the viewing angle of the emitting regions. The difference in behaviour between radio and higher energy emission would be ascribed to different viewing angles of the jet regions producing their emission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.03609v2-abstract-full').style.display = 'none'; document.getElementById('1910.03609v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 18 figures, and 4 tables. Accepted for publication in Monthly Notices of the Royal Astronomical Society</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1908.08663">arXiv:1908.08663</a> <span> [<a href="https://arxiv.org/pdf/1908.08663">pdf</a>, <a href="https://arxiv.org/format/1908.08663">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/ab3f28">10.3847/1538-4365/ab3f28 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Optical polarimetric and multiwavelength flaring activity of blazar 3C279 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fraija%2C+N">N. Fraija</a>, <a href="/search/astro-ph?searchtype=author&query=Ben%C3%ADtez%2C+E">E. Ben铆tez</a>, <a href="/search/astro-ph?searchtype=author&query=Hiriart%2C+D">D. Hiriart</a>, <a href="/search/astro-ph?searchtype=author&query=Sorcia%2C+M">M. Sorcia</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez%2C+J+M">J. M. L贸pez</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%BAjica%2C+R">R. M煤jica</a>, <a href="/search/astro-ph?searchtype=author&query=Cabrera%2C+J+I">J. I. Cabrera</a>, <a href="/search/astro-ph?searchtype=author&query=Galv%C3%A1n-G%C3%A1mez%2C+A">A. Galv谩n-G谩mez</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1908.08663v1-abstract-short" style="display: inline;"> An exhaustive analysis of 9-year optical R-band photopolarimetric data of the flat-spectrum radio quasar 3C279 from 2008 February 27 to 2017 May 25 is presented, alongside with multiwavelength observing campaigns performed during the flaring activity exhibited in 2009 February/March, 2011 June, 2014 March/April, 2015 June and 2017 February. In the R-band, this source showed the maximum brightness… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.08663v1-abstract-full').style.display = 'inline'; document.getElementById('1908.08663v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1908.08663v1-abstract-full" style="display: none;"> An exhaustive analysis of 9-year optical R-band photopolarimetric data of the flat-spectrum radio quasar 3C279 from 2008 February 27 to 2017 May 25 is presented, alongside with multiwavelength observing campaigns performed during the flaring activity exhibited in 2009 February/March, 2011 June, 2014 March/April, 2015 June and 2017 February. In the R-band, this source showed the maximum brightness state of $13.68\pm 0.11$ mag ($1.36\pm0.20$ mJy) on 2017 March 02, and the lowest brightness state ever recorded of $18.20\pm 0.87$ mag ($0.16\pm0.03$ mJy) on 2010 June 17. During the entire period of observations, the polarization degree varied between $0.48\pm0.17$% and $31.65\pm0.77$% and the electric vector position angle exhibited large rotations between $82.98^\circ \pm0.92$ and $446.32^\circ \pm1.95$. Optical polarization data show that this source has a stable polarized component that varied from $\sim$6% (before the 2009 flare) to $\sim$13% after the flare. The overall behavior of our polarized variability data supports the scenario of jet precessions as responsible of the observed large rotations of the electric vector position angle. Discrete correlation function analysis show that the lags between gamma-rays and X-rays compared to the optical R-band fluxes are $螖t \sim$ 31 d and $1$ d in 2009. Lags were also found among gamma-rays compared with X-rays and radio of $螖t \sim$ 30 d and $43$ d in 2011, and among radio and optical-R band of $螖t \sim$ 10 d in 2014. A very intense flare in 2017 was observed in optical bands with a dramatic variation in the polarization degree (from $\sim$ 6% to 20%) in 90 days without exhibiting flaring activity in other wavelengths. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.08663v1-abstract-full').style.display = 'none'; document.getElementById('1908.08663v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 August, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 10 figures. Accepted for publication in ApJS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1808.04300">arXiv:1808.04300</a> <span> [<a href="https://arxiv.org/pdf/1808.04300">pdf</a>, <a href="https://arxiv.org/ps/1808.04300">ps</a>, <a href="https://arxiv.org/format/1808.04300">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201833704">10.1051/0004-6361/201833704 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The extreme HBL behaviour of Markarian 501 during 2012 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ahnen%2C+M+L">M. L. Ahnen</a>, <a href="/search/astro-ph?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Banerjee%2C+B">B. Banerjee</a>, <a href="/search/astro-ph?searchtype=author&query=Bangale%2C+P">P. Bangale</a>, <a href="/search/astro-ph?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Bednarek%2C+W">W. Bednarek</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/astro-ph?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharyya%2C+W">W. Bhattacharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Blanch%2C+O">O. Blanch</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnoli%2C+G">G. Bonnoli</a>, <a href="/search/astro-ph?searchtype=author&query=Carosi%2C+R">R. Carosi</a>, <a href="/search/astro-ph?searchtype=author&query=Carosi%2C+A">A. Carosi</a>, <a href="/search/astro-ph?searchtype=author&query=Chatterjee%2C+A">A. Chatterjee</a>, <a href="/search/astro-ph?searchtype=author&query=Colak%2C+S+M">S. M. Colak</a>, <a href="/search/astro-ph?searchtype=author&query=Colin%2C+P">P. Colin</a>, <a href="/search/astro-ph?searchtype=author&query=Colombo%2C+E">E. Colombo</a>, <a href="/search/astro-ph?searchtype=author&query=Contreras%2C+J+L">J. L. Contreras</a>, <a href="/search/astro-ph?searchtype=author&query=Cortina%2C+J">J. Cortina</a>, <a href="/search/astro-ph?searchtype=author&query=Covino%2C+S">S. Covino</a> , et al. (254 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1808.04300v2-abstract-short" style="display: inline;"> A multiwavelength campaign was organized to take place between March and July of 2012. Excellent temporal coverage was obtained with more than 25 instruments, including the MAGIC, FACT and VERITAS Cherenkov telescopes, the instruments on board the Swift and Fermi spacecraft, and the telescopes operated by the GASP-WEBT collaboration. Mrk 501 showed a very high energy (VHE) gamma-ray flux above 0… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.04300v2-abstract-full').style.display = 'inline'; document.getElementById('1808.04300v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.04300v2-abstract-full" style="display: none;"> A multiwavelength campaign was organized to take place between March and July of 2012. Excellent temporal coverage was obtained with more than 25 instruments, including the MAGIC, FACT and VERITAS Cherenkov telescopes, the instruments on board the Swift and Fermi spacecraft, and the telescopes operated by the GASP-WEBT collaboration. Mrk 501 showed a very high energy (VHE) gamma-ray flux above 0.2 TeV of $\sim$0.5 times the Crab Nebula flux (CU) for most of the campaign. The highest activity occurred on 2012 June 9, when the VHE flux was $\sim$3 CU, and the peak of the high-energy spectral component was found to be at $\sim$2 TeV. This study reports very hard X-ray spectra, and the hardest VHE spectra measured to date for Mrk 501. The fractional variability was found to increase with energy, with the highest variability occurring at VHE, and a significant correlation between the X-ray and VHE bands. The unprecedentedly hard X-ray and VHE spectra measured imply that their low- and high-energy components peaked above 5 keV and 0.5 TeV, respectively, during a large fraction of the observing campaign, and hence that Mrk 501 behaved like an extreme high-frequency- peaked blazar (EHBL) throughout the 2012 observing season. This suggests that being an EHBL may not be a permanent characteristic of a blazar, but rather a state which may change over time. The one-zone synchrotron self-Compton (SSC) scenario can successfully describe the segments of the SED where most energy is emitted, with a significant correlation between the electron energy density and the VHE gamma-ray activity, suggesting that most of the variability may be explained by the injection of high-energy electrons. The one-zone SSC scenario used reproduces the behaviour seen between the measured X-ray and VHE gamma-ray fluxes, and predicts that the correlation becomes stronger with increasing energy of the X-rays. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.04300v2-abstract-full').style.display = 'none'; document.getElementById('1808.04300v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 9 figures, accepted for publication in A&A. Corresponding authors: Gareth Hughes (gareth.hughes@cfa.harvard.edu), David Paneque (dpaneque@mppmu.mpg.de), Amit Shukla (amit.shukla@astro.uni-wuerzburg.de)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 620, A181 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1803.07529">arXiv:1803.07529</a> <span> [<a href="https://arxiv.org/pdf/1803.07529">pdf</a>, <a href="https://arxiv.org/ps/1803.07529">ps</a>, <a href="https://arxiv.org/format/1803.07529">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/aab1f9">10.3847/1538-4357/aab1f9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Bright $纬$-ray Flare of 3C 279 in June 2015: AGILE Detection and Multifrequency Follow-up Observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pittori%2C+C">C. Pittori</a>, <a href="/search/astro-ph?searchtype=author&query=Lucarelli%2C+F">F. Lucarelli</a>, <a href="/search/astro-ph?searchtype=author&query=Verrecchia%2C+F">F. Verrecchia</a>, <a href="/search/astro-ph?searchtype=author&query=Raiteri%2C+C+M">C. M. Raiteri</a>, <a href="/search/astro-ph?searchtype=author&query=Villata%2C+M">M. Villata</a>, <a href="/search/astro-ph?searchtype=author&query=Vittorini%2C+V">V. Vittorini</a>, <a href="/search/astro-ph?searchtype=author&query=Tavani%2C+M">M. Tavani</a>, <a href="/search/astro-ph?searchtype=author&query=Puccetti%2C+S">S. Puccetti</a>, <a href="/search/astro-ph?searchtype=author&query=Perri%2C+M">M. Perri</a>, <a href="/search/astro-ph?searchtype=author&query=Donnarumma%2C+I">I. Donnarumma</a>, <a href="/search/astro-ph?searchtype=author&query=Vercellone%2C+S">S. Vercellone</a>, <a href="/search/astro-ph?searchtype=author&query=Acosta-Pulido%2C+J+A">J. A. Acosta-Pulido</a>, <a href="/search/astro-ph?searchtype=author&query=Bachev%2C+R">R. Bachev</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+E">E. Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Borman%2C+G+A">G. A. Borman</a>, <a href="/search/astro-ph?searchtype=author&query=Carnerero%2C+M+I">M. I. Carnerero</a>, <a href="/search/astro-ph?searchtype=author&query=Carosati%2C+D">D. Carosati</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W+P">W. P. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Ehgamberdiev%2C+S+A">Sh. A. Ehgamberdiev</a>, <a href="/search/astro-ph?searchtype=author&query=Goded%2C+A">A. Goded</a>, <a href="/search/astro-ph?searchtype=author&query=Grishina%2C+T+S">T. S. Grishina</a>, <a href="/search/astro-ph?searchtype=author&query=Hiriart%2C+D">D. Hiriart</a>, <a href="/search/astro-ph?searchtype=author&query=Hsiao%2C+H+Y">H. Y. Hsiao</a>, <a href="/search/astro-ph?searchtype=author&query=Jorstad%2C+S+G">S. G. Jorstad</a>, <a href="/search/astro-ph?searchtype=author&query=Kimeridze%2C+G+N">G. N. Kimeridze</a> , et al. (22 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1803.07529v1-abstract-short" style="display: inline;"> We report the AGILE detection and the results of the multifrequency follow-up observations of a bright $纬$-ray flare of the blazar 3C 279 in June 2015. We use AGILE-GRID and Fermi-LAT $纬$-ray data, together with Swift-XRT, Swift-UVOT, and ground-based GASP-WEBT optical observations, including polarization information, to study the source variability and the overall spectral energy distribution dur… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.07529v1-abstract-full').style.display = 'inline'; document.getElementById('1803.07529v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1803.07529v1-abstract-full" style="display: none;"> We report the AGILE detection and the results of the multifrequency follow-up observations of a bright $纬$-ray flare of the blazar 3C 279 in June 2015. We use AGILE-GRID and Fermi-LAT $纬$-ray data, together with Swift-XRT, Swift-UVOT, and ground-based GASP-WEBT optical observations, including polarization information, to study the source variability and the overall spectral energy distribution during the $纬$-ray flare. The $纬$-ray flaring data, compared with as yet unpublished simultaneous optical data which allow to set constraints on the big blue bump disk luminosity, show very high Compton dominance values of $\sim 100$, with a ratio of $纬$-ray to optical emission rising by a factor of three in a few hours. The multi-wavelength behavior of the source during the flare challenges one-zone leptonic theoretical models. The new observations during the June 2015 flare are also compared with already published data and non-simultaneous historical 3C 279 archival data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.07529v1-abstract-full').style.display = 'none'; document.getElementById('1803.07529v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 March, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 5 figures,5 Tables. Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1707.05624">arXiv:1707.05624</a> <span> [<a href="https://arxiv.org/pdf/1707.05624">pdf</a>, <a href="https://arxiv.org/format/1707.05624">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/aa82cc">10.3847/1538-4365/aa82cc <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Long-term optical polarization variability and multiwavelength analysis of Blazar Mrk 421 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fraija%2C+N">Nissim Fraija</a>, <a href="/search/astro-ph?searchtype=author&query=Ben%C3%ADtez%2C+E">Erika Ben铆tez</a>, <a href="/search/astro-ph?searchtype=author&query=Hiriart%2C+D">David Hiriart</a>, <a href="/search/astro-ph?searchtype=author&query=Sorcia%2C+M">Marco Sorcia</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez%2C+J+M">Jose Manuel L贸pez</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%BAjica%2C+R">Raul M煤jica</a>, <a href="/search/astro-ph?searchtype=author&query=Cabrera%2C+J+I">Jose Ignacio Cabrera</a>, <a href="/search/astro-ph?searchtype=author&query=de+Diego%2C+J+A">Jose Antonio de Diego</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas-Luis%2C+M">Miriam Rojas-Luis</a>, <a href="/search/astro-ph?searchtype=author&query=Salazar-V%C3%A1zquez%2C+F">Felipe Salazar-V谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Galv%C3%A1n-G%C3%A1mez%2C+A">Antonio Galv谩n-G谩mez</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1707.05624v1-abstract-short" style="display: inline;"> The results of 8-year R-band photopolarimetric data of blazar Mrk 421 collected from February 2008 to May 2016 are presented, along with extensive multiwavelength observations covering from radio to TeV $纬$-rays around the flares observed in May 2008, March 2010, and April 2013. The most important results are found in 2013 when the source displayed in the R-band a very high brightness state of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.05624v1-abstract-full').style.display = 'inline'; document.getElementById('1707.05624v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.05624v1-abstract-full" style="display: none;"> The results of 8-year R-band photopolarimetric data of blazar Mrk 421 collected from February 2008 to May 2016 are presented, along with extensive multiwavelength observations covering from radio to TeV $纬$-rays around the flares observed in May 2008, March 2010, and April 2013. The most important results are found in 2013 when the source displayed in the R-band a very high brightness state of $11.29\pm 0.03$ mag ($93.60\pm 1.53$ mJy) on April 10th and a polarization degree of ($11.00\pm0.44$) on May 13th. The analysis of the optical data shows that the polarization variability is due to the superposition of two polarized components that might be produced in two distinct emitting regions. An intranight photopolarimetric variability study carried out over 7 nights after the 2013 April maximum found flux and polarization variations on the nights of April 14, 15, 16 and 19. In addition, the flux shows a minimum variability timescale of $螖\,t=$2.34$\pm$0.12 hours, and that the polarization degree presented variations of $\sim$ (1 - 2) in a timescale of $螖\,t\sim$ minutes. Also, a detailed analysis of the intranight data shows a coherence length of the large-scale magnetic field of $l_B\simeq$ 0.3 pc which is the same order of magnitude to the distance traveled by the relativistic shocks. This result suggests that there is a connection between the intranight polarimetric variations and spatial changes of the magnetic field. Analysis of the complete R-band data along with the historical optical light curve found for this object shows that Mrk 421 varies with a period of 16.26 $\pm$ 1.78 years. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.05624v1-abstract-full').style.display = 'none'; document.getElementById('1707.05624v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">30 pages and 16 figures. Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1701.03809">arXiv:1701.03809</a> <span> [<a href="https://arxiv.org/pdf/1701.03809">pdf</a>, <a href="https://arxiv.org/ps/1701.03809">ps</a>, <a href="https://arxiv.org/format/1701.03809">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stw3046">10.1093/mnras/stw3046 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multi-band polarimetry of post-asymptotic giant branch stars stars. Optical measurements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Akras%2C+S">S. Akras</a>, <a href="/search/astro-ph?searchtype=author&query=Velez%2C+J+C+R">J. C. Ramirez Velez</a>, <a href="/search/astro-ph?searchtype=author&query=Nanouris%2C+N">N. Nanouris</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos-Larios%2C+G">G. Ramos-Larios</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+J+M">J. M. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Hiriart%2C+D">D. Hiriart</a>, <a href="/search/astro-ph?searchtype=author&query=Panoglou%2C+D">D. Panoglou</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1701.03809v1-abstract-short" style="display: inline;"> We present new optical broad-band (UBVRI) aperture polarimetric observations of 53 post-asymptotic giant branch (AGB) stars selected to exhibit a large near-infrared excess. 24 out of the 53 stars (45% of our sample) are presented for the first time. A statistical analysis shows four distinctive groups of polarized post-AGB stars: unpolarized or very lowly polarized (degree of polarization or DoP… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1701.03809v1-abstract-full').style.display = 'inline'; document.getElementById('1701.03809v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1701.03809v1-abstract-full" style="display: none;"> We present new optical broad-band (UBVRI) aperture polarimetric observations of 53 post-asymptotic giant branch (AGB) stars selected to exhibit a large near-infrared excess. 24 out of the 53 stars (45% of our sample) are presented for the first time. A statistical analysis shows four distinctive groups of polarized post-AGB stars: unpolarized or very lowly polarized (degree of polarization or DoP < 1%), lowly polarized (1% < DoP < 4%), moderately polarized (4% < DoP < 8%) and highly polarized (DoP > 8%). 23 out of the 53 (66%) belong to the first group, 10 (19%) to the second, five (9%) to the third and only three (6%) to the last group. Approximately, 34% of our sample was found to be unpolarized objects, which is close to the percentage of round planetary nebulae. On average, the low and moderate groups show a wavelength-dependent polarization that increases towards shorter wavelength, implying an intrinsic origin of the polarization, which signifies a Rayleigh-like scattering spectrum typical for non-symmetrical envelopes composed principally of small dust grains. The moderately polarized stars exhibit higher K-W3 and W1-W3 colour indices compared with the group of lowly polarized stars suggesting a possible relation between DoP and mass-loss rate. Moreover, they are found to be systematically colder (redder in B-V), which may be associated with the condensation process close to these stars that results in higher degree of polarization. We also provide evidence that multiple scattering in optically thin polar outflows is the mechanism that gives high DoP in post-AGB stars with a bipolar or multi-polar envelopes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1701.03809v1-abstract-full').style.display = 'none'; document.getElementById('1701.03809v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 January, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1608.03531">arXiv:1608.03531</a> <span> [<a href="https://arxiv.org/pdf/1608.03531">pdf</a>, <a href="https://arxiv.org/format/1608.03531">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/0004-637X/831/1/92">10.3847/0004-637X/831/1/92 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multifrequency Photo-polarimetric WEBT Observation Campaign on the Blazar S5 0716+714: Source Microvariability and Search for Characteristic Timescales </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bhatta%2C+G">G. Bhatta</a>, <a href="/search/astro-ph?searchtype=author&query=Stawarz%2C+%C5%81">艁. Stawarz</a>, <a href="/search/astro-ph?searchtype=author&query=Ostrowski%2C+M">M. Ostrowski</a>, <a href="/search/astro-ph?searchtype=author&query=Markowitz%2C+A">A. Markowitz</a>, <a href="/search/astro-ph?searchtype=author&query=Akitaya%2C+H">H. Akitaya</a>, <a href="/search/astro-ph?searchtype=author&query=Arkharov%2C+A+A">A. A. Arkharov</a>, <a href="/search/astro-ph?searchtype=author&query=Bachev%2C+R">R. Bachev</a>, <a href="/search/astro-ph?searchtype=author&query=Ben%C3%ADtez%2C+E">E. Ben铆tez</a>, <a href="/search/astro-ph?searchtype=author&query=Borman%2C+G+A">G. A. Borman</a>, <a href="/search/astro-ph?searchtype=author&query=Carosati%2C+D">D. Carosati</a>, <a href="/search/astro-ph?searchtype=author&query=Cason%2C+A+D">A. D. Cason</a>, <a href="/search/astro-ph?searchtype=author&query=Chanishvili%2C+R">R. Chanishvili</a>, <a href="/search/astro-ph?searchtype=author&query=Damljanovic%2C+G">G. Damljanovic</a>, <a href="/search/astro-ph?searchtype=author&query=Dhalla%2C+S">S. Dhalla</a>, <a href="/search/astro-ph?searchtype=author&query=Frasca%2C+A">A. Frasca</a>, <a href="/search/astro-ph?searchtype=author&query=Hiriart%2C+D">D. Hiriart</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+S">S-M. Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Itoh%2C+R">R. Itoh</a>, <a href="/search/astro-ph?searchtype=author&query=Jableka%2C+D">D. Jableka</a>, <a href="/search/astro-ph?searchtype=author&query=Jorstad%2C+S">S. Jorstad</a>, <a href="/search/astro-ph?searchtype=author&query=Jovanovic%2C+M+D">M. D. Jovanovic</a>, <a href="/search/astro-ph?searchtype=author&query=Kawabata%2C+K+S">K. S. Kawabata</a>, <a href="/search/astro-ph?searchtype=author&query=Klimanov%2C+S+A">S. A. Klimanov</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtanidze%2C+O">O. Kurtanidze</a>, <a href="/search/astro-ph?searchtype=author&query=Larionov%2C+V+M">V. M. Larionov</a> , et al. (21 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1608.03531v1-abstract-short" style="display: inline;"> Here we report on the results of the WEBT photo-polarimetric campaign targeting the blazar S5~0716+71, organized in March 2014 to monitor the source simultaneously in BVRI and near IR filters. The campaign resulted in an unprecedented dataset spanning $\sim 110$\,h of nearly continuous, multi-band observations, including two sets of densely sampled polarimetric data mainly in R filter. During the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1608.03531v1-abstract-full').style.display = 'inline'; document.getElementById('1608.03531v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1608.03531v1-abstract-full" style="display: none;"> Here we report on the results of the WEBT photo-polarimetric campaign targeting the blazar S5~0716+71, organized in March 2014 to monitor the source simultaneously in BVRI and near IR filters. The campaign resulted in an unprecedented dataset spanning $\sim 110$\,h of nearly continuous, multi-band observations, including two sets of densely sampled polarimetric data mainly in R filter. During the campaign, the source displayed pronounced variability with peak-to-peak variations of about $30\%$ and "bluer-when-brighter" spectral evolution, consisting of a day-timescale modulation with superimposed hourlong microflares characterized by $\sim 0.1$\,mag flux changes. We performed an in-depth search for quasi-periodicities in the source light curve; hints for the presence of oscillations on timescales of $\sim 3$\,h and $\sim 5$\,h do not represent highly significant departures from a pure red-noise power spectrum. We observed that, at a certain configuration of the optical polarization angle relative to the positional angle of the innermost radio jet in the source, changes in the polarization degree led the total flux variability by about 2\,h; meanwhile, when the relative configuration of the polarization and jet angles altered, no such lag could be noted. The microflaring events, when analyzed as separate pulse emission components, were found to be characterized by a very high polarization degree ($> 30\%$) and polarization angles which differed substantially from the polarization angle of the underlying background component, or from the radio jet positional angle. We discuss the results in the general context of blazar emission and energy dissipation models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1608.03531v1-abstract-full').style.display = 'none'; document.getElementById('1608.03531v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 August, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 17 Figures; ApJ accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1604.07864">arXiv:1604.07864</a> <span> [<a href="https://arxiv.org/pdf/1604.07864">pdf</a>, <a href="https://arxiv.org/ps/1604.07864">ps</a>, <a href="https://arxiv.org/format/1604.07864">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/0067-0049/225/1/8">10.3847/0067-0049/225/1/8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Supplement: Localization and broadband follow-up of the gravitational-wave transient GW150914 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+B+P">B. P. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abernathy%2C+M+R">M. R. Abernathy</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+T">T. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Addesso%2C+P">P. Addesso</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/astro-ph?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+B">B. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+S+B">S. B. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+W+G">W. G. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Arai%2C+K">K. Arai</a> , et al. (1522 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1604.07864v3-abstract-short" style="display: inline;"> This Supplement provides supporting material for arXiv:1602.08492 . We briefly summarize past electromagnetic (EM) follow-up efforts as well as the organization and policy of the current EM follow-up program. We compare the four probability sky maps produced for the gravitational-wave transient GW150914, and provide additional details of the EM follow-up observations that were performed in the dif… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.07864v3-abstract-full').style.display = 'inline'; document.getElementById('1604.07864v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1604.07864v3-abstract-full" style="display: none;"> This Supplement provides supporting material for arXiv:1602.08492 . We briefly summarize past electromagnetic (EM) follow-up efforts as well as the organization and policy of the current EM follow-up program. We compare the four probability sky maps produced for the gravitational-wave transient GW150914, and provide additional details of the EM follow-up observations that were performed in the different bands. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.07864v3-abstract-full').style.display = 'none'; document.getElementById('1604.07864v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 July, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 April, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">For the main Letter, see arXiv:1602.08492</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P1600137-v2 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal Supplement Series, 225:8 (15pp), 2016 July </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1603.00249">arXiv:1603.00249</a> <span> [<a href="https://arxiv.org/pdf/1603.00249">pdf</a>, <a href="https://arxiv.org/format/1603.00249">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201527725e">10.1051/0004-6361/201527725e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Polarization angle swings in blazars: The case of 3C 279 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kiehlmann%2C+S">S. Kiehlmann</a>, <a href="/search/astro-ph?searchtype=author&query=Savolainen%2C+T">T. Savolainen</a>, <a href="/search/astro-ph?searchtype=author&query=Jorstad%2C+S+G">S. G. Jorstad</a>, <a href="/search/astro-ph?searchtype=author&query=Sokolovsky%2C+K+V">K. V. Sokolovsky</a>, <a href="/search/astro-ph?searchtype=author&query=Schinzel%2C+F+K">F. K. Schinzel</a>, <a href="/search/astro-ph?searchtype=author&query=Marscher%2C+A+P">A. P. Marscher</a>, <a href="/search/astro-ph?searchtype=author&query=Larionov%2C+V+M">V. M. Larionov</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Akitaya%2C+H">H. Akitaya</a>, <a href="/search/astro-ph?searchtype=author&query=Ben%C3%ADtez%2C+E">E. Ben铆tez</a>, <a href="/search/astro-ph?searchtype=author&query=Berdyugin%2C+A">A. Berdyugin</a>, <a href="/search/astro-ph?searchtype=author&query=Blinov%2C+D+A">D. A. Blinov</a>, <a href="/search/astro-ph?searchtype=author&query=Bochkarev%2C+N+G">N. G. Bochkarev</a>, <a href="/search/astro-ph?searchtype=author&query=Borman%2C+G+A">G. A. Borman</a>, <a href="/search/astro-ph?searchtype=author&query=Burenkov%2C+A+N">A. N. Burenkov</a>, <a href="/search/astro-ph?searchtype=author&query=Casadio%2C+C">C. Casadio</a>, <a href="/search/astro-ph?searchtype=author&query=Doroshenko%2C+V+T">V. T. Doroshenko</a>, <a href="/search/astro-ph?searchtype=author&query=Efimova%2C+N+V">N. V. Efimova</a>, <a href="/search/astro-ph?searchtype=author&query=Fukazawa%2C+Y">Y. Fukazawa</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B3mez%2C+J+L">J. L. G贸mez</a>, <a href="/search/astro-ph?searchtype=author&query=Grishina%2C+T+S">T. S. Grishina</a>, <a href="/search/astro-ph?searchtype=author&query=Hagen-Thorn%2C+V+A">V. A. Hagen-Thorn</a>, <a href="/search/astro-ph?searchtype=author&query=Heidt%2C+J">J. Heidt</a>, <a href="/search/astro-ph?searchtype=author&query=Hiriart%2C+D">D. Hiriart</a>, <a href="/search/astro-ph?searchtype=author&query=Itoh%2C+R">R. Itoh</a> , et al. (39 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1603.00249v2-abstract-short" style="display: inline;"> Over the past few years, several occasions of large, continuous rotations of the electric vector position angle (EVPA) of linearly polarized optical emission from blazars have been reported. These events are often coincident with high energy gamma-ray flares and they have attracted considerable attention, as they could allow one to probe the magnetic field structure in the gamma-ray emitting regio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1603.00249v2-abstract-full').style.display = 'inline'; document.getElementById('1603.00249v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1603.00249v2-abstract-full" style="display: none;"> Over the past few years, several occasions of large, continuous rotations of the electric vector position angle (EVPA) of linearly polarized optical emission from blazars have been reported. These events are often coincident with high energy gamma-ray flares and they have attracted considerable attention, as they could allow one to probe the magnetic field structure in the gamma-ray emitting region of the jet. The flat-spectrum radio quasar 3C279 is one of the most prominent examples showing this behaviour. Our goal is to study the observed EVPA rotations and to distinguish between a stochastic and a deterministic origin of the polarization variability. We have combined multiple data sets of R-band photometry and optical polarimetry measurements of 3C279, yielding exceptionally well-sampled flux density and polarization curves that cover a period of 2008-2012. Several large EVPA rotations are identified in the data. We introduce a quantitative measure for the EVPA curve smoothness, which is then used to test a set of simple random walk polarization variability models against the data. 3C279 shows different polarization variation characteristics during an optical low-flux state and a flaring state. The polarization variation during the flaring state, especially the smooth approx. 360 degrees rotation of the EVPA in mid-2011, is not consistent with the tested stochastic processes. We conclude that during the two different optical flux states, two different processes govern the polarization variation, possibly a stochastic process during the low-brightness state and a deterministic process during the flaring activity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1603.00249v2-abstract-full').style.display = 'none'; document.getElementById('1603.00249v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 June, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 March, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 15 figures, 6 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 592, C1 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1602.08492">arXiv:1602.08492</a> <span> [<a href="https://arxiv.org/pdf/1602.08492">pdf</a>, <a href="https://arxiv.org/format/1602.08492">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8205/826/1/L13">10.3847/2041-8205/826/1/L13 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Localization and broadband follow-up of the gravitational-wave transient GW150914 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+B+P">B. P. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abernathy%2C+M+R">M. R. Abernathy</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+T">T. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Addesso%2C+P">P. Addesso</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/astro-ph?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+B">B. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+S+B">S. B. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+W+G">W. G. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Arai%2C+K">K. Arai</a> , et al. (1522 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1602.08492v4-abstract-short" style="display: inline;"> A gravitational-wave (GW) transient was identified in data recorded by the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) detectors on 2015 September 14. The event, initially designated G184098 and later given the name GW150914, is described in detail elsewhere. By prior arrangement, preliminary estimates of the time, significance, and sky location of the event were shared wit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1602.08492v4-abstract-full').style.display = 'inline'; document.getElementById('1602.08492v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1602.08492v4-abstract-full" style="display: none;"> A gravitational-wave (GW) transient was identified in data recorded by the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) detectors on 2015 September 14. The event, initially designated G184098 and later given the name GW150914, is described in detail elsewhere. By prior arrangement, preliminary estimates of the time, significance, and sky location of the event were shared with 63 teams of observers covering radio, optical, near-infrared, X-ray, and gamma-ray wavelengths with ground- and space-based facilities. In this Letter we describe the low-latency analysis of the GW data and present the sky localization of the first observed compact binary merger. We summarize the follow-up observations reported by 25 teams via private Gamma-ray Coordinates Network circulars, giving an overview of the participating facilities, the GW sky localization coverage, the timeline and depth of the observations. As this event turned out to be a binary black hole merger, there is little expectation of a detectable electromagnetic (EM) signature. Nevertheless, this first broadband campaign to search for a counterpart of an Advanced LIGO source represents a milestone and highlights the broad capabilities of the transient astronomy community and the observing strategies that have been developed to pursue neutron star binary merger events. Detailed investigations of the EM data and results of the EM follow-up campaign are being disseminated in papers by the individual teams. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1602.08492v4-abstract-full').style.display = 'none'; document.getElementById('1602.08492v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 July, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 February, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">For Supplement, see https://arxiv.org/abs/1604.07864</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P1500227-v12 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal Letters, 826:L13 (8pp), 2016 July 20 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1508.04565">arXiv:1508.04565</a> <span> [<a href="https://arxiv.org/pdf/1508.04565">pdf</a>, <a href="https://arxiv.org/format/1508.04565">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201526790">10.1051/0004-6361/201526790 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Variable-Density Absorption Event in NGC 3227 mapped with Suzaku and Swift </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Beuchert%2C+T">T. Beuchert</a>, <a href="/search/astro-ph?searchtype=author&query=Markowitz%2C+A+G">A. G. Markowitz</a>, <a href="/search/astro-ph?searchtype=author&query=Krau%C3%9F%2C+F">F. Krau脽</a>, <a href="/search/astro-ph?searchtype=author&query=Miniutti%2C+G">G. Miniutti</a>, <a href="/search/astro-ph?searchtype=author&query=Longinotti%2C+A+L">A. L. Longinotti</a>, <a href="/search/astro-ph?searchtype=author&query=Guainazzi%2C+M">M. Guainazzi</a>, <a href="/search/astro-ph?searchtype=author&query=de+La+Calle%2C+I">I. de La Calle</a>, <a href="/search/astro-ph?searchtype=author&query=Malkan%2C+M">M. Malkan</a>, <a href="/search/astro-ph?searchtype=author&query=Elvis%2C+M">M. Elvis</a>, <a href="/search/astro-ph?searchtype=author&query=Miyaji%2C+T">T. Miyaji</a>, <a href="/search/astro-ph?searchtype=author&query=Hiriart%2C+D">D. Hiriart</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez%2C+J+M">J. M. L贸pez</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Dauser%2C+T">T. Dauser</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia%2C+J">J. Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Kreikenbohm%2C+A">A. Kreikenbohm</a>, <a href="/search/astro-ph?searchtype=author&query=Kadler%2C+M">M. Kadler</a>, <a href="/search/astro-ph?searchtype=author&query=Wilms%2C+J">J. Wilms</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1508.04565v1-abstract-short" style="display: inline;"> The morphology of the circumnuclear gas accreting onto supermassive black holes in Seyfert galaxies remains a topic of much debate. As the innermost regions of Active Galactic Nuclei (AGN) are spatially unresolved, X-ray spectroscopy, and in particular line-of-sight absorption variability, is a key diagnostic to map out the distribution of gas. Observations of variable X-ray absorption in multiple… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.04565v1-abstract-full').style.display = 'inline'; document.getElementById('1508.04565v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1508.04565v1-abstract-full" style="display: none;"> The morphology of the circumnuclear gas accreting onto supermassive black holes in Seyfert galaxies remains a topic of much debate. As the innermost regions of Active Galactic Nuclei (AGN) are spatially unresolved, X-ray spectroscopy, and in particular line-of-sight absorption variability, is a key diagnostic to map out the distribution of gas. Observations of variable X-ray absorption in multiple Seyferts and over a wide range of timescales indicate the presence of clumps/clouds of gas within the circumnuclear material. Eclipse events by clumps transiting the line of sight allow us to explore the properties of the clumps over a wide range of radial distances from the optical/UV Broad Line Region (BLR) to beyond the dust sublimation radius. Time-resolved absorption events have been extremely rare so far, but suggest a range of density profiles across Seyferts. We resolve a weeks-long absorption event in the Seyfert NGC 3227. We examine six Suzaku and twelve Swift observations from a 2008 campaign spanning 5 weeks. We use a model accounting for the complex spectral interplay of three differently-ionized absorbers. We perform time-resolved spectroscopy to discern the absorption variability behavior. We also examine the IR-to-X-ray spectral energy distribution (SED) to test for reddening by dust. The 2008 absorption event is due to moderately-ionized ($\log 尉\sim 1.2-1.4$) gas covering 90% of the line of sight. We resolve the density profile to be highly irregular, in contrast to a previous symmetric and centrally-peaked event mapped with RXTE in the same object. The UV data do not show significant reddening, suggesting that the cloud is dust-free. The 2008 campaign has revealed a transit by a filamentary, moderately-ionized cloud of variable density that is likely located in the BLR, and possibly part of a disk wind. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.04565v1-abstract-full').style.display = 'none'; document.getElementById('1508.04565v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 August, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication by A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 584, A82 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1508.01438">arXiv:1508.01438</a> <span> [<a href="https://arxiv.org/pdf/1508.01438">pdf</a>, <a href="https://arxiv.org/format/1508.01438">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Flaring activity of Mrk 421 in 2012 and 2013: orphan flare and multiwavelength analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fraija%2C+N">Nissim Fraija</a>, <a href="/search/astro-ph?searchtype=author&query=Cabrera%2C+J+I">Jos茅 Ignacio Cabrera</a>, <a href="/search/astro-ph?searchtype=author&query=Ben%C3%ADtez%2C+E">Erika Ben铆tez</a>, <a href="/search/astro-ph?searchtype=author&query=Hiriart%2C+D">David Hiriart</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1508.01438v1-abstract-short" style="display: inline;"> The first one started in 2012 July 16 (MJD 56124) and the second one in 2013 April 9 (MJD 56391). The multiwavelength data analysis shows that the $纬$-ray flare observed in 2012 was not detected in the hard-X ray bands. This result is usually interpreted as an "orphan" flare. In 2013, the analysis of the multiwavelength light curves shows that there are two very bright states detected in the optic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.01438v1-abstract-full').style.display = 'inline'; document.getElementById('1508.01438v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1508.01438v1-abstract-full" style="display: none;"> The first one started in 2012 July 16 (MJD 56124) and the second one in 2013 April 9 (MJD 56391). The multiwavelength data analysis shows that the $纬$-ray flare observed in 2012 was not detected in the hard-X ray bands. This result is usually interpreted as an "orphan" flare. In 2013, the analysis of the multiwavelength light curves shows that there are two very bright states detected in the optical R-band. The first one in 2013 April 9 (R =11.74 $\pm$ 0.04) and the second one in May 12 (R =11.62 $\pm$ 0.04). Also, high activity states were detected in the soft and hard X-rays. A discrete correlation function analysis of this last flare shows a strong correlation between the GeV $纬$-rays and the optical/hard-X ray emission. These results are discussed in terms of the more adequate standard scenarios that could explain the multiwavelength variations displayed by this blazar. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.01438v1-abstract-full').style.display = 'none'; document.getElementById('1508.01438v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 August, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 2 figures. In proceedings of "Swift: 10 Years of Discovery" congress (Rome, 2-4 December 2014), PoS(SWIFT 10)152</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1507.08424">arXiv:1507.08424</a> <span> [<a href="https://arxiv.org/pdf/1507.08424">pdf</a>, <a href="https://arxiv.org/format/1507.08424">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/2041-8205/809/2/L27">10.1088/2041-8205/809/2/L27 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of a Highly Polarized Optical Microflare in the Blazar S5 0716+714 During 2014 WEBT Campaign </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bhatta%2C+G">Gopal Bhatta</a>, <a href="/search/astro-ph?searchtype=author&query=Goyal%2C+A">Arti Goyal</a>, <a href="/search/astro-ph?searchtype=author&query=Ostrowski%2C+M">Michal Ostrowski</a>, <a href="/search/astro-ph?searchtype=author&query=Stawarz%2C+%C5%81">艁ukasz Stawarz</a>, <a href="/search/astro-ph?searchtype=author&query=Arkharov%2C+A+A">A. A. Arkharov</a>, <a href="/search/astro-ph?searchtype=author&query=Akitaya%2C+H">Hiroshi Akitaya</a>, <a href="/search/astro-ph?searchtype=author&query=Bachev%2C+R">Rumen Bachev</a>, <a href="/search/astro-ph?searchtype=author&query=Ben%C3%ADtez%2C+E">Erika Ben铆tez</a>, <a href="/search/astro-ph?searchtype=author&query=Borman%2C+G+A">G. A. Borman</a>, <a href="/search/astro-ph?searchtype=author&query=Carosati%2C+D">Daniele Carosati</a>, <a href="/search/astro-ph?searchtype=author&query=Cason%2C+A">Andy Cason</a>, <a href="/search/astro-ph?searchtype=author&query=Damljanovic%2C+G">Goran Damljanovic</a>, <a href="/search/astro-ph?searchtype=author&query=Dhalla%2C+S">Sarah Dhalla</a>, <a href="/search/astro-ph?searchtype=author&query=Frasca%2C+A">Antonio Frasca</a>, <a href="/search/astro-ph?searchtype=author&query=Hiriart%2C+D">David Hiriart</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+S+M">Shao Ming Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Itoh%2C+R">Ryosuke Itoh</a>, <a href="/search/astro-ph?searchtype=author&query=Jableka%2C+D">Damian Jableka</a>, <a href="/search/astro-ph?searchtype=author&query=Jorstad%2C+S">Svetlana Jorstad</a>, <a href="/search/astro-ph?searchtype=author&query=Kawabata%2C+K">Koji Kawabata</a>, <a href="/search/astro-ph?searchtype=author&query=Klimanov%2C+S">Sergey Klimanov</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtanidze%2C+O">Omar Kurtanidze</a>, <a href="/search/astro-ph?searchtype=author&query=Larionov%2C+V">Valeri Larionov</a>, <a href="/search/astro-ph?searchtype=author&query=Laurence%2C+D">Douglas Laurence</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+G">Giuseppe Leto</a> , et al. (20 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1507.08424v2-abstract-short" style="display: inline;"> The occurrence of low-amplitude flux variations in blazars on hourly timescales, commonly known as microvariability, is still a widely debated subject in high-energy astrophysics. Several competing scenarios have been proposed to explain such occurrences, including various jet plasma instabilities leading to the formation of shocks, magnetic reconnection sites, and turbulence. In this letter we pr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1507.08424v2-abstract-full').style.display = 'inline'; document.getElementById('1507.08424v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1507.08424v2-abstract-full" style="display: none;"> The occurrence of low-amplitude flux variations in blazars on hourly timescales, commonly known as microvariability, is still a widely debated subject in high-energy astrophysics. Several competing scenarios have been proposed to explain such occurrences, including various jet plasma instabilities leading to the formation of shocks, magnetic reconnection sites, and turbulence. In this letter we present the results of our detailed investigation of a prominent, five-hour-long optical microflare detected during recent WEBT campaign in 2014, March 2-6 targeting the blazar 0716+714. After separating the flaring component from the underlying base emission continuum of the blazar, we find that the microflare is highly polarized, with the polarization degree $\sim (40-60)\%$$\pm (2-10)\%$, and the electric vector position angle $\sim (10 - 20)$deg$\pm (1-8)$deg slightly misaligned with respect to the position angle of the radio jet. The microflare evolution in the $(Q,\,U)$ Stokes parameter space exhibits a looping behavior with a counter-clockwise rotation, meaning polarization degree decreasing with the flux (but higher in the flux decaying phase), and approximately stable polarization angle. The overall very high polarization degree of the flare, its symmetric flux rise and decay profiles, and also its structured evolution in the $Q-U$ plane, all imply that the observed flux variation corresponds to a single emission region characterized by a highly ordered magnetic field. As discussed in the paper, a small-scale but strong shock propagating within the outflow, and compressing a disordered magnetic field component, provides a natural, though not unique, interpretation of our findings. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1507.08424v2-abstract-full').style.display = 'none'; document.getElementById('1507.08424v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 July, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 July, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 4 Figures, ApJ Letter accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1408.1339">arXiv:1408.1339</a> <span> [<a href="https://arxiv.org/pdf/1408.1339">pdf</a>, <a href="https://arxiv.org/ps/1408.1339">ps</a>, <a href="https://arxiv.org/format/1408.1339">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/794/1/54">10.1088/0004-637X/794/1/54 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Rotation of the optical polarization angle associated with the 2008 纬-ray flare of blazar w comae </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sorcia%2C+M">Marco Sorcia</a>, <a href="/search/astro-ph?searchtype=author&query=Ben%C3%ADtez%2C+E">Erika Ben铆tez</a>, <a href="/search/astro-ph?searchtype=author&query=Hiriart%2C+D">David Hiriart</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez%2C+J+M">Jos茅 M. L贸pez</a>, <a href="/search/astro-ph?searchtype=author&query=Cabrera%2C+J+I">Jos茅 I. Cabrera</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%BAjica%2C+R">Ra煤l M煤jica</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1408.1339v1-abstract-short" style="display: inline;"> An $R$--band photopolarimetric variability analysis of the TeV bright blazar W Comae, between 2008 February 28 and 2013 May 17, is presented. The source showed a gradual tendency to decrease its mean flux level with a total change of ~3~mJy. A maximum and minimum brightness states in the $R$-band of 14.25$\pm$0.04 and 16.52$\pm$0.1~mag respectively were observed, corresponding to a maximum variati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.1339v1-abstract-full').style.display = 'inline'; document.getElementById('1408.1339v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1408.1339v1-abstract-full" style="display: none;"> An $R$--band photopolarimetric variability analysis of the TeV bright blazar W Comae, between 2008 February 28 and 2013 May 17, is presented. The source showed a gradual tendency to decrease its mean flux level with a total change of ~3~mJy. A maximum and minimum brightness states in the $R$-band of 14.25$\pm$0.04 and 16.52$\pm$0.1~mag respectively were observed, corresponding to a maximum variation of $螖$F = 5.40 mJy. We estimated a minimum variability timescale of $螖$t=3.3 days. A maximum polarization degree $P$=33.8\%$\pm$1.6\%, with a maximum variation of $螖$P = 33.2\%, was found. One of our main results is the detection of a large rotation of the polarization angle from 78\degr to 315\degr ($螖胃\sim$237\degr) that coincides in time with the $纬$-ray flare observed in 2008 June. This result indicates that both optical and $纬$-ray emission regions could be co-spatial. During this flare, a correlation between the $R$-band flux and polarization degree was found with a correlation coefficient of $r_{F-p}=0.93\pm$0.11. From the Stokes parameters we infer the existence of two optically thin synchrotron components that contribute to the polarized flux. One of them is stable with a constant polarization degree of 11\%. Assuming a shock-in jet model during the 2008 flare, we estimated a maximum Doppler factor $未_D\sim 27$ and a minimum of $未_D\sim 16$; a minimum viewing angle of the jet $\sim$2\degr.0; and a magnetic field $B \sim$ 0.12~G. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.1339v1-abstract-full').style.display = 'none'; document.getElementById('1408.1339v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 August, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in ApJ,34 pages,6 figures,4 tables. arXiv admin note: text overlap with arXiv:1304.2819</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1311.3126">arXiv:1311.3126</a> <span> [<a href="https://arxiv.org/pdf/1311.3126">pdf</a>, <a href="https://arxiv.org/ps/1311.3126">ps</a>, <a href="https://arxiv.org/format/1311.3126">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/epjconf/20136106003">10.1051/epjconf/20136106003 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Analyzing polarization swings in 3C 279 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kiehlmann%2C+S">S. Kiehlmann</a>, <a href="/search/astro-ph?searchtype=author&query=Savolainen%2C+T">T. Savolainen</a>, <a href="/search/astro-ph?searchtype=author&query=Jorstad%2C+S+G">S. G. Jorstad</a>, <a href="/search/astro-ph?searchtype=author&query=Sokolovsky%2C+K+V">K. V. Sokolovsky</a>, <a href="/search/astro-ph?searchtype=author&query=Schinzel%2C+F+K">F. K. Schinzel</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Arkharov%2C+A+A">A. A. Arkharov</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+E">E. Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Berdyugin%2C+A">A. Berdyugin</a>, <a href="/search/astro-ph?searchtype=author&query=Blinov%2C+D+A">D. A. Blinov</a>, <a href="/search/astro-ph?searchtype=author&query=Bochkarev%2C+N+G">N. G. Bochkarev</a>, <a href="/search/astro-ph?searchtype=author&query=Borman%2C+G+A">G. A. Borman</a>, <a href="/search/astro-ph?searchtype=author&query=Burenkov%2C+A+N">A. N. Burenkov</a>, <a href="/search/astro-ph?searchtype=author&query=Casadio%2C+C">C. Casadio</a>, <a href="/search/astro-ph?searchtype=author&query=Doroshenko%2C+V+T">V. T. Doroshenko</a>, <a href="/search/astro-ph?searchtype=author&query=Efimova%2C+N+V">N. V. Efimova</a>, <a href="/search/astro-ph?searchtype=author&query=Fukazawa%2C+Y">Y. Fukazawa</a>, <a href="/search/astro-ph?searchtype=author&query=Gomez%2C+J+L">J. L. Gomez</a>, <a href="/search/astro-ph?searchtype=author&query=Hagen-Thorn%2C+V+A">V. A. Hagen-Thorn</a>, <a href="/search/astro-ph?searchtype=author&query=Heidt%2C+J">J. Heidt</a>, <a href="/search/astro-ph?searchtype=author&query=Hiriart%2C+D">D. Hiriart</a>, <a href="/search/astro-ph?searchtype=author&query=Itoh%2C+R">R. Itoh</a>, <a href="/search/astro-ph?searchtype=author&query=Joshi%2C+M">M. Joshi</a>, <a href="/search/astro-ph?searchtype=author&query=Kimeridze%2C+G+N">G. N. Kimeridze</a>, <a href="/search/astro-ph?searchtype=author&query=Konstantinova%2C+T+S">T. S. Konstantinova</a> , et al. (31 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1311.3126v2-abstract-short" style="display: inline;"> Quasar 3C 279 is known to exhibit episodes of optical polarization angle rotation. We present new, well-sampled optical polarization data for 3C 279 and introduce a method to distinguish between random and deterministic electric vector position angle (EVPA) variations. We observe EVPA rotations in both directions with different amplitudes and find that the EVPA variation shows characteristics of b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1311.3126v2-abstract-full').style.display = 'inline'; document.getElementById('1311.3126v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1311.3126v2-abstract-full" style="display: none;"> Quasar 3C 279 is known to exhibit episodes of optical polarization angle rotation. We present new, well-sampled optical polarization data for 3C 279 and introduce a method to distinguish between random and deterministic electric vector position angle (EVPA) variations. We observe EVPA rotations in both directions with different amplitudes and find that the EVPA variation shows characteristics of both random and deterministic cases. Our analysis indicates that the EVPA variation is likely dominated by a random process in the low brightness state of the jet and by a deterministic process in the flaring state. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1311.3126v2-abstract-full').style.display = 'none'; document.getElementById('1311.3126v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 November, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 November, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 2 figures, 4 tables, proceeding to appear on EPJ Web of Conferences "The Innermost Regions of Relativistic Jets and their Magnetic Fields (Granada, Spain,10-14 June 2013)"</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1309.0882">arXiv:1309.0882</a> <span> [<a href="https://arxiv.org/pdf/1309.0882">pdf</a>, <a href="https://arxiv.org/ps/1309.0882">ps</a>, <a href="https://arxiv.org/format/1309.0882">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Optical linear polarization measurements of WR massive binary and single stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Akras%2C+S">Stavros Akras</a>, <a href="/search/astro-ph?searchtype=author&query=Ramirez-Velez%2C+J">Julio Ramirez-Velez</a>, <a href="/search/astro-ph?searchtype=author&query=Hiriart%2C+D">David Hiriart</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+J+M">Jose Manuel Lopez</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1309.0882v1-abstract-short" style="display: inline;"> We present optical (UBVRI) linear polarimetric observations of 8 Wolf-Rayet (WR) massive binaries and single stars. We have corrected the observed values for the interstellar extinction and polarization by the interstellar medium to obtain the intrinsic polarization and position angle. We find three highly polarization stars between 5% and 10% (WR1, WR5 and WR146), three between 3% and 4% (WR2, WR… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1309.0882v1-abstract-full').style.display = 'inline'; document.getElementById('1309.0882v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1309.0882v1-abstract-full" style="display: none;"> We present optical (UBVRI) linear polarimetric observations of 8 Wolf-Rayet (WR) massive binaries and single stars. We have corrected the observed values for the interstellar extinction and polarization by the interstellar medium to obtain the intrinsic polarization and position angle. We find three highly polarization stars between 5% and 10% (WR1, WR5 and WR146), three between 3% and 4% (WR2, WR3 and WR4), and two between 1% and 2% (WR137 and WR140). Moreover, 5 stars show increasing degree of polarization to shorter wavelengths (e.g WR 146) indicative with asymmetric circumstellar envelope and 3 have nearly constant polarization within the errors (e.g WR 140). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1309.0882v1-abstract-full').style.display = 'none'; document.getElementById('1309.0882v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 September, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">3 pages, 2 figures, contributed paper to Massive Stars: From alpha to Omega</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1304.2819">arXiv:1304.2819</a> <span> [<a href="https://arxiv.org/pdf/1304.2819">pdf</a>, <a href="https://arxiv.org/ps/1304.2819">ps</a>, <a href="https://arxiv.org/format/1304.2819">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0067-0049/206/2/11">10.1088/0067-0049/206/2/11 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Long-term optical polarization variability of the tev blazar 1es~1959+650 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sorcia%2C+M">Marco Sorcia</a>, <a href="/search/astro-ph?searchtype=author&query=Ben%C3%ADtez%2C+E">Erika Ben铆tez</a>, <a href="/search/astro-ph?searchtype=author&query=Hiriart%2C+D">David Hiriart</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez%2C+J+M">Jos茅 M. L贸pez</a>, <a href="/search/astro-ph?searchtype=author&query=Cabrera%2C+J+I">Jos茅 I. Cabrera</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%BAjica%2C+R">Ra煤l M煤jica</a>, <a href="/search/astro-ph?searchtype=author&query=Heidt%2C+J">Jochen Heidt</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">Ivan Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Nilsson%2C+K">Kari Nilsson</a>, <a href="/search/astro-ph?searchtype=author&query=Mommert%2C+M">Michael Mommert</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1304.2819v1-abstract-short" style="display: inline;"> A detailed analysis of the optical polarimetric variability of the TeV blazar 1ES 1959+650 from 2007 October 18 to 2011 May 5 is presented. The source showed a maximum and minimum brightness states in the R-band of 14.08$\pm$0.03 mag and 15.20$\pm$0.03 mag, respectively, with a maximum variation of 1.12 mag, and also a maximum polarization degree of $P=$(12.2$\pm$0.7)%, with a maximum variation of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1304.2819v1-abstract-full').style.display = 'inline'; document.getElementById('1304.2819v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1304.2819v1-abstract-full" style="display: none;"> A detailed analysis of the optical polarimetric variability of the TeV blazar 1ES 1959+650 from 2007 October 18 to 2011 May 5 is presented. The source showed a maximum and minimum brightness states in the R-band of 14.08$\pm$0.03 mag and 15.20$\pm$0.03 mag, respectively, with a maximum variation of 1.12 mag, and also a maximum polarization degree of $P=$(12.2$\pm$0.7)%, with a maximum variation of 10.7%. From August to November 2009, a correlation between the optical $R$-band flux and the degree of linear polarization was found, with a correlation coefficient $r_{pol}$=0.984$\pm$0.025. The source presented a preferential position angle of optical polarization of $\sim153^{\circ}$, with variations of $10\degr$-$50\degr$, that is in agreement with the projected position angle of the parsec scale jet found at 43 GHz. From the Stokes parameters we infer the existence of two optically-thin synchrotron components that contribute to the polarized flux. One of them is stable, with a constant polarization degree of 4%. Assuming a stationary shock for the variable component, we estimated some parameters associated with the physics of the relativistic jet: the magnetic field, $B\sim$0.06 G, the Doppler factor, $未_{0}\sim$23, the viewing angle, $桅\sim2.4\degr$, and the size of the emission region $r_b\sim5.6\times10^{17}$ cm. Our study is consistent with the spine-sheath model to explain the polarimetric variability displayed by this source during our monitoring. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1304.2819v1-abstract-full').style.display = 'none'; document.getElementById('1304.2819v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 April, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">58 pages, 8 figures, 6 tables. Accepted for publication in ApJ Supplement</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> ApJS89764 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1212.0057">arXiv:1212.0057</a> <span> [<a href="https://arxiv.org/pdf/1212.0057">pdf</a>, <a href="https://arxiv.org/ps/1212.0057">ps</a>, <a href="https://arxiv.org/format/1212.0057">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnrasl/slt063">10.1093/mnrasl/slt063 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A hydrodynamical model for the FERMI-LAT gamma-ray light curve of Blazar PKS1510-089 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cabrera%2C+J+I">J. I. Cabrera</a>, <a href="/search/astro-ph?searchtype=author&query=Coronado%2C+Y">Y. Coronado</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+E">E. Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Mendoza%2C+S">S. Mendoza</a>, <a href="/search/astro-ph?searchtype=author&query=Hiriart%2C+D">D. Hiriart</a>, <a href="/search/astro-ph?searchtype=author&query=Sorcia%2C+M">M. Sorcia</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1212.0057v4-abstract-short" style="display: inline;"> A physical description of the formation and propagation of the working surface inside the relativistic jet of the Blazar PKS 1510-089 are used to model its gamma-ray variability light curve using FERMI-LAT data from 2008 to 2012. The physical model is based on conservation laws of mass and momentum at the working surface as explained by Mendoza et al. (2009). The hydrodynamical description of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1212.0057v4-abstract-full').style.display = 'inline'; document.getElementById('1212.0057v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1212.0057v4-abstract-full" style="display: none;"> A physical description of the formation and propagation of the working surface inside the relativistic jet of the Blazar PKS 1510-089 are used to model its gamma-ray variability light curve using FERMI-LAT data from 2008 to 2012. The physical model is based on conservation laws of mass and momentum at the working surface as explained by Mendoza et al. (2009). The hydrodynamical description of the working surface is parametrised by the initial velocity and mass injection rate at the base of the jet. We show that periodic variations on the injected velocity profiles are able to account for the observed luminosity. With this, we are able to obtain mass ejection rates of the central engine which are injected at the base of the jet, and oscillation frequencies of the flow, amongst other physical parameters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1212.0057v4-abstract-full').style.display = 'none'; document.getElementById('1212.0057v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 May, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 November, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 2 figures, 1 table, accepted for publication in MNRAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Monthly Notices of the Royal Astronomical Society: Letters, Volume 434, Issue 1, p.L6-L10, 2013 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1207.3979">arXiv:1207.3979</a> <span> [<a href="https://arxiv.org/pdf/1207.3979">pdf</a>, <a href="https://arxiv.org/ps/1207.3979">ps</a>, <a href="https://arxiv.org/format/1207.3979">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201219492">10.1051/0004-6361/201219492 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Variability of the blazar 4C 38.41 (B3 1633+382) from GHz frequencies to GeV energies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Raiteri%2C+C+M">C. M. Raiteri</a>, <a href="/search/astro-ph?searchtype=author&query=Villata%2C+M">M. Villata</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+P+S">P. S. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Larionov%2C+V+M">V. M. Larionov</a>, <a href="/search/astro-ph?searchtype=author&query=Acosta-Pulido%2C+J+A">J. A. Acosta-Pulido</a>, <a href="/search/astro-ph?searchtype=author&query=Aller%2C+M+F">M. F. Aller</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ammando%2C+F">F. D'Ammando</a>, <a href="/search/astro-ph?searchtype=author&query=Gurwell%2C+M+A">M. A. Gurwell</a>, <a href="/search/astro-ph?searchtype=author&query=Jorstad%2C+S+G">S. G. Jorstad</a>, <a href="/search/astro-ph?searchtype=author&query=Joshi%2C+M">M. Joshi</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtanidze%2C+O+M">O. M. Kurtanidze</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%A4hteenm%C3%A4ki%2C+A">A. L盲hteenm盲ki</a>, <a href="/search/astro-ph?searchtype=author&query=Mirzaqulov%2C+D+O">D. O. Mirzaqulov</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Aller%2C+H+D">H. D. Aller</a>, <a href="/search/astro-ph?searchtype=author&query=Ar%C3%A9valo%2C+M+J">M. J. Ar茅valo</a>, <a href="/search/astro-ph?searchtype=author&query=Arkharov%2C+A+A">A. A. Arkharov</a>, <a href="/search/astro-ph?searchtype=author&query=Bach%2C+U">U. Bach</a>, <a href="/search/astro-ph?searchtype=author&query=Ben%C3%ADtez%2C+E">E. Ben铆tez</a>, <a href="/search/astro-ph?searchtype=author&query=Berdyugin%2C+A">A. Berdyugin</a>, <a href="/search/astro-ph?searchtype=author&query=Blinov%2C+D+A">D. A. Blinov</a>, <a href="/search/astro-ph?searchtype=author&query=Blumenthal%2C+K">K. Blumenthal</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Bueno%2C+A">A. Bueno</a>, <a href="/search/astro-ph?searchtype=author&query=Carleton%2C+T+M">T. M. Carleton</a> , et al. (52 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1207.3979v1-abstract-short" style="display: inline;"> The quasar-type blazar 4C 38.41 (B3 1633+382) experienced a large outburst in 2011, which was detected throughout the entire electromagnetic spectrum. We present the results of low-energy multifrequency monitoring by the GASP project of the WEBT consortium and collaborators, as well as those of spectropolarimetric/spectrophotometric monitoring at the Steward Observatory. We also analyse high-energ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1207.3979v1-abstract-full').style.display = 'inline'; document.getElementById('1207.3979v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1207.3979v1-abstract-full" style="display: none;"> The quasar-type blazar 4C 38.41 (B3 1633+382) experienced a large outburst in 2011, which was detected throughout the entire electromagnetic spectrum. We present the results of low-energy multifrequency monitoring by the GASP project of the WEBT consortium and collaborators, as well as those of spectropolarimetric/spectrophotometric monitoring at the Steward Observatory. We also analyse high-energy observations of the Swift and Fermi satellites. In the optical-UV band, several results indicate that there is a contribution from a QSO-like emission component, in addition to both variable and polarised jet emission. The unpolarised emission component is likely thermal radiation from the accretion disc that dilutes the jet polarisation. We estimate its brightness to be R(QSO) ~ 17.85 - 18 and derive the intrinsic jet polarisation degree. We find no clear correlation between the optical and radio light curves, while the correlation between the optical and 纬-ray flux apparently fades in time, likely because of an increasing optical to 纬-ray flux ratio. As suggested for other blazars, the long-term variability of 4C 38.41 can be interpreted in terms of an inhomogeneous bent jet, where different emitting regions can change their alignment with respect to the line of sight, leading to variations in the Doppler factor 未. Under the hypothesis that in the period 2008-2011 all the 纬-ray and optical variability on a one-week timescale were due to changes in 未, this would range between ~ 7 and ~ 21. If the variability were caused by changes in the viewing angle 胃 only, then 胃 would go from ~ 2.6 degr to ~ 5 degr. Variations in the viewing angle would also account for the dependence of the polarisation degree on the source brightness in the framework of a shock-in-jet model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1207.3979v1-abstract-full').style.display = 'none'; document.getElementById('1207.3979v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 July, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 23 figures, in press for Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 545, A48 (2012) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1207.2932">arXiv:1207.2932</a> <span> [<a href="https://arxiv.org/pdf/1207.2932">pdf</a>, <a href="https://arxiv.org/ps/1207.2932">ps</a>, <a href="https://arxiv.org/format/1207.2932">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/751/2/159">10.1088/0004-637X/751/2/159 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multi-wavelength observations of blazar AO 0235+164 in the 2008-2009 flaring state </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Ajello%2C+M">M. Ajello</a>, <a href="/search/astro-ph?searchtype=author&query=Ballet%2C+J">J. Ballet</a>, <a href="/search/astro-ph?searchtype=author&query=Barbiellini%2C+G">G. Barbiellini</a>, <a href="/search/astro-ph?searchtype=author&query=Bastieri%2C+D">D. Bastieri</a>, <a href="/search/astro-ph?searchtype=author&query=Bellazzini%2C+R">R. Bellazzini</a>, <a href="/search/astro-ph?searchtype=author&query=Blandford%2C+R+D">R. D. Blandford</a>, <a href="/search/astro-ph?searchtype=author&query=Bloom%2C+E+D">E. D. Bloom</a>, <a href="/search/astro-ph?searchtype=author&query=Bonamente%2C+E">E. Bonamente</a>, <a href="/search/astro-ph?searchtype=author&query=Borgland%2C+A+W">A. W. Borgland</a>, <a href="/search/astro-ph?searchtype=author&query=Bottacini%2C+E">E. Bottacini</a>, <a href="/search/astro-ph?searchtype=author&query=Bregeon%2C+J">J. Bregeon</a>, <a href="/search/astro-ph?searchtype=author&query=Brigida%2C+M">M. Brigida</a>, <a href="/search/astro-ph?searchtype=author&query=Bruel%2C+P">P. Bruel</a>, <a href="/search/astro-ph?searchtype=author&query=Buehler%2C+R">R. Buehler</a>, <a href="/search/astro-ph?searchtype=author&query=Buson%2C+S">S. Buson</a>, <a href="/search/astro-ph?searchtype=author&query=Caliandro%2C+G+A">G. A. Caliandro</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+R+A">R. A. Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Caraveo%2C+P+A">P. A. Caraveo</a>, <a href="/search/astro-ph?searchtype=author&query=Casandjian%2C+J+M">J. M. Casandjian</a>, <a href="/search/astro-ph?searchtype=author&query=Cavazzuti%2C+E">E. Cavazzuti</a>, <a href="/search/astro-ph?searchtype=author&query=Cecchi%2C+C">C. Cecchi</a>, <a href="/search/astro-ph?searchtype=author&query=Charles%2C+E">E. Charles</a>, <a href="/search/astro-ph?searchtype=author&query=Chekhtman%2C+A">A. Chekhtman</a>, <a href="/search/astro-ph?searchtype=author&query=Chiang%2C+J">J. Chiang</a> , et al. (186 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1207.2932v1-abstract-short" style="display: inline;"> The blazar AO 0235+164 (z = 0.94) has been one of the most active objects observed by Fermi Large Area Telescope (LAT) since its launch in Summer 2008. In addition to the continuous coverage by Fermi, contemporaneous observations were carried out from the radio to 纬 -ray bands between 2008 September and 2009 February. In this paper, we summarize the rich multi-wavelength data collected during the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1207.2932v1-abstract-full').style.display = 'inline'; document.getElementById('1207.2932v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1207.2932v1-abstract-full" style="display: none;"> The blazar AO 0235+164 (z = 0.94) has been one of the most active objects observed by Fermi Large Area Telescope (LAT) since its launch in Summer 2008. In addition to the continuous coverage by Fermi, contemporaneous observations were carried out from the radio to 纬 -ray bands between 2008 September and 2009 February. In this paper, we summarize the rich multi-wavelength data collected during the campaign (including F-GAMMA, GASP- WEBT, Kanata, OVRO, RXTE, SMARTS, Swift, and other instruments), examine the cross-correlation between the light curves measured in the different energy bands, and interpret the resulting spectral energy distributions in the context of well-known blazar emission models. We find that the 纬 -ray activity is well correlated with a series of near-IR/optical flares, accompanied by an increase in the optical polarization degree. On the other hand, the X-ray light curve shows a distinct 20 day high state of unusually soft spectrum, which does not match the extrapolation of the optical/UV synchrotron spectrum. We tentatively interpret this feature as the bulk Compton emission by cold electrons contained in the jet, which requires an accretion disk corona with an effective covering factor of 19% at a distance of 100 Rg . We model the broadband spectra with a leptonic model with external radiation dominated by the infrared emission from the dusty torus. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1207.2932v1-abstract-full').style.display = 'none'; document.getElementById('1207.2932v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 July, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">48 pages, 8 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 751, 159 (2012) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1206.0745">arXiv:1206.0745</a> <span> [<a href="https://arxiv.org/pdf/1206.0745">pdf</a>, <a href="https://arxiv.org/ps/1206.0745">ps</a>, <a href="https://arxiv.org/format/1206.0745">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/754/2/114">10.1088/0004-637X/754/2/114 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The structure and emission model of the relativistic jet in the quasar 3C 279 inferred from radio to high-energy gamma-ray observations in 2008-2010 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hayashida%2C+M">M. Hayashida</a>, <a href="/search/astro-ph?searchtype=author&query=Madejski%2C+G+M">G. M. Madejski</a>, <a href="/search/astro-ph?searchtype=author&query=Nalewajko%2C+K">K. Nalewajko</a>, <a href="/search/astro-ph?searchtype=author&query=Sikora%2C+M">M. Sikora</a>, <a href="/search/astro-ph?searchtype=author&query=Wehrle%2C+A+E">A. E. Wehrle</a>, <a href="/search/astro-ph?searchtype=author&query=Ogle%2C+P">P. Ogle</a>, <a href="/search/astro-ph?searchtype=author&query=Collmar%2C+W">W. Collmar</a>, <a href="/search/astro-ph?searchtype=author&query=Larsson%2C+S">S. Larsson</a>, <a href="/search/astro-ph?searchtype=author&query=Fukazawa%2C+Y">Y. Fukazawa</a>, <a href="/search/astro-ph?searchtype=author&query=Itoh%2C+R">R. Itoh</a>, <a href="/search/astro-ph?searchtype=author&query=Chiang%2C+J">J. Chiang</a>, <a href="/search/astro-ph?searchtype=author&query=Stawarz%2C+L">L. Stawarz</a>, <a href="/search/astro-ph?searchtype=author&query=Blandford%2C+R+D">R. D. Blandford</a>, <a href="/search/astro-ph?searchtype=author&query=Richards%2C+J+L">J. L. Richards</a>, <a href="/search/astro-ph?searchtype=author&query=Max-Moerbeck%2C+W">W. Max-Moerbeck</a>, <a href="/search/astro-ph?searchtype=author&query=Readhead%2C+A">A. Readhead</a>, <a href="/search/astro-ph?searchtype=author&query=Buehler%2C+R">R. Buehler</a>, <a href="/search/astro-ph?searchtype=author&query=Cavazzuti%2C+E">E. Cavazzuti</a>, <a href="/search/astro-ph?searchtype=author&query=Ciprini%2C+S">S. Ciprini</a>, <a href="/search/astro-ph?searchtype=author&query=Gehrels%2C+N">N. Gehrels</a>, <a href="/search/astro-ph?searchtype=author&query=Reimer%2C+A">A. Reimer</a>, <a href="/search/astro-ph?searchtype=author&query=Szostek%2C+A">A. Szostek</a>, <a href="/search/astro-ph?searchtype=author&query=Tanaka%2C+T">T. Tanaka</a>, <a href="/search/astro-ph?searchtype=author&query=Tosti%2C+G">G. Tosti</a>, <a href="/search/astro-ph?searchtype=author&query=Uchiyama%2C+Y">Y. Uchiyama</a> , et al. (68 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1206.0745v1-abstract-short" style="display: inline;"> We present time-resolved broad-band observations of the quasar 3C 279 obtained from multi-wavelength campaigns conducted during the first two years of the Fermi Gamma-ray Space Telescope mission. While investigating the previously reported gamma-ray/optical flare accompanied by a change in optical polarization, we found that the optical emission appears delayed with respect to the gamma-ray emissi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1206.0745v1-abstract-full').style.display = 'inline'; document.getElementById('1206.0745v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1206.0745v1-abstract-full" style="display: none;"> We present time-resolved broad-band observations of the quasar 3C 279 obtained from multi-wavelength campaigns conducted during the first two years of the Fermi Gamma-ray Space Telescope mission. While investigating the previously reported gamma-ray/optical flare accompanied by a change in optical polarization, we found that the optical emission appears delayed with respect to the gamma-ray emission by about 10 days. X-ray observations reveal a pair of `isolated' flares separated by ~90 days, with only weak gamma-ray/optical counterparts. The spectral structure measured by Spitzer reveals a synchrotron component peaking in the mid-infrared band with a sharp break at the far-infrared band during the gamma-ray flare, while the peak appears in the mm/sub-mm band in the low state. Selected spectral energy distributions are fitted with leptonic models including Comptonization of external radiation produced in a dusty torus or the broad-line region. Adopting the interpretation of the polarization swing involving propagation of the emitting region along a curved trajectory, we can explain the evolution of the broad-band spectra during the gamma-ray flaring event by a shift of its location from ~ 1 pc to ~ 4 pc from the central black hole. On the other hand, if the gamma-ray flare is generated instead at sub-pc distance from the central black hole, the far-infrared break can be explained by synchrotron self-absorption. We also model the low spectral state, dominated by the mm/sub-mm peaking synchrotron component, and suggest that the corresponding inverse-Compton component explains the steady X-ray emission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1206.0745v1-abstract-full').style.display = 'none'; document.getElementById('1206.0745v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 June, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 18 figures 5 tables, Accepted for publication in The Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1105.0549">arXiv:1105.0549</a> <span> [<a href="https://arxiv.org/pdf/1105.0549">pdf</a>, <a href="https://arxiv.org/ps/1105.0549">ps</a>, <a href="https://arxiv.org/format/1105.0549">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/2041-8205/735/1/L10">10.1088/2041-8205/735/1/L10 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On the Location of the Gamma-ray Emission in the 2008 Outburst in the BL Lacertae Object AO 0235+164 through Observations across the Electromagnetic Spectrum </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">Ivan Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Marscher%2C+A+P">Alan P. Marscher</a>, <a href="/search/astro-ph?searchtype=author&query=Jorstad%2C+S+G">Svetlana G. Jorstad</a>, <a href="/search/astro-ph?searchtype=author&query=Larionov%2C+V+M">Valeri M. Larionov</a>, <a href="/search/astro-ph?searchtype=author&query=Gomez%2C+J+L">Jose L. Gomez</a>, <a href="/search/astro-ph?searchtype=author&query=Lahteenmaki%2C+A">Anne Lahteenmaki</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+P+S">Paul S. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Nilsson%2C+K">Kari Nilsson</a>, <a href="/search/astro-ph?searchtype=author&query=Readhead%2C+A+C+S">Anthony C. S. Readhead</a>, <a href="/search/astro-ph?searchtype=author&query=Aller%2C+M+F">Margo F. Aller</a>, <a href="/search/astro-ph?searchtype=author&query=Heidt%2C+J">Jochen Heidt</a>, <a href="/search/astro-ph?searchtype=author&query=Gurwell%2C+M">Mark Gurwell</a>, <a href="/search/astro-ph?searchtype=author&query=Thum%2C+C">Clemens Thum</a>, <a href="/search/astro-ph?searchtype=author&query=Wehrle%2C+A+E">Ann E. Wehrle</a>, <a href="/search/astro-ph?searchtype=author&query=Nikolashvili%2C+M+G">Maria G. Nikolashvili</a>, <a href="/search/astro-ph?searchtype=author&query=Aller%2C+H+D">Hugh D. Aller</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+E">Erika Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Blinov%2C+D+A">Dmitriy A. Blinov</a>, <a href="/search/astro-ph?searchtype=author&query=Hagen-Thorn%2C+V+A">Vladimir A. Hagen-Thorn</a>, <a href="/search/astro-ph?searchtype=author&query=Hiriart%2C+D">David Hiriart</a>, <a href="/search/astro-ph?searchtype=author&query=Jannuzi%2C+B+T">Buell T. Jannuzi</a>, <a href="/search/astro-ph?searchtype=author&query=Joshi%2C+M">Manasvita Joshi</a>, <a href="/search/astro-ph?searchtype=author&query=Kimeridze%2C+G+N">Givi N. Kimeridze</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtanidze%2C+O+M">Omar M. Kurtanidze</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtanidze%2C+S+O">Sofia O. Kurtanidze</a> , et al. (16 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1105.0549v2-abstract-short" style="display: inline;"> We present observations of a major outburst at centimeter, millimeter, optical, X-ray, and gamma-ray wavelengths of the BL Lacertae object AO 0235+164. We analyze the timing of multi-waveband variations in the flux and linear polarization, as well as changes in Very Long Baseline Array (VLBA) images at 7mm with 0.15 milliarcsecond resolution. The association of the events at different wavebands is… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1105.0549v2-abstract-full').style.display = 'inline'; document.getElementById('1105.0549v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1105.0549v2-abstract-full" style="display: none;"> We present observations of a major outburst at centimeter, millimeter, optical, X-ray, and gamma-ray wavelengths of the BL Lacertae object AO 0235+164. We analyze the timing of multi-waveband variations in the flux and linear polarization, as well as changes in Very Long Baseline Array (VLBA) images at 7mm with 0.15 milliarcsecond resolution. The association of the events at different wavebands is confirmed at high statistical significance by probability arguments and Monte-Carlo simulations. A series of sharp peaks in optical linear polarization, as well as a pronounced maximum in the 7 mm polarization of a superluminal jet knot, indicate rapid fluctuations in the degree of ordering of the magnetic field. These results lead us to conclude that the outburst occurred in the jet both in the quasi-stationary "core" and in the superluminal knot, both parsecs downstream of the supermassive black hole. We interpret the outburst as a consequence of the propagation of a disturbance, elongated along the line of sight by light-travel time delays, that passes through a standing recollimation shock in the core and propagates down the jet to create the superluminal knot. The multi-wavelength light curves vary together on long time-scales (months/years), but the correspondence is poorer on shorter time-scales. This, as well as the variability of the polarization and the dual location of the outburst, agrees with the expectations of a multi-zone emission model in which turbulence plays a major role in modulating the synchrotron and inverse Compton fluxes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1105.0549v2-abstract-full').style.display = 'none'; document.getElementById('1105.0549v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 May, 2011; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 May, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for Publication in the Astrophysical Journal Letters. 7 pages (including 5 figures). Minor corrections with regard to previous version, as proposed by the referee</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1103.5778">arXiv:1103.5778</a> <span> [<a href="https://arxiv.org/pdf/1103.5778">pdf</a>, <a href="https://arxiv.org/ps/1103.5778">ps</a>, <a href="https://arxiv.org/format/1103.5778">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/734/1/17">10.1088/0004-637X/734/1/17 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A study of the photometric variability of the peculiar magnetic white dwarf WD1953-011 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Valyavin%2C+G">G. Valyavin</a>, <a href="/search/astro-ph?searchtype=author&query=Antonyuk%2C+K">K. Antonyuk</a>, <a href="/search/astro-ph?searchtype=author&query=Plachinda%2C+S">S. Plachinda</a>, <a href="/search/astro-ph?searchtype=author&query=Clark%2C+D+M">D. M. Clark</a>, <a href="/search/astro-ph?searchtype=author&query=Wade%2C+G+A">G. A. Wade</a>, <a href="/search/astro-ph?searchtype=author&query=Machado%2C+L+F">L. Fox Machado</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+J+M">J. M. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Hiriart%2C+D">D. Hiriart</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+I">Inwoo Han</a>, <a href="/search/astro-ph?searchtype=author&query=Jeon%2C+Y">Young-Beom Jeon</a>, <a href="/search/astro-ph?searchtype=author&query=Bagnulo%2C+S">S. Bagnulo</a>, <a href="/search/astro-ph?searchtype=author&query=Zharikov%2C+S+V">S. V. Zharikov</a>, <a href="/search/astro-ph?searchtype=author&query=Zurita%2C+C">C. Zurita</a>, <a href="/search/astro-ph?searchtype=author&query=Mujica%2C+R">R. Mujica</a>, <a href="/search/astro-ph?searchtype=author&query=Shulyak%2C+D">D. Shulyak</a>, <a href="/search/astro-ph?searchtype=author&query=Burlakova%2C+T">T. Burlakova</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1103.5778v1-abstract-short" style="display: inline;"> We present and interpret simultaneous new photometric and spectroscopic observations of the peculiar magnetic white dwarf WD1953-011. The flux in the V-band filter and intensity of the Balmer spectral lines demonstrate variability with the rotation period of about 1.45 days. According to previous studies, this variability can be explained by the presence of a dark spot having a magnetic nature, an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1103.5778v1-abstract-full').style.display = 'inline'; document.getElementById('1103.5778v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1103.5778v1-abstract-full" style="display: none;"> We present and interpret simultaneous new photometric and spectroscopic observations of the peculiar magnetic white dwarf WD1953-011. The flux in the V-band filter and intensity of the Balmer spectral lines demonstrate variability with the rotation period of about 1.45 days. According to previous studies, this variability can be explained by the presence of a dark spot having a magnetic nature, analogous to a sunspot. Motivated by this idea, we examine possible physical relationships between the suggested dark spot and the strong-field magnetic structure (magnetic "spot", or "tube") recently identified on the surface of this star. Comparing the rotationally-modulated flux with the variable spectral observables related to the magnetic "spot" we establish their correlation, and therefore their physical relationship. Modeling the variable photometric flux assuming that it is associated with temperature variations in the stellar photosphere, we argue that the strong-field area and dark, low-temperature spot are comparable in size and located at the same latitudes, essentially overlapping each other with a possible slight longitudinal shift. In this paper we also present a new, improved value of the star's rotational period and constrain the characteristics of the thermal inhomogeneity over the degenerate's surface. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1103.5778v1-abstract-full').style.display = 'none'; document.getElementById('1103.5778v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 March, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted to the ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1103.3647">arXiv:1103.3647</a> <span> [<a href="https://arxiv.org/pdf/1103.3647">pdf</a>, <a href="https://arxiv.org/ps/1103.3647">ps</a>, <a href="https://arxiv.org/format/1103.3647">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201016128">10.1051/0004-6361/201016128 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> AGILE detection of extreme gamma-ray activity from the blazar PKS 1510-089 during March 2009. Multifrequency analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=D%27Ammando%2C+F">F. D'Ammando</a>, <a href="/search/astro-ph?searchtype=author&query=Raiteri%2C+C+M">C. M. Raiteri</a>, <a href="/search/astro-ph?searchtype=author&query=Villata%2C+M">M. Villata</a>, <a href="/search/astro-ph?searchtype=author&query=Romano%2C+P">P. Romano</a>, <a href="/search/astro-ph?searchtype=author&query=Pucella%2C+G">G. Pucella</a>, <a href="/search/astro-ph?searchtype=author&query=Krimm%2C+H+A">H. A. Krimm</a>, <a href="/search/astro-ph?searchtype=author&query=Covino%2C+S">S. Covino</a>, <a href="/search/astro-ph?searchtype=author&query=Orienti%2C+M">M. Orienti</a>, <a href="/search/astro-ph?searchtype=author&query=Giovannini%2C+G">G. Giovannini</a>, <a href="/search/astro-ph?searchtype=author&query=Vercellone%2C+S">S. Vercellone</a>, <a href="/search/astro-ph?searchtype=author&query=Pian%2C+E">E. Pian</a>, <a href="/search/astro-ph?searchtype=author&query=Donnarumma%2C+I">I. Donnarumma</a>, <a href="/search/astro-ph?searchtype=author&query=Vittorini%2C+V">V. Vittorini</a>, <a href="/search/astro-ph?searchtype=author&query=Tavani%2C+M">M. Tavani</a>, <a href="/search/astro-ph?searchtype=author&query=Argan%2C+A">A. Argan</a>, <a href="/search/astro-ph?searchtype=author&query=Barbiellini%2C+G">G. Barbiellini</a>, <a href="/search/astro-ph?searchtype=author&query=Boffelli%2C+F">F. Boffelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bulgarelli%2C+A">A. Bulgarelli</a>, <a href="/search/astro-ph?searchtype=author&query=Caraveo%2C+P">P. Caraveo</a>, <a href="/search/astro-ph?searchtype=author&query=Cattaneo%2C+P+W">P. W. Cattaneo</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+A+W">A. W. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cocco%2C+V">V. Cocco</a>, <a href="/search/astro-ph?searchtype=author&query=Costa%2C+E">E. Costa</a>, <a href="/search/astro-ph?searchtype=author&query=Del+Monte%2C+E">E. Del Monte</a>, <a href="/search/astro-ph?searchtype=author&query=De+Paris%2C+G">G. De Paris</a> , et al. (90 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1103.3647v1-abstract-short" style="display: inline;"> We report on the extreme gamma-ray activity from the FSRQ PKS 1510-089 observed by AGILE in March 2009. In the same period a radio-to-optical monitoring of the source was provided by the GASP-WEBT and REM. Moreover, several Swift ToO observations were triggered, adding important information on the source behaviour from optical/UV to hard X-rays. We paid particular attention to the calibration of t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1103.3647v1-abstract-full').style.display = 'inline'; document.getElementById('1103.3647v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1103.3647v1-abstract-full" style="display: none;"> We report on the extreme gamma-ray activity from the FSRQ PKS 1510-089 observed by AGILE in March 2009. In the same period a radio-to-optical monitoring of the source was provided by the GASP-WEBT and REM. Moreover, several Swift ToO observations were triggered, adding important information on the source behaviour from optical/UV to hard X-rays. We paid particular attention to the calibration of the Swift/UVOT data to make it suitable to the blazars spectra. Simultaneous observations from radio to gamma rays allowed us to study in detail the correlation among the emission variability at different frequencies and to investigate the mechanisms at work. In the period 9-30 March 2009, AGILE detected an average gamma-ray flux of (311+/-21)x10^-8 ph cm^-2 s^-1 for E>100 MeV, and a peak level of (702+/-131)x10^-8 ph cm^-2 s^-1 on daily integration. The gamma-ray activity occurred during a period of increasing activity from near-IR to UV, with a flaring episode detected on 26-27 March 2009, suggesting that a single mechanism is responsible for the flux enhancement observed from near-IR to UV. By contrast, Swift/XRT observations seem to show no clear correlation of the X-ray fluxes with the optical and gamma-ray ones. However, the X-ray observations show a harder photon index (1.3-1.6) with respect to most FSRQs and a hint of harder-when-brighter behaviour, indicating the possible presence of a second emission component at soft X-ray energies. Moreover, the broad band spectrum from radio-to-UV confirmed the evidence of thermal features in the optical/UV spectrum of PKS 1510-089 also during high gamma-ray state. On the other hand, during 25-26 March 2009 a flat spectrum in the optical/UV energy band was observed, suggesting an important contribution of the synchrotron emission in this part of the spectrum during the brightest gamma-ray flare, therefore a significant shift of the synchrotron peak. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1103.3647v1-abstract-full').style.display = 'none'; document.getElementById('1103.3647v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 March, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 7 figures, 3 tables. Accepted for publication in Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astron.Astrophys.529:A145,2011 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1002.1020">arXiv:1002.1020</a> <span> [<a href="https://arxiv.org/pdf/1002.1020">pdf</a>, <a href="https://arxiv.org/ps/1002.1020">ps</a>, <a href="https://arxiv.org/format/1002.1020">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/712/1/405">10.1088/0004-637X/712/1/405 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multiwavelength observations of 3C 454.3. III. Eighteen months of AGILE monitoring of the "Crazy Diamond" </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vercellone%2C+S">S. Vercellone</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ammando%2C+F">F. D'Ammando</a>, <a href="/search/astro-ph?searchtype=author&query=Vittorini%2C+V">V. Vittorini</a>, <a href="/search/astro-ph?searchtype=author&query=Donnarumma%2C+I">I. Donnarumma</a>, <a href="/search/astro-ph?searchtype=author&query=Pucella%2C+G">G. Pucella</a>, <a href="/search/astro-ph?searchtype=author&query=Tavani%2C+M">M. Tavani</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrari%2C+A">A. Ferrari</a>, <a href="/search/astro-ph?searchtype=author&query=Raiteri%2C+C+M">C. M. Raiteri</a>, <a href="/search/astro-ph?searchtype=author&query=Villata%2C+M">M. Villata</a>, <a href="/search/astro-ph?searchtype=author&query=Romano%2C+P">P. Romano</a>, <a href="/search/astro-ph?searchtype=author&query=Krimm%2C+H">H. Krimm</a>, <a href="/search/astro-ph?searchtype=author&query=Tiengo%2C+A">A. Tiengo</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+A+W">A. W. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Giovannini%2C+G">G. Giovannini</a>, <a href="/search/astro-ph?searchtype=author&query=Venturi%2C+T">T. Venturi</a>, <a href="/search/astro-ph?searchtype=author&query=Giroletti%2C+M">M. Giroletti</a>, <a href="/search/astro-ph?searchtype=author&query=Kovalev%2C+Y+Y">Y. Y. Kovalev</a>, <a href="/search/astro-ph?searchtype=author&query=Sokolovsky%2C+K">K. Sokolovsky</a>, <a href="/search/astro-ph?searchtype=author&query=Pushkarev%2C+A+B">A. B. Pushkarev</a>, <a href="/search/astro-ph?searchtype=author&query=Lister%2C+M+L">M. L. Lister</a>, <a href="/search/astro-ph?searchtype=author&query=Argan%2C+A">A. Argan</a>, <a href="/search/astro-ph?searchtype=author&query=Barbiellini%2C+G">G. Barbiellini</a>, <a href="/search/astro-ph?searchtype=author&query=Bulgarelli%2C+A">A. Bulgarelli</a>, <a href="/search/astro-ph?searchtype=author&query=Caraveo%2C+P">P. Caraveo</a>, <a href="/search/astro-ph?searchtype=author&query=Cattaneo%2C+P+W">P. W. Cattaneo</a> , et al. (88 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1002.1020v1-abstract-short" style="display: inline;"> We report on 18 months of multiwavelength observations of the blazar 3C 454.3 (Crazy Diamond) carried out in July 2007-January 2009. We show the results of the AGILE campaigns which took place on May-June 2008, July-August 2008, and October 2008-January 2009. During the May 2008-January 2009 period, the source average flux was highly variable, from an average gamma-ray flux F(E>100MeV) > 200E-8… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1002.1020v1-abstract-full').style.display = 'inline'; document.getElementById('1002.1020v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1002.1020v1-abstract-full" style="display: none;"> We report on 18 months of multiwavelength observations of the blazar 3C 454.3 (Crazy Diamond) carried out in July 2007-January 2009. We show the results of the AGILE campaigns which took place on May-June 2008, July-August 2008, and October 2008-January 2009. During the May 2008-January 2009 period, the source average flux was highly variable, from an average gamma-ray flux F(E>100MeV) > 200E-8 ph/cm2/s in May-June 2008, to F(E>100MeV)~80E-8 ph/cm2/s in October 2008-January 2009. The average gamma-ray spectrum between 100 MeV and 1 GeV can be fit by a simple power law (Gamma_GRID ~ 2.0 to 2.2). Only 3-sigma upper limits can be derived in the 20-60 keV energy band with Super-AGILE. During July-August 2007 and May-June 2008, RXTE measured a flux of F(3-20 keV)= 8.4E-11 erg/cm2/s, and F(3-20 keV)=4.5E-11 erg/cm2/s, respectively and a constant photon index Gamma_PCA=1.65. Swift/XRT observations were carried out during all AGILE campaigns, obtaining a F(2-10 keV)=(0.9-7.5)E-11 erg/cm2/s and a photon index Gamma_XRT=1.33-2.04. BAT measured an average flux of ~5 mCrab. GASP-WEBT monitored 3C 454.3 during the whole 2007-2008 period from the radio to the optical. A correlation analysis between the optical and the gamma-ray fluxes shows a time lag of tau=-0.4 days. An analysis of 15 GHz and 43 GHz VLBI core radio flux observations shows an increasing trend of the core radio flux, anti- correlated with the higher frequency data. The modeling SEDs, and the behavior of the long-term light curves in different energy bands, allow us to compare the jet properties during different emission states, and to study the geometrical properties of the jet on a time-span longer than one year. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1002.1020v1-abstract-full').style.display = 'none'; document.getElementById('1002.1020v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 February, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ. Adapted Abstract. 17 pages, 19 Figures, 5 Tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0910.3750">arXiv:0910.3750</a> <span> [<a href="https://arxiv.org/pdf/0910.3750">pdf</a>, <a href="https://arxiv.org/ps/0910.3750">ps</a>, <a href="https://arxiv.org/format/0910.3750">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/707/1/612">10.1088/0004-637X/707/1/612 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multiwavelength observations of a TeV-Flare from W Comae </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=VERITAS+collaboration"> VERITAS collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/astro-ph?searchtype=author&query=Aliu%2C+E">E. Aliu</a>, <a href="/search/astro-ph?searchtype=author&query=Aune%2C+T">T. Aune</a>, <a href="/search/astro-ph?searchtype=author&query=Beilicke%2C+M">M. Beilicke</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">W. Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Bottcher%2C+M">M. Bottcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boltuch%2C+D">D. Boltuch</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Bradbury%2C+S+M">S. M. Bradbury</a>, <a href="/search/astro-ph?searchtype=author&query=Bugaev%2C+V">V. Bugaev</a>, <a href="/search/astro-ph?searchtype=author&query=Byrum%2C+K">K. Byrum</a>, <a href="/search/astro-ph?searchtype=author&query=Cannon%2C+A">A. Cannon</a>, <a href="/search/astro-ph?searchtype=author&query=Cesarini%2C+A">A. Cesarini</a>, <a href="/search/astro-ph?searchtype=author&query=Ciupik%2C+L">L. Ciupik</a>, <a href="/search/astro-ph?searchtype=author&query=Cogan%2C+P">P. Cogan</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+W">W. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Dickherber%2C+R">R. Dickherber</a>, <a href="/search/astro-ph?searchtype=author&query=Duke%2C+C">C. Duke</a>, <a href="/search/astro-ph?searchtype=author&query=Falcone%2C+A">A. Falcone</a>, <a href="/search/astro-ph?searchtype=author&query=Finley%2C+J+P">J. P. Finley</a>, <a href="/search/astro-ph?searchtype=author&query=Fortin%2C+P">P. Fortin</a>, <a href="/search/astro-ph?searchtype=author&query=Fortson%2C+L">L. Fortson</a>, <a href="/search/astro-ph?searchtype=author&query=Furniss%2C+A">A. Furniss</a>, <a href="/search/astro-ph?searchtype=author&query=Galante%2C+N">N. Galante</a> , et al. (145 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0910.3750v1-abstract-short" style="display: inline;"> We report results from an intensive multiwavelength campaign on the intermediate-frequency-peaked BL Lacertae object W Com (z=0.102) during a strong outburst of very high energy gamma-ray emission in June 2008. The very high energy gamma-ray signal was detected by VERITAS on 2008 June 7-8 with a flux F(>200 GeV) = (5.7+-0.6)x10^-11 cm-2s-1, about three times brighter than during the discovery of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0910.3750v1-abstract-full').style.display = 'inline'; document.getElementById('0910.3750v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0910.3750v1-abstract-full" style="display: none;"> We report results from an intensive multiwavelength campaign on the intermediate-frequency-peaked BL Lacertae object W Com (z=0.102) during a strong outburst of very high energy gamma-ray emission in June 2008. The very high energy gamma-ray signal was detected by VERITAS on 2008 June 7-8 with a flux F(>200 GeV) = (5.7+-0.6)x10^-11 cm-2s-1, about three times brighter than during the discovery of gamma-ray emission from W Com by VERITAS in 2008 March. The initial detection of this flare by VERITAS at energies above 200 GeV was followed by observations in high energy gamma-rays (AGILE, E>100 MeV), and X-rays (Swift and XMM-Newton), and at UV, and ground-based optical and radio monitoring through the GASP-WEBT consortium and other observatories. Here we describe the multiwavelength data and derive the spectral energy distribution (SED) of the source from contemporaneous data taken throughout the flare. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0910.3750v1-abstract-full').style.display = 'none'; document.getElementById('0910.3750v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 October, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 pages, 5 figures; Accepted for publication by The Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0909.3484">arXiv:0909.3484</a> <span> [<a href="https://arxiv.org/pdf/0909.3484">pdf</a>, <a href="https://arxiv.org/ps/0909.3484">ps</a>, <a href="https://arxiv.org/format/0909.3484">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/200912560">10.1051/0004-6361/200912560 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> AGILE detection of a rapid gamma-ray flare from the blazar PKS 1510-089 during the GASP-WEBT monitoring </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=D%27Ammando%2C+F">F. D'Ammando</a>, <a href="/search/astro-ph?searchtype=author&query=Pucella%2C+G">G. Pucella</a>, <a href="/search/astro-ph?searchtype=author&query=Raiteri%2C+C+M">C. M. Raiteri</a>, <a href="/search/astro-ph?searchtype=author&query=Villata%2C+M">M. Villata</a>, <a href="/search/astro-ph?searchtype=author&query=Vittorini%2C+V">V. Vittorini</a>, <a href="/search/astro-ph?searchtype=author&query=Vercellone%2C+S">S. Vercellone</a>, <a href="/search/astro-ph?searchtype=author&query=Donnarumma%2C+I">I. Donnarumma</a>, <a href="/search/astro-ph?searchtype=author&query=Longo%2C+F">F. Longo</a>, <a href="/search/astro-ph?searchtype=author&query=Tavani%2C+M">M. Tavani</a>, <a href="/search/astro-ph?searchtype=author&query=Argan%2C+A">A. Argan</a>, <a href="/search/astro-ph?searchtype=author&query=Barbiellini%2C+G">G. Barbiellini</a>, <a href="/search/astro-ph?searchtype=author&query=Boffelli%2C+F">F. Boffelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bulgarelli%2C+A">A. Bulgarelli</a>, <a href="/search/astro-ph?searchtype=author&query=Caraveo%2C+P">P. Caraveo</a>, <a href="/search/astro-ph?searchtype=author&query=Cattaneo%2C+P+W">P. W. Cattaneo</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+A+W">A. W. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cocco%2C+V">V. Cocco</a>, <a href="/search/astro-ph?searchtype=author&query=Costa%2C+E">E. Costa</a>, <a href="/search/astro-ph?searchtype=author&query=Del+Monte%2C+E">E. Del Monte</a>, <a href="/search/astro-ph?searchtype=author&query=De+Paris%2C+G">G. De Paris</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Cocco%2C+G">G. Di Cocco</a>, <a href="/search/astro-ph?searchtype=author&query=Evangelista%2C+Y">Y. Evangelista</a>, <a href="/search/astro-ph?searchtype=author&query=Feroci%2C+M">M. Feroci</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrari%2C+A">A. Ferrari</a>, <a href="/search/astro-ph?searchtype=author&query=Fiorini%2C+M">M. Fiorini</a> , et al. (81 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0909.3484v1-abstract-short" style="display: inline;"> We report the detection by the AGILE satellite of a rapid gamma-ray flare from the powerful gamma-ray quasar PKS 1510-089, during a pointing centered on the Galactic Center region from 1 March to 30 March 2008. This source has been continuosly monitored in the radio-to-optical bands by the GLAST-AGILE Support Program (GASP) of the Whole Earth Blazar Telescope (WEBT). Moreover, the gamma-ray flar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0909.3484v1-abstract-full').style.display = 'inline'; document.getElementById('0909.3484v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0909.3484v1-abstract-full" style="display: none;"> We report the detection by the AGILE satellite of a rapid gamma-ray flare from the powerful gamma-ray quasar PKS 1510-089, during a pointing centered on the Galactic Center region from 1 March to 30 March 2008. This source has been continuosly monitored in the radio-to-optical bands by the GLAST-AGILE Support Program (GASP) of the Whole Earth Blazar Telescope (WEBT). Moreover, the gamma-ray flaring episode triggered three ToO observations by the Swift satellite in three consecutive days, starting from 20 March 2008. In the period 1-16 March 2008, AGILE detected gamma-ray emission from PKS 1510-089 at a significance level of 6.2-sigma with an average flux over the entire period of (84 +/- 17) x 10^{-8} photons cm^{-2} s^{-1} for photon energies above 100 MeV. After a predefined satellite re-pointing, between 17 and 21 March 2008, AGILE detected the source at a significance level of 7.3-sigma, with an average flux (E > 100 MeV) of (134 +/- 29) x 10^{-8} photons cm^{-2} s^{-1} and a peak level of (281 +/- 68) x 10^{-8} photons cm^{-2} s^{-1} with daily integration. During the observing period January-April 2008, the source also showed an intense and variable optical activity, with several flaring episodes and a significant increase of the flux was observed at millimetric frequencies. Moreover, in the X-ray band the Swift/XRT observations seem to show an harder-when-brighter behaviour of the source spectrum. The spectral energy distribution of mid-March 2008 is modelled with a homogeneous one-zone synchrotron self Compton emission plus contributions from inverse Compton scattering of external photons from both the accretion disc and the broad line region. Indeed, some features in the optical-UV spectrum seem to indicate the presence of Seyfert-like components, such as the little blue bump and the big blue bump. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0909.3484v1-abstract-full').style.display = 'none'; document.getElementById('0909.3484v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 September, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 4 figures and 2 tables, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astron.Astrophys.508:181-189,2009 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0812.1774">arXiv:0812.1774</a> <span> [<a href="https://arxiv.org/pdf/0812.1774">pdf</a>, <a href="https://arxiv.org/ps/0812.1774">ps</a>, <a href="https://arxiv.org/format/0812.1774">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.5303/JKAS.2008.41.6.147">10.5303/JKAS.2008.41.6.147 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> UBVI CCD Photometry of the Old Open Cluster NGC 1193 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kyeong%2C+J">Jaemann Kyeong</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S+C">Sang Chul Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Hiriart%2C+D">David Hiriart</a>, <a href="/search/astro-ph?searchtype=author&query=Sung%2C+E">Eon-Chang Sung</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0812.1774v1-abstract-short" style="display: inline;"> We present UBVI photometry of the old open cluster NGC 1193. Color-magnitude diagrams (CMDs) of this cluster show a well defined main sequence and a sparse red giant branch. For the inner region of r<50 arcsec, three blue straggler candidates are newly found in addition to the objects Kaluzny (1988) already found. The color-color diagrams show that the reddening value toward NGC 1193 is E(B-V) =… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0812.1774v1-abstract-full').style.display = 'inline'; document.getElementById('0812.1774v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0812.1774v1-abstract-full" style="display: none;"> We present UBVI photometry of the old open cluster NGC 1193. Color-magnitude diagrams (CMDs) of this cluster show a well defined main sequence and a sparse red giant branch. For the inner region of r<50 arcsec, three blue straggler candidates are newly found in addition to the objects Kaluzny (1988) already found. The color-color diagrams show that the reddening value toward NGC 1193 is E(B-V) =0.19 +/- 0.04. From the ultraviolet excess measurement, we derived the metallicity to be [Fe/H]=-0.45 +/- 0.12. A distance modulus of (m-M)_0 =13.3 +/- 0.15 is obtained from zero age main sequence fitting with the empirically calibrated Hyades isochrone of Pinsonneault et al. (2004). CMD comparison with the Padova isochrones by Bertelli et al. (1994) gives an age of log t =9.7 +/- 0.1. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0812.1774v1-abstract-full').style.display = 'none'; document.getElementById('0812.1774v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 December, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2008. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">JKAS (J. of the Korean Astron. Soc.) in press (Dec 2008 issue)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0408395">arXiv:astro-ph/0408395</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0408395">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0408395">ps</a>, <a href="https://arxiv.org/format/astro-ph/0408395">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/425528">10.1086/425528 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Molecular Hydrogen Kinematics in Cepheus A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hiriart%2C+D">David Hiriart</a>, <a href="/search/astro-ph?searchtype=author&query=Salas%2C+L">Luis Salas</a>, <a href="/search/astro-ph?searchtype=author&query=Cruz-Gonzalez%2C+I">Irene Cruz-Gonzalez</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0408395v1-abstract-short" style="display: inline;"> We present the radial velocity structure of the molecular hydrogen outflows associated to the star forming region Cepheus A. This structure is derived from doppler shift of the H_2 v=1-0 S(1) emission line obtained by Fabry-Perot spectroscopy. The East and West regions of emission, called Cep A(E) and Cep A(W), show radial velocities in the range -20 to 0 km/s with respect to the molecular cloud… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0408395v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0408395v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0408395v1-abstract-full" style="display: none;"> We present the radial velocity structure of the molecular hydrogen outflows associated to the star forming region Cepheus A. This structure is derived from doppler shift of the H_2 v=1-0 S(1) emission line obtained by Fabry-Perot spectroscopy. The East and West regions of emission, called Cep A(E) and Cep A(W), show radial velocities in the range -20 to 0 km/s with respect to the molecular cloud. Cep A(W) shows an increasing velocity with position offset from the core indicating the existence of a possible accelarating machanism. Cep A(E) has an almost constant mean radial velocity of -18 km/s along the region although with a large dispersion in velocity, indicating the possibility of a turbulent outflow. A detailed analysis of the Cep A(E) region shows evidence for the presence of a Mach disk on that outflow. Also, we argue that the presence of a velocity gradient in Cep A(W) is indicative of a C-shock in this region. Following Riera et al. (2003), we analyzed the data using wavelet analysis to study the line width and the central radial velocity distributions. We found that both outflows have complex spatial and velocity structures characteristic of a turbulent flow. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0408395v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0408395v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 August, 2004; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2004. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 15 figures</span> </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div 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