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</div> <div class="control"> <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/2402.16498">arXiv:2402.16498</a> <span> [<a href="https://arxiv.org/pdf/2402.16498">pdf</a>, <a href="https://arxiv.org/format/2402.16498">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"> Results of the follow-up of ANTARES neutrino alerts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+S">S. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+S">S. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</a>, <a href="/search/astro-ph?searchtype=author&query=Bendahman%2C+M">M. Bendahman</a>, <a href="/search/astro-ph?searchtype=author&query=Benfenati%2C+F">F. Benfenati</a>, <a href="/search/astro-ph?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/astro-ph?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/astro-ph?searchtype=author&query=Bissinger%2C+M">M. Bissinger</a>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%A2nzas%2C+H">H. Br芒nzas</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/astro-ph?searchtype=author&query=Caiffi%2C+B">B. Caiffi</a>, <a href="/search/astro-ph?searchtype=author&query=Calvo%2C+D">D. Calvo</a> , et al. (166 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="2402.16498v1-abstract-short" style="display: inline;"> High-energy neutrinos could be produced in the interaction of charged cosmic rays with matter or radiation surrounding astrophysical sources. To look for transient sources associated with neutrino emission, a follow-up program of neutrino alerts has been operating within the ANTARES Collaboration since 2009. This program, named TAToO, has triggered robotic optical telescopes (MASTER, TAROT, ROTSE… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.16498v1-abstract-full').style.display = 'inline'; document.getElementById('2402.16498v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.16498v1-abstract-full" style="display: none;"> High-energy neutrinos could be produced in the interaction of charged cosmic rays with matter or radiation surrounding astrophysical sources. To look for transient sources associated with neutrino emission, a follow-up program of neutrino alerts has been operating within the ANTARES Collaboration since 2009. This program, named TAToO, has triggered robotic optical telescopes (MASTER, TAROT, ROTSE and the SVOM ground based telescopes) immediately after the detection of any relevant neutrino candidate and scheduled several observations in the weeks following the detection. A subset of ANTARES events with highest probabilities of being of cosmic origin has also been followed by the Swift and the INTEGRAL satellites, the Murchison Widefield Array radio telescope and the H.E.S.S. high-energy gamma-ray telescope. The results of twelve years of observations are reported. No optical counterpart has been significantly associated with an ANTARES candidate neutrino signal during image analysis. Constraints on transient neutrino emission have been set. In September 2015, ANTARES issued a neutrino alert and during the follow-up, a potential transient counterpart was identified by Swift and MASTER. A multi-wavelength follow-up campaign has allowed to identify the nature of this source and has proven its fortuitous association with the neutrino. The return of experience is particularly important for the design of the alert system of KM3NeT, the next generation neutrino telescope in the Mediterranean Sea. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.16498v1-abstract-full').style.display = 'none'; document.getElementById('2402.16498v1-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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, 14 figures, submitted to JCAP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.15947">arXiv:2310.15947</a> <span> [<a href="https://arxiv.org/pdf/2310.15947">pdf</a>, <a href="https://arxiv.org/format/2310.15947">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/stad3229">10.1093/mnras/stad3229 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A two-component jet model for the optical plateau in the afterglow of GRB 191221B </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+Y">Yi-Ming Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y">Yun Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+H">Hao Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V">Vladimir Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+D+A+H">David A. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P">Pavel Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+Z">Zhi-Ping Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Wei%2C+D">Da-Ming Wei</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="2310.15947v1-abstract-short" style="display: inline;"> The long gamma-ray burst GRB 191221B has abundant observations in X-ray, optical and radio bands. In the literature, the observed optical light curve of GRB 191221B displays a plateau around 0.1-day, which is rather peculiar in gamma-ray bursts. Here we performed detailed analysis of the observational data from Swift/UVOT, VLT and LCO, obtained the light curve of the multi-band afterglow of GRB 19… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.15947v1-abstract-full').style.display = 'inline'; document.getElementById('2310.15947v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.15947v1-abstract-full" style="display: none;"> The long gamma-ray burst GRB 191221B has abundant observations in X-ray, optical and radio bands. In the literature, the observed optical light curve of GRB 191221B displays a plateau around 0.1-day, which is rather peculiar in gamma-ray bursts. Here we performed detailed analysis of the observational data from Swift/UVOT, VLT and LCO, obtained the light curve of the multi-band afterglow of GRB 191221B. By examining optical, ultraviolet, X-ray, and radio data for this event, we demonstrate that an on-axis two-component jet model can explain the observations. Our analysis suggests that the narrow component has an initial Lorentz factor of 400 and a jet opening half-angle of $1.4^{\circ}$, while the wide component has an initial Lorentz factor of 25 and a jet opening half-angle of $2.8^{\circ}$. The narrow jet dominates the early decay, whereas the wider jet causes the optical plateau and dominates late decay. According to this model, the reason for the absence of the X-ray plateau is due to the steeper spectral index of the wide component, resulting in a less significant flux contribution from the wide jet in the X-ray bands than in the optical bands. Moreover, we have explained the inconsistency in the decay indices of the UVOT and Rc-band data around 2000 seconds using reverse shock emission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.15947v1-abstract-full').style.display = 'none'; document.getElementById('2310.15947v1-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> 24 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">10 pages, 7 figures, Accepted by the 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/2302.05924">arXiv:2302.05924</a> <span> [<a href="https://arxiv.org/pdf/2302.05924">pdf</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/stac1906">10.1093/mnras/stac1906 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Orphan optical flare as SOSS emission afterglow, localization in time </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V">V. Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Kornilov%2C+V">V. Kornilov</a>, <a href="/search/astro-ph?searchtype=author&query=Zhirkov%2C+K">K. Zhirkov</a>, <a href="/search/astro-ph?searchtype=author&query=Tyurina%2C+N">N. Tyurina</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E">E. Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Vlasenko%2C+D">D. Vlasenko</a>, <a href="/search/astro-ph?searchtype=author&query=Simakov%2C+S">S. Simakov</a>, <a href="/search/astro-ph?searchtype=author&query=Topolev%2C+V">V. Topolev</a>, <a href="/search/astro-ph?searchtype=author&query=Francile%2C+C">C. Francile</a>, <a href="/search/astro-ph?searchtype=author&query=Podesta%2C+R">R. Podesta</a>, <a href="/search/astro-ph?searchtype=author&query=Podesta%2C+F">F. Podesta</a>, <a href="/search/astro-ph?searchtype=author&query=Svinkin%2C+D">D. Svinkin</a>, <a href="/search/astro-ph?searchtype=author&query=Budnev%2C+N">N. Budnev</a>, <a href="/search/astro-ph?searchtype=author&query=Gress%2C+O">O. Gress</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P">P. Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Kuznetsov%2C+A">A. Kuznetsov</a>, <a href="/search/astro-ph?searchtype=author&query=Chasovnikov%2C+A">A. Chasovnikov</a>, <a href="/search/astro-ph?searchtype=author&query=Serra-Ricart%2C+M">M. Serra-Ricart</a>, <a href="/search/astro-ph?searchtype=author&query=Gabovich%2C+A">A. Gabovich</a>, <a href="/search/astro-ph?searchtype=author&query=Minkina%2C+E">E. Minkina</a>, <a href="/search/astro-ph?searchtype=author&query=Antipov%2C+G">G. Antipov</a>, <a href="/search/astro-ph?searchtype=author&query=Svertilov%2C+S">S. Svertilov</a>, <a href="/search/astro-ph?searchtype=author&query=Tlatov%2C+A">A. Tlatov</a>, <a href="/search/astro-ph?searchtype=author&query=Senik%2C+V">V. Senik</a>, <a href="/search/astro-ph?searchtype=author&query=Tselik%2C+Y">Yu. Tselik</a> , et al. (2 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="2302.05924v1-abstract-short" style="display: inline;"> We report on MASTER optical observations of an afterglow-like optical and X-ray transient AT2021lfa/ZTF21aayokph. We detected the initial steady brightening of the transient at 7蟽 confidence level. This allowed us to use smooth optical self-similar emission of GRBs model to constrain the explosion time to better than 14 min as well as to estimate its initial Lorentz factor 螕0 = 20 +/- 10. Taking i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.05924v1-abstract-full').style.display = 'inline'; document.getElementById('2302.05924v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.05924v1-abstract-full" style="display: none;"> We report on MASTER optical observations of an afterglow-like optical and X-ray transient AT2021lfa/ZTF21aayokph. We detected the initial steady brightening of the transient at 7蟽 confidence level. This allowed us to use smooth optical self-similar emission of GRBs model to constrain the explosion time to better than 14 min as well as to estimate its initial Lorentz factor 螕0 = 20 +/- 10. Taking into consideration the low 螕0 and non-detection in gamma-rays, we classify this transient as the first failed GRB afterglow. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.05924v1-abstract-full').style.display = 'none'; document.getElementById('2302.05924v1-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 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">8 pages, 5 figures, 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> MNRAS 514, 4, 4980-4987 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.05920">arXiv:2302.05920</a> <span> [<a href="https://arxiv.org/pdf/2302.05920">pdf</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/ac9307">10.3847/1538-4357/ac9307 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Three-stage Collapse of the Long Gamma-Ray Burst from GRB 160625B Prompt Multiwavelength Observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V+M">V. M. Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Sadovnichy%2C+V+A">V. A. Sadovnichy</a>, <a href="/search/astro-ph?searchtype=author&query=Panasyuk%2C+M+I">M. I. Panasyuk</a>, <a href="/search/astro-ph?searchtype=author&query=Yashin%2C+I+V">I. V. Yashin</a>, <a href="/search/astro-ph?searchtype=author&query=Svertilov%2C+S+I">S. I. Svertilov</a>, <a href="/search/astro-ph?searchtype=author&query=Simakov%2C+S+G">S. G. Simakov</a>, <a href="/search/astro-ph?searchtype=author&query=Svinkin%2C+D">D. Svinkin</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E">E. Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Lipunova%2C+G+V">G. V. Lipunova</a>, <a href="/search/astro-ph?searchtype=author&query=Kornilov%2C+V+G">V. G. Kornilov</a>, <a href="/search/astro-ph?searchtype=author&query=Frederiks%2C+D">D. Frederiks</a>, <a href="/search/astro-ph?searchtype=author&query=Topolev%2C+V">V. Topolev</a>, <a href="/search/astro-ph?searchtype=author&query=Rebolo%2C+R">R. Rebolo</a>, <a href="/search/astro-ph?searchtype=author&query=Serra%2C+M">M. Serra</a>, <a href="/search/astro-ph?searchtype=author&query=Tiurina%2C+N">N. Tiurina</a>, <a href="/search/astro-ph?searchtype=author&query=Minkina%2C+E">E. Minkina</a>, <a href="/search/astro-ph?searchtype=author&query=Bogomolov%2C+V+V">V. V. Bogomolov</a>, <a href="/search/astro-ph?searchtype=author&query=Bogomolov%2C+A+V">A. V. Bogomolov</a>, <a href="/search/astro-ph?searchtype=author&query=Iyudin%2C+A+F">A. F. Iyudin</a>, <a href="/search/astro-ph?searchtype=author&query=Chasovnikov%2C+A">A. Chasovnikov</a>, <a href="/search/astro-ph?searchtype=author&query=Gabovich%2C+A">A. Gabovich</a>, <a href="/search/astro-ph?searchtype=author&query=Tsvetkova%2C+A">A. Tsvetkova</a>, <a href="/search/astro-ph?searchtype=author&query=Budnev%2C+N+M">N. M. Budnev</a>, <a href="/search/astro-ph?searchtype=author&query=Gress%2C+O+A">O. A. Gress</a>, <a href="/search/astro-ph?searchtype=author&query=Antipov%2C+G">G. Antipov</a> , et al. (15 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="2302.05920v1-abstract-short" style="display: inline;"> This article presents the early results of synchronous multiwavelength observations of one of the brightest gamma-ray bursts (GRBs) GRB 160625B with the detailed continuous fast optical photometry of its optical counterpart obtained by MASTER and with hard X-ray and gamma-ray emission, obtained by the Lomonosov and Konus-Wind spacecraft. The detailed photometry led us to detect the quasi-periodica… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.05920v1-abstract-full').style.display = 'inline'; document.getElementById('2302.05920v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.05920v1-abstract-full" style="display: none;"> This article presents the early results of synchronous multiwavelength observations of one of the brightest gamma-ray bursts (GRBs) GRB 160625B with the detailed continuous fast optical photometry of its optical counterpart obtained by MASTER and with hard X-ray and gamma-ray emission, obtained by the Lomonosov and Konus-Wind spacecraft. The detailed photometry led us to detect the quasi-periodical emission components in the intrinsic optical emission. As a result of our analysis of synchronous multiwavelength observations, we propose a three-stage collapse scenario for this long and bright GRB. We suggest that quasiperiodic fluctuations may be associated with forced precession of a self-gravitating rapidly rotating superdense body (spinar), whose evolution is determined by a powerful magnetic field. The spinar's mass allows it to collapse into a black hole at the end of evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.05920v1-abstract-full').style.display = 'none'; document.getElementById('2302.05920v1-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 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">22 pages, 12 figures, 4 tables, accepted for publication in ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 943 181 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.01167">arXiv:2201.01167</a> <span> [<a href="https://arxiv.org/pdf/2201.01167">pdf</a>, <a href="https://arxiv.org/format/2201.01167">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/stac015">10.1093/mnras/stac015 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Probing into emission mechanisms of GRB 190530A using time-resolved spectra and polarization studies: Synchrotron Origin? </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=Gupta%2C+S">S. Gupta</a>, <a href="/search/astro-ph?searchtype=author&query=Chattopadhyay%2C+T">T. Chattopadhyay</a>, <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V">V. Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Castro-Tirado%2C+A+J">A. J. Castro-Tirado</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharya%2C+D">D. Bhattacharya</a>, <a href="/search/astro-ph?searchtype=author&query=Pandey%2C+S+B">S. B. Pandey</a>, <a href="/search/astro-ph?searchtype=author&query=Oates%2C+S+R">S. R. Oates</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+A">Amit Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+Y+-">Y. -D. Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Valeev%2C+A+F">A. F. Valeev</a>, <a href="/search/astro-ph?searchtype=author&query=Minaev%2C+P+Y">P. Yu. Minaev</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+H">H. Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Vinko%2C+J">J. Vinko</a>, <a href="/search/astro-ph?searchtype=author&query=Dimple"> Dimple</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=Castell%C3%B3n%2C+A">A. Castell贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Gabovich%2C+A">A. Gabovich</a>, <a href="/search/astro-ph?searchtype=author&query=Moskvitin%2C+A">A. Moskvitin</a>, <a href="/search/astro-ph?searchtype=author&query=Ordasi%2C+A">A. Ordasi</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A1l%2C+A">A. P谩l</a>, <a href="/search/astro-ph?searchtype=author&query=Pozanenko%2C+A">A. Pozanenko</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+B+-">B. -B. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+B">B. Kumar</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="2201.01167v1-abstract-short" style="display: inline;"> Multi-pulsed GRB 190530A, detected by the GBM and LAT onboard \fermi, is the sixth most fluent GBM burst detected so far. This paper presents the timing, spectral, and polarimetric analysis of the prompt emission observed using \AstroSat and \fermi to provide insight into the prompt emission radiation mechanisms. The time-integrated spectrum shows conclusive proof of two breaks due to peak energy… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.01167v1-abstract-full').style.display = 'inline'; document.getElementById('2201.01167v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.01167v1-abstract-full" style="display: none;"> Multi-pulsed GRB 190530A, detected by the GBM and LAT onboard \fermi, is the sixth most fluent GBM burst detected so far. This paper presents the timing, spectral, and polarimetric analysis of the prompt emission observed using \AstroSat and \fermi to provide insight into the prompt emission radiation mechanisms. The time-integrated spectrum shows conclusive proof of two breaks due to peak energy and a second lower energy break. Time-integrated (55.43 $\pm$ 21.30 \%) as well as time-resolved polarization measurements, made by the Cadmium Zinc Telluride Imager (CZTI) onboard \AstroSat, show a hint of high degree of polarization. The presence of a hint of high degree of polarization and the values of low energy spectral index ($伪_{\rm pt}$) do not run over the synchrotron limit for the first two pulses, supporting the synchrotron origin in an ordered magnetic field. However, during the third pulse, $伪_{\rm pt}$ exceeds the synchrotron line of death in few bins, and a thermal signature along with the synchrotron component in the time-resolved spectra is observed. Furthermore, we also report the earliest optical observations constraining afterglow polarization using the MASTER (P $<$ 1.3 \%) and the redshift measurement ($z$= 0.9386) obtained with the 10.4m GTC telescopes. The broadband afterglow can be described with a forward shock model for an ISM-like medium with a wide jet opening angle. We determine a circumburst density of $n_{0} \sim$ 7.41, kinetic energy $E_{\rm K} \sim$ 7.24 $\times 10^{54}$ erg, and radiated $纬$-ray energy $E_{\rm 纬, iso} \sim$ 6.05 $\times 10^{54}$ erg, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.01167v1-abstract-full').style.display = 'none'; document.getElementById('2201.01167v1-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 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">28 pages, 17 figures, 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/2111.14861">arXiv:2111.14861</a> <span> [<a href="https://arxiv.org/pdf/2111.14861">pdf</a>, <a href="https://arxiv.org/format/2111.14861">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/stac454">10.1093/mnras/stac454 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The early afterglow of GRB 190829A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dichiara%2C+S">S. Dichiara</a>, <a href="/search/astro-ph?searchtype=author&query=Troja%2C+E">E. Troja</a>, <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V">V. Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+R">R. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Oates%2C+S+R">S. R. Oates</a>, <a href="/search/astro-ph?searchtype=author&query=Butler%2C+N+R">N. R. Butler</a>, <a href="/search/astro-ph?searchtype=author&query=Liuzzo%2C+E">E. Liuzzo</a>, <a href="/search/astro-ph?searchtype=author&query=Ryan%2C+G">G. Ryan</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Connor%2C+B">B. O'Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Cenko%2C+S+B">S. B. Cenko</a>, <a href="/search/astro-ph?searchtype=author&query=Cosentino%2C+R+G">R. G. Cosentino</a>, <a href="/search/astro-ph?searchtype=author&query=Lien%2C+A+Y">A. Y. Lien</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E">E. Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Tyurina%2C+N">N. Tyurina</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P">P. Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Vlasenko%2C+D">D. Vlasenko</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbunov%2C+I">I. Gorbunov</a>, <a href="/search/astro-ph?searchtype=author&query=Podesta%2C+R">R. Podesta</a>, <a href="/search/astro-ph?searchtype=author&query=Podesta%2C+F">F. Podesta</a>, <a href="/search/astro-ph?searchtype=author&query=Rebolo%2C+R">R. Rebolo</a>, <a href="/search/astro-ph?searchtype=author&query=Serra%2C+M">M. Serra</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+D+A+H">D. A. H. Buckley</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="2111.14861v2-abstract-short" style="display: inline;"> GRB 190829A at z=0.0785 is the fourth closest long GRB ever detected by the Neil Gehrels Swift observatory, and the third confirmed case with a very high energy component. We present our multi-wavelength analysis of this rare event, focusing on its early stages of evolution, and including data from Swift, the MASTER global network of optical telescopes, ALMA, and ATCA. We report sensitive limits o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.14861v2-abstract-full').style.display = 'inline'; document.getElementById('2111.14861v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.14861v2-abstract-full" style="display: none;"> GRB 190829A at z=0.0785 is the fourth closest long GRB ever detected by the Neil Gehrels Swift observatory, and the third confirmed case with a very high energy component. We present our multi-wavelength analysis of this rare event, focusing on its early stages of evolution, and including data from Swift, the MASTER global network of optical telescopes, ALMA, and ATCA. We report sensitive limits on the linear polarization of the optical emission, disfavouring models of off-axis jets to explain the delayed afterglow peak. The study of the multi-wavelength light curves and broadband spectra supports a model with at least two emission components: a bright reverse shock emission, visible at early times in the optical and X-rays and, later, in the radio band; and a forward shock component dominating at later times and lower radio frequencies. A combined study of the prompt and afterglow properties shows many similarities with cosmological long GRBs, suggesting that GRB 190829A is an example of classical GRBs in the nearby universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.14861v2-abstract-full').style.display = 'none'; document.getElementById('2111.14861v2-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 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </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, 8 figures, 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/2006.04918">arXiv:2006.04918</a> <span> [<a href="https://arxiv.org/pdf/2006.04918">pdf</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="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Applied Physics">physics.app-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/10.3847/2041-8213/ab96ba">10.3847/2041-8213/ab96ba <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Optical Observations Reveal Strong Evidence for High Energy Neutrino Progenitor </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V+M">V. M. Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Kornilov%2C+V+G">V. G. Kornilov</a>, <a href="/search/astro-ph?searchtype=author&query=Zhirkov%2C+K+K">K. K. Zhirkov</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E+S">E. S. Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Budnev%2C+N+M">N. M. Budnev</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+D+A+H">D. A. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Rebolo%2C+R">R. Rebolo</a>, <a href="/search/astro-ph?searchtype=author&query=Serra-Ricart%2C+M">M. Serra-Ricart</a>, <a href="/search/astro-ph?searchtype=author&query=Podesta%2C+R">R. Podesta</a>, <a href="/search/astro-ph?searchtype=author&query=Tyurina%2C+N">N. Tyurina</a>, <a href="/search/astro-ph?searchtype=author&query=Gress%2C+O">O. Gress</a>, <a href="/search/astro-ph?searchtype=author&query=Sergienko%2C+Y">Yu. Sergienko</a>, <a href="/search/astro-ph?searchtype=author&query=Yurkov%2C+V">V. Yurkov</a>, <a href="/search/astro-ph?searchtype=author&query=Gabovich%2C+A">A. Gabovich</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P">P. Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbunov%2C+I">I. Gorbunov</a>, <a href="/search/astro-ph?searchtype=author&query=Vlasenko%2C+D">D. Vlasenko</a>, <a href="/search/astro-ph?searchtype=author&query=Balakin%2C+F">F. Balakin</a>, <a href="/search/astro-ph?searchtype=author&query=Topolev%2C+V">V. Topolev</a>, <a href="/search/astro-ph?searchtype=author&query=Pozdnyakov%2C+A">A. Pozdnyakov</a>, <a href="/search/astro-ph?searchtype=author&query=Kuznetsov%2C+A">A. Kuznetsov</a>, <a href="/search/astro-ph?searchtype=author&query=Vladimirov%2C+V">V. Vladimirov</a>, <a href="/search/astro-ph?searchtype=author&query=Chasovnikov%2C+A">A. Chasovnikov</a>, <a href="/search/astro-ph?searchtype=author&query=Kuvshinov%2C+D">D. Kuvshinov</a>, <a href="/search/astro-ph?searchtype=author&query=Grinshpun%2C+V">V. Grinshpun</a> , et al. (10 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="2006.04918v1-abstract-short" style="display: inline;"> We present the earliest astronomical observation of a high energy neutrino error box in which its variability was discovered after high-energy neutrinos detection. The one robotic telescope of the MASTER global international network (Lipunov et al. 2010) automatically imaged the error box of the very high-energy neutrino event IceCube-170922A. Observations were carried out in minute after the IceC… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.04918v1-abstract-full').style.display = 'inline'; document.getElementById('2006.04918v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.04918v1-abstract-full" style="display: none;"> We present the earliest astronomical observation of a high energy neutrino error box in which its variability was discovered after high-energy neutrinos detection. The one robotic telescope of the MASTER global international network (Lipunov et al. 2010) automatically imaged the error box of the very high-energy neutrino event IceCube-170922A. Observations were carried out in minute after the IceCube-170922A neutrino event was detected by the IceCube observatory at the South Pole. MASTER found the blazar TXS 0506+056 to be in the off-state after one minute and then switched to the on-state no later than two hours after the event. The effect is observed at a 50-sigma significance level. Also we present own unique 16-years light curve of blazar TXS 0506+056 (518 data set). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.04918v1-abstract-full').style.display = 'none'; document.getElementById('2006.04918v1-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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, 3 figures, 1 Table accepted to The Astrophysical Journal Letters</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal Letters, 2020 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1910.10747">arXiv:1910.10747</a> <span> [<a href="https://arxiv.org/pdf/1910.10747">pdf</a>, <a href="https://arxiv.org/ps/1910.10747">ps</a>, <a href="https://arxiv.org/format/1910.10747">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/10.1051/0004-6361/201834959">10.1051/0004-6361/201834959 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multiwavelength observations of GRB 140629A. A long burst with an achromatic jet break in the optical and X-ray afterglow </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hu%2C+Y+-">Y. -D. Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Oates%2C+S+R">S. R. Oates</a>, <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V+M">V. M. Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+B+-">B. -B. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Castro-Tirado%2C+A+J">A. J. Castro-Tirado</a>, <a href="/search/astro-ph?searchtype=author&query=Jeong%2C+S">S. Jeong</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Ram%C3%ADrez%2C+R">R. S谩nchez-Ram铆rez</a>, <a href="/search/astro-ph?searchtype=author&query=Tello%2C+J+C">J. C. Tello</a>, <a href="/search/astro-ph?searchtype=author&query=Cunniffe%2C+R">R. Cunniffe</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E">E. Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Caballero-Garc%C3%ADa%2C+M+D">M. D. Caballero-Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Pandey%2C+S+B">S. B. Pandey</a>, <a href="/search/astro-ph?searchtype=author&query=Kornilov%2C+V+G">V. G. Kornilov</a>, <a href="/search/astro-ph?searchtype=author&query=Tyurina%2C+N+V">N. V. Tyurina</a>, <a href="/search/astro-ph?searchtype=author&query=Kuznetsov%2C+A+S">A. S. Kuznetsov</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P+V">P. V. Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Gress%2C+O+A">O. A. Gress</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbunov%2C+I">I. Gorbunov</a>, <a href="/search/astro-ph?searchtype=author&query=Vlasenko%2C+D+M">D. M. Vlasenko</a>, <a href="/search/astro-ph?searchtype=author&query=Vladimirov%2C+V+V">V. V. Vladimirov</a>, <a href="/search/astro-ph?searchtype=author&query=Budnev%2C+N+M">N. M. Budnev</a>, <a href="/search/astro-ph?searchtype=author&query=Balakin%2C+F">F. Balakin</a>, <a href="/search/astro-ph?searchtype=author&query=Ershova%2C+O">O. Ershova</a>, <a href="/search/astro-ph?searchtype=author&query=Krushinski%2C+V+V">V. V. Krushinski</a>, <a href="/search/astro-ph?searchtype=author&query=Gabovich%2C+A+V">A. V. Gabovich</a> , et al. (9 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="1910.10747v1-abstract-short" style="display: inline;"> We investigate the long GRB140629A through multiwavelength observations, which cover optical, infrared and X-rays between 40s and 3yr after the burst, to derive the properties of the dominant jet and its host galaxy. Polarisation observations by the MASTER telescope indicate that this burst is weakly polarised. The optical spectrum contains absorption features, from which we confirm the redshift o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.10747v1-abstract-full').style.display = 'inline'; document.getElementById('1910.10747v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.10747v1-abstract-full" style="display: none;"> We investigate the long GRB140629A through multiwavelength observations, which cover optical, infrared and X-rays between 40s and 3yr after the burst, to derive the properties of the dominant jet and its host galaxy. Polarisation observations by the MASTER telescope indicate that this burst is weakly polarised. The optical spectrum contains absorption features, from which we confirm the redshift of the GRB as originating at z=2.276. We performed spectral fitting of the X-rays to optical afterglow data and find there is no strong spectral evolution. We determine the hydrogen column density to be 7.2x10^21cm^-2 along the line of sight. The afterglow in this burst can be explained by a blast wave jet with a long-lasting central engine expanding into a uniform medium in the slow cooling regime. At the end of energy injection, a normal decay phase is observed in both the optical and X-ray bands. An achromatic jet break is also found in the afterglow light curves 0.4d after trigger. We fit the multiwavelength data simultaneously with a model based on a numerical simulation and find that the observations can be explained by a narrow uniform jet in a dense environment with an opening angle of 6.7deg viewed 3.8deg off-axis, which released a total energy of 1.4x10^54erg. Using the redshift and opening angle, we find GRB 140629A follows both the Ghirlanda and Amati relations. From the peak time of the light curve, identified as the onset of the forward shock (181s after trigger), the initial Lorentz factor is constrained in the range 82-118. Fitting the host galaxy photometry, we find the host to be a low mass, star-forming galaxy with a star formation rate of logSFR=1.1^+0.9_-0.4Myr^-1. We obtain a value of the neutral hydrogen density by fitting the optical spectrum, logN(HI)=21.0+-0.3, classifying this host as a damped Lyman-alpha. High ionisation lines are also detected in the spectrum. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.10747v1-abstract-full').style.display = 'none'; document.getElementById('1910.10747v1-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 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">18 pages, 13 figures, 8 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> A&A 632, A100 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1903.06243">arXiv:1903.06243</a> <span> [<a href="https://arxiv.org/pdf/1903.06243">pdf</a>, <a href="https://arxiv.org/format/1903.06243">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="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/stz752">10.1093/mnras/stz752 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observational properties of a Type Ib Supernova MASTER OT J120451.50+265946.6 in NGC 4080 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Singh%2C+M">Mridweeka Singh</a>, <a href="/search/astro-ph?searchtype=author&query=Misra%2C+K">Kuntal Misra</a>, <a href="/search/astro-ph?searchtype=author&query=Sahu%2C+D+K">D. K. Sahu</a>, <a href="/search/astro-ph?searchtype=author&query=Dastidar%2C+R">Raya Dastidar</a>, <a href="/search/astro-ph?searchtype=author&query=Gangopadhyay%2C+A">Anjasha Gangopadhyay</a>, <a href="/search/astro-ph?searchtype=author&query=Srivastav%2C+S">Shubham Srivastav</a>, <a href="/search/astro-ph?searchtype=author&query=Anupama%2C+G+C">G. C. Anupama</a>, <a href="/search/astro-ph?searchtype=author&query=Bose%2C+S">Subhash Bose</a>, <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V">Vladimir Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Chakradhari%2C+N+K">N. K. Chakradhari</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+B">Brajesh Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+B">Brijesh Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Pandey%2C+S+B">S. B. Pandey</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E">Evgeny Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P">Pavel Balanutsa</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="1903.06243v1-abstract-short" style="display: inline;"> MASTER OT J120451.50+265946.6 (M12045), discovered by the MASTER Global Robotic Net, is a Type Ib supernova (SN) that exploded in NGC 4080. We present the {\it BVRI} photometric and spectroscopic observations upto $\sim$250 days since $B_{max}$. At the time of discovery the SN was a few weeks past maximum light and our observations capture the linearly declining light curve phase. M12045 declines… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.06243v1-abstract-full').style.display = 'inline'; document.getElementById('1903.06243v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.06243v1-abstract-full" style="display: none;"> MASTER OT J120451.50+265946.6 (M12045), discovered by the MASTER Global Robotic Net, is a Type Ib supernova (SN) that exploded in NGC 4080. We present the {\it BVRI} photometric and spectroscopic observations upto $\sim$250 days since $B_{max}$. At the time of discovery the SN was a few weeks past maximum light and our observations capture the linearly declining light curve phase. M12045 declines faster as compared to SNe 1999dn and 2009jf at comparable epochs. Rigorous spectroscopic monitoring reveals that M12045 is a normal Type Ib SN. The analysis of the nebular phase spectra indicates that $\sim$ 0.90 M$_\odot$ of O is ejected in the explosion. The line ratio of [\ion{O}{I}] and [\ion{Ca}{II}] in the nebular phase supports a massive WR progenitor with main sequence mass of $\sim$ 20 M$_\odot$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.06243v1-abstract-full').style.display = 'none'; document.getElementById('1903.06243v1-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 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">16 pages, 6 tables, 12 figures, 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/1901.02669">arXiv:1901.02669</a> <span> [<a href="https://arxiv.org/pdf/1901.02669">pdf</a>, <a href="https://arxiv.org/format/1901.02669">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/stz056">10.1093/mnras/stz056 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery, observations and modelling of a new eclipsing polar: MASTER OT J061451.70-272535.5 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Breytenbach%2C+H">H. Breytenbach</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+D+A+H">D. A. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Hakala%2C+P">P. Hakala</a>, <a href="/search/astro-ph?searchtype=author&query=Thorstensen%2C+J+R">J. R. Thorstensen</a>, <a href="/search/astro-ph?searchtype=author&query=Kniazev%2C+A+Y">A. Y. Kniazev</a>, <a href="/search/astro-ph?searchtype=author&query=Motsoaledi%2C+M">M. Motsoaledi</a>, <a href="/search/astro-ph?searchtype=author&query=Woudt%2C+P+A">P. A. Woudt</a>, <a href="/search/astro-ph?searchtype=author&query=Potter%2C+S+B">S. B. Potter</a>, <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V">V. Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E">E. Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P">P. Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Tyurina%2C+N">N. Tyurina</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="1901.02669v1-abstract-short" style="display: inline;"> We report the discovery of a new eclipsing polar, MASTER OT J061451.70-272535.5, detected as an optical transient by MASTER auto-detection software at the recently commissioned MASTER-SAAO telescope. Time resolved (10-20 s) photometry with the SAAO 1.9-m, and 1.0-m telescopes, utilizing the SHOC EM-CCD cameras, revealed that the source eclipses, with a period of 2.08 hours (7482.9$\pm$3.5$\,$s). T… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.02669v1-abstract-full').style.display = 'inline'; document.getElementById('1901.02669v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1901.02669v1-abstract-full" style="display: none;"> We report the discovery of a new eclipsing polar, MASTER OT J061451.70-272535.5, detected as an optical transient by MASTER auto-detection software at the recently commissioned MASTER-SAAO telescope. Time resolved (10-20 s) photometry with the SAAO 1.9-m, and 1.0-m telescopes, utilizing the SHOC EM-CCD cameras, revealed that the source eclipses, with a period of 2.08 hours (7482.9$\pm$3.5$\,$s). The eclipse light curve has a peculiar morphology, comprising an initial dip, where the source brightness drops to ${\sim}$50% of the pre-eclipse level before gradually increasing again in brightness. A second rapid ingress follows, where the brightness drops by ${\sim}$60-80%, followed by a more gradual decrease to zero flux. We interpret the eclipse profile as the result of an initial obscuration of the accretion hot-spot on the magnetic white dwarf by the accretion stream, followed by an eclipse of both the hot-spot and the partially illuminated stream by the red dwarf donor star. This is similar to what has been observed in other eclipsing polars such as HU Aqr, but here the stream absorption is more pronounced. The object was subsequently observed with South African Large Telescope (SALT) using the Robert Stobie Spectrograph (RSS). This revealed a spectrum with all of the Balmer lines in emission, a strong HeII 4686脜 line with a peak flux greater than that of H$尾$, as well as weaker HeI lines. The spectral features, along with the structure of the light curve, suggest that MASTER OT J061451.70-272535.5 is a new magnetic cataclysmic variable, most likely of the synchronised Polar subclass. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.02669v1-abstract-full').style.display = 'none'; document.getElementById('1901.02669v1-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 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">15 pages, 11 figures, 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/1710.05835">arXiv:1710.05835</a> <span> [<a href="https://arxiv.org/pdf/1710.05835">pdf</a>, <a href="https://arxiv.org/format/1710.05835">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/10.1038/nature24471">10.1038/nature24471 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A gravitational-wave standard siren measurement of the Hubble constant </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=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=Afrough%2C+M">M. Afrough</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+B">B. Agarwal</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=Allen%2C+G">G. 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=Amato%2C+A">A. Amato</a> , et al. (1289 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="1710.05835v1-abstract-short" style="display: inline;"> The detection of GW170817 in both gravitational waves and electromagnetic waves heralds the age of gravitational-wave multi-messenger astronomy. On 17 August 2017 the Advanced LIGO and Virgo detectors observed GW170817, a strong signal from the merger of a binary neutron-star system. Less than 2 seconds after the merger, a gamma-ray burst (GRB 170817A) was detected within a region of the sky consi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.05835v1-abstract-full').style.display = 'inline'; document.getElementById('1710.05835v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1710.05835v1-abstract-full" style="display: none;"> The detection of GW170817 in both gravitational waves and electromagnetic waves heralds the age of gravitational-wave multi-messenger astronomy. On 17 August 2017 the Advanced LIGO and Virgo detectors observed GW170817, a strong signal from the merger of a binary neutron-star system. Less than 2 seconds after the merger, a gamma-ray burst (GRB 170817A) was detected within a region of the sky consistent with the LIGO-Virgo-derived location of the gravitational-wave source. This sky region was subsequently observed by optical astronomy facilities, resulting in the identification of an optical transient signal within $\sim 10$ arcsec of the galaxy NGC 4993. These multi-messenger observations allow us to use GW170817 as a standard siren, the gravitational-wave analog of an astronomical standard candle, to measure the Hubble constant. This quantity, which represents the local expansion rate of the Universe, sets the overall scale of the Universe and is of fundamental importance to cosmology. Our measurement combines the distance to the source inferred purely from the gravitational-wave signal with the recession velocity inferred from measurements of the redshift using electromagnetic data. This approach does not require any form of cosmic "distance ladder;" the gravitational wave analysis can be used to estimate the luminosity distance out to cosmological scales directly, without the use of intermediate astronomical distance measurements. We determine the Hubble constant to be $70.0^{+12.0}_{-8.0} \, \mathrm{km} \, \mathrm{s}^{-1} \, \mathrm{Mpc}^{-1}$ (maximum a posteriori and 68% credible interval). This is consistent with existing measurements, while being completely independent of them. Additional standard-siren measurements from future gravitational-wave sources will provide precision constraints of this important cosmological parameter. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.05835v1-abstract-full').style.display = 'none'; document.getElementById('1710.05835v1-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 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">26 pages, 5 figures, Nature in press. For more information see https://dcc.ligo.org/LIGO-P1700296/public</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO P1700296 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1710.05461">arXiv:1710.05461</a> <span> [<a href="https://arxiv.org/pdf/1710.05461">pdf</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/10.3847/2041-8213/aa92c0">10.3847/2041-8213/aa92c0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MASTER optical detection of the first LIGO/Virgo neutron stars merging GW170817 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V+M">V. M. Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E">E. Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Kornilov%2C+V+G">V. G. Kornilov</a>, <a href="/search/astro-ph?searchtype=author&query=Tyurina%2C+N+.">N . Tyurina</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P">P. Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Kuznetsov%2C+A">A. Kuznetsov</a>, <a href="/search/astro-ph?searchtype=author&query=Vlasenko%2C+D">D. Vlasenko</a>, <a href="/search/astro-ph?searchtype=author&query=Kuvshinov%2C+D">D. Kuvshinov</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbunov%2C+I">I. Gorbunov</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+D+A+H">D. A. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Krylov%2C+A+V">A. V. Krylov</a>, <a href="/search/astro-ph?searchtype=author&query=Podesta%2C+R">R. Podesta</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+C">C. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Podesta%2C+F">F. Podesta</a>, <a href="/search/astro-ph?searchtype=author&query=Levato%2C+H">H. Levato</a>, <a href="/search/astro-ph?searchtype=author&query=Saffe%2C+C">C. Saffe</a>, <a href="/search/astro-ph?searchtype=author&query=Mallamachi%2C+C">C. Mallamachi</a>, <a href="/search/astro-ph?searchtype=author&query=Potter%2C+S">S. Potter</a>, <a href="/search/astro-ph?searchtype=author&query=Budnev%2C+N+M">N. M. Budnev</a>, <a href="/search/astro-ph?searchtype=author&query=Gress%2C+O">O. Gress</a>, <a href="/search/astro-ph?searchtype=author&query=Ishmuhametova%2C+Y">Yu. Ishmuhametova</a>, <a href="/search/astro-ph?searchtype=author&query=Vladimirov%2C+V">V. Vladimirov</a>, <a href="/search/astro-ph?searchtype=author&query=Zimnukhov%2C+D">D. Zimnukhov</a>, <a href="/search/astro-ph?searchtype=author&query=Yurkov%2C+V">V. Yurkov</a>, <a href="/search/astro-ph?searchtype=author&query=Sergienko%2C+Y">Yu. Sergienko</a> , et al. (8 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="1710.05461v2-abstract-short" style="display: inline;"> Following the reported discovery of the gravitational-wave pulse GW170817/ G298048 by three LIGO/Virgo antennae (Abbott et al., 2017a), the MASTER Global Robotic Net telescopes obtained the first image of the NGC 4993 galaxy after the NS+NS merging. The optical transient MASTER OTJ130948.10-232253.3/SSS17a was later found, which appears to be a kilonova resulting from a merger of two neutron stars… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.05461v2-abstract-full').style.display = 'inline'; document.getElementById('1710.05461v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1710.05461v2-abstract-full" style="display: none;"> Following the reported discovery of the gravitational-wave pulse GW170817/ G298048 by three LIGO/Virgo antennae (Abbott et al., 2017a), the MASTER Global Robotic Net telescopes obtained the first image of the NGC 4993 galaxy after the NS+NS merging. The optical transient MASTER OTJ130948.10-232253.3/SSS17a was later found, which appears to be a kilonova resulting from a merger of two neutron stars. In this paper we report the independent detection and photometry of the kilonova made in white light and in B, V, and R filters. We note that luminosity of the discovered kilonova NGC 4993 is very close to another possible kilonova proposed early GRB 130603 and GRB 080503. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.05461v2-abstract-full').style.display = 'none'; document.getElementById('1710.05461v2-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 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">17 pages, 5 pages, 3 tables,accepted to ApJL, LVC release on 2017-10-16</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1704.08178">arXiv:1704.08178</a> <span> [<a href="https://arxiv.org/pdf/1704.08178">pdf</a>, <a href="https://arxiv.org/ps/1704.08178">ps</a>, <a href="https://arxiv.org/format/1704.08178">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/stx1107">10.1093/mnras/stx1107 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MASTER OT J004207.99+405501.1/M31LRN 2015 Luminous Red Nova in M31: Discovery, Light Curve, Hydrodynamics, Evolution </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V+M">V. M. Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Blinnikov%2C+S">S. Blinnikov</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E">E. Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Tutukov%2C+A">A. Tutukov</a>, <a href="/search/astro-ph?searchtype=author&query=Baklanov%2C+P">P. Baklanov</a>, <a href="/search/astro-ph?searchtype=author&query=Krushinski%2C+V">V. Krushinski</a>, <a href="/search/astro-ph?searchtype=author&query=Tiurina%2C+N">N. Tiurina</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P">P. Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Kuznetsov%2C+A">A. Kuznetsov</a>, <a href="/search/astro-ph?searchtype=author&query=Kornilov%2C+V">V. Kornilov</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbunov%2C+I">I. Gorbunov</a>, <a href="/search/astro-ph?searchtype=author&query=Shumkov%2C+V">V. Shumkov</a>, <a href="/search/astro-ph?searchtype=author&query=Vladimirov%2C+V">V. Vladimirov</a>, <a href="/search/astro-ph?searchtype=author&query=Gress%2C+O">O. Gress</a>, <a href="/search/astro-ph?searchtype=author&query=Budnev%2C+N+M">N. M. Budnev</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+K">K. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Tlatov%2C+A">A. Tlatov</a>, <a href="/search/astro-ph?searchtype=author&query=Zalozhnykh%2C+I">I. Zalozhnykh</a>, <a href="/search/astro-ph?searchtype=author&query=Sergienko%2C+Y">Yu. Sergienko</a>, <a href="/search/astro-ph?searchtype=author&query=Gabovich%2C+A">A. Gabovich</a>, <a href="/search/astro-ph?searchtype=author&query=Yurkov%2C+V">V. Yurkov</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="1704.08178v1-abstract-short" style="display: inline;"> We report the discovery and multicolor (VRIW) photometry of a rare explosive star MASTER OT J004207.99+405501.1 - a luminous red nova - in the Andromeda galaxy M31N2015-01a. We use our original light curve acquired with identical MASTER Global Robotic Net telescopes in one photometric system: VRI during first 30 days and W (unfiltered) during 70 days. Also we added publishied multicolor photometry… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1704.08178v1-abstract-full').style.display = 'inline'; document.getElementById('1704.08178v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1704.08178v1-abstract-full" style="display: none;"> We report the discovery and multicolor (VRIW) photometry of a rare explosive star MASTER OT J004207.99+405501.1 - a luminous red nova - in the Andromeda galaxy M31N2015-01a. We use our original light curve acquired with identical MASTER Global Robotic Net telescopes in one photometric system: VRI during first 30 days and W (unfiltered) during 70 days. Also we added publishied multicolor photometry data to estimate the mass and energy of the ejected shell, and discuss the likely formation scenarios of outbursts of this type. We propose the interpretation of the explosion, that is consistent with the evolutionary scenario where star merger is a natural stage of the evolution of close-mass stars and may serve as an extra channel for the formation of nova outbursts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1704.08178v1-abstract-full').style.display = 'none'; document.getElementById('1704.08178v1-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 April, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">16 pages, 9 figures, 2 tables, accepted to 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/1702.06131">arXiv:1702.06131</a> <span> [<a href="https://arxiv.org/pdf/1702.06131">pdf</a>, <a href="https://arxiv.org/format/1702.06131">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/10.1051/0004-6361/201730620">10.1051/0004-6361/201730620 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multiwavelength follow-up of a rare IceCube neutrino multiplet </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aartsen%2C+M+G">M. G. Aartsen</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Ahrens%2C+M">M. Ahrens</a>, <a href="/search/astro-ph?searchtype=author&query=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Altmann%2C+D">D. Altmann</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+T">T. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Ansseau%2C+I">I. Ansseau</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Archinger%2C+M">M. Archinger</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Auffenberg%2C+J">J. Auffenberg</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S">S. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Baum%2C+V">V. Baum</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+-">K. -H. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/astro-ph?searchtype=author&query=Berley%2C+D">D. Berley</a> , et al. (479 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="1702.06131v3-abstract-short" style="display: inline;"> On February 17 2016, the IceCube real-time neutrino search identified, for the first time, three muon neutrino candidates arriving within 100 s of one another, consistent with coming from the same point in the sky. Such a triplet is expected once every 13.7 years as a random coincidence of background events. However, considering the lifetime of the follow-up program the probability of detecting at… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1702.06131v3-abstract-full').style.display = 'inline'; document.getElementById('1702.06131v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1702.06131v3-abstract-full" style="display: none;"> On February 17 2016, the IceCube real-time neutrino search identified, for the first time, three muon neutrino candidates arriving within 100 s of one another, consistent with coming from the same point in the sky. Such a triplet is expected once every 13.7 years as a random coincidence of background events. However, considering the lifetime of the follow-up program the probability of detecting at least one triplet from atmospheric background is 32%. Follow-up observatories were notified in order to search for an electromagnetic counterpart. Observations were obtained by Swift's X-ray telescope, by ASAS-SN, LCO and MASTER at optical wavelengths, and by VERITAS in the very-high-energy gamma-ray regime. Moreover, the Swift BAT serendipitously observed the location 100 s after the first neutrino was detected, and data from the Fermi LAT and HAWC observatory were analyzed. We present details of the neutrino triplet and the follow-up observations. No likely electromagnetic counterpart was detected, and we discuss the implications of these constraints on candidate neutrino sources such as gamma-ray bursts, core-collapse supernovae and active galactic nucleus flares. This study illustrates the potential of and challenges for future follow-up campaigns. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1702.06131v3-abstract-full').style.display = 'none'; document.getElementById('1702.06131v3-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> 28 November, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 February, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">23 pages, 13 figures, accepted by A&A on July 30 2017</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 607, A115 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1608.02764">arXiv:1608.02764</a> <span> [<a href="https://arxiv.org/pdf/1608.02764">pdf</a>, <a href="https://arxiv.org/ps/1608.02764">ps</a>, <a href="https://arxiv.org/format/1608.02764">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</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/10.3847/1538-4357/833/2/198">10.3847/1538-4357/833/2/198 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MASTER optical polarization variability detection in the Microquasar V404 Cyg/GS2023+33 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V+M">Vladimir M. Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E">E. Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Kornilov%2C+V">V. Kornilov</a>, <a href="/search/astro-ph?searchtype=author&query=Krushinskiy%2C+V">V. Krushinskiy</a>, <a href="/search/astro-ph?searchtype=author&query=Vlasenko%2C+D">D. Vlasenko</a>, <a href="/search/astro-ph?searchtype=author&query=Tiurina%2C+N">N. Tiurina</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P">P. Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Kuznetsov%2C+A">A. Kuznetsov</a>, <a href="/search/astro-ph?searchtype=author&query=Budnev%2C+N">N. Budnev</a>, <a href="/search/astro-ph?searchtype=author&query=Gress%2C+O">O. Gress</a>, <a href="/search/astro-ph?searchtype=author&query=Tlatov%2C+A">A. Tlatov</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+R+R">R. Rebolo Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Serra-Ricart%2C+M">M. Serra-Ricart</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+D+A+H">D. A. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Israelian%2C+G">G. Israelian</a>, <a href="/search/astro-ph?searchtype=author&query=Lodieu%2C+N">N. Lodieu</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+K">K. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Yazev%2C+S">S. Yazev</a>, <a href="/search/astro-ph?searchtype=author&query=Sergienko%2C+Y">Yu. Sergienko</a>, <a href="/search/astro-ph?searchtype=author&query=Gabovich%2C+A">A. Gabovich</a>, <a href="/search/astro-ph?searchtype=author&query=Yurkov%2C+V">V. Yurkov</a>, <a href="/search/astro-ph?searchtype=author&query=Levato%2C+H">H. Levato</a>, <a href="/search/astro-ph?searchtype=author&query=Saffe%2C+C">C. Saffe</a>, <a href="/search/astro-ph?searchtype=author&query=Podesta%2C+R">R. Podesta</a>, <a href="/search/astro-ph?searchtype=author&query=Mallamaci%2C+C">C. Mallamaci</a> , et al. (1 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="1608.02764v1-abstract-short" style="display: inline;"> On 2015 June 15 the Swift space observatory discovered that the Galactic black hole candidate V404 Cyg was undergoing another active X-ray phase, after 25 years of inactivity (Barthelmy et al. 2015). Twelve telescopes of the MASTER Global Robotic Net located at six sites across four continents were the first ground based observatories to start optical monitoring of the microquasar after its gamma-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1608.02764v1-abstract-full').style.display = 'inline'; document.getElementById('1608.02764v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1608.02764v1-abstract-full" style="display: none;"> On 2015 June 15 the Swift space observatory discovered that the Galactic black hole candidate V404 Cyg was undergoing another active X-ray phase, after 25 years of inactivity (Barthelmy et al. 2015). Twelve telescopes of the MASTER Global Robotic Net located at six sites across four continents were the first ground based observatories to start optical monitoring of the microquasar after its gamma-ray wakeup at 18h 34m 09s U.T. on 2015 June 15 (Lipunov et al. 2015). In this paper we report, for the first time, the discovery of variable optical linear polarization, changing by 4-6% over a timescale of approximately 1 h, on two different epochs. We can conclude that the additional variable polarization arisies from the relativistic jet generated by the black hole in V404Cyg. The polarization variability correlates with optical brightness changes, increasing when the flux decreases. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1608.02764v1-abstract-full').style.display = 'none'; document.getElementById('1608.02764v1-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 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">10 pages, 1 figures, 4 tables, accepted for publication in the 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/1605.01607">arXiv:1605.01607</a> <span> [<a href="https://arxiv.org/pdf/1605.01607">pdf</a>, <a href="https://arxiv.org/ps/1605.01607">ps</a>, <a href="https://arxiv.org/format/1605.01607">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/stw2669">10.1093/mnras/stw2669 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First Gravitational-Wave Burst GW150914: Part II. MASTER Optical Follow-Up Observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V+M">V. M. Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Kornilov%2C+V">V. Kornilov</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E">E. Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Tiurina%2C+N">N. Tiurina</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P">P. Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Kuznetsov%2C+A">A. Kuznetsov</a>, <a href="/search/astro-ph?searchtype=author&query=Vladimirov%2C+V">V. Vladimirov</a>, <a href="/search/astro-ph?searchtype=author&query=Vlasenko%2C+D">D. Vlasenko</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbunov%2C+I">I. Gorbunov</a>, <a href="/search/astro-ph?searchtype=author&query=Chazov%2C+V">V. Chazov</a>, <a href="/search/astro-ph?searchtype=author&query=Kuvshinov%2C+D">D. Kuvshinov</a>, <a href="/search/astro-ph?searchtype=author&query=Gabovich%2C+A">A. Gabovich</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+D+A+H">D. A. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Potter%2C+S+B">S. B. Potter</a>, <a href="/search/astro-ph?searchtype=author&query=Kniazev%2C+A">A. Kniazev</a>, <a href="/search/astro-ph?searchtype=author&query=Crawford%2C+S">S. Crawford</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+R+R">R. Rebolo Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Ricart%2C+M+S">M. Serra Ricart</a>, <a href="/search/astro-ph?searchtype=author&query=Israelian%2C+G">G. Israelian</a>, <a href="/search/astro-ph?searchtype=author&query=Lodieu%2C+N">N. Lodieu</a>, <a href="/search/astro-ph?searchtype=author&query=Gress%2C+O+A">O. A. Gress</a>, <a href="/search/astro-ph?searchtype=author&query=Budnev%2C+N+M">N. M. Budnev</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+K+I">K. I. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Poleschuk%2C+V">V. Poleschuk</a>, <a href="/search/astro-ph?searchtype=author&query=Yazev%2C+S">S. Yazev</a> , et al. (11 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="1605.01607v1-abstract-short" style="display: inline;"> The Advanced LIGO observatory recently reported the first direct detection of gravitational waves predicted by Einstein (1916). We report on the first optical observations of the Gravitational Wave (GW) source GW150914 error region with the Global MASTER Robotic Net. We detected several optical transients, which proved to be unconnected with the GW event. Our result is consistent with the assumpti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.01607v1-abstract-full').style.display = 'inline'; document.getElementById('1605.01607v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1605.01607v1-abstract-full" style="display: none;"> The Advanced LIGO observatory recently reported the first direct detection of gravitational waves predicted by Einstein (1916). We report on the first optical observations of the Gravitational Wave (GW) source GW150914 error region with the Global MASTER Robotic Net. We detected several optical transients, which proved to be unconnected with the GW event. Our result is consistent with the assumption that gravitational waves were produced by a binary black hole merger. The detection of the event confirmed the main prediction of the population synthesis performed with the "Scenario Machine" formulated in Lipunov1997b. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.01607v1-abstract-full').style.display = 'none'; document.getElementById('1605.01607v1-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 May, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">11 pages, 7 figures, 4 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/1605.01604">arXiv:1605.01604</a> <span> [<a href="https://arxiv.org/pdf/1605.01604">pdf</a>, <a href="https://arxiv.org/ps/1605.01604">ps</a>, <a href="https://arxiv.org/format/1605.01604">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/10.1016/j.newast.2016.08.017">10.1016/j.newast.2016.08.017 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The first gravitational-wave burst GW150914, as predicted by the scenario machine </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V+M">V. M. Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Kornilov%2C+V">V. Kornilov</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E">E. Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Tiurina%2C+N">N. Tiurina</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P">P. Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Kuznetsov%2C+A">A. Kuznetsov</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="1605.01604v2-abstract-short" style="display: inline;"> The Advanced LIGO observatory recently reported (Abbott et al., 2016a) the first direct detection of gravitational waves predicted by Einstein (1916). The detection of this event was predicted in 1997 on the basis of the Scenario Machine population synthesis calculations (Lipunov et al., NewA, 2, 43). Now we discuss the parameters of binary black holes and event rates predicted by different scenar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.01604v2-abstract-full').style.display = 'inline'; document.getElementById('1605.01604v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1605.01604v2-abstract-full" style="display: none;"> The Advanced LIGO observatory recently reported (Abbott et al., 2016a) the first direct detection of gravitational waves predicted by Einstein (1916). The detection of this event was predicted in 1997 on the basis of the Scenario Machine population synthesis calculations (Lipunov et al., NewA, 2, 43). Now we discuss the parameters of binary black holes and event rates predicted by different scenarios of binary evolution. We give a simple explanation of the big difference between detected black hole masses and the mean black hole masses observed in of X-ray Nova systems. The proximity of the masses of the components of GW150914 is in good agreement with the observed initial mass ratio distribution in massive binary systems, as is used in Scenario Machine calculations for massive binaries. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.01604v2-abstract-full').style.display = 'none'; document.getElementById('1605.01604v2-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 September, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 May, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">13 pages, 4 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> New Astronomy, 2017, 51, 122-127 </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/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/1602.06010">arXiv:1602.06010</a> <span> [<a href="https://arxiv.org/pdf/1602.06010">pdf</a>, <a href="https://arxiv.org/ps/1602.06010">ps</a>, <a href="https://arxiv.org/format/1602.06010">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/10.1051/0004-6361/201526528">10.1051/0004-6361/201526528 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of an unusual bright eclipsing binary with the longest known period: TYC 2505-672-1 / MASTER OT J095310.04+335352.8 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V">V. Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E">E. Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Afanasiev%2C+V">V. Afanasiev</a>, <a href="/search/astro-ph?searchtype=author&query=Tatarnikova%2C+A">A. Tatarnikova</a>, <a href="/search/astro-ph?searchtype=author&query=Denisenko%2C+D">D. Denisenko</a>, <a href="/search/astro-ph?searchtype=author&query=Makarov%2C+D">D. Makarov</a>, <a href="/search/astro-ph?searchtype=author&query=Tiurina%2C+N">N. Tiurina</a>, <a href="/search/astro-ph?searchtype=author&query=Krushinsky%2C+V">V. Krushinsky</a>, <a href="/search/astro-ph?searchtype=author&query=Vinokurov%2C+A">A. Vinokurov</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P">P. Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Kuznetsov%2C+A">A. Kuznetsov</a>, <a href="/search/astro-ph?searchtype=author&query=Gress%2C+O">O. Gress</a>, <a href="/search/astro-ph?searchtype=author&query=Sergienko%2C+Y">Yu. Sergienko</a>, <a href="/search/astro-ph?searchtype=author&query=Yurkov%2C+V">V. Yurkov</a>, <a href="/search/astro-ph?searchtype=author&query=Gabovich%2C+A">A. Gabovich</a>, <a href="/search/astro-ph?searchtype=author&query=Tlatov%2C+A">A. Tlatov</a>, <a href="/search/astro-ph?searchtype=author&query=Senik%2C+V">V. Senik</a>, <a href="/search/astro-ph?searchtype=author&query=Vladimirov%2C+V">V. Vladimirov</a>, <a href="/search/astro-ph?searchtype=author&query=Popova%2C+E">E. Popova</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="1602.06010v2-abstract-short" style="display: inline;"> We report on the MASTER Global Robotic Net discovery of an eclipsing binary, MASTER OT J095310.04+335352.8, previously known as unremarkable star TYC 2505-672-1, which displays extreme orbital parameters. The orbital period P=69.1 yr is more than 2.5 times longer than that of epsilon-Aurigae, which is the previous record holder. The light curve is characterized by an extremely deep total eclipse w… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1602.06010v2-abstract-full').style.display = 'inline'; document.getElementById('1602.06010v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1602.06010v2-abstract-full" style="display: none;"> We report on the MASTER Global Robotic Net discovery of an eclipsing binary, MASTER OT J095310.04+335352.8, previously known as unremarkable star TYC 2505-672-1, which displays extreme orbital parameters. The orbital period P=69.1 yr is more than 2.5 times longer than that of epsilon-Aurigae, which is the previous record holder. The light curve is characterized by an extremely deep total eclipse with a depth of more than 4.5 mag, which is symmetrically shaped and has a total duration of 3.5 yrs. The eclipse is essentially gray. The spectra acquired with the Russian 6 m BTA telescope both at minimum and maximum light mainly correspond to an M0-1III--type red giant, but the spectra taken at the bottom of eclipse show small traces of a sufficiently hot source. The observed properties of this system can be better explained as the red giant eclipsed by a large cloud (the disk) of small particles surrounding the invisible secondary companion. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1602.06010v2-abstract-full').style.display = 'none'; document.getElementById('1602.06010v2-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> 27 March, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 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">8 figures, 9 pages, Astronomy and astrophysics in print</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1511.02641">arXiv:1511.02641</a> <span> [<a href="https://arxiv.org/pdf/1511.02641">pdf</a>, <a href="https://arxiv.org/ps/1511.02641">ps</a>, <a href="https://arxiv.org/format/1511.02641">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/stv2515">10.1093/mnras/stv2515 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Early polarization observations of the optical emission of gamma-ray bursts: GRB150301B and GRB150413A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E+S">E. S. Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V+M">V. M. Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+D">D. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Kornilov%2C+V+G">V. G. Kornilov</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P+V">P. V. Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Tyurina%2C+N+V">N. V. Tyurina</a>, <a href="/search/astro-ph?searchtype=author&query=Kuznetsov%2C+A+S">A. S. Kuznetsov</a>, <a href="/search/astro-ph?searchtype=author&query=Kuvshinov%2C+D+A">D. A. Kuvshinov</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbunov%2C+I+A">I. A. Gorbunov</a>, <a href="/search/astro-ph?searchtype=author&query=Vlasenko%2C+D">D. Vlasenko</a>, <a href="/search/astro-ph?searchtype=author&query=Popova%2C+E">E. Popova</a>, <a href="/search/astro-ph?searchtype=author&query=Chazov%2C+V+V">V. V. Chazov</a>, <a href="/search/astro-ph?searchtype=author&query=Potter%2C+S">S. Potter</a>, <a href="/search/astro-ph?searchtype=author&query=Kotze%2C+M">M. Kotze</a>, <a href="/search/astro-ph?searchtype=author&query=Kniazev%2C+A">A. Kniazev</a>, <a href="/search/astro-ph?searchtype=author&query=Gress%2C+O+A">O. A. Gress</a>, <a href="/search/astro-ph?searchtype=author&query=Budnev%2C+N+M">N. M. Budnev</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+K+I">K. I. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Yazev%2C+S+A">S. A. Yazev</a>, <a href="/search/astro-ph?searchtype=author&query=Tlatov%2C+A+G">A. G. Tlatov</a>, <a href="/search/astro-ph?searchtype=author&query=Senik%2C+V+A">V. A. Senik</a>, <a href="/search/astro-ph?searchtype=author&query=Dormidontov%2C+D+V">D. V. Dormidontov</a>, <a href="/search/astro-ph?searchtype=author&query=Parhomenko%2C+A+V">A. V. Parhomenko</a>, <a href="/search/astro-ph?searchtype=author&query=Krushinski%2C+V+V">V. V. Krushinski</a>, <a href="/search/astro-ph?searchtype=author&query=Zalozhnich%2C+I+S">I. S. Zalozhnich</a> , et al. (10 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="1511.02641v1-abstract-short" style="display: inline;"> We report early optical linear polarization observations of two gamma-ray bursts made with the MASTER robotic telescope network. We found the minimum polar- ization for GRB150301B to be 8% at the beginning of the initial stage, whereas we detected no polarization for GRB150413A either at the rising branch or after the burst reached the power-law afterglow stage. This is the earliest measurement of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.02641v1-abstract-full').style.display = 'inline'; document.getElementById('1511.02641v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1511.02641v1-abstract-full" style="display: none;"> We report early optical linear polarization observations of two gamma-ray bursts made with the MASTER robotic telescope network. We found the minimum polar- ization for GRB150301B to be 8% at the beginning of the initial stage, whereas we detected no polarization for GRB150413A either at the rising branch or after the burst reached the power-law afterglow stage. This is the earliest measurement of the polarization (in cosmological rest frame) of gamma-ray bursts. The primary intent of the paper is to discover optical emission and publish extremely rare (unique) high- quality light curves of the prompt optical emission of gamma-ray bursts during the non-monotonic stage of their evolution. We report that our team has discovered the optical counterpart of one of the bursts, GRB150413A. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.02641v1-abstract-full').style.display = 'none'; document.getElementById('1511.02641v1-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 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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, MNRAS, 2015</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1510.07807">arXiv:1510.07807</a> <span> [<a href="https://arxiv.org/pdf/1510.07807">pdf</a>, <a href="https://arxiv.org/ps/1510.07807">ps</a>, <a href="https://arxiv.org/format/1510.07807">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/stv2228">10.1093/mnras/stv2228 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The optical identifcation of events with poorly defined locations: The case of the Fermi GBM GRB140801A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V+M">V. M. Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Gorosabel%2C+J">J. Gorosabel</a>, <a href="/search/astro-ph?searchtype=author&query=Pruzhinskaya%2C+M+V">M. V. Pruzhinskaya</a>, <a href="/search/astro-ph?searchtype=author&query=Postigo%2C+A+d+U">A. de Ugarte Postigo</a>, <a href="/search/astro-ph?searchtype=author&query=Pelassa%2C+V">V. Pelassa</a>, <a href="/search/astro-ph?searchtype=author&query=Tsvetkova%2C+A+E">A. E. Tsvetkova</a>, <a href="/search/astro-ph?searchtype=author&query=Sokolov%2C+I+V">I. V. Sokolov</a>, <a href="/search/astro-ph?searchtype=author&query=Kann%2C+D+A">D. A. Kann</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+D">Dong Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E+S">E. S. Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Krushinski%2C+V+V">V. V. Krushinski</a>, <a href="/search/astro-ph?searchtype=author&query=Kornilov%2C+V+G">V. G. Kornilov</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P+V">P. V. Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Boronina%2C+S+V">S. V. Boronina</a>, <a href="/search/astro-ph?searchtype=author&query=Budnev%2C+N+M">N. M. Budnev</a>, <a href="/search/astro-ph?searchtype=author&query=Cano%2C+Z">Z. Cano</a>, <a href="/search/astro-ph?searchtype=author&query=Castro-Tirado%2C+A+J">A. J. Castro-Tirado</a>, <a href="/search/astro-ph?searchtype=author&query=Chazov%2C+V+V">V. V. Chazov</a>, <a href="/search/astro-ph?searchtype=author&query=Connaughton%2C+V">V. Connaughton</a>, <a href="/search/astro-ph?searchtype=author&query=Delvaux%2C+C">C. Delvaux</a>, <a href="/search/astro-ph?searchtype=author&query=Frederiks%2C+D+D">D. D. Frederiks</a>, <a href="/search/astro-ph?searchtype=author&query=Fynbo%2C+J+F+U">J. F. U. Fynbo</a>, <a href="/search/astro-ph?searchtype=author&query=Gabovich%2C+A+V">A. V. Gabovich</a>, <a href="/search/astro-ph?searchtype=author&query=Goldstein%2C+A">A. Goldstein</a>, <a href="/search/astro-ph?searchtype=author&query=Greiner%2C+J">J. Greiner</a> , et al. (28 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="1510.07807v1-abstract-short" style="display: inline;"> We report the early discovery of the optical afterglow of gamma-ray burst (GRB) 140801A in the 137 deg$^2$ 3-$蟽$ error-box of the Fermi Gamma-ray Burst Monitor (GBM). MASTER is the only observatory that automatically react to all Fermi alerts. GRB 140801A is one of the few GRBs whose optical counterpart was discovered solely from its GBM localization. The optical afterglow of GRB 140801A was found… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.07807v1-abstract-full').style.display = 'inline'; document.getElementById('1510.07807v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1510.07807v1-abstract-full" style="display: none;"> We report the early discovery of the optical afterglow of gamma-ray burst (GRB) 140801A in the 137 deg$^2$ 3-$蟽$ error-box of the Fermi Gamma-ray Burst Monitor (GBM). MASTER is the only observatory that automatically react to all Fermi alerts. GRB 140801A is one of the few GRBs whose optical counterpart was discovered solely from its GBM localization. The optical afterglow of GRB 140801A was found by MASTER Global Robotic Net 53 sec after receiving the alert, making it the fastest optical detection of a GRB from a GBM error-box. Spectroscopy obtained with the 10.4-m Gran Telescopio Canarias and the 6-m BTA of SAO RAS reveals a redshift of $z=1.32$. We performed optical and near-infrared photometry of GRB 140801A using different telescopes with apertures ranging from 0.4-m to 10.4-m. GRB 140801A is a typical burst in many ways. The rest-frame bolometric isotropic energy release and peak energy of the burst is $E_\mathrm{iso} = 5.54_{-0.24}^{+0.26} \times 10^{52}$ erg and $E_\mathrm{p, rest}\simeq280$ keV, respectively, which is consistent with the Amati relation. The absence of a jet break in the optical light curve provides a lower limit on the half-opening angle of the jet $胃=6.1$ deg. The observed $E_\mathrm{peak}$ is consistent with the limit derived from the Ghirlanda relation. The joint Fermi GBM and Konus-Wind analysis shows that GRB 140801A could belong to the class of intermediate duration. The rapid detection of the optical counterpart of GRB 140801A is especially important regarding the upcoming experiments with large coordinate error-box areas. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.07807v1-abstract-full').style.display = 'none'; document.getElementById('1510.07807v1-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> 27 October, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">in press MNRAS, 2015</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> MNRAS, 455, 712 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1401.3221">arXiv:1401.3221</a> <span> [<a href="https://arxiv.org/pdf/1401.3221">pdf</a>, <a href="https://arxiv.org/ps/1401.3221">ps</a>, <a href="https://arxiv.org/format/1401.3221">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/10.1016/j.newast.2013.12.003">10.1016/j.newast.2013.12.003 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Optical polarization observations with the MASTER robotic net </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pruzhinskaya%2C+M+V">M. V. Pruzhinskaya</a>, <a href="/search/astro-ph?searchtype=author&query=Krushinsky%2C+V+V">V. V. Krushinsky</a>, <a href="/search/astro-ph?searchtype=author&query=Lipunova%2C+G+V">G. V. Lipunova</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E+S">E. S. Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P+V">P. V. Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Kuznetsov%2C+A+S">A. S. Kuznetsov</a>, <a href="/search/astro-ph?searchtype=author&query=Denisenko%2C+D+V">D. V. Denisenko</a>, <a href="/search/astro-ph?searchtype=author&query=Kornilov%2C+V+G">V. G. Kornilov</a>, <a href="/search/astro-ph?searchtype=author&query=Tyurina%2C+N+V">N. V. Tyurina</a>, <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V+M">V. M. Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Tlatov%2C+A+G">A. G. Tlatov</a>, <a href="/search/astro-ph?searchtype=author&query=Parkhomenko%2C+A+V">A. V. Parkhomenko</a>, <a href="/search/astro-ph?searchtype=author&query=Budnev%2C+N+M">N. M. Budnev</a>, <a href="/search/astro-ph?searchtype=author&query=Yazev%2C+S+A">S. A. Yazev</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+K+I">K. I. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Gress%2C+O+A">O. A. Gress</a>, <a href="/search/astro-ph?searchtype=author&query=Yurkov%2C+V+V">V. V. Yurkov</a>, <a href="/search/astro-ph?searchtype=author&query=Gabovich%2C+A+V">A. V. Gabovich</a>, <a href="/search/astro-ph?searchtype=author&query=Sergienko%2C+Y+P">Yu. P. Sergienko</a>, <a href="/search/astro-ph?searchtype=author&query=Sinyakov%2C+E+V">E. V. Sinyakov</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="1401.3221v3-abstract-short" style="display: inline;"> We present results of optical polarization observations performed with the MASTER robotic net for three types of objects: gamma-ray bursts, supernovae, and blazars. For the Swift gamma-ray bursts GRB100906A, GRB110422A, GRB121011A, polarization observations were obtained during very early stages of optical emission. For GRB100906A it was the first prompt optical polarization observation in the wor… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.3221v3-abstract-full').style.display = 'inline'; document.getElementById('1401.3221v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1401.3221v3-abstract-full" style="display: none;"> We present results of optical polarization observations performed with the MASTER robotic net for three types of objects: gamma-ray bursts, supernovae, and blazars. For the Swift gamma-ray bursts GRB100906A, GRB110422A, GRB121011A, polarization observations were obtained during very early stages of optical emission. For GRB100906A it was the first prompt optical polarization observation in the world. Photometry in polarizers is presented for Type Ia Supernova 2012bh during 20 days, starting on March 27, 2012. We find that the linear polarization of SN 2012bh at the early stage of the envelope expansion was less than 3%. Polarization measurements for the blazars OC 457, 3C 454.3, QSO B1215+303, 87GB 165943.2+395846 at single nights are presented. We infer the degree of the linear polarization and polarization angle. The blazars OC 457 and 3C 454.3 were observed during their periods of activity. The results show that MASTER is able to measure substantially polarized light; at the same time it is not suitable for determining weak polarization (less than 5%) of dim objects (fainter than 16$^m$). Polarimetric observations of the optical emission from gamma-ray bursts and supernovae are necessary to investigate the nature of these transient objects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.3221v3-abstract-full').style.display = 'none'; document.getElementById('1401.3221v3-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 April, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 January, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">31 pages, 12 figures, 4 tables; Exposure times in Table 2 have been corrected</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> New Astronomy 29C (2014), pp. 65-74 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1307.7396">arXiv:1307.7396</a> <span> [<a href="https://arxiv.org/pdf/1307.7396">pdf</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> <p class="title is-5 mathjax"> New Cataclysmic Variable 1RXS J161659.5+620014 in Draco </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P">P. Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Denisenko%2C+D">D. Denisenko</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E">E. Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V">V. Lipunov</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="1307.7396v1-abstract-short" style="display: inline;"> We report the discovery of a new cataclysmic variable MASTER OT J161700.81+620024.9 which is identical to the faint ROSAT X-ray source 1RXS J161659.5+620014. The object was observed in outbursts to 14.4m on 2012 Sep. 11 by MASTER-Tunka and to 14.3m on 2013 Jan. 21/22 by MASTER-Kislovodsk, but was not detected by the routine search procedures. Analysis of the archival MASTER data and CRTS light cur… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.7396v1-abstract-full').style.display = 'inline'; document.getElementById('1307.7396v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1307.7396v1-abstract-full" style="display: none;"> We report the discovery of a new cataclysmic variable MASTER OT J161700.81+620024.9 which is identical to the faint ROSAT X-ray source 1RXS J161659.5+620014. The object was observed in outbursts to 14.4m on 2012 Sep. 11 by MASTER-Tunka and to 14.3m on 2013 Jan. 21/22 by MASTER-Kislovodsk, but was not detected by the routine search procedures. Analysis of the archival MASTER data and CRTS light curve shows the variability from 17.8m at quiescence to 14.3m in outbursts, confirming that the new variable is a dwarf nova. SDSS colors suggest a small contribution from the secondary component and are telling in favor of the short orbital period. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.7396v1-abstract-full').style.display = 'none'; document.getElementById('1307.7396v1-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> 28 July, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">2 pages, 3 figures, submitted to Peremennye Zvezdy (Variable Stars)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1305.1620">arXiv:1305.1620</a> <span>  </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/10.1134/S1063772913040033">10.1134/S1063772913040033 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MASTER-II Network of Robotic Optical Telescopes. First Results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E+S">E. S. Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V+M">V. M. Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Kornilov%2C+V+G">V. G. Kornilov</a>, <a href="/search/astro-ph?searchtype=author&query=Belinski%2C+A+A">A. A. Belinski</a>, <a href="/search/astro-ph?searchtype=author&query=Kuvshinov%2C+D+A">D. A. Kuvshinov</a>, <a href="/search/astro-ph?searchtype=author&query=Tyurina%2C+N+V">N. V. Tyurina</a>, <a href="/search/astro-ph?searchtype=author&query=Sankovich%2C+A+V">A. V. Sankovich</a>, <a href="/search/astro-ph?searchtype=author&query=Krylov%2C+A+V">A. V. Krylov</a>, <a href="/search/astro-ph?searchtype=author&query=Shatskiy%2C+N+I">N. I. Shatskiy</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P+V">P. V. Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Chazov%2C+V+V">V. V. Chazov</a>, <a href="/search/astro-ph?searchtype=author&query=Kuznetsov%2C+A+S">A. S. Kuznetsov</a>, <a href="/search/astro-ph?searchtype=author&query=Zimnukhov%2C+A+S">A. S. Zimnukhov</a>, <a href="/search/astro-ph?searchtype=author&query=Shumkov%2C+V+P">V. P. Shumkov</a>, <a href="/search/astro-ph?searchtype=author&query=Shurpakov%2C+S+E">S. E. Shurpakov</a>, <a href="/search/astro-ph?searchtype=author&query=Senik%2C+V+A">V. A. Senik</a>, <a href="/search/astro-ph?searchtype=author&query=Gareeva%2C+D+V">D. V. Gareeva</a>, <a href="/search/astro-ph?searchtype=author&query=Pruzhinskaya%2C+M+V">M. V. Pruzhinskaya</a>, <a href="/search/astro-ph?searchtype=author&query=Tlatov%2C+A+G">A. G. Tlatov</a>, <a href="/search/astro-ph?searchtype=author&query=Parkhomenko%2C+A+V">A. V. Parkhomenko</a>, <a href="/search/astro-ph?searchtype=author&query=Dormidontov%2C+D+V">D. V. Dormidontov</a>, <a href="/search/astro-ph?searchtype=author&query=Krushinsky%2C+V+V">V. V. Krushinsky</a>, <a href="/search/astro-ph?searchtype=author&query=Punanova%2C+A+F">A. F. Punanova</a>, <a href="/search/astro-ph?searchtype=author&query=Zalozhnyh%2C+I+S">I. S. Zalozhnyh</a>, <a href="/search/astro-ph?searchtype=author&query=Popov%2C+A+A">A. A. Popov</a> , et al. (14 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="1305.1620v1-abstract-short" style="display: inline;"> Erroneous submission in violation of copyright, removed by arXiv admin. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1305.1620v1-abstract-full" style="display: none;"> Erroneous submission in violation of copyright, removed by arXiv admin. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1305.1620v1-abstract-full').style.display = 'none'; document.getElementById('1305.1620v1-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 May, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">Erroneous submission in violation of copyright</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astronomy Reports April 2013, Volume 57, Issue 4, pp 233-286 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1205.6973">arXiv:1205.6973</a> <span> [<a href="https://arxiv.org/pdf/1205.6973">pdf</a>, <a href="https://arxiv.org/ps/1205.6973">ps</a>, <a href="https://arxiv.org/format/1205.6973">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/10.1134/S1063773711110053">10.1134/S1063773711110053 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Photometric observations of the supernova 2009nr </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tsvetkov%2C+D+Y">D. Yu. Tsvetkov</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P+V">P. V. Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V+M">V. M. Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Volkov%2C+I+M">I. M. Volkov</a>, <a href="/search/astro-ph?searchtype=author&query=Tuchin%2C+O+A">O. A. Tuchin</a>, <a href="/search/astro-ph?searchtype=author&query=Kudelina%2C+I+P">I. P. Kudelina</a>, <a href="/search/astro-ph?searchtype=author&query=Pruzhinskaya%2C+M+V">M. V. Pruzhinskaya</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E+S">E. S. Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Kornilov%2C+V+G">V. G. Kornilov</a>, <a href="/search/astro-ph?searchtype=author&query=Belinskii%2C+A+A">A. A. Belinskii</a>, <a href="/search/astro-ph?searchtype=author&query=Tyurina%2C+N+V">N. V. Tyurina</a>, <a href="/search/astro-ph?searchtype=author&query=Yurkov%2C+V+V">V. V. Yurkov</a>, <a href="/search/astro-ph?searchtype=author&query=Sergienko%2C+Y+P">Yu. P. Sergienko</a>, <a href="/search/astro-ph?searchtype=author&query=Tlatov%2C+A+G">A. G. Tlatov</a>, <a href="/search/astro-ph?searchtype=author&query=Parkhomenko%2C+A+V">A. V. Parkhomenko</a>, <a href="/search/astro-ph?searchtype=author&query=Dormidontov%2C+D+V">D. V. Dormidontov</a>, <a href="/search/astro-ph?searchtype=author&query=Senik%2C+V+A">V. A. Senik</a>, <a href="/search/astro-ph?searchtype=author&query=Krushinskii%2C+V+V">V. V. Krushinskii</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="1205.6973v1-abstract-short" style="display: inline;"> We present the results of our UBVRI CCD photometry for the second brightest supernova of 2009, SN 2009nr, discovered during a sky survey with the telescopes of the MASTER robotic network. Its light and color curves and bolometric light curves have been constructed. The light-curve parameters and the maximum luminosity have been determined. SN 2009nr is shown to be similar in light-curve shape and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1205.6973v1-abstract-full').style.display = 'inline'; document.getElementById('1205.6973v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1205.6973v1-abstract-full" style="display: none;"> We present the results of our UBVRI CCD photometry for the second brightest supernova of 2009, SN 2009nr, discovered during a sky survey with the telescopes of the MASTER robotic network. Its light and color curves and bolometric light curves have been constructed. The light-curve parameters and the maximum luminosity have been determined. SN 2009nr is shown to be similar in light-curve shape and maximum luminosity to SN 1991T, which is the prototype of the class of supernovae Ia with an enhanced luminosity. SN 2009nr exploded far from the center of the spiral galaxy UGC 8255 and most likely belongs to its old halo population. We hypothesize that this explosion is a consequence of the merger of white dwarfs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1205.6973v1-abstract-full').style.display = 'none'; document.getElementById('1205.6973v1-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 May, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astronomy Letters, Vol.37, No.11, pp.775-782, 2011 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1111.6904">arXiv:1111.6904</a> <span> [<a href="https://arxiv.org/pdf/1111.6904">pdf</a>, <a href="https://arxiv.org/ps/1111.6904">ps</a>, <a href="https://arxiv.org/format/1111.6904">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</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/10.1007/s10686-011-9280-z">10.1007/s10686-011-9280-z <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Robotic optical telescopes global network MASTER II. Equipment, structure, algorithms </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kornilov%2C+V">Victor Kornilov</a>, <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V">Vladimir Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E">Evgeny Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Belinski%2C+A">Aleksander Belinski</a>, <a href="/search/astro-ph?searchtype=author&query=Kuvshinov%2C+D">Dmitry Kuvshinov</a>, <a href="/search/astro-ph?searchtype=author&query=Tyurina%2C+N">Natalia Tyurina</a>, <a href="/search/astro-ph?searchtype=author&query=Shatsky%2C+N">Nikolai Shatsky</a>, <a href="/search/astro-ph?searchtype=author&query=Sankovich%2C+A">Anatoly Sankovich</a>, <a href="/search/astro-ph?searchtype=author&query=Krylov%2C+A">Aleksander Krylov</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P">Pavel Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Chazov%2C+V">Vadim Chazov</a>, <a href="/search/astro-ph?searchtype=author&query=Kuznetsov%2C+A">Artem Kuznetsov</a>, <a href="/search/astro-ph?searchtype=author&query=Zimnuhov%2C+D">Dmitry Zimnuhov</a>, <a href="/search/astro-ph?searchtype=author&query=Senik%2C+V">Victor Senik</a>, <a href="/search/astro-ph?searchtype=author&query=Tlatov%2C+A">Andrey Tlatov</a>, <a href="/search/astro-ph?searchtype=author&query=Parkhomenko%2C+A">Aleksander Parkhomenko</a>, <a href="/search/astro-ph?searchtype=author&query=Dormidontov%2C+D">Denis Dormidontov</a>, <a href="/search/astro-ph?searchtype=author&query=Krushinsky%2C+V">Vadim Krushinsky</a>, <a href="/search/astro-ph?searchtype=author&query=Zalozhnyh%2C+I">Ivan Zalozhnyh</a>, <a href="/search/astro-ph?searchtype=author&query=Popov%2C+A">Aleksander Popov</a>, <a href="/search/astro-ph?searchtype=author&query=Yazev%2C+S">Sergey Yazev</a>, <a href="/search/astro-ph?searchtype=author&query=Budnev%2C+N">Nikolai Budnev</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+K">Kirill Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Konstantinov%2C+E">Evgeny Konstantinov</a>, <a href="/search/astro-ph?searchtype=author&query=Gress%2C+O">Oleg Gress</a> , et al. (4 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="1111.6904v1-abstract-short" style="display: inline;"> Presented paper describes the basic principles and features of the implementation of a robotic network of optical telescopes MASTER, designed to study the prompt (simultaneous with gamma radiation) optical emission of gamma-ray bursts and to perform the sky survey to detect unknown objects and transient phenomena. With joint efforts of Sternberg astronomical institute, High altitude astronomical s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.6904v1-abstract-full').style.display = 'inline'; document.getElementById('1111.6904v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1111.6904v1-abstract-full" style="display: none;"> Presented paper describes the basic principles and features of the implementation of a robotic network of optical telescopes MASTER, designed to study the prompt (simultaneous with gamma radiation) optical emission of gamma-ray bursts and to perform the sky survey to detect unknown objects and transient phenomena. With joint efforts of Sternberg astronomical institute, High altitude astronomical station of the Pulkovo observatory, Ural state university, Irkutsk state university, Blagoveshchensk pedagogical university, the robotic telescopes MASTER II near Kislovodsk, Yekaterinburg, Irkutsk and Blagoveshchensk were installed and tested. The network spread over the longitudes is greater than 6 hours. A further expansion of the network is considered. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.6904v1-abstract-full').style.display = 'none'; document.getElementById('1111.6904v1-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 November, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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 Experimental Astronomy, 18 pages, 11 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/1111.3625">arXiv:1111.3625</a> <span> [<a href="https://arxiv.org/pdf/1111.3625">pdf</a>, <a href="https://arxiv.org/ps/1111.3625">ps</a>, <a href="https://arxiv.org/format/1111.3625">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/10.1111/j.1365-2966.2012.20195.x">10.1111/j.1365-2966.2012.20195.x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Prompt, early, and afterglow optical observations of five gamma-ray bursts (GRBs 100901A, 100902A, 100905A, 100906A, and 101020A) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E+S">E. S. Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Lipunova%2C+G+V">G. V. Lipunova</a>, <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V+M">V. M. Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Kornilov%2C+V+G">V. G. Kornilov</a>, <a href="/search/astro-ph?searchtype=author&query=Belinski%2C+A+A">A. A. Belinski</a>, <a href="/search/astro-ph?searchtype=author&query=Shatskiy%2C+N+I">N. I. Shatskiy</a>, <a href="/search/astro-ph?searchtype=author&query=Tyurina%2C+N+V">N. V. Tyurina</a>, <a href="/search/astro-ph?searchtype=author&query=Kuvshinov%2C+D+A">D. A. Kuvshinov</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P+V">P. V. Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Chazov%2C+V+V">V. V. Chazov</a>, <a href="/search/astro-ph?searchtype=author&query=Kuznetsov%2C+A">A. Kuznetsov</a>, <a href="/search/astro-ph?searchtype=author&query=Zimnukhov%2C+D+S">D. S. Zimnukhov</a>, <a href="/search/astro-ph?searchtype=author&query=Kornilov%2C+M+V">M. V. Kornilov</a>, <a href="/search/astro-ph?searchtype=author&query=Sankovich%2C+A+V">A. V. Sankovich</a>, <a href="/search/astro-ph?searchtype=author&query=Krylov%2C+A">A. Krylov</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+K+I">K. I. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Chvalaev%2C+O">O. Chvalaev</a>, <a href="/search/astro-ph?searchtype=author&query=Poleschuk%2C+V+A">V. A. Poleschuk</a>, <a href="/search/astro-ph?searchtype=author&query=Konstantinov%2C+E+N">E. N. Konstantinov</a>, <a href="/search/astro-ph?searchtype=author&query=Gress%2C+O+A">O. A. Gress</a>, <a href="/search/astro-ph?searchtype=author&query=Yazev%2C+S+A">S. A. Yazev</a>, <a href="/search/astro-ph?searchtype=author&query=Budnev%2C+N+M">N. M. Budnev</a>, <a href="/search/astro-ph?searchtype=author&query=Krushinski%2C+V+V">V. V. Krushinski</a>, <a href="/search/astro-ph?searchtype=author&query=Zalozhnich%2C+I+S">I. S. Zalozhnich</a>, <a href="/search/astro-ph?searchtype=author&query=Popov%2C+A+A">A. A. Popov</a> , et al. (13 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="1111.3625v1-abstract-short" style="display: inline;"> We present results of the prompt, early, and afterglow optical observations of five gamma-ray bursts, GRBs 100901A, 100902A, 100905A, 100906A, and 101020A, made with the Mobile Astronomical System of TElescope-Robots in Russia (MASTER-II net), the 1.5-m telescope of Sierra-Nevada Observatory, and the 2.56-m Nordic Optical Telescope. For two sources, GRB 100901A and GRB 100906A, we detected optical… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.3625v1-abstract-full').style.display = 'inline'; document.getElementById('1111.3625v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1111.3625v1-abstract-full" style="display: none;"> We present results of the prompt, early, and afterglow optical observations of five gamma-ray bursts, GRBs 100901A, 100902A, 100905A, 100906A, and 101020A, made with the Mobile Astronomical System of TElescope-Robots in Russia (MASTER-II net), the 1.5-m telescope of Sierra-Nevada Observatory, and the 2.56-m Nordic Optical Telescope. For two sources, GRB 100901A and GRB 100906A, we detected optical counterparts and obtained light curves starting before cessation of gamma-ray emission, at 113 s and 48 s after the trigger, respectively. Observations of GRB 100906A were conducted with two polarizing filters. Observations of the other three bursts gave the upper limits on the optical flux; their properties are briefly discussed. More detailed analysis of GRB 100901A and GRB 100906A supplemented by Swift data provides the following results and indicates different origins of the prompt optical radiation in the two bursts. The light curves patterns and spectral distributions suggest a common production site of the prompt optical and high-energy emission in GRB 100901A. Results of spectral fits for GRB 100901A in the range from the optical to X-rays favor power-law energy distributions with similar values of the optical extinction in the host galaxy. GRB 100906A produced a smoothly peaking optical light curve suggesting that the prompt optical radiation in this GRB originated in a front shock. This is supported by a spectral analysis. We have found that the Amati and Ghirlanda relations are satisfied for GRB 100906A. An upper limit on the value of the optical extinction on the host of GRB 100906A is obtained. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.3625v1-abstract-full').style.display = 'none'; document.getElementById('1111.3625v1-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, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">18 pages, 14 figures, 14 tables, 5 machine readable tables; 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/1004.5200">arXiv:1004.5200</a> <span> [<a href="https://arxiv.org/pdf/1004.5200">pdf</a>, <a href="https://arxiv.org/ps/1004.5200">ps</a>, <a href="https://arxiv.org/format/1004.5200">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> <p class="title is-5 mathjax"> The light curves of type Ia Supernova 2008gy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tsvetkov%2C+D+Y">D. Yu. Tsvetkov</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P">P. Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E+S">E. S. Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Kuvshinov%2C+D+A">D. A. Kuvshinov</a>, <a href="/search/astro-ph?searchtype=author&query=Krylov%2C+A+V">A. V. Krylov</a>, <a href="/search/astro-ph?searchtype=author&query=Kopytova%2C+T">T. Kopytova</a>, <a href="/search/astro-ph?searchtype=author&query=Kryachko%2C+T">T. Kryachko</a>, <a href="/search/astro-ph?searchtype=author&query=Korotkiy%2C+S">S. Korotkiy</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="1004.5200v1-abstract-short" style="display: inline;"> CCD BVRI photometry is presented for type Ia supernova 2008gy. The light curves match the template curves for fast-declining SN Ia, but the colors appear redder than average, and the SN may also be slightly subluminous. SN 2008gy is found to be located far outside the boundaries of three nearest galaxies, each of them has nearly equal probability to be the host galaxy. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1004.5200v1-abstract-full" style="display: none;"> CCD BVRI photometry is presented for type Ia supernova 2008gy. The light curves match the template curves for fast-declining SN Ia, but the colors appear redder than average, and the SN may also be slightly subluminous. SN 2008gy is found to be located far outside the boundaries of three nearest galaxies, each of them has nearly equal probability to be the host galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1004.5200v1-abstract-full').style.display = 'none'; document.getElementById('1004.5200v1-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 April, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">6 pages, 3 figures, submitted to Variable Stars</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0907.1118">arXiv:0907.1118</a> <span> [<a href="https://arxiv.org/pdf/0907.1118">pdf</a>, <a href="https://arxiv.org/ps/0907.1118">ps</a>, <a href="https://arxiv.org/format/0907.1118">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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/10.1155/2010/917584">10.1155/2010/917584 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Transient detections and other real-time data processing from wide-field chambers MASTER-VWF </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E">Evgeny Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+K">Kirill Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V">Vladimir Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Kornilov%2C+V">Victor Kornilov</a>, <a href="/search/astro-ph?searchtype=author&query=Belinski%2C+A">Alexander Belinski</a>, <a href="/search/astro-ph?searchtype=author&query=Shatskij%2C+N">Nikolaj Shatskij</a>, <a href="/search/astro-ph?searchtype=author&query=Kuvshinov%2C+D">Dmitry Kuvshinov</a>, <a href="/search/astro-ph?searchtype=author&query=Tyurina%2C+N">Nataly Tyurina</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P">Pavel Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Chazov%2C+V">Vadim Chazov</a>, <a href="/search/astro-ph?searchtype=author&query=Kuznetsov%2C+A">Artem Kuznetsov</a>, <a href="/search/astro-ph?searchtype=author&query=Kortunov%2C+P">Petr Kortunov</a>, <a href="/search/astro-ph?searchtype=author&query=Tlatov%2C+A">Andrey Tlatov</a>, <a href="/search/astro-ph?searchtype=author&query=Parkhomenko%2C+A">Alexander Parkhomenko</a>, <a href="/search/astro-ph?searchtype=author&query=Krushinsky%2C+V">Vadim Krushinsky</a>, <a href="/search/astro-ph?searchtype=author&query=Zalozhnyh%2C+I">Ivan Zalozhnyh</a>, <a href="/search/astro-ph?searchtype=author&query=Popov%2C+A">Alexander Popov</a>, <a href="/search/astro-ph?searchtype=author&query=Kopytova%2C+T">Taisia Kopytova</a>, <a href="/search/astro-ph?searchtype=author&query=Yazev%2C+S">Sergey Yazev</a>, <a href="/search/astro-ph?searchtype=author&query=Krylov%2C+A">Alexander Krylov</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="0907.1118v2-abstract-short" style="display: inline;"> At present time Robotic observatory making is of current importance. Having a large field of view and being able to point at anywhere, Robotic astronomical systems are indispensable when they looking for transients like grb, supernovae explosions, novae etc, as it's impossible in these cases to foresee what you should point you telescope at and when. In work are described prompt GRB observations… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0907.1118v2-abstract-full').style.display = 'inline'; document.getElementById('0907.1118v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0907.1118v2-abstract-full" style="display: none;"> At present time Robotic observatory making is of current importance. Having a large field of view and being able to point at anywhere, Robotic astronomical systems are indispensable when they looking for transients like grb, supernovae explosions, novae etc, as it's impossible in these cases to foresee what you should point you telescope at and when. In work are described prompt GRB observations received on wide-field chambers MASTER-VWF, and also methods of the images analysis and transients classifications applied in real-time data processing in this experiment. For 7 months of operation 6 synchronous observations of gamma-ray burst had been made by MASTER VWF in Kislovodsk and Irkutsk. In all cases a high upper limits have been received (see tabl \ref {tab_grbwf} and fig. \ref {allgrb}). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0907.1118v2-abstract-full').style.display = 'none'; document.getElementById('0907.1118v2-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> 24 December, 2009; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 July, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">21 pages, 21 figure, 2 tables, Advances in Astronomy in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0907.1036">arXiv:0907.1036</a> <span> [<a href="https://arxiv.org/pdf/0907.1036">pdf</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/10.1155/2010/763629">10.1155/2010/763629 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MASTER prompt and follow-up GRB observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tyurina%2C+N">Nataly Tyurina</a>, <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V">Vladimir Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Kornilov%2C+V">Victor Kornilov</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E">Evgeny Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Shatskij%2C+N">Nikolaj Shatskij</a>, <a href="/search/astro-ph?searchtype=author&query=Kuvshinov%2C+D">Dmitry Kuvshinov</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P">Pavel Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Belinski%2C+A">Alexander Belinski</a>, <a href="/search/astro-ph?searchtype=author&query=Krushinsky%2C+V">Vadim Krushinsky</a>, <a href="/search/astro-ph?searchtype=author&query=Zalozhnyh%2C+I">Ivan Zalozhnyh</a>, <a href="/search/astro-ph?searchtype=author&query=Tlatov%2C+A">Andrey Tlatov</a>, <a href="/search/astro-ph?searchtype=author&query=Parkhomenko%2C+A">Alexander Parkhomenko</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+K">Kirill Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Yazev%2C+S">Sergey Yazev</a>, <a href="/search/astro-ph?searchtype=author&query=Kortunov%2C+P">Petr Kortunov</a>, <a href="/search/astro-ph?searchtype=author&query=Sankovich%2C+A">Anatoly Sankovich</a>, <a href="/search/astro-ph?searchtype=author&query=Kuznetsov%2C+A">Artem Kuznetsov</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="0907.1036v1-abstract-short" style="display: inline;"> There are the results of gamma-ray bursts observations obtained using the MASTER robotic telescope in 2007 - 2009. We observed 20 error-boxes of gamma-ray bursts this period.The limits on their optical brightnesses have been derived. There are 5 prompt observations among them, obtained at our very wide field cameras. Also we present the results of the earliest observations of the optical emissio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0907.1036v1-abstract-full').style.display = 'inline'; document.getElementById('0907.1036v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0907.1036v1-abstract-full" style="display: none;"> There are the results of gamma-ray bursts observations obtained using the MASTER robotic telescope in 2007 - 2009. We observed 20 error-boxes of gamma-ray bursts this period.The limits on their optical brightnesses have been derived. There are 5 prompt observations among them, obtained at our very wide field cameras. Also we present the results of the earliest observations of the optical emission of the gamma-ray bursts GRB 050824 and GRB 060926. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0907.1036v1-abstract-full').style.display = 'none'; document.getElementById('0907.1036v1-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 July, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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, 2 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/0907.0827">arXiv:0907.0827</a> <span> [<a href="https://arxiv.org/pdf/0907.0827">pdf</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="Instrumentation and Methods for Astrophysics">astro-ph.IM</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/10.1155/2010/349171">10.1155/2010/349171 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Master Robotic Net </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lipunov%2C+V">Vladimir Lipunov</a>, <a href="/search/astro-ph?searchtype=author&query=Kornilov%2C+V">Victor Kornilov</a>, <a href="/search/astro-ph?searchtype=author&query=Gorbovskoy%2C+E">Evgeny Gorbovskoy</a>, <a href="/search/astro-ph?searchtype=author&query=Shatskij%2C+N">Nikolaj Shatskij</a>, <a href="/search/astro-ph?searchtype=author&query=Kuvshinov%2C+D">Dmitry Kuvshinov</a>, <a href="/search/astro-ph?searchtype=author&query=Tyurina%2C+N">Nataly Tyurina</a>, <a href="/search/astro-ph?searchtype=author&query=Belinski%2C+A">Alexander Belinski</a>, <a href="/search/astro-ph?searchtype=author&query=Krylov%2C+A">Alexander Krylov</a>, <a href="/search/astro-ph?searchtype=author&query=Balanutsa%2C+P">Pavel Balanutsa</a>, <a href="/search/astro-ph?searchtype=author&query=Chazov%2C+V">Vadim Chazov</a>, <a href="/search/astro-ph?searchtype=author&query=Kuznetsov%2C+A">Artem Kuznetsov</a>, <a href="/search/astro-ph?searchtype=author&query=Kortunov%2C+P">Petr Kortunov</a>, <a href="/search/astro-ph?searchtype=author&query=Sankovich%2C+A">Anatoly Sankovich</a>, <a href="/search/astro-ph?searchtype=author&query=Tlatov%2C+A">Andrey Tlatov</a>, <a href="/search/astro-ph?searchtype=author&query=Parkhomenko%2C+A">Alexander Parkhomenko</a>, <a href="/search/astro-ph?searchtype=author&query=Krushinsky%2C+V">Vadim Krushinsky</a>, <a href="/search/astro-ph?searchtype=author&query=Zalozhnyh%2C+I">Ivan Zalozhnyh</a>, <a href="/search/astro-ph?searchtype=author&query=Popov%2C+A">Alexander Popov</a>, <a href="/search/astro-ph?searchtype=author&query=Kopytova%2C+T">Taisia Kopytova</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+K">Kirill Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Yazev%2C+S">Sergey Yazev</a>, <a href="/search/astro-ph?searchtype=author&query=Yurkov%2C+V">Vladimir Yurkov</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="0907.0827v1-abstract-short" style="display: inline;"> The main goal of the MASTER-Net project is to produce a unique fast sky survey with all sky observed over a single night down to a limiting magnitude of 19 - 20mag. Such a survey will make it possible to address a number of fundamental problems: search for dark energy via the discovery and photometry of supernovas (including SNIa), search for exoplanets, microlensing effects, discovery of minor… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0907.0827v1-abstract-full').style.display = 'inline'; document.getElementById('0907.0827v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0907.0827v1-abstract-full" style="display: none;"> The main goal of the MASTER-Net project is to produce a unique fast sky survey with all sky observed over a single night down to a limiting magnitude of 19 - 20mag. Such a survey will make it possible to address a number of fundamental problems: search for dark energy via the discovery and photometry of supernovas (including SNIa), search for exoplanets, microlensing effects, discovery of minor bodies in the Solar System and space-junk monitoring. All MASTER telescopes can be guided by alerts, and we plan to observe prompt optical emission from gamma-ray bursts synchronously in several filters and in several polarization planes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0907.0827v1-abstract-full').style.display = 'none'; document.getElementById('0907.0827v1-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 July, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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, 8 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 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