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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Barnacka%2C+A&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Barnacka%2C+A&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Barnacka%2C+A&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Barnacka%2C+A&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> </ul> </nav> <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/2210.00014">arXiv:2210.00014</a> <span> [<a href="https://arxiv.org/pdf/2210.00014">pdf</a>, <a href="https://arxiv.org/format/2210.00014">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Strongly Lensed Supermassive Black Hole Binaries as Nanohertz Gravitational-Wave Sources </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Khusid%2C+N+M">Nicole M. Khusid</a>, <a href="/search/astro-ph?searchtype=author&query=Mingarelli%2C+C+M+F">Chiara M. F. Mingarelli</a>, <a href="/search/astro-ph?searchtype=author&query=Natarajan%2C+P">Priyamvada Natarajan</a>, <a href="/search/astro-ph?searchtype=author&query=Casey-Clyde%2C+J+A">J. Andrew Casey-Clyde</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">Anna Barnacka</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="2210.00014v2-abstract-short" style="display: inline;"> Supermassive black hole binary systems (SMBHBs) should be the most powerful sources of gravitational waves (GWs) in the Universe. Once Pulsar Timing Arrays (PTAs) detect the stochastic GW background from their cosmic merger history, searching for individually resolvable binaries will take on new importance. Since these individual SMBHBs are expected to be rare, here we explore how strong gravitati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.00014v2-abstract-full').style.display = 'inline'; document.getElementById('2210.00014v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.00014v2-abstract-full" style="display: none;"> Supermassive black hole binary systems (SMBHBs) should be the most powerful sources of gravitational waves (GWs) in the Universe. Once Pulsar Timing Arrays (PTAs) detect the stochastic GW background from their cosmic merger history, searching for individually resolvable binaries will take on new importance. Since these individual SMBHBs are expected to be rare, here we explore how strong gravitational lensing can act as a tool for increasing their detection prospects by magnifying fainter sources and bringing them into view. Unlike for electromagnetic waves, when the geometric optics limit is nearly always valid, for GWs the wave-diffraction-interference effects can become important when the wavelength of the GWs is larger than the Schwarzchild radius of the lens, i.e. $M_{\rm lens} \sim 10^8\,(\frac{f}{mHz})^{-1}\,M_\odot$. For the GW frequency range explored in this work, the geometric optics limit holds. We investigate GW signals from SMBHBs that might be detectable with current and future PTAs under the assumption that quasars serve as bright beacons that signal a recent merger. Using the black hole mass function derived from quasars and a physically motivated magnification distribution, we expect to detect a few strongly lensed binary systems out to $z \approx 2$. Additionally, for a range of fixed magnifications $2 \leq 渭\leq 100$, strong lensing adds up to $\sim$30 more detectable binaries for PTAs. Finally, we investigate the possibility of observing both time-delayed electromagnetic signals and GW signals from these strongly lensed binary systems -- that will provide us with unprecedented multimessenger insights into their orbital evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.00014v2-abstract-full').style.display = 'none'; document.getElementById('2210.00014v2-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 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 7 figures (now 16 pages, 8 figures); updated method/results & pre-publication revisions, references added</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.04245">arXiv:2203.04245</a> <span> [<a href="https://arxiv.org/pdf/2203.04245">pdf</a>, <a href="https://arxiv.org/format/2203.04245">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/10.3847/1538-4357/ac68eb">10.3847/1538-4357/ac68eb <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Milliarcsecond X-ray astrometry to resolve inner regions of AGN at $z>1$ using gravitational lensing </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Spingola%2C+C">C. Spingola</a>, <a href="/search/astro-ph?searchtype=author&query=Schwartz%2C+D">D. Schwartz</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.04245v2-abstract-short" style="display: inline;"> We report the localization of the X-ray emission from two strongly lensed AGN, CLASS B0712+472 ($z=1.34$) and CLASS B1608+656 ($z=1.394$). We obtain milliarcsecond X-ray astrometry by developing a novel method that combines parametric lens modelling with a Bayesian analysis. We spatially locate the X-ray sources in CLASS B0712+472 and CLASS B1608+656 within 11 mas and 9 mas from the radio source,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.04245v2-abstract-full').style.display = 'inline'; document.getElementById('2203.04245v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.04245v2-abstract-full" style="display: none;"> We report the localization of the X-ray emission from two strongly lensed AGN, CLASS B0712+472 ($z=1.34$) and CLASS B1608+656 ($z=1.394$). We obtain milliarcsecond X-ray astrometry by developing a novel method that combines parametric lens modelling with a Bayesian analysis. We spatially locate the X-ray sources in CLASS B0712+472 and CLASS B1608+656 within 11 mas and 9 mas from the radio source, respectively. For CLASS B0712+472, we find that the X-ray emission is co-spatial with the radio and optical emission. While, in CLASS B1608+656, the X-ray emission is co-spatial with radio, but displaced with respect to the optical emission at 1$蟽$ level, which positions this source as an offset AGN candidate. This high astrometric precision improves on the limitations of existing X-ray instruments by two orders of magnitude. The demonstrated method opens a path to search for offset and binary AGN at $z>1$, and to directly test supermassive black hole formation models in a redshift range that has been mostly underconstrained to date. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.04245v2-abstract-full').style.display = 'none'; document.getElementById('2203.04245v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 7 figures. Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.12926">arXiv:2111.12926</a> <span> [<a href="https://arxiv.org/pdf/2111.12926">pdf</a>, <a href="https://arxiv.org/ps/2111.12926">ps</a>, <a href="https://arxiv.org/format/2111.12926">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stab3454">10.1093/mnras/stab3454 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multiwavelength study of the gravitationally lensed blazar QSO B0218+357 between 2016 and 2020 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=MAGIC+Collaboration"> MAGIC Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/astro-ph?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Engels%2C+A+A">A. Arbet Engels</a>, <a href="/search/astro-ph?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Baack%2C+D">D. Baack</a>, <a href="/search/astro-ph?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Baquero%2C+A">A. Baquero</a>, <a href="/search/astro-ph?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/astro-ph?searchtype=author&query=Batkovi%C4%87%2C+I">I. Batkovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Bednarek%2C+W">W. Bednarek</a>, <a href="/search/astro-ph?searchtype=author&query=Bellizzi%2C+L">L. Bellizzi</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardos%2C+M">M. Bernardos</a>, <a href="/search/astro-ph?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/astro-ph?searchtype=author&query=Besenrieder%2C+J">J. Besenrieder</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharyya%2C+W">W. Bhattacharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Bigongiari%2C+C">C. Bigongiari</a>, <a href="/search/astro-ph?searchtype=author&query=Biland%2C+A">A. Biland</a>, <a href="/search/astro-ph?searchtype=author&query=Blanch%2C+O">O. Blanch</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnoli%2C+G">G. Bonnoli</a> , et al. (186 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.12926v1-abstract-short" style="display: inline;"> We report multiwavelength observations of the gravitationally lensed blazar QSO B0218+357 in 2016-2020. Optical, X-ray and GeV flares were detected. The contemporaneous MAGIC observations do not show significant very-high-energy (VHE, >= 100 GeV) gamma-ray emission. The lack of enhancement in radio emission measured by OVRO indicates the multi-zone nature of the emission from this object. We const… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.12926v1-abstract-full').style.display = 'inline'; document.getElementById('2111.12926v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.12926v1-abstract-full" style="display: none;"> We report multiwavelength observations of the gravitationally lensed blazar QSO B0218+357 in 2016-2020. Optical, X-ray and GeV flares were detected. The contemporaneous MAGIC observations do not show significant very-high-energy (VHE, >= 100 GeV) gamma-ray emission. The lack of enhancement in radio emission measured by OVRO indicates the multi-zone nature of the emission from this object. We constrain the VHE duty cycle of the source to be < 16 2014-like flares per year (95% confidence). For the first time for this source, a broadband low-state SED is constructed with a deep exposure up to the VHE range. A flux upper limit on the low-state VHE gamma-ray emission of an order of magnitude below that of the 2014 flare is determined. The X-ray data are used to fit the column density of (8.10 +- 0.93 stat ) x 10^21 cm^-2 of the dust in the lensing galaxy. VLBI observations show a clear radio core and jet components in both lensed images, yet no significant movement of the components is seen. The radio measurements are used to model the source-lens-observer geometry and determine the magnifications and time delays for both components. The quiescent emission is modeled with the high-energy bump explained as a combination of synchrotron-self-Compton and external Compton emission from a region located outside of the broad line region. The bulk of the low-energy emission is explained as originating from a tens-of-parsecs scale jet. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.12926v1-abstract-full').style.display = 'none'; document.getElementById('2111.12926v1-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> 25 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">21 pages, 12 figures, 5 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/2110.00636">arXiv:2110.00636</a> <span> [<a href="https://arxiv.org/pdf/2110.00636">pdf</a>, <a href="https://arxiv.org/format/2110.00636">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac0fe1">10.3847/1538-4357/ac0fe1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searching for TeV gamma-ray emission from SGR\,1935+2154 during its 2020 X-ray and radio bursting phase </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abdalla%2C+H">H. Abdalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%7Funer%2C+E+O">E. O. Anguner</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Armand%2C+C">C. Armand</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baghmanyan%2C+V">V. Baghmanyan</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Barnard%2C+M">M. Barnard</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%7Fohr%2C+K">K. Bernlohr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%7Fottcher%2C+M">M. Bottcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a> , et al. (230 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="2110.00636v1-abstract-short" style="display: inline;"> Magnetar hyperflares are the most plausible explanation for fast radio bursts (FRB) -- enigmatic powerful radio pulses with durations of several milliseconds and high brightness temperatures. The first observational evidence for this scenario was obtained in 2020 April when a FRB was detected from the direction of the Galactic magnetar and soft gamma-ray repeater SGR\,1935+2154. The FRB was preced… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.00636v1-abstract-full').style.display = 'inline'; document.getElementById('2110.00636v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.00636v1-abstract-full" style="display: none;"> Magnetar hyperflares are the most plausible explanation for fast radio bursts (FRB) -- enigmatic powerful radio pulses with durations of several milliseconds and high brightness temperatures. The first observational evidence for this scenario was obtained in 2020 April when a FRB was detected from the direction of the Galactic magnetar and soft gamma-ray repeater SGR\,1935+2154. The FRB was preceded by two gamma-ray outburst alerts by the BAT instrument aboard the Swift satellite, which triggered follow-up observations by the High Energy Stereoscopic System (H.E.S.S.). H.E.S.S. has observed SGR\,1935+2154 for 2 hr on 2020 April 28. The observations are coincident with X-ray bursts from the magnetar detected by INTEGRAL and Fermi-GBM, thus providing the first very high energy (VHE) gamma-ray observations of a magnetar in a flaring state. High-quality data acquired during these follow-up observations allow us to perform a search for short-time transients. No significant signal at energies $E>0.6$~TeV is found and upper limits on the persistent and transient emission are derived. We here present the analysis of these observations and discuss the obtained results and prospects of the H.E.S.S. follow-up program for soft gamma-ray repeaters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.00636v1-abstract-full').style.display = 'none'; document.getElementById('2110.00636v1-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> 1 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">Received 2021 June 13; accepted 2021 June 28; published 2021 September 29</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.02015">arXiv:2108.02015</a> <span> [<a href="https://arxiv.org/pdf/2108.02015">pdf</a>, <a href="https://arxiv.org/format/2108.02015">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/10.1051/0004-6361/202141486">10.1051/0004-6361/202141486 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> LMC N132D: A mature supernova remnant with a power-law gamma-ray spectrum extending beyond 8 TeV </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abdalla%2C+H">H. Abdalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Armand%2C+C">C. Armand</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baghmanyan%2C+V">V. Baghmanyan</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Barnard%2C+M">M. Barnard</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a> , et al. (212 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="2108.02015v1-abstract-short" style="display: inline;"> We analyzed 252 hours of High Energy Stereoscopic System (H.E.S.S.) observations towards the supernova remnant (SNR) LMC N132D that were accumulated between December 2004 and March 2016 during a deep survey of the Large Magellanic Cloud, adding 104 hours of observations to the previously published data set to ensure a > 5 sigma detection. To broaden the gamma-ray spectral coverage required for mod… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.02015v1-abstract-full').style.display = 'inline'; document.getElementById('2108.02015v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.02015v1-abstract-full" style="display: none;"> We analyzed 252 hours of High Energy Stereoscopic System (H.E.S.S.) observations towards the supernova remnant (SNR) LMC N132D that were accumulated between December 2004 and March 2016 during a deep survey of the Large Magellanic Cloud, adding 104 hours of observations to the previously published data set to ensure a > 5 sigma detection. To broaden the gamma-ray spectral coverage required for modeling the spectral energy distribution, an analysis of Fermi-LAT Pass 8 data was also included. We unambiguously detect N132D at very high energies (VHE) with a significance of 5.7 sigma. We report the results of a detailed analysis of its spectrum and localization based on the extended H.E.S.S. data set. The joint analysis of the extended H.E.S.S and Fermi-LAT data results in a spectral energy distribution in the energy range from 1.7 GeV to 14.8 TeV, which suggests a high luminosity of N132D at GeV and TeV energies. We set a lower limit on a gamma-ray cutoff energy of 8 TeV with a confidence level of 95%. The new gamma-ray spectrum as well as multiwavelength observations of N132D when compared to physical models suggests a hadronic origin of the VHE gamma-ray emission. SNR N132D is a VHE gamma-ray source that shows a spectrum extending to the VHE domain without a spectral cutoff at a few TeV, unlike the younger oxygen-rich SNR Cassiopeia A. The gamma-ray properties of N132D may be affected by an interaction with a nearby molecular cloud that partially lies inside the 95% confidence region of the source position. [Abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.02015v1-abstract-full').style.display = 'none'; document.getElementById('2108.02015v1-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 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">Accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 655, A7 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.01425">arXiv:2107.01425</a> <span> [<a href="https://arxiv.org/pdf/2107.01425">pdf</a>, <a href="https://arxiv.org/format/2107.01425">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/10.3847/1538-4357/abf64b">10.3847/1538-4357/abf64b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> TeV emission of Galactic plane sources with HAWC and H.E.S.S </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abdalla%2C+H">H. Abdalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Armand%2C+C">C. Armand</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baghmanyan%2C+V">V. Baghmanyan</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Barnard%2C+M">M. Barnard</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+P">P. Brun</a> , et al. (299 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="2107.01425v3-abstract-short" style="display: inline;"> The High Altitude Water Cherenkov (HAWC) observatory and the High Energy Stereoscopic System (H.E.S.S.) are two leading instruments in the ground-based very-high-energy gamma-ray domain. HAWC employs the water Cherenkov detection (WCD) technique, while H.E.S.S. is an array of Imaging Atmospheric Cherenkov Telescopes (IACTs). The two facilities therefore differ in multiple aspects, including their… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.01425v3-abstract-full').style.display = 'inline'; document.getElementById('2107.01425v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.01425v3-abstract-full" style="display: none;"> The High Altitude Water Cherenkov (HAWC) observatory and the High Energy Stereoscopic System (H.E.S.S.) are two leading instruments in the ground-based very-high-energy gamma-ray domain. HAWC employs the water Cherenkov detection (WCD) technique, while H.E.S.S. is an array of Imaging Atmospheric Cherenkov Telescopes (IACTs). The two facilities therefore differ in multiple aspects, including their observation strategy, the size of their field of view and their angular resolution, leading to different analysis approaches. Until now, it has been unclear if the results of observations by both types of instruments are consistent: several of the recently discovered HAWC sources have been followed up by IACTs, resulting in a confirmed detection only in a minority of cases. With this paper, we go further and try to resolve the tensions between previous results by performing a new analysis of the H.E.S.S. Galactic plane survey data, applying an analysis technique comparable between H.E.S.S. and HAWC. Events above 1 TeV are selected for both datasets, the point spread function of H.E.S.S. is broadened to approach that of HAWC, and a similar background estimation method is used. This is the first detailed comparison of the Galactic plane observed by both instruments. H.E.S.S. can confirm the gamma-ray emission of four HAWC sources among seven previously undetected by IACTs, while the three others have measured fluxes below the sensitivity of the H.E.S.S. dataset. Remaining differences in the overall gamma-ray flux can be explained by the systematic uncertainties. Therefore, we confirm a consistent view of the gamma-ray sky between WCD and IACT techniques. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.01425v3-abstract-full').style.display = 'none'; document.getElementById('2107.01425v3-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 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.06405">arXiv:2106.06405</a> <span> [<a href="https://arxiv.org/pdf/2106.06405">pdf</a>, <a href="https://arxiv.org/format/2106.06405">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/10.1051/0004-6361/202140962">10.1051/0004-6361/202140962 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Evidence of 100 TeV $纬$-ray emission from HESS J1702-420: A new PeVatron candidate </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abdalla%2C+H">H. Abdalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Armand%2C+C">C. Armand</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baghmanyan%2C+V">V. Baghmanyan</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Barnard%2C+M">M. Barnard</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+P">P. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bryan%2C+M">M. Bryan</a> , et al. (211 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="2106.06405v2-abstract-short" style="display: inline;"> The identification of PeVatrons, hadronic particle accelerators reaching the knee of the cosmic ray spectrum (few $10^{15}$ eV), is crucial to understand the origin of cosmic rays in the Galaxy. We provide an update on the unidentified source HESS J1702-420, a promising PeVatron candidate. We present new observations of HESS J1702-420 made with the High Energy Stereoscopic System (H.E.S.S.), and p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.06405v2-abstract-full').style.display = 'inline'; document.getElementById('2106.06405v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.06405v2-abstract-full" style="display: none;"> The identification of PeVatrons, hadronic particle accelerators reaching the knee of the cosmic ray spectrum (few $10^{15}$ eV), is crucial to understand the origin of cosmic rays in the Galaxy. We provide an update on the unidentified source HESS J1702-420, a promising PeVatron candidate. We present new observations of HESS J1702-420 made with the High Energy Stereoscopic System (H.E.S.S.), and processed using improved analysis techniques. The analysis configuration was optimized to enhance the collection area at the highest energies. We applied a three-dimensional (3D) likelihood analysis to model the source region and adjust non thermal radiative spectral models to the $纬$-ray data. We also analyzed archival data from the Fermi Large Area Telescope (LAT) to constrain the source spectrum at $纬$-ray energies >10 GeV. We report the detection of a new source component called HESS J1702-420A, that was separated from the bulk of TeV emission at a $5.4蟽$ confidence level. The power law $纬$-ray spectrum of HESS J1702-420A extends with an index of $螕=1.53\pm0.19_\text{stat}\pm0.20_\text{sys}$ and without curvature up to the energy band 64-113 TeV, in which it was detected by H.E.S.S. at a $4.0蟽$ confidence level. This brings evidence for the source emission up to $100\,\text{TeV}$, which makes HESS J1702-420A a compelling candidate site for the presence of extremely high energy cosmic rays. Remarkably, in a hadronic scenario, the cut-off energy of the proton distribution powering HESS J1702-420A is found to be higher than 0.5 PeV at a 95% confidence level. HESS J1702-420A becomes therefore one of the most solid PeVatron candidates detected so far in H.E.S.S. data, altough a leptonic origin of its emission could not be ruled out either. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.06405v2-abstract-full').style.display = 'none'; document.getElementById('2106.06405v2-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">Accepted for publication in the 2. Astrophysical processes section of Astronomy & Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.00551">arXiv:2106.00551</a> <span> [<a href="https://arxiv.org/pdf/2106.00551">pdf</a>, <a href="https://arxiv.org/format/2106.00551">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/abff59">10.3847/1538-4357/abff59 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for dark matter annihilation signals from unidentified Fermi-LAT objects with H.E.S.S </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abdallah%2C+H">H. Abdallah</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Armand%2C+C">C. Armand</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baghmanyan%2C+V">V. Baghmanyan</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Barnard%2C+M">M. Barnard</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a> , et al. (205 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="2106.00551v2-abstract-short" style="display: inline;"> Cosmological $N$-body simulations show that Milky Way-sized galaxies harbor a population of unmerged dark matter subhalos. These subhalos could shine in gamma-rays and be eventually detected in gamma-ray surveys as unidentified sources. We performed a thorough selection among unidentified Fermi-LAT Objects (UFOs) to identify them as possible TeV-scale dark matter subhalo candidates. We search for… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.00551v2-abstract-full').style.display = 'inline'; document.getElementById('2106.00551v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.00551v2-abstract-full" style="display: none;"> Cosmological $N$-body simulations show that Milky Way-sized galaxies harbor a population of unmerged dark matter subhalos. These subhalos could shine in gamma-rays and be eventually detected in gamma-ray surveys as unidentified sources. We performed a thorough selection among unidentified Fermi-LAT Objects (UFOs) to identify them as possible TeV-scale dark matter subhalo candidates. We search for very-high-energy (E $\gtrsim$ 100 GeV) gamma-ray emissions using H.E.S.S. observations towards four selected UFOs. Since no significant very-high-energy gamma-ray emission is detected in any dataset of the four observed UFOs nor in the combined UFO dataset, strong constraints are derived on the product of the velocity-weighted annihilation cross section $\langle 蟽v \rangle$ by the $J$-factor for the dark matter models. The 95% C.L. observed upper limits derived from combined H.E.S.S. observations reach $\langle 蟽v \rangle J$ values of 3.7$\times$10$^{-5}$ and 8.1$\times$10$^{-6}$ GeV$^2$cm$^{-2}$s$^{-1}$ in the $W^+W^-$ and $蟿^+蟿^-$ channels, respectively, for a 1 TeV dark matter mass. Focusing on thermal WIMPs, the H.E.S.S. constraints restrict the $J$-factors to lie in the range 6.1$\times$10$^{19}$ - 2.0$\times$10$^{21}$ GeV$^2$cm$^{-5}$, and the masses to lie between 0.2 and 6 TeV in the $W^+W^-$ channel. For the $蟿^+蟿^-$ channel, the $J$-factors lie in the range 7.0$\times$10$^{19}$ - 7.1$\times$10$^{20}$ GeV$^2$cm$^{-5}$ and the masses lie between 0.2 and 0.5 TeV. Assuming model-dependent predictions from cosmological N-body simulations on the $J$-factor distribution for Milky Way-sized galaxies, the dark matter models with masses greater than 0.3 TeV for the UFO emissions can be ruled out at high confidence level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.00551v2-abstract-full').style.display = 'none'; document.getElementById('2106.00551v2-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">11 pages, 7 figures, matches accepted version in The Astrophysical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J., 918, 17 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.04325">arXiv:2105.04325</a> <span> [<a href="https://arxiv.org/pdf/2105.04325">pdf</a>, <a href="https://arxiv.org/format/2105.04325">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="High Energy Physics - Experiment">hep-ex</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/10.1103/PhysRevD.103.102002">10.1103/PhysRevD.103.102002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for dark matter annihilation in the dwarf irregular galaxy WLM with H.E.S.S </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abdallah%2C+H">H. Abdallah</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Armand%2C+C">C. Armand</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baghmanyan%2C+V">V. Baghmanyan</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Barnard%2C+M">M. Barnard</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a> , et al. (211 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="2105.04325v1-abstract-short" style="display: inline;"> We search for an indirect signal of dark matter through very high-energy gamma rays from the Wolf-Lundmark-Melotte (WLM) dwarf irregular galaxy. The pair annihilation of dark matter particles would produce Standard Model particles in the final state such as gamma rays, which might be detected by ground-based Cherenkov telescopes. Dwarf irregular galaxies represent promising targets as they are dar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.04325v1-abstract-full').style.display = 'inline'; document.getElementById('2105.04325v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.04325v1-abstract-full" style="display: none;"> We search for an indirect signal of dark matter through very high-energy gamma rays from the Wolf-Lundmark-Melotte (WLM) dwarf irregular galaxy. The pair annihilation of dark matter particles would produce Standard Model particles in the final state such as gamma rays, which might be detected by ground-based Cherenkov telescopes. Dwarf irregular galaxies represent promising targets as they are dark matter dominated objects with well measured kinematics and small uncertainties on their dark matter distribution profiles. In 2018, the H.E.S.S. five-telescope array observed the dwarf irregular galaxy WLM for 18 hours. We present the first analysis based on data obtained from an imaging atmospheric Cherenkov telescope for this subclass of dwarf galaxy. As we do not observe any significant excess in the direction of WLM, we interpret the result in terms of constraints on the velocity-weighted cross section for dark matter pair annihilation as a function of the dark matter particle mass for various continuum channels as well as the prompt gamma-gamma emission. For the $蟿^+蟿^-$ channel the limits reach a $\langle 蟽v \rangle$ value of about $4\times 10^{-22}$ cm3s-1 for a dark matter particle mass of 1 TeV. For the prompt gamma-gamma channel, the upper limit reaches a $\langle 蟽v \rangle$ value of about $5 \times10^{-24}$ cm3s-1 for a mass of 370 GeV. These limits represent an improvement of up to a factor 200 with respect to previous results for the dwarf irregular galaxies for TeV dark matter search. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.04325v1-abstract-full').style.display = 'none'; document.getElementById('2105.04325v1-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> 10 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 103, 102002 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.08537">arXiv:2103.08537</a> <span> [<a href="https://arxiv.org/pdf/2103.08537">pdf</a>, <a href="https://arxiv.org/format/2103.08537">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac0909">10.3847/1538-4357/ac0909 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Resolving Complex Inner X-ray Structure of the Gravitationaly Lensed AGN MGB2016+112 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Schwartz%2C+D">Daniel Schwartz</a>, <a href="/search/astro-ph?searchtype=author&query=Spingola%2C+C">Cristiana Spingola</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">Anna Barnacka</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="2103.08537v1-abstract-short" style="display: inline;"> We use a Chandra X-ray observation of the gravitationally lensed system MGB2016+112 at z=3.273 to elucidate presence of at least two X-ray sources. We find that these sources are consistent with the VLBI components measured by \citet{Spingola19}, which are separated by $\sim 200$ pc. Their intrinsic 0.5 -- 7 keV source frame luminosities are 2.6$\times$10$^{43}$ and 4.2$\times$10$^{44}$ erg s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.08537v1-abstract-full').style.display = 'inline'; document.getElementById('2103.08537v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.08537v1-abstract-full" style="display: none;"> We use a Chandra X-ray observation of the gravitationally lensed system MGB2016+112 at z=3.273 to elucidate presence of at least two X-ray sources. We find that these sources are consistent with the VLBI components measured by \citet{Spingola19}, which are separated by $\sim 200$ pc. Their intrinsic 0.5 -- 7 keV source frame luminosities are 2.6$\times$10$^{43}$ and 4.2$\times$10$^{44}$ erg s$^{-1}$. Most likely this system contains a dual active galactic nucleus (AGN), but we possibly are detecting an AGN plus a pc-scale X-ray jet, the latter lying in a region at very high magnification. The quadruply lensed X-ray source is within $\pm$40 pc (1$蟽$) of its VLBI counterpart. Using a gravitational lens as a telescope, and a novel statistical application, we have achieved unprecedented accuracy for measuring metric distances at such large redshifts in X-ray astronomy, which is tens of mas if the source is located close to the caustics, while it is of hundreds of mas if the source is in a region at lower amplification. The present demonstration of this approach has implications for future X-ray investigations of large numbers of lensed systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.08537v1-abstract-full').style.display = 'none'; document.getElementById('2103.08537v1-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 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">9 pages, 5 figures, submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.10254">arXiv:2012.10254</a> <span> [<a href="https://arxiv.org/pdf/2012.10254">pdf</a>, <a href="https://arxiv.org/format/2012.10254">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202038949">10.1051/0004-6361/202038949 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observation of a sudden cessation of a very-high-energy gamma-ray flare in PKS 1510-089 with H.E.S.S. and MAGIC in May 2016 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abdalla%2C+H">H. Abdalla</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Arm%2C+C">C. Arm</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baghmanyan%2C+V">V. Baghmanyan</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Barnard%2C+M">M. Barnard</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnefoy%2C+S">S. Bonnefoy</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Bregeon%2C+J">J. Bregeon</a> , et al. (409 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="2012.10254v1-abstract-short" style="display: inline;"> The flat spectrum radio quasar (FSRQ) PKS 1510-089 is known for its complex multiwavelength behavior, and is one of only a few FSRQs detected at very high energy (VHE, $E>100\,$GeV) $纬$-rays. VHE $纬$-ray observations with H.E.S.S. and MAGIC during late May and early June 2016 resulted in the detection of an unprecedented flare, which reveals for the first time VHE $纬$-ray intranight variability in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.10254v1-abstract-full').style.display = 'inline'; document.getElementById('2012.10254v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.10254v1-abstract-full" style="display: none;"> The flat spectrum radio quasar (FSRQ) PKS 1510-089 is known for its complex multiwavelength behavior, and is one of only a few FSRQs detected at very high energy (VHE, $E>100\,$GeV) $纬$-rays. VHE $纬$-ray observations with H.E.S.S. and MAGIC during late May and early June 2016 resulted in the detection of an unprecedented flare, which reveals for the first time VHE $纬$-ray intranight variability in this source. While a common variability timescale of $1.5\,$hr is found, there is a significant deviation near the end of the flare with a timescale of $\sim 20\,$min marking the cessation of the event. The peak flux is nearly two orders of magnitude above the low-level emission. For the first time, curvature is detected in the VHE $纬$-ray spectrum of PKS 1510-089, which is fully explained through absorption by the extragalactic background light. Optical R-band observations with ATOM reveal a counterpart of the $纬$-ray flare, even though the detailed flux evolution differs from the VHE ightcurve. Interestingly, a steep flux decrease is observed at the same time as the cessation of the VHE flare. In the high energy (HE, $E>100\,$MeV) $纬$-ray band only a moderate flux increase is observed with Fermi-LAT, while the HE $纬$-ray spectrum significantly hardens up to a photon index of 1.6. A search for broad-line region (BLR) absorption features in the $纬$-ray spectrum indicates that the emission region is located outside of the BLR. Radio VLBI observations reveal a fast moving knot interacting with a standing jet feature around the time of the flare. As the standing feature is located $\sim 50\,$pc from the black hole, the emission region of the flare may have been located at a significant distance from the black hole. If this correlation is indeed true, VHE $纬$ rays have been produced far down the jet where turbulent plasma crosses a standing shock. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.10254v1-abstract-full').style.display = 'none'; document.getElementById('2012.10254v1-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 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">25 pages, 17 figures. Accepted for publication by Astronomy & Astrophysics. Corresponding authors: M. Zacharias, J. Sitarek, D. Sanchez, T. Terzic</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 648, A23 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.13101">arXiv:2010.13101</a> <span> [<a href="https://arxiv.org/pdf/2010.13101">pdf</a>, <a href="https://arxiv.org/format/2010.13101">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/10.1051/0004-6361/202038851">10.1051/0004-6361/202038851 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An extreme particle accelerator in the Galactic plane: HESS J1826$-$130 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abdalla%2C+H">H. Abdalla</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Armand%2C+C">C. Armand</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baghmanyan%2C+V">V. Baghmanyan</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Barnard%2C+M">M. Barnard</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Bordas%2C+P">P. Bordas</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a> , et al. (215 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="2010.13101v1-abstract-short" style="display: inline;"> The unidentified very-high-energy (VHE; E $>$ 0.1 TeV) $纬$-ray source, HESS J1826$-$130, was discovered with the High Energy Stereoscopic System (HESS) in the Galactic plane. The analysis of 215 h of HESS data has revealed a steady $纬$-ray flux from HESS J1826$-$130, which appears extended with a half-width of 0.21$^{\circ}$ $\pm$ 0.02$^{\circ}_{\text{stat}}$ $\pm$ 0.05$^{\circ}_{\text{sys}}$. The… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.13101v1-abstract-full').style.display = 'inline'; document.getElementById('2010.13101v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.13101v1-abstract-full" style="display: none;"> The unidentified very-high-energy (VHE; E $>$ 0.1 TeV) $纬$-ray source, HESS J1826$-$130, was discovered with the High Energy Stereoscopic System (HESS) in the Galactic plane. The analysis of 215 h of HESS data has revealed a steady $纬$-ray flux from HESS J1826$-$130, which appears extended with a half-width of 0.21$^{\circ}$ $\pm$ 0.02$^{\circ}_{\text{stat}}$ $\pm$ 0.05$^{\circ}_{\text{sys}}$. The source spectrum is best fit with either a power-law function with a spectral index $螕$ = 1.78 $\pm$ 0.10$_{\text{stat}}$ $\pm$ 0.20$_{\text{sys}}$ and an exponential cut-off at 15.2$^{+5.5}_{-3.2}$ TeV, or a broken power-law with $螕_{1}$ = 1.96 $\pm$ 0.06$_{\text{stat}}$ $\pm$ 0.20$_{\text{sys}}$, $螕_{2}$ = 3.59 $\pm$ 0.69$_{\text{stat}}$ $\pm$ 0.20$_{\text{sys}}$ for energies below and above $E_{\rm{br}}$ = 11.2 $\pm$ 2.7 TeV, respectively. The VHE flux from HESS J1826$-$130 is contaminated by the extended emission of the bright, nearby pulsar wind nebula (PWN), HESS J1825$-$137, particularly at the low end of the energy spectrum. Leptonic scenarios for the origin of HESS J1826$-$130 VHE emission related to PSR J1826$-$1256 are confronted by our spectral and morphological analysis. In a hadronic framework, taking into account the properties of dense gas regions surrounding HESS J1826$-$130, the source spectrum would imply an astrophysical object capable of accelerating the parent particle population up to $\gtrsim$200 TeV. Our results are also discussed in a multiwavelength context, accounting for both the presence of nearby supernova remnants (SNRs), molecular clouds, and counterparts detected in radio, X-rays, and TeV energies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.13101v1-abstract-full').style.display = 'none'; document.getElementById('2010.13101v1-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> 25 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">9 Pages, 5 Figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 644, A112 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.00688">arXiv:2008.00688</a> <span> [<a href="https://arxiv.org/pdf/2008.00688">pdf</a>, <a href="https://arxiv.org/format/2008.00688">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/10.1103/PhysRevD.102.062001">10.1103/PhysRevD.102.062001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for dark matter signals towards a selection of recently-detected DES dwarf galaxy satellites of the Milky Way with H.E.S.S </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abdallah%2C+H">H. Abdallah</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Arakawa%2C+M">M. Arakawa</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Armand%2C+C">C. Armand</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baghmanyan%2C+V">V. Baghmanyan</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Barnard%2C+M">M. Barnard</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnefoy%2C+S">S. Bonnefoy</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a> , et al. (206 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="2008.00688v2-abstract-short" style="display: inline;"> Dwarf spheroidal galaxy satellites of the Milky Way are prime targets for indirect detection of dark matter with gamma rays due to their proximity, high dark matter content and absence of non-thermal emission processes. Recently, the Dark Energy Survey (DES) revealed the existence of new ultra-faint dwarf spheroidal galaxies in the southern-hemisphere sky, therefore ideally located for ground-base… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.00688v2-abstract-full').style.display = 'inline'; document.getElementById('2008.00688v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.00688v2-abstract-full" style="display: none;"> Dwarf spheroidal galaxy satellites of the Milky Way are prime targets for indirect detection of dark matter with gamma rays due to their proximity, high dark matter content and absence of non-thermal emission processes. Recently, the Dark Energy Survey (DES) revealed the existence of new ultra-faint dwarf spheroidal galaxies in the southern-hemisphere sky, therefore ideally located for ground-based observations with the imaging atmospheric Cherenkov telescope array H.E.S.S. We present a search for very-high-energy ($E\gtrsim100$ GeV) gamma-ray emission using H.E.S.S. observations carried out recently towards Reticulum II, Tucana II, Tucana III, Tucana IV and Grus II satellites. No significant very-high-energy gamma-ray excess is found from the observations on any individual object nor in the combined analysis of all the datasets. Using the most recent modeling of the dark matter distribution in the dwarf galaxy halo, we compute for the first time on DES satellites individual and combined constraints from Cherenkov telescope observations on the annihilation cross section of dark matter particles in the form of Weakly Interacting Massive Particles. The combined 95% C.L. observed upper limits reach $\langle 蟽v \rangle \simeq 1 \times 10^{-23}$ cm$^3$s$^{-1}$ in the $W^+W^-$ channel and $4 \times 10^{-26}$ cm$^3$s$^{-1}$ in the $纬纬$ channels for a dark matter mass of 1.5 TeV. The H.E.S.S. constraints well complement the results from Fermi-LAT, HAWC, MAGIC and VERITAS and are currently the most stringent in the $纬纬$ channels in the multi-GeV/multi-TeV mass range. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.00688v2-abstract-full').style.display = 'none'; document.getElementById('2008.00688v2-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 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">20 pages, 12 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 102, 062001 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2004.10105">arXiv:2004.10105</a> <span> [<a href="https://arxiv.org/pdf/2004.10105">pdf</a>, <a href="https://arxiv.org/format/2004.10105">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ab8b59">10.3847/2041-8213/ab8b59 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Probing the magnetic field in the GW170817 outflow using H.E.S.S. observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abdalla%2C+H">H. Abdalla</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Arakawa%2C+M">M. Arakawa</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Armand%2C+C">C. Armand</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baghmanyan%2C+V">V. Baghmanyan</a>, <a href="/search/astro-ph?searchtype=author&query=Barbosa-Martins%2C+V">V. Barbosa-Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Barnard%2C+M">M. Barnard</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Blackwell%2C+R">R. Blackwell</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnefoy%2C+S">S. Bonnefoy</a> , et al. (209 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="2004.10105v2-abstract-short" style="display: inline;"> The detection of the first electromagnetic counterpart to the binary neutron star (BNS) merger remnant GW170817 established the connection between short $纬$-ray bursts and BNS mergers. It also confirmed the forging of heavy elements in the ejecta (a so-called kilonova) via the r-process nucleosynthesis. The appearance of non-thermal radio and X-ray emission, as well as the brightening, which laste… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.10105v2-abstract-full').style.display = 'inline'; document.getElementById('2004.10105v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.10105v2-abstract-full" style="display: none;"> The detection of the first electromagnetic counterpart to the binary neutron star (BNS) merger remnant GW170817 established the connection between short $纬$-ray bursts and BNS mergers. It also confirmed the forging of heavy elements in the ejecta (a so-called kilonova) via the r-process nucleosynthesis. The appearance of non-thermal radio and X-ray emission, as well as the brightening, which lasted more than 100 days, were somewhat unexpected. Current theoretical models attempt to explain this temporal behavior as either originating from a relativistic off-axis jet or a kilonova-like outflow. In either scenario, there is some ambiguity regarding how much energy is transported in the non-thermal electrons versus the magnetic field of the emission region. Combining the VLA (radio) and Chandra (X-ray) measurements with observations in the GeV-TeV domain can help break this ambiguity, almost independently of the assumed origin of the emission. Here we report for the first time on deep H.E.S.S. observations of GW170817 / GRB 170817A between 124 and 272 days after the BNS merger with the full H.E.S.S. array of telescopes, as well as on an updated analysis of the prompt (<5 days) observations with the upgraded H.E.S.S. phase-I telescopes. We discuss implications of the H.E.S.S. measurement for the magnetic field in the context of different source scenarios. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.10105v2-abstract-full').style.display = 'none'; document.getElementById('2004.10105v2-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 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">7 pages, 2 figures, 1 table</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, 894, L16, 2020 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2004.03306">arXiv:2004.03306</a> <span> [<a href="https://arxiv.org/pdf/2004.03306">pdf</a>, <a href="https://arxiv.org/ps/2004.03306">ps</a>, <a href="https://arxiv.org/format/2004.03306">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/staa999">10.1093/mnras/staa999 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Very high energy $纬$-ray emission from two blazars of unknown redshift and upper limits on their distance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abdalla%2C+H">H. Abdalla</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Arakawa%2C+M">M. Arakawa</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Armand%2C+C">C. Armand</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baghmanyan%2C+V">V. Baghmanyan</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Barnard%2C+M">M. Barnard</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnefoy%2C+S">S. Bonnefoy</a>, <a href="/search/astro-ph?searchtype=author&query=Bregeon%2C+J">J. Bregeon</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a> , et al. (204 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="2004.03306v2-abstract-short" style="display: inline;"> We report on the detection of very-high-energy (VHE; $E > 100$ GeV) $纬$-ray emission from the BL Lac objects KUV 00311-1938 and PKS 1440-389 with the High Energy Stereoscopic System (H.E.S.S.). H.E.S.S. observations were accompanied or preceded by multi-wavelength observations with Fermi/LAT, XRT and UVOT on board the Swift satellite, and ATOM. Based on an extrapolation of the Fermi/LAT spectrum t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.03306v2-abstract-full').style.display = 'inline'; document.getElementById('2004.03306v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.03306v2-abstract-full" style="display: none;"> We report on the detection of very-high-energy (VHE; $E > 100$ GeV) $纬$-ray emission from the BL Lac objects KUV 00311-1938 and PKS 1440-389 with the High Energy Stereoscopic System (H.E.S.S.). H.E.S.S. observations were accompanied or preceded by multi-wavelength observations with Fermi/LAT, XRT and UVOT on board the Swift satellite, and ATOM. Based on an extrapolation of the Fermi/LAT spectrum towards the VHE $纬$-ray regime, we deduce a 95% confidence level upper limit on the unknown redshift of KUV 00311-1938 of z < 0.98, and of PKS 1440-389 of z < 0.53. When combined with previous spectroscopy results the redshift of KUV 00311-1938 is constrained to $0.51 \leq z < 0.98$ and for PKS 1440-389 to $0.14 \lessapprox z < 0.53$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.03306v2-abstract-full').style.display = 'none'; document.getElementById('2004.03306v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">Accepted for publication in MNRAS. 13 pages, 4 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/2003.11551">arXiv:2003.11551</a> <span> [<a href="https://arxiv.org/pdf/2003.11551">pdf</a>, <a href="https://arxiv.org/format/2003.11551">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/staa870">10.1093/mnras/staa870 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraining VLBI-optical offsets in high redshift galaxies using strong gravitational lensing </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Spingola%2C+C">C. Spingola</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</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="2003.11551v1-abstract-short" style="display: inline;"> We present a multi-wavelength analysis of two highly magnified strong gravitationally lensed galaxies, CLASS B0712+472 and CLASS B1608+656, at redshifts $1.34$ and $1.394$, respectively, using new VLBI and archival HST observations. We reconstruct the positions of the radio and optical emissions with their uncertainties using Monte Carlo sampling. We find that in CLASS B0712+472 the optical and ra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.11551v1-abstract-full').style.display = 'inline'; document.getElementById('2003.11551v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2003.11551v1-abstract-full" style="display: none;"> We present a multi-wavelength analysis of two highly magnified strong gravitationally lensed galaxies, CLASS B0712+472 and CLASS B1608+656, at redshifts $1.34$ and $1.394$, respectively, using new VLBI and archival HST observations. We reconstruct the positions of the radio and optical emissions with their uncertainties using Monte Carlo sampling. We find that in CLASS B0712+472 the optical and radio emissions are co-spatial within $2\pm5$ mas ($17\pm 42$ pc at redshift of 1.34). But, in CLASS B1608+656, we reconstruct an optical-radio offset of $25\pm16$ mas ($214\pm137$ pc at redshift of 1.394), the smallest offset measured for an AGN at such high redshift. The spectral features indicate that CLASS B1608+656 is a post-merger galaxy, which, in combination with the optical-VLBI offset reported here, makes CLASS B1608+656 a promising candidate for a high-$z$ offset-AGN. Furthermore, the milliarcsecond angular resolution of the VLBI observations combined with the precise lens models allow us to spatially locate the radio emission at $0.05$ mas precision ($0.4$ pc) in CLASS B0712+472, and $0.009$ mas precision ($0.08$ pc) in CLASS B1608+656. The search for optical-radio offsets in high redshift galaxies will be eased by the upcoming synoptic all-sky surveys, including E-ELT and SKA, which are expected to find $\sim 10^5$ strongly lensed galaxies, opening an era of large strong lensing samples observed at high angular resolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.11551v1-abstract-full').style.display = 'none'; document.getElementById('2003.11551v1-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> 25 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">16 pages, 7 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/1810.07265">arXiv:1810.07265</a> <span> [<a href="https://arxiv.org/pdf/1810.07265">pdf</a>, <a href="https://arxiv.org/format/1810.07265">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</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.physrep.2018.10.001">10.1016/j.physrep.2018.10.001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gravitational Lenses as High-Resolution Telescopes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">Anna Barnacka</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="1810.07265v1-abstract-short" style="display: inline;"> The inner regions of active galaxies host the most extreme and energetic phenomena in the universe including, relativistic jets, supermassive black hole binaries, and recoiling supermassive black holes. However, many of these sources cannot be resolved with direct observations. I review how strong gravitational lensing can be used to elucidate the structures of these sources from radio frequencies… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.07265v1-abstract-full').style.display = 'inline'; document.getElementById('1810.07265v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1810.07265v1-abstract-full" style="display: none;"> The inner regions of active galaxies host the most extreme and energetic phenomena in the universe including, relativistic jets, supermassive black hole binaries, and recoiling supermassive black holes. However, many of these sources cannot be resolved with direct observations. I review how strong gravitational lensing can be used to elucidate the structures of these sources from radio frequencies up to very high energy gamma rays. The deep gravitational potentials surrounding galaxies act as natural gravitational lenses. These gravitational lenses split background sources into multiple images, each with a gravitationally-induced time delay. These time delays and positions of lensed images depend on the source location, and thus, can be used to infer the spatial origins of the emission. For example, using gravitationally-induced time delays improves angular resolution of modern gamma-ray instruments by six orders of magnitude, and provides evidence that gamma-ray outbursts can be produced at even thousands of light years from a supermassive black hole, and that the compact radio emission does not always trace the position of the supermassive black hole. These findings provide unique physical information about the central structure of active galaxies, force us to revise our models of operating particle acceleration mechanisms, and challenge our assumptions about the origin of compact radio emission. Future surveys, including LSST, SKA, and Euclid, will provide observations for hundreds of thousands of gravitationally lensed sources, which will allow us to apply strong gravitational lensing to study the multi-wavelength structure for large ensembles of sources. This large ensemble of gravitationally lensed active galaxies will allow us to elucidate the physical origins of multi-wavelength emissions, their connections to supermassive black holes, and their cosmic evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.07265v1-abstract-full').style.display = 'none'; document.getElementById('1810.07265v1-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 October, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Invited (Accepted) review for Physics Reports</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1705.00690">arXiv:1705.00690</a> <span> [<a href="https://arxiv.org/pdf/1705.00690">pdf</a>, <a href="https://arxiv.org/format/1705.00690">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.3847/1538-4357/aa86ec">10.3847/1538-4357/aa86ec <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxies as High-Resolution Telescopes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">Anna Barnacka</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="1705.00690v2-abstract-short" style="display: inline;"> Recent observations show a population of active galaxies with milliarcseconds offsets between optical and radio emission. Such offsets can be an indication of extreme phenomena associated with supermassive black holes including relativistic jets, binary supermassive black holes, or even recoiling supermassive black holes. However, the multi-wavelength structure of active galaxies at a few milliarc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.00690v2-abstract-full').style.display = 'inline'; document.getElementById('1705.00690v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1705.00690v2-abstract-full" style="display: none;"> Recent observations show a population of active galaxies with milliarcseconds offsets between optical and radio emission. Such offsets can be an indication of extreme phenomena associated with supermassive black holes including relativistic jets, binary supermassive black holes, or even recoiling supermassive black holes. However, the multi-wavelength structure of active galaxies at a few milliarcseconds cannot be fathomed with direct observations. We propose using strong gravitational lensing to elucidate the multi-wavelength structure of sources. When sources are located close to the caustic of lensing galaxy, even small offset in the position of the sources results in a drastic difference in the position and magnification of mirage images. We show that the angular offset in the position of the sources can be amplified more than 50 times in the observed position of mirage images. We find that at least 8% of the observed gravitationally lensed quasars will be in the caustic configuration. The synergy between SKA and Euclid will provide an ideal set of observations for thousands of gravitationally lensed sources in the caustic configuration, which will allow us to elucidate the multi-wavelength structure for a large ensemble of sources, and study the physical origin of radio emissions, their connection to supermassive black holes, and their cosmic evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.00690v2-abstract-full').style.display = 'none'; document.getElementById('1705.00690v2-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 August, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 May, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1610.05151">arXiv:1610.05151</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> <p class="title is-5 mathjax"> Contributions of the Cherenkov Telescope Array (CTA) to the 6th International Symposium on High-Energy Gamma-Ray Astronomy (Gamma 2016) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Consortium%2C+T+C">The CTA Consortium</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abchiche%2C+A">A. Abchiche</a>, <a href="/search/astro-ph?searchtype=author&query=Abeysekara%2C+U">U. Abeysekara</a>, <a href="/search/astro-ph?searchtype=author&query=Abril%2C+%C3%93">脫. Abril</a>, <a href="/search/astro-ph?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/astro-ph?searchtype=author&query=Acharya%2C+B+S">B. S. Acharya</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agnetta%2C+G">G. Agnetta</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Akhperjanian%2C+A">A. Akhperjanian</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alcubierre%2C+M">M. Alcubierre</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Allafort%2C+A+J">A. J. Allafort</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Amans%2C+J+-">J. -P. Amans</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrogi%2C+L">L. Ambrogi</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Anduze%2C+M">M. Anduze</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a> , et al. (1387 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="1610.05151v1-abstract-short" style="display: inline;"> List of contributions from the Cherenkov Telescope Array (CTA) Consortium presented at the 6th International Symposium on High-Energy Gamma-Ray Astronomy (Gamma 2016), July 11-15, 2016, in Heidelberg, Germany. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1610.05151v1-abstract-full" style="display: none;"> List of contributions from the Cherenkov Telescope Array (CTA) Consortium presented at the 6th International Symposium on High-Energy Gamma-Ray Astronomy (Gamma 2016), July 11-15, 2016, in Heidelberg, Germany. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.05151v1-abstract-full').style.display = 'none'; document.getElementById('1610.05151v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 October, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">Index of CTA conference proceedings for the Gamma 2016, Heidelberg, Germany</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1608.02769">arXiv:1608.02769</a> <span> [<a href="https://arxiv.org/pdf/1608.02769">pdf</a>, <a href="https://arxiv.org/ps/1608.02769">ps</a>, <a href="https://arxiv.org/format/1608.02769">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/stw1319">10.1093/mnras/stw1319 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of Very High Energy Gamma Rays from 1ES 1440+122 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=VERITAS+Collaboration"> VERITAS Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Archambault%2C+S">S. Archambault</a>, <a href="/search/astro-ph?searchtype=author&query=Archer%2C+A">A. Archer</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Behera%2C+B">B. Behera</a>, <a href="/search/astro-ph?searchtype=author&query=Beilicke%2C+M">M. Beilicke</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">W. Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+K">K. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Bird%2C+R">R. Bird</a>, <a href="/search/astro-ph?searchtype=author&query=Boettcher%2C+M">M. Boettcher</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Bugaev%2C+V">V. Bugaev</a>, <a href="/search/astro-ph?searchtype=author&query=Cardenzana%2C+J+V">J. V Cardenzana</a>, <a href="/search/astro-ph?searchtype=author&query=Cerruti%2C+M">M. Cerruti</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">X. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Christiansen%2C+J+L">J. L. Christiansen</a>, <a href="/search/astro-ph?searchtype=author&query=Ciupik%2C+L">L. Ciupik</a>, <a href="/search/astro-ph?searchtype=author&query=Collins-Hughes%2C+E">E. Collins-Hughes</a>, <a href="/search/astro-ph?searchtype=author&query=Connolly%2C+M+P">M. P. Connolly</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+W">W. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+H+J">H. J. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Dumm%2C+J">J. Dumm</a>, <a href="/search/astro-ph?searchtype=author&query=Eisch%2C+J+D">J. D. Eisch</a>, <a href="/search/astro-ph?searchtype=author&query=Errando%2C+M">M. Errando</a>, <a href="/search/astro-ph?searchtype=author&query=Falcone%2C+A">A. Falcone</a> , et al. (65 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="1608.02769v1-abstract-short" style="display: inline;"> The BL Lacertae object 1ES 1440+122 was observed in the energy range from 85 GeV to 30 TeV by the VERITAS array of imaging atmospheric Cherenkov telescopes. The observations, taken between 2008 May and 2010 June and totalling 53 hours, resulted in the discovery of $纬$-ray emission from the blazar, which has a redshift $z$=0.163. 1ES 1440+122 is detected at a statistical significance of 5.5 standar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1608.02769v1-abstract-full').style.display = 'inline'; document.getElementById('1608.02769v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1608.02769v1-abstract-full" style="display: none;"> The BL Lacertae object 1ES 1440+122 was observed in the energy range from 85 GeV to 30 TeV by the VERITAS array of imaging atmospheric Cherenkov telescopes. The observations, taken between 2008 May and 2010 June and totalling 53 hours, resulted in the discovery of $纬$-ray emission from the blazar, which has a redshift $z$=0.163. 1ES 1440+122 is detected at a statistical significance of 5.5 standard deviations above the background with an integral flux of (2.8$\pm0.7_{\mathrm{stat}}\pm0.8_{\mathrm{sys}}$) $\times$ 10$^{-12}$ cm$^{-2}$ s$^{-1}$ (1.2\% of the Crab Nebula's flux) above 200 GeV. The measured spectrum is described well by a power law from 0.2 TeV to 1.3 TeV with a photon index of 3.1 $\pm$ 0.4$_{\mathrm{stat}}$ $\pm$ 0.2$_{\mathrm{sys}}$. Quasi-simultaneous multi-wavelength data from the Fermi Large Area Telescope (0.3--300 GeV) and the Swift X-ray Telescope (0.2--10 keV) are additionally used to model the properties of the emission region. A synchrotron self-Compton model produces a good representation of the multi-wavelength data. Adding an external-Compton or a hadronic component also adequately describes the data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1608.02769v1-abstract-full').style.display = 'none'; document.getElementById('1608.02769v1-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">8 pages, 4 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/1608.01569">arXiv:1608.01569</a> <span> [<a href="https://arxiv.org/pdf/1608.01569">pdf</a>, <a href="https://arxiv.org/format/1608.01569">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/10.1051/0004-6361/201628744">10.1051/0004-6361/201628744 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Very High Energy outburst of Markarian 501 in May 2009 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aliu%2C+E">E. Aliu</a>, <a href="/search/astro-ph?searchtype=author&query=Archambault%2C+S">S. Archambault</a>, <a href="/search/astro-ph?searchtype=author&query=Archer%2C+A">A. Archer</a>, <a href="/search/astro-ph?searchtype=author&query=Arlen%2C+T">T. Arlen</a>, <a href="/search/astro-ph?searchtype=author&query=Aune%2C+T">T. Aune</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Behera%2C+B">B. Behera</a>, <a href="/search/astro-ph?searchtype=author&query=Beilicke%2C+M">M. Beilicke</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">W. Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+K">K. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Bird%2C+R">R. Bird</a>, <a href="/search/astro-ph?searchtype=author&query=Bouvier%2C+A">A. Bouvier</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Buchovecky%2C+M">M. Buchovecky</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Bugaev%2C+V">V. Bugaev</a>, <a href="/search/astro-ph?searchtype=author&query=Cardenzana%2C+J+V">J. V Cardenzana</a>, <a href="/search/astro-ph?searchtype=author&query=Cerruti%2C+M">M. Cerruti</a>, <a href="/search/astro-ph?searchtype=author&query=Cesarini%2C+A">A. Cesarini</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">X. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Ciupik%2C+L">L. Ciupik</a>, <a href="/search/astro-ph?searchtype=author&query=Collins-Hughes%2C+E">E. Collins-Hughes</a>, <a href="/search/astro-ph?searchtype=author&query=Connolly%2C+M+P">M. P. Connolly</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+W">W. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Dumm%2C+J">J. Dumm</a> , et al. (86 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="1608.01569v1-abstract-short" style="display: inline;"> The very high energy (VHE; E $>$ 100 GeV) blazar Markarian 501 was observed between April 17 and May 5 (MJD 54938--54956), 2009, as part of an extensive multi-wavelength campaign from radio to VHE. Strong VHE $纬$-ray activity was detected on May 1st with Whipple and VERITAS, when the flux (E $>$ 400 GeV) increased to 10 times the pre-flare baseline flux (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1608.01569v1-abstract-full').style.display = 'inline'; document.getElementById('1608.01569v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1608.01569v1-abstract-full" style="display: none;"> The very high energy (VHE; E $>$ 100 GeV) blazar Markarian 501 was observed between April 17 and May 5 (MJD 54938--54956), 2009, as part of an extensive multi-wavelength campaign from radio to VHE. Strong VHE $纬$-ray activity was detected on May 1st with Whipple and VERITAS, when the flux (E $>$ 400 GeV) increased to 10 times the pre-flare baseline flux ($3.9{\times 10^{-11}}~{\rm ph~cm^{-2}~s^{-1}}$), reaching five times the flux of the Crab Nebula. This coincided with a decrease in the optical polarization and a rotation of the polarization angle by 15$^{\circ}$. This VHE flare showed a fast flux variation with an increase of a factor $\sim$4 in 25 minutes, and a falling time of $\sim$50 minutes. We present the observations of the quiescent state previous to the flare and of the high state after the flare, focusing on the flux and spectral variability from Whipple, VERITAS, Fermi-LAT, RXTE, and Swift combined with optical and radio data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1608.01569v1-abstract-full').style.display = 'none'; document.getElementById('1608.01569v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 August, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 10 figures. Accepted for publication in Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 594, A76 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1601.01812">arXiv:1601.01812</a> <span> [<a href="https://arxiv.org/pdf/1601.01812">pdf</a>, <a href="https://arxiv.org/format/1601.01812">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8205/817/1/L7">10.3847/2041-8205/817/1/L7 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Exceptionally bright TeV flares from the binary LS I +61$^\circ$ 303 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=VERITAS+Collaboration"> VERITAS Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Archambault%2C+S">S. Archambault</a>, <a href="/search/astro-ph?searchtype=author&query=Archer%2C+A">A. Archer</a>, <a href="/search/astro-ph?searchtype=author&query=Aune%2C+T">T. Aune</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">W. Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Bird%2C+R">R. Bird</a>, <a href="/search/astro-ph?searchtype=author&query=Buchovecky%2C+M">M. Buchovecky</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Bugaev%2C+V">V. Bugaev</a>, <a href="/search/astro-ph?searchtype=author&query=Byrum%2C+K">K. Byrum</a>, <a href="/search/astro-ph?searchtype=author&query=Cardenzana%2C+J+V">J. V. Cardenzana</a>, <a href="/search/astro-ph?searchtype=author&query=Cerruti%2C+M">M. Cerruti</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">X. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Ciupik%2C+L">L. Ciupik</a>, <a href="/search/astro-ph?searchtype=author&query=Collins-Hughes%2C+E">E. Collins-Hughes</a>, <a href="/search/astro-ph?searchtype=author&query=Connolly%2C+M+P">M. P. Connolly</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+W">W. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+H+J">H. J. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Dumm%2C+J">J. Dumm</a>, <a href="/search/astro-ph?searchtype=author&query=Eisch%2C+J+D">J. D. Eisch</a>, <a href="/search/astro-ph?searchtype=author&query=Falcone%2C+A">A. Falcone</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+Q">Q. Feng</a>, <a href="/search/astro-ph?searchtype=author&query=Finley%2C+J+P">J. P. Finley</a>, <a href="/search/astro-ph?searchtype=author&query=Fleischhack%2C+H">H. Fleischhack</a> , et al. (64 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="1601.01812v1-abstract-short" style="display: inline;"> The TeV binary system LS I +61$^\circ$ 303 is known for its regular, non-thermal emission pattern which traces the orbital period of the compact object in its 26.5 day orbit around its B0 Ve star companion. The system typically presents elevated TeV emission around apastron passage with flux levels between 5% and 15% of the steady flux from the Crab Nebula (> 300 GeV). In this article, VERITAS obs… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1601.01812v1-abstract-full').style.display = 'inline'; document.getElementById('1601.01812v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1601.01812v1-abstract-full" style="display: none;"> The TeV binary system LS I +61$^\circ$ 303 is known for its regular, non-thermal emission pattern which traces the orbital period of the compact object in its 26.5 day orbit around its B0 Ve star companion. The system typically presents elevated TeV emission around apastron passage with flux levels between 5% and 15% of the steady flux from the Crab Nebula (> 300 GeV). In this article, VERITAS observations of LS I +61$^\circ$ 303 taken in late 2014 are presented, during which bright TeV flares around apastron at flux levels peaking above 30% of the Crab Nebula flux were detected. This is the brightest such activity from this source ever seen in the TeV regime. The strong outbursts have rise and fall times of less than a day. The short timescale of the flares, in conjunction with the observation of 10 TeV photons from LS I +61$^\circ$ 303 during the flares, provides constraints on the properties of the accelerator in the source. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1601.01812v1-abstract-full').style.display = 'none'; document.getElementById('1601.01812v1-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 January, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">9 pages, 2 figures. Accepted for publication by ApJL</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 817 L7 2016 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1512.04434">arXiv:1512.04434</a> <span> [<a href="https://arxiv.org/pdf/1512.04434">pdf</a>, <a href="https://arxiv.org/format/1512.04434">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/2041-8205/815/2/L22">10.1088/2041-8205/815/2/L22 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gamma rays from the quasar PKS 1441+25: story of an escape </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abeysekara%2C+A+U">A. U. Abeysekara</a>, <a href="/search/astro-ph?searchtype=author&query=Archambault%2C+S">S. Archambault</a>, <a href="/search/astro-ph?searchtype=author&query=Archer%2C+A">A. Archer</a>, <a href="/search/astro-ph?searchtype=author&query=Aune%2C+T">T. Aune</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">W. Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Bird%2C+R">R. Bird</a>, <a href="/search/astro-ph?searchtype=author&query=Biteau%2C+J">J. Biteau</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Bugaev%2C+V">V. Bugaev</a>, <a href="/search/astro-ph?searchtype=author&query=Cardenzana%2C+J+V">J. V Cardenzana</a>, <a href="/search/astro-ph?searchtype=author&query=Cerruti%2C+M">M. Cerruti</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">X. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Christiansen%2C+J+L">J. L. Christiansen</a>, <a href="/search/astro-ph?searchtype=author&query=Ciupik%2C+L">L. Ciupik</a>, <a href="/search/astro-ph?searchtype=author&query=Connolly%2C+M+P">M. P. Connolly</a>, <a href="/search/astro-ph?searchtype=author&query=Coppi%2C+P">P. Coppi</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+W">W. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+H+J">H. J. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Dumm%2C+J">J. Dumm</a>, <a href="/search/astro-ph?searchtype=author&query=Eisch%2C+J+D">J. D. Eisch</a>, <a href="/search/astro-ph?searchtype=author&query=Errando%2C+M">M. Errando</a>, <a href="/search/astro-ph?searchtype=author&query=Falcone%2C+A">A. Falcone</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+Q">Q. Feng</a>, <a href="/search/astro-ph?searchtype=author&query=Finley%2C+J+P">J. P. Finley</a> , et al. (81 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1512.04434v1-abstract-short" style="display: inline;"> Outbursts from gamma-ray quasars provide insights on the relativistic jets of active galactic nuclei and constraints on the diffuse radiation fields that fill the Universe. The detection of significant emission above 100 GeV from a distant quasar would show that some of the radiated gamma rays escape pair-production interactions with low-energy photons, be it the extragalactic background light (EB… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.04434v1-abstract-full').style.display = 'inline'; document.getElementById('1512.04434v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1512.04434v1-abstract-full" style="display: none;"> Outbursts from gamma-ray quasars provide insights on the relativistic jets of active galactic nuclei and constraints on the diffuse radiation fields that fill the Universe. The detection of significant emission above 100 GeV from a distant quasar would show that some of the radiated gamma rays escape pair-production interactions with low-energy photons, be it the extragalactic background light (EBL), or the radiation near the supermassive black hole lying at the jet's base. VERITAS detected gamma-ray emission up to 200 GeV from PKS 1441+25 (z=0.939) during April 2015, a period of high activity across all wavelengths. This observation of PKS 1441+25 suggests that the emission region is located thousands of Schwarzschild radii away from the black hole. The gamma-ray detection also sets a stringent upper limit on the near-ultraviolet to near-infrared EBL intensity, suggesting that galaxy surveys have resolved most, if not all, of the sources of the EBL at these wavelengths. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.04434v1-abstract-full').style.display = 'none'; document.getElementById('1512.04434v1-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 December, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">7 pages, 3 figures, published in ApJ Letters 815, L22 (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/1512.02235">arXiv:1512.02235</a> <span> [<a href="https://arxiv.org/pdf/1512.02235">pdf</a>, <a href="https://arxiv.org/ps/1512.02235">ps</a>, <a href="https://arxiv.org/format/1512.02235">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/0004-637X/819/2/156">10.3847/0004-637X/819/2/156 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multiwavelength Study of Quiescent States of Mrk 421 with Unprecedented Hard X-Ray Coverage Provided by NuSTAR in 2013 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Balokovi%C4%87%2C+M">M. Balokovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Paneque%2C+D">D. Paneque</a>, <a href="/search/astro-ph?searchtype=author&query=Madejski%2C+G">G. Madejski</a>, <a href="/search/astro-ph?searchtype=author&query=Furniss%2C+A">A. Furniss</a>, <a href="/search/astro-ph?searchtype=author&query=Chiang%2C+J">J. Chiang</a>, <a href="/search/astro-ph?searchtype=author&query=team%2C+t+N">the NuSTAR team</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Ajello%2C+M">M. Ajello</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Barret%2C+D">D. Barret</a>, <a href="/search/astro-ph?searchtype=author&query=Blandford%2C+R">R. Blandford</a>, <a href="/search/astro-ph?searchtype=author&query=Boggs%2C+S+E">S. E. Boggs</a>, <a href="/search/astro-ph?searchtype=author&query=Christensen%2C+F+E">F. E. Christensen</a>, <a href="/search/astro-ph?searchtype=author&query=Craig%2C+W+W">W. W. Craig</a>, <a href="/search/astro-ph?searchtype=author&query=Forster%2C+K">K. Forster</a>, <a href="/search/astro-ph?searchtype=author&query=Giommi%2C+P">P. Giommi</a>, <a href="/search/astro-ph?searchtype=author&query=Grefenstette%2C+B+W">B. W. Grefenstette</a>, <a href="/search/astro-ph?searchtype=author&query=Hailey%2C+C+J">C. J. Hailey</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F+A">F. A. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Hornstrup%2C+A">A. Hornstrup</a>, <a href="/search/astro-ph?searchtype=author&query=Kitaguchi%2C+T">T. Kitaguchi</a>, <a href="/search/astro-ph?searchtype=author&query=Koglin%2C+J+E">J. E. Koglin</a>, <a href="/search/astro-ph?searchtype=author&query=Madsen%2C+K+K">K. K. Madsen</a>, <a href="/search/astro-ph?searchtype=author&query=Mao%2C+P+H">P. H. Mao</a>, <a href="/search/astro-ph?searchtype=author&query=Miyasaka%2C+H">H. Miyasaka</a> , et al. (286 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="1512.02235v1-abstract-short" style="display: inline;"> We present coordinated multiwavelength observations of the bright, nearby BL Lac object Mrk 421 taken in 2013 January-March, involving GASP-WEBT, Swift, NuSTAR, Fermi-LAT, MAGIC, VERITAS, and other collaborations and instruments, providing data from radio to very-high-energy (VHE) gamma-ray bands. NuSTAR yielded previously unattainable sensitivity in the 3-79 keV range, revealing that the spectrum… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.02235v1-abstract-full').style.display = 'inline'; document.getElementById('1512.02235v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1512.02235v1-abstract-full" style="display: none;"> We present coordinated multiwavelength observations of the bright, nearby BL Lac object Mrk 421 taken in 2013 January-March, involving GASP-WEBT, Swift, NuSTAR, Fermi-LAT, MAGIC, VERITAS, and other collaborations and instruments, providing data from radio to very-high-energy (VHE) gamma-ray bands. NuSTAR yielded previously unattainable sensitivity in the 3-79 keV range, revealing that the spectrum softens when the source is dimmer until the X-ray spectral shape saturates into a steep power law with a photon index of approximately 3, with no evidence for an exponential cutoff or additional hard components up to about 80 keV. For the first time, we observed both the synchrotron and the inverse-Compton peaks of the spectral energy distribution (SED) simultaneously shifted to frequencies below the typical quiescent state by an order of magnitude. The fractional variability as a function of photon energy shows a double-bump structure which relates to the two bumps of the broadband SED. In each bump, the variability increases with energy which, in the framework of the synchrotron self-Compton model, implies that the electrons with higher energies are more variable. The measured multi-band variability, the significant X-ray-to-VHE correlation down to some of the lowest fluxes ever observed in both bands, the lack of correlation between optical/UV and X-ray flux, the low degree of polarization and its significant (random) variations, the short estimated electron cooling time, and the significantly longer variability timescale observed in the NuSTAR light curves point toward in-situ electron acceleration, and suggest that there are multiple compact regions contributing to the broadband emission of Mrk 421 during low-activity states. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.02235v1-abstract-full').style.display = 'none'; document.getElementById('1512.02235v1-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> 7 December, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">32 pages, 14 figures; 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> The Astrophysical Journal, 819, 156 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1511.02891">arXiv:1511.02891</a> <span> [<a href="https://arxiv.org/pdf/1511.02891">pdf</a>, <a href="https://arxiv.org/format/1511.02891">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/10.3847/0004-637X/821/1/58">10.3847/0004-637X/821/1/58 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Structure of the Strongly Lensed Gamma-ray Source B2 0218+35 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">Anna Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Geller%2C+M+J">Margaret J. Geller</a>, <a href="/search/astro-ph?searchtype=author&query=Dell%27Antonio%2C+I+P">Ian P. Dell'Antonio</a>, <a href="/search/astro-ph?searchtype=author&query=Zitrin%2C+A">Adi Zitrin</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="1511.02891v2-abstract-short" style="display: inline;"> Strong gravitational lensing is a powerful tool for resolving the high energy universe. We combine the temporal resolution of Fermi-LAT, the angular resolution of radio telescopes, and the independently and precisely known Hubble constant from Planck, to resolve the spatial origin of gamma-ray flares in the strongly lensed source B2 0218+35. The lensing model achieves 1 milliarcsecond spatial reso… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.02891v2-abstract-full').style.display = 'inline'; document.getElementById('1511.02891v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1511.02891v2-abstract-full" style="display: none;"> Strong gravitational lensing is a powerful tool for resolving the high energy universe. We combine the temporal resolution of Fermi-LAT, the angular resolution of radio telescopes, and the independently and precisely known Hubble constant from Planck, to resolve the spatial origin of gamma-ray flares in the strongly lensed source B2 0218+35. The lensing model achieves 1 milliarcsecond spatial resolution of the source at gamma-ray energies. The data imply that the gamma-ray flaring sites are separate from the radio core: the bright gamma-ray flare (MJD: 56160 - 56280) occurred $51\pm8$ pc from the 15 GHz radio core, toward the central engine. This displacement is significant at the $\sim3蟽$ level, and is limited primarily by the precision of the Hubble constant. B2 0218+35 is the first source where the position of the gamma-ray emitting region relative to the radio core can be resolved. We discuss the potential of an ensemble of strongly lensed high energy sources for elucidating the physics of distant variable sources based on data from Chandra and SKA. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.02891v2-abstract-full').style.display = 'none'; document.getElementById('1511.02891v2-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 February, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 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 for publication, ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1510.01639">arXiv:1510.01639</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> <p class="title is-5 mathjax"> VERITAS Collaboration Contributions to the 34th International Cosmic Ray Conference </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+VERITAS+Collaboration"> The VERITAS Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abeysekara%2C+A+U">A. U. Abeysekara</a>, <a href="/search/astro-ph?searchtype=author&query=Archambault%2C+S">S. Archambault</a>, <a href="/search/astro-ph?searchtype=author&query=Archer%2C+A">A. Archer</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">W. Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Bird%2C+R">R. Bird</a>, <a href="/search/astro-ph?searchtype=author&query=Biteau%2C+J">J. Biteau</a>, <a href="/search/astro-ph?searchtype=author&query=Buchovecky%2C+M">M. Buchovecky</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Bugaev%2C+V">V. Bugaev</a>, <a href="/search/astro-ph?searchtype=author&query=Byrum%2C+K">K. Byrum</a>, <a href="/search/astro-ph?searchtype=author&query=Cardenzana%2C+J+V">J. V Cardenzana</a>, <a href="/search/astro-ph?searchtype=author&query=Cerruti%2C+M">M. Cerruti</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">X. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Christiansen%2C+J+L">J. L. Christiansen</a>, <a href="/search/astro-ph?searchtype=author&query=Ciupik%2C+L">L. Ciupik</a>, <a href="/search/astro-ph?searchtype=author&query=Collins-Hughes%2C+E">E. Collins-Hughes</a>, <a href="/search/astro-ph?searchtype=author&query=Connolly%2C+M+P">M. P. Connolly</a>, <a href="/search/astro-ph?searchtype=author&query=Coppi%2C+P">P. Coppi</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+W">W. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Dwarkadas%2C+V+V">V. V. Dwarkadas</a>, <a href="/search/astro-ph?searchtype=author&query=Eisch%2C+J+D">J. D. Eisch</a>, <a href="/search/astro-ph?searchtype=author&query=Errando%2C+M">M. Errando</a>, <a href="/search/astro-ph?searchtype=author&query=Falcone%2C+A">A. Falcone</a> , et al. (68 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1510.01639v1-abstract-short" style="display: inline;"> Compilation of papers presented by the VERITAS Collaboration at the 34th International Cosmic Ray Conference (ICRC), held July 30 through August 6, 2015 in The Hague, The Netherlands. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1510.01639v1-abstract-full" style="display: none;"> Compilation of papers presented by the VERITAS Collaboration at the 34th International Cosmic Ray Conference (ICRC), held July 30 through August 6, 2015 in The Hague, The Netherlands. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.01639v1-abstract-full').style.display = 'none'; document.getElementById('1510.01639v1-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 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">1 html page. 2015 ICRC, The Hague, The Netherlands. A full list of author affiliations can be found at this link: http://veritas.sao.arizona.edu/conferences/authors?icrc2015</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1510.01269">arXiv:1510.01269</a> <span> [<a href="https://arxiv.org/pdf/1510.01269">pdf</a>, <a href="https://arxiv.org/format/1510.01269">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"> Science Highlights from VERITAS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Staszak%2C+D">D. Staszak</a>, <a href="/search/astro-ph?searchtype=author&query=Abeysekara%2C+A+U">A. U. Abeysekara</a>, <a href="/search/astro-ph?searchtype=author&query=Archambault%2C+S">S. Archambault</a>, <a href="/search/astro-ph?searchtype=author&query=Archer%2C+A">A. Archer</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">W. Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Bird%2C+R">R. Bird</a>, <a href="/search/astro-ph?searchtype=author&query=Biteau%2C+J">J. Biteau</a>, <a href="/search/astro-ph?searchtype=author&query=Buchovecky%2C+M">M. Buchovecky</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Bugaev%2C+V">V. Bugaev</a>, <a href="/search/astro-ph?searchtype=author&query=Byrum%2C+K">K. Byrum</a>, <a href="/search/astro-ph?searchtype=author&query=Cardenzana%2C+J+V">J. V Cardenzana</a>, <a href="/search/astro-ph?searchtype=author&query=Cerruti%2C+M">M. Cerruti</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">X. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Christiansen%2C+J+L">J. L. Christiansen</a>, <a href="/search/astro-ph?searchtype=author&query=Ciupik%2C+L">L. Ciupik</a>, <a href="/search/astro-ph?searchtype=author&query=Collins-Hughes%2C+E">E. Collins-Hughes</a>, <a href="/search/astro-ph?searchtype=author&query=Connolly%2C+M+P">M. P. Connolly</a>, <a href="/search/astro-ph?searchtype=author&query=Coppi%2C+P">P. Coppi</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+W">W. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Dwarkadas%2C+V+V">V. V. Dwarkadas</a>, <a href="/search/astro-ph?searchtype=author&query=Eisch%2C+J+D">J. D. Eisch</a>, <a href="/search/astro-ph?searchtype=author&query=Errando%2C+M">M. Errando</a>, <a href="/search/astro-ph?searchtype=author&query=Falcone%2C+A">A. Falcone</a> , et al. (66 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="1510.01269v1-abstract-short" style="display: inline;"> The Very Energetic Radiation Imaging Telescope Array System (VERITAS) is a ground-based array located at the Fred Lawrence Whipple Observatory in southern Arizona and is one of the world's most sensitive gamma-ray instruments at energies of 85 GeV to $>$30 TeV. VERITAS has a wide scientific reach that includes the study of extragalactic and Galactic objects as well as the search for astrophysical… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.01269v1-abstract-full').style.display = 'inline'; document.getElementById('1510.01269v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1510.01269v1-abstract-full" style="display: none;"> The Very Energetic Radiation Imaging Telescope Array System (VERITAS) is a ground-based array located at the Fred Lawrence Whipple Observatory in southern Arizona and is one of the world's most sensitive gamma-ray instruments at energies of 85 GeV to $>$30 TeV. VERITAS has a wide scientific reach that includes the study of extragalactic and Galactic objects as well as the search for astrophysical signatures of dark matter and the measurement of cosmic rays. In this paper, we will summarize the current status of the VERITAS observatory and present some of the scientific highlights from the last two years, focusing in particular on those results shown at the 2015 ICRC in The Hague, Netherlands. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.01269v1-abstract-full').style.display = 'none'; document.getElementById('1510.01269v1-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 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">To appear in the Proceedings of the 34th International Cosmic Ray Conference (ICRC2015), The Hague, The Netherlands</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1508.05894">arXiv:1508.05894</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> <p class="title is-5 mathjax"> CTA Contributions to the 34th International Cosmic Ray Conference (ICRC2015) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Consortium%2C+T+C">The CTA Consortium</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abchiche%2C+A">A. Abchiche</a>, <a href="/search/astro-ph?searchtype=author&query=Abeysekara%2C+U">U. Abeysekara</a>, <a href="/search/astro-ph?searchtype=author&query=Abril%2C+%C3%93">脫. Abril</a>, <a href="/search/astro-ph?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/astro-ph?searchtype=author&query=Acharya%2C+B+S">B. S. Acharya</a>, <a href="/search/astro-ph?searchtype=author&query=Actis%2C+M">M. Actis</a>, <a href="/search/astro-ph?searchtype=author&query=Agnetta%2C+G">G. Agnetta</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=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Akhperjanian%2C+A">A. Akhperjanian</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alcubierre%2C+M">M. Alcubierre</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Aliu%2C+E">E. Aliu</a>, <a href="/search/astro-ph?searchtype=author&query=Allafort%2C+A+J">A. J. Allafort</a>, <a href="/search/astro-ph?searchtype=author&query=Allan%2C+D">D. Allan</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Amans%2C+J+-">J. -P. Amans</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrogi%2C+L">L. Ambrogi</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a> , et al. (1290 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="1508.05894v2-abstract-short" style="display: inline;"> List of contributions from the CTA Consortium presented at the 34th International Cosmic Ray Conference, 30 July - 6 August 2015, The Hague, The Netherlands. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1508.05894v2-abstract-full" style="display: none;"> List of contributions from the CTA Consortium presented at the 34th International Cosmic Ray Conference, 30 July - 6 August 2015, The Hague, The Netherlands. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.05894v2-abstract-full').style.display = 'none'; document.getElementById('1508.05894v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 August, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Index of CTA conference proceedings at the ICRC2015, The Hague (The Netherlands). v1: placeholder with no arXiv links yet, to be replaced once individual contributions have been all submitted; v2: final with arXiv links to all CTA contributions and full author list</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1504.05210">arXiv:1504.05210</a> <span> [<a href="https://arxiv.org/pdf/1504.05210">pdf</a>, <a href="https://arxiv.org/format/1504.05210">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/809/1/100">10.1088/0004-637X/809/1/100 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Resolving the High Energy Universe with Strong Gravitational Lensing: The Case of PKS 1830-211 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">Anna Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Geller%2C+M+J">Margaret J. Geller</a>, <a href="/search/astro-ph?searchtype=author&query=Dell%27Antonio%2C+I+P">Ian P. Dell'Antonio</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">Wystan Benbow</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="1504.05210v2-abstract-short" style="display: inline;"> Gravitational lensing is a potentially powerful tool for elucidating the origin of gamma-ray emission from distant sources. Cosmic lenses magnify the emission from distance sources and produce time delays between mirage images. Gravitationally-induced time delays depend on the position of the emitting regions in the source plane. The Fermi/LAT satellite continuously monitors the entire sky and det… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.05210v2-abstract-full').style.display = 'inline'; document.getElementById('1504.05210v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1504.05210v2-abstract-full" style="display: none;"> Gravitational lensing is a potentially powerful tool for elucidating the origin of gamma-ray emission from distant sources. Cosmic lenses magnify the emission from distance sources and produce time delays between mirage images. Gravitationally-induced time delays depend on the position of the emitting regions in the source plane. The Fermi/LAT satellite continuously monitors the entire sky and detects gamma-ray flares, including those from gravitationally-lensed blazars. Therefore, temporal resolution at gamma-ray energies can be used to measure these time delays, which, in turn, can be used to resolve the origin of the gamma-ray flares spatially. We provide a guide to the application and Monte Carlo simulation of three techniques for analyzing these unresolved light curves: the Autocorrelation Function, the Double Power Spectrum, and the Maximum Peak Method. We apply these methods to derive time delays from the gamma-ray light curve of the gravitationally-lensed blazar PKS 1830-211. The result of temporal analysis combined with the properties of the lens from radio observations yield an improvement in spatial resolution at gamma-ray energies by a factor of 10000. We analyze four active periods. For two of these periods, the emission is consistent with origination from the core and for the other two, the data suggest that the emission region is displaced from the core by more that ~1.5 kpc. For the core emission, the gamma-ray time delays, $23\pm0.5$ days and $19.7\pm1.2$ days, are consistent with the radio time delay $26^{+4}_{-5}$ days. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.05210v2-abstract-full').style.display = 'none'; document.getElementById('1504.05210v2-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 July, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 April, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1502.03244">arXiv:1502.03244</a> <span> [<a href="https://arxiv.org/pdf/1502.03244">pdf</a>, <a href="https://arxiv.org/ps/1502.03244">ps</a>, <a href="https://arxiv.org/format/1502.03244">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/10.1103/PhysRevLett.114.081301">10.1103/PhysRevLett.114.081301 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraints on an Annihilation Signal from a Core of Constant Dark Matter Density around the Milky Way Center with H.E.S.S </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=HESS+Collaboration"> HESS Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abramowski%2C+A">A. Abramowski</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Akhperjanian%2C+A+G">A. G. Akhperjanian</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Balenderan%2C+S">S. Balenderan</a>, <a href="/search/astro-ph?searchtype=author&query=Balzer%2C+A">A. Balzer</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</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=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernhard%2C+S">S. Bernhard</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Birsin%2C+E">E. Birsin</a>, <a href="/search/astro-ph?searchtype=author&query=Biteau%2C+J">J. Biteau</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=Bordas%2C+P">P. Bordas</a>, <a href="/search/astro-ph?searchtype=author&query=Bregeon%2C+J">J. Bregeon</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+P">P. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bryan%2C+M">M. Bryan</a> , et al. (201 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="1502.03244v2-abstract-short" style="display: inline;"> An annihilation signal of dark matter is searched for from the central region of the Milky Way. Data acquired in dedicated ON/OFF observations of the Galactic center region with H.E.S.S. are analyzed for this purpose. No significant signal is found in a total of $\sim 9$ h of ON/OFF observations. Upper limits on the velocity averaged cross section, $<蟽v >$, for the annihilation of dark matter part… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1502.03244v2-abstract-full').style.display = 'inline'; document.getElementById('1502.03244v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1502.03244v2-abstract-full" style="display: none;"> An annihilation signal of dark matter is searched for from the central region of the Milky Way. Data acquired in dedicated ON/OFF observations of the Galactic center region with H.E.S.S. are analyzed for this purpose. No significant signal is found in a total of $\sim 9$ h of ON/OFF observations. Upper limits on the velocity averaged cross section, $<蟽v >$, for the annihilation of dark matter particles with masses in the range of $\sim 300$ GeV to $\sim 10$ TeV are derived. In contrast to previous constraints derived from observations of the Galactic center region, the constraints that are derived here apply also under the assumption of a central core of constant dark matter density around the center of the Galaxy. Values of $<蟽v >$ that are larger than $3\cdot 10^{-24}\:\mathrm{cm^3/s}$ are excluded for dark matter particles with masses between $\sim 1$ and $\sim 4$ TeV at 95% CL if the radius of the central dark matter density core does not exceed $500$ pc. This is the strongest constraint that is derived on $<蟽v>$ for annihilating TeV mass dark matter without the assumption of a centrally cusped dark matter density distribution in the search region. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1502.03244v2-abstract-full').style.display = 'none'; document.getElementById('1502.03244v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 February, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 February, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication by Physical Review Letters, contact authors: Ullrich Schwanke (schwanke@physik.hu-berlin.de, Humboldt Universitaet zu Berlin, Berlin) and Gerrit Spengler (gerrit.spengler@fysik.su.se, Oscar Klein Centre for Cosmoparticle Physics, Stockholm)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 114, 081301 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1501.06578">arXiv:1501.06578</a> <span> [<a href="https://arxiv.org/pdf/1501.06578">pdf</a>, <a href="https://arxiv.org/format/1501.06578">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/10.1126/science.1261313">10.1126/science.1261313 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The exceptionally powerful TeV gamma-ray emitters in the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abramowski%2C+A">A. Abramowski</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Akhperjanian%2C+A+G">A. G. Akhperjanian</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Balenderan%2C+S">S. Balenderan</a>, <a href="/search/astro-ph?searchtype=author&query=Balzer%2C+A">A. Balzer</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Becker-Tjus%2C+J">J. Becker-Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernhard%2C+S">S. Bernhard</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Birsin%2C+E">E. Birsin</a>, <a href="/search/astro-ph?searchtype=author&query=Biteau%2C+J">J. Biteau</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=Bordas%2C+P">P. Bordas</a>, <a href="/search/astro-ph?searchtype=author&query=Bregeon%2C+J">J. Bregeon</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+P">P. Brun</a> , et al. (204 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="1501.06578v1-abstract-short" style="display: inline;"> The Large Magellanic Cloud, a satellite galaxy of the Milky Way, has been observed with the High Energy Stereoscopic System (H.E.S.S.) above an energy of 100 billion electron volts for a deep exposure of 210 hours. Three sources of different types were detected: the pulsar wind nebula of the most energetic pulsar known N 157B, the radio-loud supernova remnant N 132D and the largest non-thermal X-r… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1501.06578v1-abstract-full').style.display = 'inline'; document.getElementById('1501.06578v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1501.06578v1-abstract-full" style="display: none;"> The Large Magellanic Cloud, a satellite galaxy of the Milky Way, has been observed with the High Energy Stereoscopic System (H.E.S.S.) above an energy of 100 billion electron volts for a deep exposure of 210 hours. Three sources of different types were detected: the pulsar wind nebula of the most energetic pulsar known N 157B, the radio-loud supernova remnant N 132D and the largest non-thermal X-ray shell - the superbubble 30 Dor C. The unique object SN 1987A is, surprisingly, not detected, which constrains the theoretical framework of particle acceleration in very young supernova remnants. These detections reveal the most energetic tip of a gamma-ray source population in an external galaxy, and provide via 30 Dor C the unambiguous detection of gamma-ray emission from a superbubble. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1501.06578v1-abstract-full').style.display = 'none'; document.getElementById('1501.06578v1-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 January, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">Published in Science Magazine (Jan. 23, 2015). This ArXiv version has the supplementary online material incorporated as an appendix to the main paper</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Science, 2015, 347, issue 6220, p. 406 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1501.05087">arXiv:1501.05087</a> <span> [<a href="https://arxiv.org/pdf/1501.05087">pdf</a>, <a href="https://arxiv.org/ps/1501.05087">ps</a>, <a href="https://arxiv.org/format/1501.05087">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/802/1/65">10.1088/0004-637X/802/1/65 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The 2012 flare of PG 1553+113 seen with H.E.S.S. and Fermi-LAT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abramowski%2C+A">A. Abramowski</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Akhperjanian%2C+A+G">A. G. Akhperjanian</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Balenderan%2C+S">S. Balenderan</a>, <a href="/search/astro-ph?searchtype=author&query=Balzer%2C+A">A. Balzer</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</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=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernhard%2C+S">S. Bernhard</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Birsin%2C+E">E. Birsin</a>, <a href="/search/astro-ph?searchtype=author&query=Biteau%2C+J">J. Biteau</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=Bordas%2C+P">P. Bordas</a>, <a href="/search/astro-ph?searchtype=author&query=Bregeon%2C+J">J. Bregeon</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+P">P. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bryan%2C+M">M. Bryan</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a> , et al. (202 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="1501.05087v1-abstract-short" style="display: inline;"> Very high energy (VHE, $E>$100 GeV) $纬$-ray flaring activity of the high-frequency peaked BL Lac object \pg\ has been detected by the \hess\ telescopes. The flux of the source increased by a factor of 3 during the nights of 2012 April 26 and 27 with respect to the archival measurements with hint of intra-night variability. No counterpart of this event has been detected in the \fla\ data. This patt… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1501.05087v1-abstract-full').style.display = 'inline'; document.getElementById('1501.05087v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1501.05087v1-abstract-full" style="display: none;"> Very high energy (VHE, $E>$100 GeV) $纬$-ray flaring activity of the high-frequency peaked BL Lac object \pg\ has been detected by the \hess\ telescopes. The flux of the source increased by a factor of 3 during the nights of 2012 April 26 and 27 with respect to the archival measurements with hint of intra-night variability. No counterpart of this event has been detected in the \fla\ data. This pattern is consistent with VHE $纬$ ray flaring being caused by the injection of ultrarelativistic particles, emitting $纬$ rays at the highest energies. The dataset offers a unique opportunity to constrain the redshift of this source at \bestz\ using a novel method based on Bayesian statistics. The indication of intra-night variability is used to introduce a novel method to probe for a possible Lorentz Invariance Violation (LIV), and to set limits on the energy scale at which Quantum Gravity (QG) effects causing LIV may arise. For the subluminal case, the derived limits are $\textrm{E}_{\rm QG,1}>4.10\times 10^{17}$ GeV and $\textrm{E}_{\rm QG,2}>2.10\times 10^{10}$ GeV for linear and quadratic LIV effects, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1501.05087v1-abstract-full').style.display = 'none'; document.getElementById('1501.05087v1-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 January, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">39 pages, 9 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/1412.6997">arXiv:1412.6997</a> <span> [<a href="https://arxiv.org/pdf/1412.6997">pdf</a>, <a href="https://arxiv.org/format/1412.6997">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/10.1051/0004-6361/201424805">10.1051/0004-6361/201424805 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> H.E.S.S. reveals a lack of TeV emission from the supernova remnant Puppis A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abramowski%2C+A">A. Abramowski</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Akhperjanian%2C+A+G">A. G. Akhperjanian</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Balenderan%2C+S">S. Balenderan</a>, <a href="/search/astro-ph?searchtype=author&query=Balzer%2C+A">A. Balzer</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</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=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernhard%2C+S">S. Bernhard</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Birsin%2C+E">E. Birsin</a>, <a href="/search/astro-ph?searchtype=author&query=Biteau%2C+J">J. Biteau</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=Bordas%2C+P">P. Bordas</a>, <a href="/search/astro-ph?searchtype=author&query=Bregeon%2C+J">J. Bregeon</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+P">P. Brun</a> , et al. (202 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="1412.6997v2-abstract-short" style="display: inline;"> Puppis A is an interesting ~4 kyr-old supernova remnant (SNR) that shows strong evidence of interaction between the forward shock and a molecular cloud. It has been studied in detail from radio frequencies to high-energy (HE, 0.1-100 GeV) gamma-rays. An analysis of the Fermi-LAT data has shown an extended HE gamma-ray emission with a 0.2-100 GeV spectrum exhibiting no significant deviation from a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.6997v2-abstract-full').style.display = 'inline'; document.getElementById('1412.6997v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1412.6997v2-abstract-full" style="display: none;"> Puppis A is an interesting ~4 kyr-old supernova remnant (SNR) that shows strong evidence of interaction between the forward shock and a molecular cloud. It has been studied in detail from radio frequencies to high-energy (HE, 0.1-100 GeV) gamma-rays. An analysis of the Fermi-LAT data has shown an extended HE gamma-ray emission with a 0.2-100 GeV spectrum exhibiting no significant deviation from a power law, unlike most of the GeV-emitting SNRs known to be interacting with molecular clouds. This makes it a promising target for imaging atmospheric Cherenkov telescopes (IACTs) to probe the gamma-ray emission above 100 GeV. Very-high-energy (VHE, E >= 0.1 TeV) gamma-ray emission from Puppis A is for the first time searched for with the High Energy Stereoscopic System (H.E.S.S.). The analysis of the H.E.S.S. data does not reveal any significant emission towards Puppis A. The derived upper limits on the differential photon flux imply that its broadband gamma-ray spectrum must exhibit a spectral break or cutoff. By combining Fermi-LAT and H.E.S.S. measurements, the 99% confidence level upper limits on such a cutoff are found to be 450 and 280 GeV, assuming a power law with a simple exponential and a sub-exponential cutoff, respectively. It is concluded that none of the standard limitations (age, size, radiative losses) on the particle acceleration mechanism, assumed to be still on-going at present, can explain the lack of VHE signal. The scenario in which particle acceleration has ceased some time ago is considered as an alternative explanation. The HE/VHE spectrum of Puppis A could then exhibit a break of non-radiative origin, (as observed in several other interacting SNRs, albeit at somewhat higher energies) owing to the interaction with dense and neutral material in particular towards the northeastern region. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.6997v2-abstract-full').style.display = 'none'; document.getElementById('1412.6997v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 March, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 December, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">Published in A&A 27 Jan 2015. 7 pages, 2 figures, 1 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 575, A81 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1412.4734">arXiv:1412.4734</a> <span> [<a href="https://arxiv.org/pdf/1412.4734">pdf</a>, <a href="https://arxiv.org/format/1412.4734">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/800/1/61">10.1088/0004-637X/800/1/61 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Search for Pulsations from Geminga Above 100 GeV with VERITAS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aliu%2C+E">E. Aliu</a>, <a href="/search/astro-ph?searchtype=author&query=Archambault%2C+S">S. Archambault</a>, <a href="/search/astro-ph?searchtype=author&query=Archer%2C+A">A. Archer</a>, <a href="/search/astro-ph?searchtype=author&query=Aune%2C+T">T. Aune</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Beilicke%2C+M">M. Beilicke</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">W. Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Bird%2C+R">R. Bird</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Bugaev%2C+V">V. Bugaev</a>, <a href="/search/astro-ph?searchtype=author&query=Byrum%2C+K">K. Byrum</a>, <a href="/search/astro-ph?searchtype=author&query=Cardenzana%2C+J+V">J. V Cardenzana</a>, <a href="/search/astro-ph?searchtype=author&query=Cerruti%2C+M">M. Cerruti</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">X. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Ciupik%2C+L">L. Ciupik</a>, <a href="/search/astro-ph?searchtype=author&query=Connolly%2C+M+P">M. P. Connolly</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+W">W. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+H+J">H. J. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Dumm%2C+J">J. Dumm</a>, <a href="/search/astro-ph?searchtype=author&query=Eisch%2C+J+D">J. D. Eisch</a>, <a href="/search/astro-ph?searchtype=author&query=Errando%2C+M">M. Errando</a>, <a href="/search/astro-ph?searchtype=author&query=Falcone%2C+A">A. Falcone</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+Q">Q. Feng</a>, <a href="/search/astro-ph?searchtype=author&query=Finley%2C+J+P">J. P. Finley</a>, <a href="/search/astro-ph?searchtype=author&query=Fleischhack%2C+H">H. Fleischhack</a> , et al. (59 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="1412.4734v1-abstract-short" style="display: inline;"> We present the results of 71.6 hours of observations of the Geminga pulsar (PSR J0633+1746) with the VERITAS very-high-energy gamma-ray telescope array. Data taken with VERITAS between November 2007 and February 2013 were phase-folded using a Geminga pulsar timing solution derived from data recorded by the XMM-\emph{Newton} and \emph{Fermi}-LAT space telescopes. No significant pulsed emission abov… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.4734v1-abstract-full').style.display = 'inline'; document.getElementById('1412.4734v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1412.4734v1-abstract-full" style="display: none;"> We present the results of 71.6 hours of observations of the Geminga pulsar (PSR J0633+1746) with the VERITAS very-high-energy gamma-ray telescope array. Data taken with VERITAS between November 2007 and February 2013 were phase-folded using a Geminga pulsar timing solution derived from data recorded by the XMM-\emph{Newton} and \emph{Fermi}-LAT space telescopes. No significant pulsed emission above 100 GeV is observed, and we report upper limits at the 95% confidence level on the integral flux above 135 GeV (spectral analysis threshold) of 4.0$\times10^{-13}$ s$^{-1}$ cm$^{-2}$ and 1.7$\times10^{-13}$ s$^{-1}$ cm$^{-2}$ for the two principal peaks in the emission profile. These upper limits, placed in context with phase-resolved spectral energy distributions determined from five years of data from the \emph{Fermi}-LAT, constrain possible hardening of the Geminga pulsar emission spectra above $\sim$50 GeV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.4734v1-abstract-full').style.display = 'none'; document.getElementById('1412.4734v1-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 December, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">7 pages, 2 figures, 2 tables. Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1412.2251">arXiv:1412.2251</a> <span> [<a href="https://arxiv.org/pdf/1412.2251">pdf</a>, <a href="https://arxiv.org/format/1412.2251">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/10.1051/0004-6361/201425070">10.1051/0004-6361/201425070 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> H.E.S.S. detection of TeV emission from the interaction region between the supernova remnant G349.7+0.2 and a molecular cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abramowski%2C+A">A. Abramowski</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Akhperjanian%2C+A+G">A. G. Akhperjanian</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Balenderan%2C+S">S. Balenderan</a>, <a href="/search/astro-ph?searchtype=author&query=Balzer%2C+A">A. Balzer</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</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=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernhard%2C+S">S. Bernhard</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Birsin%2C+E">E. Birsin</a>, <a href="/search/astro-ph?searchtype=author&query=Biteau%2C+J">J. Biteau</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=Bordas%2C+P">P. Bordas</a>, <a href="/search/astro-ph?searchtype=author&query=Bregeon%2C+J">J. Bregeon</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+P">P. Brun</a> , et al. (202 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="1412.2251v2-abstract-short" style="display: inline;"> G349.7+0.2 is a young Galactic supernova remnant (SNR) located at the distance of 11.5 kpc and observed across the entire electromagnetic spectrum from radio to high energy (HE) Gamma-rays. Radio and infrared observations indicate that the remnant is interacting with a molecular cloud. In this paper, the detection of very high energy (VHE) Gamma-ray emission coincident with this SNR with the High… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.2251v2-abstract-full').style.display = 'inline'; document.getElementById('1412.2251v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1412.2251v2-abstract-full" style="display: none;"> G349.7+0.2 is a young Galactic supernova remnant (SNR) located at the distance of 11.5 kpc and observed across the entire electromagnetic spectrum from radio to high energy (HE) Gamma-rays. Radio and infrared observations indicate that the remnant is interacting with a molecular cloud. In this paper, the detection of very high energy (VHE) Gamma-ray emission coincident with this SNR with the High Energy Stereoscopic System (H.E.S.S.) is reported. An integral flux F(E>400GeV)=(6.5 +-1.1stat +-1.3syst) x 10^{-13} ph/cm/s corresponding to 0.7% of that of the Crab Nebula and to a luminosity of 10^34 erg/s above the same energy threshold, and a steep photon index Gamma_VHE = 2.8 +-0.27stat +-0.20syst are measured. The analysis of more than 5 yr of Fermi-LAT data towards this source shows a power-law like spectrum with a best-fit photon index Gamma_HE = 2.2 +-0.04stat +0.13-0.31syst. The combined Gamma-ray spectrum of G349.7+0.2 can be described by either a broken power-law (BPL) or a power-law with exponential (or sub-exponential) cutoff (PLC). In the former case, the photon break energy is found at E_br,gamma = 55 +70-30 GeV, slightly higher than what is usually observed in the HE/VHE Gamma-ray emitting middle-aged SNRs known to be interacting with molecular clouds. In the latter case, the exponential (respectively sub-exponential) cutoff energy is measured at E_cut,gamma = 1.4 +1.6-0.55 (respectively 0.35 +0.75-0.21) TeV. A pion-decay process resulting from the interaction of the accelerated protons and nuclei with the dense surrounding medium is clearly the preferred scenario to explain the Gamma-ray emission. The BPL with a spectral steepening of 0.5-1 and the PLC provide equally good fits to the data. The product of the average gas density and the total energy content of accelerated protons and nuclei amounts to nH Wp ~ 5 x 10^51 erg/cm3. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.2251v2-abstract-full').style.display = 'none'; document.getElementById('1412.2251v2-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 December, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 December, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A on November 24, 2014</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 574, A100 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1412.1031">arXiv:1412.1031</a> <span> [<a href="https://arxiv.org/pdf/1412.1031">pdf</a>, <a href="https://arxiv.org/ps/1412.1031">ps</a>, <a href="https://arxiv.org/format/1412.1031">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/797/2/89">10.1088/0004-637X/797/2/89 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Investigating Broadband Variability of the TeV Blazar 1ES 1959+650 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aliu%2C+E">E. Aliu</a>, <a href="/search/astro-ph?searchtype=author&query=Archambault%2C+S">S. Archambault</a>, <a href="/search/astro-ph?searchtype=author&query=Arlen%2C+T">T. Arlen</a>, <a href="/search/astro-ph?searchtype=author&query=Aune%2C+T">T. Aune</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Beilicke%2C+M">M. Beilicke</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">W. Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+K">K. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Bird%2C+R">R. Bird</a>, <a href="/search/astro-ph?searchtype=author&query=Bouvier%2C+A">A. Bouvier</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Bugaev%2C+V">V. Bugaev</a>, <a href="/search/astro-ph?searchtype=author&query=Cerruti%2C+M">M. Cerruti</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">X. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Ciupik%2C+L">L. Ciupik</a>, <a href="/search/astro-ph?searchtype=author&query=Collins-Hughes%2C+E">E. Collins-Hughes</a>, <a href="/search/astro-ph?searchtype=author&query=Connolly%2C+M+P">M. P. Connolly</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+W">W. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Dumm%2C+J">J. Dumm</a>, <a href="/search/astro-ph?searchtype=author&query=Eisch%2C+J+D">J. D. Eisch</a>, <a href="/search/astro-ph?searchtype=author&query=Falcone%2C+A">A. Falcone</a>, <a href="/search/astro-ph?searchtype=author&query=Federici%2C+S">S. Federici</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+Q">Q. Feng</a>, <a href="/search/astro-ph?searchtype=author&query=Finley%2C+J+P">J. P. Finley</a>, <a href="/search/astro-ph?searchtype=author&query=Fleischhack%2C+H">H. Fleischhack</a> , et al. (70 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="1412.1031v1-abstract-short" style="display: inline;"> We summarize broadband observations of the TeV-emitting blazar 1ES 1959+650, including optical R-band observations by the robotic telescopes Super-LOTIS and iTelescope, UV observations by Swift UVOT, X-ray observations by the Swift X-ray Telescope (XRT), high-energy gamma-ray observations with the Fermi Large Area Telescope (LAT) and very-high-energy (VHE) gamma-ray observations by VERITAS above 3… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.1031v1-abstract-full').style.display = 'inline'; document.getElementById('1412.1031v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1412.1031v1-abstract-full" style="display: none;"> We summarize broadband observations of the TeV-emitting blazar 1ES 1959+650, including optical R-band observations by the robotic telescopes Super-LOTIS and iTelescope, UV observations by Swift UVOT, X-ray observations by the Swift X-ray Telescope (XRT), high-energy gamma-ray observations with the Fermi Large Area Telescope (LAT) and very-high-energy (VHE) gamma-ray observations by VERITAS above 315 GeV, all taken between 17 April 2012 and 1 June 2012 (MJD 56034 and 56079). The contemporaneous variability of the broadband spectral energy distribution is explored in the context of a simple synchrotron self Compton (SSC) model. In the SSC emission scenario, we find that the parameters required to represent the high state are significantly different than those in the low state. Motivated by possible evidence of gas in the vicinity of the blazar, we also investigate a reflected-emission model to describe the observed variability pattern. This model assumes that the non-thermal emission from the jet is reflected by a nearby cloud of gas, allowing the reflected emission to re-enter the blob and produce an elevated gamma-ray state with no simultaneous elevated synchrotron flux. The model applied here, although not required to explain the observed variability pattern, represents one possible scenario which can describe the observations. As applied to an elevated VHE state of 66% of the Crab Nebula flux, observed on a single night during the observation period, the reflected-emission scenario does not support a purely leptonic non-thermal emission mechanism. The reflected emission model does, however, predict a reflected photon field with sufficient energy to enable elevated gamma-ray emission via pion production with protons of energies between 10 and 100 TeV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.1031v1-abstract-full').style.display = 'none'; document.getElementById('1412.1031v1-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> 2 December, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1411.7568">arXiv:1411.7568</a> <span> [<a href="https://arxiv.org/pdf/1411.7568">pdf</a>, <a href="https://arxiv.org/ps/1411.7568">ps</a>, <a href="https://arxiv.org/format/1411.7568">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/10.1103/PhysRevD.90.122007">10.1103/PhysRevD.90.122007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Diffuse Galactic gamma-ray emission with H.E.S.S </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abramowski%2C+A">A. Abramowski</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Akhperjanian%2C+A+G">A. G. Akhperjanian</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Balenderan%2C+S">S. Balenderan</a>, <a href="/search/astro-ph?searchtype=author&query=Balzer%2C+A">A. Balzer</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</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=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernhard%2C+S">S. Bernhard</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Birsin%2C+E">E. Birsin</a>, <a href="/search/astro-ph?searchtype=author&query=Biteau%2C+J">J. Biteau</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=Bordas%2C+P">P. Bordas</a>, <a href="/search/astro-ph?searchtype=author&query=Bregeon%2C+J">J. Bregeon</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+P">P. Brun</a> , et al. (203 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="1411.7568v1-abstract-short" style="display: inline;"> Diffuse $纬$-ray emission is the most prominent observable signature of celestial cosmic-ray interactions at high energies. While already being investigated at GeV energies over several decades, assessments of diffuse $纬$-ray emission at TeV energies remain sparse. After completion of the systematic survey of the inner Galaxy, the H.E.S.S. experiment is in a prime position to observe large-scale di… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1411.7568v1-abstract-full').style.display = 'inline'; document.getElementById('1411.7568v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1411.7568v1-abstract-full" style="display: none;"> Diffuse $纬$-ray emission is the most prominent observable signature of celestial cosmic-ray interactions at high energies. While already being investigated at GeV energies over several decades, assessments of diffuse $纬$-ray emission at TeV energies remain sparse. After completion of the systematic survey of the inner Galaxy, the H.E.S.S. experiment is in a prime position to observe large-scale diffuse emission at TeV energies. Data of the H.E.S.S. Galactic Plane Survey are investigated in regions off known $纬$-ray sources. Corresponding $纬$-ray flux measurements were made over an extensive grid of celestial locations. Longitudinal and latitudinal profiles of the observed $纬$-ray fluxes show characteristic excess emission not attributable to known $纬$-ray sources. For the first time large-scale $纬$-ray emission along the Galactic Plane using imaging atmospheric Cherenkov telescopes has been observed. While the background subtraction technique limits the ability to recover modest variation on the scale of the H.E.S.S. field of view or larger, which is characteristic of the inverse Compton scatter-induced Galactic diffuse emission, contributions of neutral pion decay as well as emission from unresolved $纬$-ray sources can be recovered in the observed signal to a large fraction. Calculations show that the minimum $纬$-ray emission from $蟺^0$-decay represents a significant contribution to the total signal. This detection is interpreted as a mix of diffuse Galactic $纬$-ray emission and unresolved sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1411.7568v1-abstract-full').style.display = 'none'; document.getElementById('1411.7568v1-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 November, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">8 pages, 2 figures, accepted for publication in Physical Review D</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1411.1439">arXiv:1411.1439</a> <span> [<a href="https://arxiv.org/pdf/1411.1439">pdf</a>, <a href="https://arxiv.org/format/1411.1439">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/799/1/7">10.1088/0004-637X/799/1/7 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VERITAS Observations of the BL Lac Object PG 1553+113 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aliu%2C+E">E. Aliu</a>, <a href="/search/astro-ph?searchtype=author&query=Archer%2C+A">A. Archer</a>, <a href="/search/astro-ph?searchtype=author&query=Aune%2C+T">T. Aune</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Behera%2C+B">B. Behera</a>, <a href="/search/astro-ph?searchtype=author&query=Beilicke%2C+M">M. Beilicke</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">W. Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+K">K. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Bird%2C+R">R. Bird</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Bugaev%2C+V">V. Bugaev</a>, <a href="/search/astro-ph?searchtype=author&query=Byrum%2C+K">K. Byrum</a>, <a href="/search/astro-ph?searchtype=author&query=Cardenzana%2C+J+V">J. V Cardenzana</a>, <a href="/search/astro-ph?searchtype=author&query=Cerruti%2C+M">M. Cerruti</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">X. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Ciupik%2C+L">L. Ciupik</a>, <a href="/search/astro-ph?searchtype=author&query=Connolly%2C+M+P">M. P. Connolly</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+W">W. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+H+J">H. J. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Dumm%2C+J">J. Dumm</a>, <a href="/search/astro-ph?searchtype=author&query=Eisch%2C+J+D">J. D. Eisch</a>, <a href="/search/astro-ph?searchtype=author&query=Errando%2C+M">M. Errando</a>, <a href="/search/astro-ph?searchtype=author&query=Falcone%2C+A">A. Falcone</a>, <a href="/search/astro-ph?searchtype=author&query=Federici%2C+S">S. Federici</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+Q">Q. Feng</a> , et al. (62 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="1411.1439v1-abstract-short" style="display: inline;"> We present results from VERITAS observations of the BL Lac object PG 1553+113 spanning the years 2010, 2011, and 2012. The time-averaged spectrum, measured between 160 and 560\,GeV, is well described by a power law with a spectral index of $4.33 \pm 0.09$. The time-averaged integral flux above $200\,$GeV measured for this period was… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1411.1439v1-abstract-full').style.display = 'inline'; document.getElementById('1411.1439v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1411.1439v1-abstract-full" style="display: none;"> We present results from VERITAS observations of the BL Lac object PG 1553+113 spanning the years 2010, 2011, and 2012. The time-averaged spectrum, measured between 160 and 560\,GeV, is well described by a power law with a spectral index of $4.33 \pm 0.09$. The time-averaged integral flux above $200\,$GeV measured for this period was $(1.69 \pm 0.06) \times 10^{-11} \, \mathrm{ph} \, \mathrm{cm}^{-2} \, \mathrm{s}^{-1}$, corresponding to 6.9\% of the Crab Nebula flux. We also present the combined $纬$-ray spectrum from the Fermi Large Area Telescope and VERITAS covering an energy range from 100~MeV to 560~GeV. The data are well fit by a power law with an exponential cutoff at $\rm {101.9 \pm 3.2 \, \mathrm{GeV}} $. The origin of the cutoff could be intrinsic to PG~1553+113 or be due to the $纬$-ray opacity of our universe through pair production off the extragalactic background light (EBL). Given lower limits to the redshift of $\rm z \negthinspace > \negthinspace 0.395$ based on optical/UV observations of PG~1553+113, the cutoff would be dominated by EBL absorption. Conversely, the small statistical uncertainties of the VERITAS energy spectrum have allowed us to provide a robust upper limit on the redshift of PG 1553+113 of $z \negthinspace \leq \negthinspace 0.62$. A strongly-elevated mean flux of $(2.50 \pm 0.14) \times 10^{-11} \, \mathrm{ph} \, \mathrm{cm}^{-2} \, \mathrm{s}^{-1}$ (10.3\% of the Crab Nebula flux) was observed during 2012, with the daily flux reaching as high as $(4.44 \pm 0.71) \times 10^{-11} \, \mathrm{ph} \, \mathrm{cm}^{-2} \, \mathrm{s}^{-1}$ (18.3\% of the Crab Nebula flux) on MJD 56048. The light curve measured during the 2012 observing season is marginally inconsistent with a steady flux, giving a $蠂^2$ probability for a steady flux of 0.03\%. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1411.1439v1-abstract-full').style.display = 'none'; document.getElementById('1411.1439v1-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 November, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">in press in ApJ, 2014</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1411.0572">arXiv:1411.0572</a> <span> [<a href="https://arxiv.org/pdf/1411.0572">pdf</a>, <a href="https://arxiv.org/ps/1411.0572">ps</a>, <a href="https://arxiv.org/format/1411.0572">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/stu2148">10.1093/mnras/stu2148 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of the VHE gamma-ray source HESS J1832-093 in the vicinity of SNR G22.7-0.2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abramowski%2C+A">A. Abramowski</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Akhperjanian%2C+A+G">A. G. Akhperjanian</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E">E. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Balenderan%2C+S">S. Balenderan</a>, <a href="/search/astro-ph?searchtype=author&query=Balzer%2C+A">A. Balzer</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</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=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Birsin%2C+E">E. Birsin</a>, <a href="/search/astro-ph?searchtype=author&query=Bissaldi%2C+E">E. Bissaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Biteau%2C+J">J. Biteau</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=Bordas%2C+P">P. Bordas</a>, <a href="/search/astro-ph?searchtype=author&query=Brucker%2C+J">J. Brucker</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+P">P. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a> , et al. (196 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="1411.0572v1-abstract-short" style="display: inline;"> The region around the supernova remnant (SNR) W41 contains several TeV sources and has prompted the H.E.S.S. Collaboration to perform deep observations of this field of view. This resulted in the discovery of the new very high energy (VHE) source HESS J1832-093, at the position… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1411.0572v1-abstract-full').style.display = 'inline'; document.getElementById('1411.0572v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1411.0572v1-abstract-full" style="display: none;"> The region around the supernova remnant (SNR) W41 contains several TeV sources and has prompted the H.E.S.S. Collaboration to perform deep observations of this field of view. This resulted in the discovery of the new very high energy (VHE) source HESS J1832-093, at the position $\rm RA=18^h 32^m 50^s \pm 3^s_{stat} \pm 2^s_{syst}, \rm Dec=-9^\circ 22' 36'' \pm 32''_{stat} \pm 20''_{syst} (J2000)$, spatially coincident with a part of the radio shell of the neighboring remnant G22.7-0.2. The photon spectrum is well described by a power-law of index $螕= 2.6 \pm 0.3_{\rm stat} \pm 0.1_{\rm syst}$ and a normalization at 1 TeV of $桅_0=(4.8 \pm 0.8_{\rm stat}\pm 1.0_{\rm syst})\,\times\,10^{-13}\,\rm{cm} ^{-2}\,s^{-1}\,TeV^{-1}$. The location of the gamma-ray emission on the edge of the SNR rim first suggested a signature of escaping cosmic-rays illuminating a nearby molecular cloud. Then a dedicated XMM-Newton observation led to the discovery of a new X-ray point source spatially coincident with the TeV excess. Two other scenarios were hence proposed to identify the nature of HESS J1832-093. Gamma-rays from inverse Compton radiation in the framework of a pulsar wind nebula scenario or the possibility of gamma-ray production within a binary system are therefore also considered. Deeper multi-wavelength observations will help to shed new light on this intriguing VHE source. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1411.0572v1-abstract-full').style.display = 'none'; document.getElementById('1411.0572v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 November, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">6 pages, 4 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/1410.5367">arXiv:1410.5367</a> <span> [<a href="https://arxiv.org/pdf/1410.5367">pdf</a>, <a href="https://arxiv.org/format/1410.5367">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/2041-8205/795/1/L3">10.1088/2041-8205/795/1/L3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraints on Very High Energy Emission from GRB 130427A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aliu%2C+E">E. Aliu</a>, <a href="/search/astro-ph?searchtype=author&query=Aune%2C+T">T. Aune</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Beilicke%2C+M">M. Beilicke</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">W. Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+K">K. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Biteau%2C+J">J. Biteau</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Bugaev%2C+V">V. Bugaev</a>, <a href="/search/astro-ph?searchtype=author&query=Byrum%2C+K">K. Byrum</a>, <a href="/search/astro-ph?searchtype=author&query=Cardenzana%2C+J+V">J. V Cardenzana</a>, <a href="/search/astro-ph?searchtype=author&query=Cerruti%2C+M">M. Cerruti</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">X. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Ciupik%2C+L">L. Ciupik</a>, <a href="/search/astro-ph?searchtype=author&query=Connaughton%2C+V">V. Connaughton</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+W">W. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+H+J">H. J. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Eisch%2C+J+D">J. D. Eisch</a>, <a href="/search/astro-ph?searchtype=author&query=Errando%2C+M">M. Errando</a>, <a href="/search/astro-ph?searchtype=author&query=Falcone%2C+A">A. Falcone</a>, <a href="/search/astro-ph?searchtype=author&query=Federici%2C+S">S. Federici</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+Q">Q. Feng</a>, <a href="/search/astro-ph?searchtype=author&query=Finley%2C+J+P">J. P. Finley</a>, <a href="/search/astro-ph?searchtype=author&query=Fleischhack%2C+H">H. Fleischhack</a>, <a href="/search/astro-ph?searchtype=author&query=Fortin%2C+P">P. Fortin</a> , et al. (67 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="1410.5367v1-abstract-short" style="display: inline;"> Prompt emission from the very fluent and nearby (z=0.34) gamma-ray burst GRB 130427A was detected by several orbiting telescopes and by ground-based, wide-field-of-view optical transient monitors. Apart from the intensity and proximity of this GRB, it is exceptional due to the extremely long-lived high-energy (100 MeV to 100 GeV) gamma-ray emission, which was detected by the Large Area Telescope o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1410.5367v1-abstract-full').style.display = 'inline'; document.getElementById('1410.5367v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1410.5367v1-abstract-full" style="display: none;"> Prompt emission from the very fluent and nearby (z=0.34) gamma-ray burst GRB 130427A was detected by several orbiting telescopes and by ground-based, wide-field-of-view optical transient monitors. Apart from the intensity and proximity of this GRB, it is exceptional due to the extremely long-lived high-energy (100 MeV to 100 GeV) gamma-ray emission, which was detected by the Large Area Telescope on the Fermi Gamma-ray Space Telescope for ~70 ks after the initial burst. The persistent, hard-spectrum, high-energy emission suggests that the highest-energy gamma rays may have been produced via synchrotron self-Compton processes though there is also evidence that the high-energy emission may instead be an extension of the synchrotron spectrum. VERITAS, a ground-based imaging atmospheric Cherenkov telescope array, began follow-up observations of GRB 130427A ~71 ks (~20 hr) after the onset of the burst. The GRB was not detected with VERITAS; however, the high elevation of the observations, coupled with the low redshift of the GRB, make VERITAS a very sensitive probe of the emission from GRB 130427A for E > 100 GeV. The non-detection and consequent upper limit derived place constraints on the synchrotron self-Compton model of high-energy gamma-ray emission from this burst. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1410.5367v1-abstract-full').style.display = 'none'; document.getElementById('1410.5367v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 October, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">22 pages, 4 figures, 1 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophysical Journal Letters, 795, 2014, L3 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1410.2589">arXiv:1410.2589</a> <span> [<a href="https://arxiv.org/pdf/1410.2589">pdf</a>, <a href="https://arxiv.org/format/1410.2589">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/10.1103/PhysRevD.90.112012">10.1103/PhysRevD.90.112012 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for dark matter annihilation signatures in H.E.S.S. observations of Dwarf Spheroidal Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abramowski%2C+A">A. Abramowski</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Akhperjanian%2C+A+G">A. G. Akhperjanian</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E">E. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Balenderan%2C+S">S. Balenderan</a>, <a href="/search/astro-ph?searchtype=author&query=Balzer%2C+A">A. Balzer</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</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=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernhard%2C+S">S. Bernhard</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Birsin%2C+E">E. Birsin</a>, <a href="/search/astro-ph?searchtype=author&query=Biteau%2C+J">J. Biteau</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=Bordas%2C+P">P. Bordas</a>, <a href="/search/astro-ph?searchtype=author&query=Bregeon%2C+J">J. Bregeon</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+P">P. Brun</a> , et al. (207 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="1410.2589v3-abstract-short" style="display: inline;"> Dwarf spheroidal galaxies of the Local Group are close satellites of the Milky Way characterized by a large mass-to-light ratio and are not expected to be the site of non-thermal high-energy gamma-ray emission or intense star formation. Therefore they are amongst the most promising candidates for indirect dark matter searches. During the last years the High Energy Stereoscopic System (H.E.S.S.) of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1410.2589v3-abstract-full').style.display = 'inline'; document.getElementById('1410.2589v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1410.2589v3-abstract-full" style="display: none;"> Dwarf spheroidal galaxies of the Local Group are close satellites of the Milky Way characterized by a large mass-to-light ratio and are not expected to be the site of non-thermal high-energy gamma-ray emission or intense star formation. Therefore they are amongst the most promising candidates for indirect dark matter searches. During the last years the High Energy Stereoscopic System (H.E.S.S.) of imaging atmospheric Cherenkov telescopes observed five of these dwarf galaxies for more than 140 hours in total, searching for TeV gamma-ray emission from annihilation of dark matter particles. The new results of the deep exposure of the Sagittarius dwarf spheroidal galaxy, the first observations of the Coma Berenices and Fornax dwarves and the re-analysis of two more dwarf spheroidal galaxies already published by the H.E.S.S. Collaboration, Carina and Sculptor, are presented. In the absence of a significant signal new constraints on the annihilation cross-section applicable to Weakly Interacting Massive Particles (WIMPs) are derived by combining the observations of the five dwarf galaxies. The combined exclusion limit depends on the WIMP mass and the best constraint is reached at 1-2 TeV masses with a cross-section upper bound of ~3.9x10-24 cm^3 s-1 at a 95% confidence level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1410.2589v3-abstract-full').style.display = 'none'; document.getElementById('1410.2589v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 October, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 October, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">to be published in Physical Review D journal; Contact authors: E. Birsin, C. Farnier, G. Lamanna</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1409.1232">arXiv:1409.1232</a> <span> [<a href="https://arxiv.org/pdf/1409.1232">pdf</a>, <a href="https://arxiv.org/ps/1409.1232">ps</a>, <a href="https://arxiv.org/format/1409.1232">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/2041-8205/794/1/L8">10.1088/2041-8205/794/1/L8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A size-duration trend for gamma-ray burst progenitors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">Anna Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Loeb%2C+A">Abraham Loeb</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="1409.1232v2-abstract-short" style="display: inline;"> Gamma-ray bursts (GRBs) show a bimodal distribution of durations, separated at a duration of ~2 s. Observations have confirmed the association of long GRBs with the collapse of massive stars. The origin of short GRBs is still being explored. We examine constraints on the emission region size in short and long GRBs detected by Fermi/GBM. We find that the emission region size during the prompt emiss… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.1232v2-abstract-full').style.display = 'inline'; document.getElementById('1409.1232v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1409.1232v2-abstract-full" style="display: none;"> Gamma-ray bursts (GRBs) show a bimodal distribution of durations, separated at a duration of ~2 s. Observations have confirmed the association of long GRBs with the collapse of massive stars. The origin of short GRBs is still being explored. We examine constraints on the emission region size in short and long GRBs detected by Fermi/GBM. We find that the emission region size during the prompt emission, R, and the burst duration, T$_{90}$, are consistent with the relation R ~ c x T$_{90}$, for both long and short GRBs. We find the characteristic size for the prompt emission region to be ~2 x 10$^{10}$ cm, and ~4 x 10$^{11}$ cm for short and long GRBs, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.1232v2-abstract-full').style.display = 'none'; document.getElementById('1409.1232v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 September, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 September, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1409.0253">arXiv:1409.0253</a> <span> [<a href="https://arxiv.org/pdf/1409.0253">pdf</a>, <a href="https://arxiv.org/format/1409.0253">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/10.1051/0004-6361/201424142">10.1051/0004-6361/201424142 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Long-term monitoring of PKS 2155$-$304 with ATOM and H.E.S.S.: investigation of optical/$纬$-ray correlations in different spectral states </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abramowski%2C+A">A. Abramowski</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Akhperjanian%2C+A+G">A. G. Akhperjanian</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Balenderan%2C+S">S. Balenderan</a>, <a href="/search/astro-ph?searchtype=author&query=Balzer%2C+A">A. Balzer</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</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=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernhard%2C+S">S. Bernhard</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Birsin%2C+E">E. Birsin</a>, <a href="/search/astro-ph?searchtype=author&query=Biteau%2C+J">J. Biteau</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=Bordas%2C+P">P. Bordas</a>, <a href="/search/astro-ph?searchtype=author&query=Bregeon%2C+J">J. Bregeon</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+P">P. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bryan%2C+M">M. Bryan</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a> , et al. (203 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="1409.0253v1-abstract-short" style="display: inline;"> In this paper we report on the analysis of all the available optical and very high-energy $纬$-ray ($>$200 GeV) data for the BL Lac object PKS 2155$-$304, collected simultaneously with the ATOM and H.E.S.S. telescopes from 2007 until 2009. This study also includes X-ray (RXTE, Swift) and high-energy $纬$-ray (Fermi-LAT) data. During the period analysed, the source was transitioning from its flaring… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.0253v1-abstract-full').style.display = 'inline'; document.getElementById('1409.0253v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1409.0253v1-abstract-full" style="display: none;"> In this paper we report on the analysis of all the available optical and very high-energy $纬$-ray ($>$200 GeV) data for the BL Lac object PKS 2155$-$304, collected simultaneously with the ATOM and H.E.S.S. telescopes from 2007 until 2009. This study also includes X-ray (RXTE, Swift) and high-energy $纬$-ray (Fermi-LAT) data. During the period analysed, the source was transitioning from its flaring to quiescent optical states,and was characterized by only moderate flux changes at different wavelengths on the timescales of days and months. A flattening of the optical continuum with an increasing optical flux can be noted in the collected dataset, but only occasionally and only at higher flux levels. We did not find any universal relation between the very high-energy $纬$-ray and optical flux changes on the timescales from days and weeks up to several years. On the other hand, we noted that at higher flux levels the source can follow two distinct tracks in the optical flux-colour diagrams, which seem to be related to distinct $纬$-ray states of the blazar. The obtained results therefore indicate a complex scaling between the optical and $纬$-ray emission of PKS 2155$-$304, with different correlation patterns holding at different epochs, and a $纬$-ray flux depending on the combination of an optical flux and colour rather than a flux alone. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.0253v1-abstract-full').style.display = 'none'; document.getElementById('1409.0253v1-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 August, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">10 pages, 5 figures, Accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 571, A39 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1408.5898">arXiv:1408.5898</a> <span> [<a href="https://arxiv.org/pdf/1408.5898">pdf</a>, <a href="https://arxiv.org/ps/1408.5898">ps</a>, <a href="https://arxiv.org/format/1408.5898">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/799/1/48">10.1088/0004-637X/799/1/48 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Strongly Lensed Jets, Time Delays, and the Value of H0 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">Anna Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Geller%2C+M">Margaret Geller</a>, <a href="/search/astro-ph?searchtype=author&query=Dell%27Antonio%2C+I+P">Ian P. Dell'Antonio</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">Wystan Benbow</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1408.5898v2-abstract-short" style="display: inline;"> In principle, the most straightforward method of estimating the Hubble constant relies on time delays between mirage images of strongly-lensed sources. It is a puzzle, then, that the values of H0 obtained with this method span a range from 50 - 100 km/s/Mpc. Quasars monitored to measure these time delays, are multi-component objects. The variability may arise from different components of the quas… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.5898v2-abstract-full').style.display = 'inline'; document.getElementById('1408.5898v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1408.5898v2-abstract-full" style="display: none;"> In principle, the most straightforward method of estimating the Hubble constant relies on time delays between mirage images of strongly-lensed sources. It is a puzzle, then, that the values of H0 obtained with this method span a range from 50 - 100 km/s/Mpc. Quasars monitored to measure these time delays, are multi-component objects. The variability may arise from different components of the quasar or may even originate from a jet. Misidentifying a variable emitting region in a jet with emission from the core region may introduce an error in the Hubble constant derived from a time delay. Here, we investigate the complex structure of sources as the underlying physical explanation of the widespread in values of the Hubble constant based on gravitational lensing. Our Monte Carlo simulations demonstrate that the derived value of the Hubble constant is very sensitive to the offset between the center of the emission and the center of the variable emitting region. Thus, we propose using the value of H0 known from other techniques to spatially resolve the origin of the variable emission once the time delay is measured. We advocate this method particularly for gamma-ray astronomy, where the angular resolution of detectors reaches approximately 0.1 degree; lensed blazars offer the only route for identify the origin of gamma-ray flares. Large future samples of gravitationally lensed sources identified with Euclid, SKA, and LSST will enable a statistical determination of H0. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.5898v2-abstract-full').style.display = 'none'; document.getElementById('1408.5898v2-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> 10 November, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 August, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1408.5280">arXiv:1408.5280</a> <span> [<a href="https://arxiv.org/pdf/1408.5280">pdf</a>, <a href="https://arxiv.org/ps/1408.5280">ps</a>, <a href="https://arxiv.org/format/1408.5280">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/2041-8205/794/1/L1">10.1088/2041-8205/794/1/L1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of the hard spectrum VHE gamma-ray source HESS J1641-463 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abramowski%2C+A">A. Abramowski</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Akhperjanian%2C+A+G">A. G. Akhperjanian</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Balenderan%2C+S">S. Balenderan</a>, <a href="/search/astro-ph?searchtype=author&query=Balzer%2C+A">A. Balzer</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</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=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernhard%2C+S">S. Bernhard</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Birsin%2C+E">E. Birsin</a>, <a href="/search/astro-ph?searchtype=author&query=Biteau%2C+J">J. Biteau</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=Bordas%2C+P">P. Bordas</a>, <a href="/search/astro-ph?searchtype=author&query=Bregeon%2C+J">J. Bregeon</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+P">P. Brun</a> , et al. (208 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="1408.5280v3-abstract-short" style="display: inline;"> This letter reports the discovery of a remarkably hard spectrum source, HESS J1641-463, by the High Energy Stereoscopic System (H.E.S.S.) in the very-high energy (VHE) domain. HESS J1641-463 remained unnoticed by the usual analysis techniques due to confusion with the bright nearby source HESS J1640-465. It emerged at a significance level of 8.5 standard deviations after restricting the analysis t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.5280v3-abstract-full').style.display = 'inline'; document.getElementById('1408.5280v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1408.5280v3-abstract-full" style="display: none;"> This letter reports the discovery of a remarkably hard spectrum source, HESS J1641-463, by the High Energy Stereoscopic System (H.E.S.S.) in the very-high energy (VHE) domain. HESS J1641-463 remained unnoticed by the usual analysis techniques due to confusion with the bright nearby source HESS J1640-465. It emerged at a significance level of 8.5 standard deviations after restricting the analysis to events with energies above 4 TeV. It shows a moderate flux level of F(E > 1 TeV) = (3.64 +/- 0.44_stat +/- 0.73_sys) x 10^-13 cm^-2s-1, corresponding to 1.8% of the Crab Nebula flux above the same energy, and a hard spectrum with a photon index of Gamma = 2.07 +/- 0.11_stat +/- 0.20_sys. It is a point-like source, although an extension up to Gaussian width of sigma = 3 arcmin cannot be discounted due to uncertainties in the H.E.S.S. PSF. The VHE gamma-ray flux of HESS J1641-463 is found to be constant over the observed period when checking time binnings from year-by-year to the 28 min exposures timescales. HESS J1641-463 is positionally coincident with the radio supernova remnant SNR G338.5+0.1. No X-ray candidate stands out as a clear association, however Chandra and XMM-Newton data reveal some potential weak counterparts. Various VHE gamma-ray production scenarios are discussed. If the emission from HESS J1641-463 is produced by cosmic ray protons colliding with the ambient gas, then their spectrum must extend close to 1 PeV. This object may represent a source population contributing significantly to the galactic cosmic ray flux around the knee. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.5280v3-abstract-full').style.display = 'none'; document.getElementById('1408.5280v3-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> 7 October, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 August, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 4 figures. Published version</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, 794:L1 (6pp), 2014 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1407.0862">arXiv:1407.0862</a> <span> [<a href="https://arxiv.org/pdf/1407.0862">pdf</a>, <a href="https://arxiv.org/ps/1407.0862">ps</a>, <a href="https://arxiv.org/format/1407.0862">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/10.1051/0004-6361/201322694">10.1051/0004-6361/201322694 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Probing the gamma-ray emission from HESS J1834-087 using H.E.S.S. and Fermi LAT observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+T+H+E+S+S">The H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abramowski%2C+A">A. Abramowski</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Akhperjanian%2C+A+G">A. G. Akhperjanian</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E">E. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Balenderan%2C+S">S. Balenderan</a>, <a href="/search/astro-ph?searchtype=author&query=Balzer%2C+A">A. Balzer</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</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=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Birsin%2C+E">E. Birsin</a>, <a href="/search/astro-ph?searchtype=author&query=Bissaldi%2C+E">E. Bissaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Biteau%2C+J">J. Biteau</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=Bordas%2C+P">P. Bordas</a>, <a href="/search/astro-ph?searchtype=author&query=Brucker%2C+J">J. Brucker</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+P">P. Brun</a> , et al. (206 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="1407.0862v1-abstract-short" style="display: inline;"> Previous observations with HESS have revealed the existence of an extended very-high-energy (VHE; E>100 GeV) gamma-ray source, HESS J1834-087, coincident with the SNR W41. The origin of the gamma-ray emission has been further investigated with HESS and the Fermi-LAT. The gamma-ray data provided by 61h (HESS) and 4 yrs (Fermi LAT) of observations cover over 5 decades in energy (1.8GeV - 30TeV). The… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.0862v1-abstract-full').style.display = 'inline'; document.getElementById('1407.0862v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1407.0862v1-abstract-full" style="display: none;"> Previous observations with HESS have revealed the existence of an extended very-high-energy (VHE; E>100 GeV) gamma-ray source, HESS J1834-087, coincident with the SNR W41. The origin of the gamma-ray emission has been further investigated with HESS and the Fermi-LAT. The gamma-ray data provided by 61h (HESS) and 4 yrs (Fermi LAT) of observations cover over 5 decades in energy (1.8GeV - 30TeV). The morphology and spectrum of the TeV and GeV sources have been studied and multi-wavelength data have been used to investigate the origin of the observed emission. The TeV source can be modeled with a sum of two components: one point-like and one significantly extended (sig_TeV = 0.17掳), both centered on SNR W41 and exhibiting spectra described by a power law of index 2.6. The GeV source detected with Fermi is extended (sig_GeV =0.15掳) and morphologically matches the VHE emission. Its spectrum can be described by a power-law with index 2.15 and joins smoothly the one of the whole TeV source. A break appears in the spectra around 100 GeV. Two main scenarios are proposed to explain the emission: a pulsar wind nebula (PWN) or the interaction of SNR W41 with a molecular cloud. X-ray observations suggest the presence of a point-like source (pulsar candidate) near the center of the SNR and non-thermal X-ray diffuse emission which could arise from a potential PWN. The PWN scenario is supported by the match of of the TeV and GeV positions with the putative pulsar. However, the overall spectrum is reproduced by a 1-zone leptonic model only if an excess of low-energy electrons is injected by a high spin-down power pulsar. This low-energy component is not needed if the point-like TeV source is unrelated to the extended GeV and TeV sources. The interacting SNR scenario is supported by the spatial coincidence between the gamma-ray sources, the detection of OH maser lines and the hadronic modeling. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.0862v1-abstract-full').style.display = 'none'; document.getElementById('1407.0862v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 July, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">12 pages, 8 figures, Accepted for publication in Astronomy & Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1405.0488">arXiv:1405.0488</a> <span> [<a href="https://arxiv.org/pdf/1405.0488">pdf</a>, <a href="https://arxiv.org/format/1405.0488">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/10.1051/0004-6361/201322984">10.1051/0004-6361/201322984 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for TeV Gamma-ray Emission from GRB 100621A, an extremely bright GRB in X-rays, with H.E.S.S </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abramowski%2C+A">A. Abramowski</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Akhperjanian%2C+A+G">A. G. Akhperjanian</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E">E. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Balenderan%2C+S">S. Balenderan</a>, <a href="/search/astro-ph?searchtype=author&query=Balzer%2C+A">A. Balzer</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</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=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Birsin%2C+E">E. Birsin</a>, <a href="/search/astro-ph?searchtype=author&query=Bissaldi%2C+E">E. Bissaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Biteau%2C+J">J. Biteau</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=Bordas%2C+P">P. Bordas</a>, <a href="/search/astro-ph?searchtype=author&query=Brucker%2C+J">J. Brucker</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+P">P. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Carrigan%2C+S">S. Carrigan</a> , et al. (191 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="1405.0488v1-abstract-short" style="display: inline;"> The long gamma-ray burst (GRB) 100621A, at the time the brightest X-ray transient ever detected by Swift-XRT in the $0.3\textrm{--}10$ keV range, has been observed with the H.E.S.S. imaging air Cherenkov telescope array, sensitive to gamma radiation in the very-high-energy (VHE, $>100$ GeV) regime. Due to its relatively small redshift of $z\sim0.5$, the favourable position in the southern sky and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.0488v1-abstract-full').style.display = 'inline'; document.getElementById('1405.0488v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1405.0488v1-abstract-full" style="display: none;"> The long gamma-ray burst (GRB) 100621A, at the time the brightest X-ray transient ever detected by Swift-XRT in the $0.3\textrm{--}10$ keV range, has been observed with the H.E.S.S. imaging air Cherenkov telescope array, sensitive to gamma radiation in the very-high-energy (VHE, $>100$ GeV) regime. Due to its relatively small redshift of $z\sim0.5$, the favourable position in the southern sky and the relatively short follow-up time ($<700 \rm{s}$ after the satellite trigger) of the H.E.S.S. observations, this GRB could be within the sensitivity reach of the H.E.S.S. instrument. The analysis of the H.E.S.S. data shows no indication of emission and yields an integral flux upper limit above $\sim$380 GeV of $4.2\times10^{-12} \rm cm^{-2}s^{-1}$ (95 % confidence level), assuming a simple Band function extension model. A comparison to a spectral-temporal model, normalised to the prompt flux at sub-MeV energies, constraints the existence of a temporally extended and strong additional hard power law, as has been observed in the other bright X-ray GRB 130427A. A comparison between the H.E.S.S. upper limit and the contemporaneous energy output in X-rays constrains the ratio between the X-ray and VHE gamma-ray fluxes to be greater than 0.4. This value is an important quantity for modelling the afterglow and can constrain leptonic emission scenarios, where leptons are responsible for the X-ray emission and might produce VHE gamma rays. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.0488v1-abstract-full').style.display = 'none'; document.getElementById('1405.0488v1-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> 2 May, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">8 pages, 2 figures. Published in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astronomy & Astrophysics, Volume 565, 05/2014, A16 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1404.4422">arXiv:1404.4422</a> <span> [<a href="https://arxiv.org/pdf/1404.4422">pdf</a>, <a href="https://arxiv.org/ps/1404.4422">ps</a>, <a href="https://arxiv.org/format/1404.4422">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/790/2/147">10.1088/0004-637X/790/2/147 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> How gravitational lensing helps gamma-ray photons avoid $纬- 纬$ absorption </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">Anna Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Bottcher%2C+M">Markus Bottcher</a>, <a href="/search/astro-ph?searchtype=author&query=Sushch%2C+I">Iurii Sushch</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="1404.4422v1-abstract-short" style="display: inline;"> We investigate potential $纬-纬$ absorption of gamma-ray emission from blazars arising from inhomogeneities along the line of sight, beyond the diffuse Extragalactic Background Light (EBL). As plausible sources of excess $纬-纬$ opacity, we consider (1) foreground galaxies, including cases in which this configuration leads to strong gravitational lensing, (2) individual stars within these foreground g… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1404.4422v1-abstract-full').style.display = 'inline'; document.getElementById('1404.4422v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1404.4422v1-abstract-full" style="display: none;"> We investigate potential $纬-纬$ absorption of gamma-ray emission from blazars arising from inhomogeneities along the line of sight, beyond the diffuse Extragalactic Background Light (EBL). As plausible sources of excess $纬-纬$ opacity, we consider (1) foreground galaxies, including cases in which this configuration leads to strong gravitational lensing, (2) individual stars within these foreground galaxies, and (3) individual stars within our own galaxy, which may act as lenses for microlensing events. We found that intervening galaxies close to the line-of-sight are unlikely to lead to significant excess $纬-纬$ absorption. This opens up the prospect of detecting lensed gamma-ray blazars at energies above 10 GeV with their gamma-ray spectra effectively only affected by the EBL. The most luminous stars located either in intervening galaxy or in our galaxy provides an environment in which these gamma-rays could, in principle, be significantly absorbed. However, despite a large microlensing probability due to stars located in intervening galaxies, gamma-rays avoid absorption by being deflected by the gravitational potentials of such intervening stars to projected distances ("impact parameters"') where the resulting $纬-纬$ opacities are negligible. Thus, neither of the intervening excess photon fields considered here, provide a substantial source of excess $纬-纬$ opacity beyond the EBL, even in the case of very close alignments between the background blazar and a foreground star or galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1404.4422v1-abstract-full').style.display = 'none'; document.getElementById('1404.4422v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 April, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">Submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1404.1613">arXiv:1404.1613</a> <span> [<a href="https://arxiv.org/pdf/1404.1613">pdf</a>, <a href="https://arxiv.org/ps/1404.1613">ps</a>, <a href="https://arxiv.org/format/1404.1613">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/stu459">10.1093/mnras/stu459 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> TeV 纬-ray observations of the young synchrotron-dominated SNRs G1.9+0.3 and G330.2+1.0 with H.E.S.S </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abramowski%2C+A">A. Abramowski</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Akhperjanian%2C+A+G">A. G. Akhperjanian</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E">E. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Balenderan%2C+S">S. Balenderan</a>, <a href="/search/astro-ph?searchtype=author&query=Balzer%2C+A">A. Balzer</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</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=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Birsin%2C+E">E. Birsin</a>, <a href="/search/astro-ph?searchtype=author&query=Bissaldi%2C+E">E. Bissaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Biteau%2C+J">J. Biteau</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=Bordas%2C+P">P. Bordas</a>, <a href="/search/astro-ph?searchtype=author&query=Brucker%2C+J">J. Brucker</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+P">P. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Carrigan%2C+S">S. Carrigan</a> , et al. (195 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="1404.1613v1-abstract-short" style="display: inline;"> The non-thermal nature of the X-ray emission from the shell-type supernova remnants (SNRs) G1.9+0.3 and G330.2+1.0 is an indication of intense particle acceleration in the shock fronts of both objects. This suggests that the SNRs are prime candidates for very-high-energy (VHE; E $>$ 0.1 TeV) 纬-ray observations. G1.9+0.3, recently established as the youngest known SNR in the Galaxy, also offers a u… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1404.1613v1-abstract-full').style.display = 'inline'; document.getElementById('1404.1613v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1404.1613v1-abstract-full" style="display: none;"> The non-thermal nature of the X-ray emission from the shell-type supernova remnants (SNRs) G1.9+0.3 and G330.2+1.0 is an indication of intense particle acceleration in the shock fronts of both objects. This suggests that the SNRs are prime candidates for very-high-energy (VHE; E $>$ 0.1 TeV) 纬-ray observations. G1.9+0.3, recently established as the youngest known SNR in the Galaxy, also offers a unique opportunity to study the earliest stages of SNR evolution in the VHE domain. The purpose of this work is to probe the level of VHE 纬-ray emission from both SNRs and use this to constrain their physical properties. Observations were conducted with the H.E.S.S. (High Energy Stereoscopic System) Cherenkov telescope array over a more than six-year period spanning 2004-2010. The obtained data have effective livetimes of 67 h for G1.9+0.3 and 16 h for G330.2+1.0. The data are analyzed in the context of the multi-wavelength observations currently available and in the framework of both leptonic and hadronic particle acceleration scenarios. No significant 纬-ray signal from G1.9+0.3 or G330.2+1.0 was detected. Upper limits (99% confidence level) to the TeV flux from G1.9+0.3 and G330.2+1.0 for the assumed spectral index 螕 = 2.5 were set at 5.6 $\times$ 10$^{-13}$ cm$^{-2}$ s$^{-1}$ above 0.26 TeV and 3.2 $\times$ 10$^{-12}$ cm$^{-2}$ s$^{-1}$ above 0.38 TeV, respectively. In a one-zone leptonic scenario, these upper limits imply lower limits on the interior magnetic field to B$_{\mathrm{G1.9}}$ $\gtrsim$ 11 渭G for G1.9+0.3 and to B$_{\mathrm{G330}}$ $\gtrsim$ 8 渭G for G330.2+1.0. In a hadronic scenario, the low ambient densities and the large distances to the SNRs result in very low predicted fluxes, for which the H.E.S.S. upper limits are not constraining. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1404.1613v1-abstract-full').style.display = 'none'; document.getElementById('1404.1613v1-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 April, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">9 pages, 2 figures, 4 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/1403.5316">arXiv:1403.5316</a> <span> [<a href="https://arxiv.org/pdf/1403.5316">pdf</a>, <a href="https://arxiv.org/ps/1403.5316">ps</a>, <a href="https://arxiv.org/format/1403.5316">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/788/2/139">10.1088/0004-637X/788/2/139 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Strong gravitational lensing as a tool to investigate the structure of jets at high energies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">Anna Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Geller%2C+M+J">Margaret J. Geller</a>, <a href="/search/astro-ph?searchtype=author&query=Dell%27antonio%2C+I+P">Ian P. Dell'antonio</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">Wystan Benbow</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="1403.5316v2-abstract-short" style="display: inline;"> The components of blazar jets that emit radiation span a factor of $10^{10}$ in scale. The spatial structure of these emitting regions depends on the observed energy. Photons emitted at different sites cross the lens plane at different distances from the mass-weighted center of the lens. Thus there are differences in magnification ratios and time delays between the images of lensed blazars observe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1403.5316v2-abstract-full').style.display = 'inline'; document.getElementById('1403.5316v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1403.5316v2-abstract-full" style="display: none;"> The components of blazar jets that emit radiation span a factor of $10^{10}$ in scale. The spatial structure of these emitting regions depends on the observed energy. Photons emitted at different sites cross the lens plane at different distances from the mass-weighted center of the lens. Thus there are differences in magnification ratios and time delays between the images of lensed blazars observed at different energies. When the lens structure and redshift are known from optical observations, these constraints can elucidate the structure of the source at high energies. At these energies, current technology is inadequate to resolve these sources and the observed light curve is thus the sum of the images. Durations of $纬$-ray flares are short compared with typical time delays; thus both the magnification ratio and the time delay can be measured for the delayed counterparts. These measurements are a basis for localizing the emitting region along the jet. To demonstrate the power of strong gravitational lensing, we build a toy model based on the best studied and the nearest relativistic jet M87. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1403.5316v2-abstract-full').style.display = 'none'; document.getElementById('1403.5316v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 June, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 March, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted 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> The Astrophysical Journal, 788:139 (6pp), 2014 June 20 </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Barnacka%2C+A&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Barnacka%2C+A&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Barnacka%2C+A&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Barnacka%2C+A&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> </ul> </nav> <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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