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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.08189">arXiv:2411.08189</a> <span> [<a href="https://arxiv.org/pdf/2411.08189">pdf</a>, <a href="https://arxiv.org/format/2411.08189">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.133.221001">10.1103/PhysRevLett.133.221001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> High-Statistics Measurement of the Cosmic-Ray Electron Spectrum with H.E.S.S </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Aschersleben%2C+J">J. Aschersleben</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=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</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=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bouyahiaoui%2C+M">M. Bouyahiaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+C">C. Burger-Scheidlin</a>, <a href="/search/astro-ph?searchtype=author&query=Bylund%2C+T">T. Bylund</a>, <a href="/search/astro-ph?searchtype=author&query=Casanova%2C+S">S. Casanova</a> , et al. (123 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="2411.08189v1-abstract-short" style="display: inline;"> Owing to their rapid cooling rate and hence loss-limited propagation distance, cosmic-ray electrons and positrons (CRe) at very high energies probe local cosmic-ray accelerators and provide constraints on exotic production mechanisms such as annihilation of dark matter particles. We present a high-statistics measurement of the spectrum of CRe candidate events from 0.3 to 40 TeV with the High Energ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.08189v1-abstract-full').style.display = 'inline'; document.getElementById('2411.08189v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.08189v1-abstract-full" style="display: none;"> Owing to their rapid cooling rate and hence loss-limited propagation distance, cosmic-ray electrons and positrons (CRe) at very high energies probe local cosmic-ray accelerators and provide constraints on exotic production mechanisms such as annihilation of dark matter particles. We present a high-statistics measurement of the spectrum of CRe candidate events from 0.3 to 40 TeV with the High Energy Stereoscopic System (H.E.S.S.), covering two orders of magnitude in energy and reaching a proton rejection power of better than $10^{4}$. The measured spectrum is well described by a broken power law, with a break around 1 TeV, where the spectral index increases from $螕_1 = 3.25$ $\pm$ 0.02 (stat) $\pm$ 0.2 (sys) to $螕_2 = 4.49$ $\pm$ 0.04 (stat) $\pm$ 0.2 (sys). Apart from the break, the spectrum is featureless. The absence of distinct signatures at multi-TeV energies imposes constraints on the presence of nearby CRe accelerators and the local CRe propagation mechanisms. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.08189v1-abstract-full').style.display = 'none'; document.getElementById('2411.08189v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">main paper: 8 pages, 4 figures, supplemental material: 12 pages, 14 figures, accepted for publication in Physical Review Letters https://journals.aps.org/prl/</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 133, 221001 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.16219">arXiv:2407.16219</a> <span> [<a href="https://arxiv.org/pdf/2407.16219">pdf</a>, <a href="https://arxiv.org/format/2407.16219">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/ad5e67">10.3847/2041-8213/ad5e67 <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 young massive star clusters in the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Aschersleben%2C+J">J. Aschersleben</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=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</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=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=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+C">C. Burger-Scheidlin</a>, <a href="/search/astro-ph?searchtype=author&query=Casanova%2C+S">S. Casanova</a>, <a href="/search/astro-ph?searchtype=author&query=Celic%2C+J">J. Celic</a>, <a href="/search/astro-ph?searchtype=author&query=Cerruti%2C+M">M. Cerruti</a>, <a href="/search/astro-ph?searchtype=author&query=Chand%2C+T">T. Chand</a>, <a href="/search/astro-ph?searchtype=author&query=Chandra%2C+S">S. Chandra</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+A">A. Chen</a> , et al. (107 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="2407.16219v1-abstract-short" style="display: inline;"> The Tarantula Nebula in the Large Magellanic Cloud is known for its high star formation activity. At its center lies the young massive star cluster R136, providing a significant amount of the energy that makes the nebula shine so brightly at many wavelengths. Recently, young massive star clusters have been suggested to also efficiently produce high-energy cosmic rays, potentially beyond PeV energi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.16219v1-abstract-full').style.display = 'inline'; document.getElementById('2407.16219v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.16219v1-abstract-full" style="display: none;"> The Tarantula Nebula in the Large Magellanic Cloud is known for its high star formation activity. At its center lies the young massive star cluster R136, providing a significant amount of the energy that makes the nebula shine so brightly at many wavelengths. Recently, young massive star clusters have been suggested to also efficiently produce high-energy cosmic rays, potentially beyond PeV energies. Here, we report the detection of very-high-energy $纬$-ray emission from the direction of R136 with the High Energy Stereoscopic System, achieved through a multicomponent, likelihood-based modeling of the data. This supports the hypothesis that R136 is indeed a very powerful cosmic-ray accelerator. Moreover, from the same analysis, we provide an updated measurement of the $纬$-ray emission from 30 Dor C, the only superbubble detected at TeV energies presently. The $纬$-ray luminosity above $0.5\,\mathrm{TeV}$ of both sources is $(2-3)\times 10^{35}\,\mathrm{erg}\,\mathrm{s}^{-1}$. This exceeds by more than a factor of 2 the luminosity of HESS J1646$-$458, which is associated with the most massive young star cluster in the Milky Way, Westerlund 1. Furthermore, the $纬$-ray emission from each source is extended with a significance of $>3蟽$ and a Gaussian width of about $30\,\mathrm{pc}$. For 30 Dor C, a connection between the $纬$-ray emission and the nonthermal X-ray emission appears likely. Different interpretations of the $纬$-ray signal from R136 are discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.16219v1-abstract-full').style.display = 'none'; document.getElementById('2407.16219v1-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10+11 pages, 4+6 figures. Corresponding authors: L. Mohrmann, N. Komin</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophysical Journal Letters 970, L21 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.18167">arXiv:2406.18167</a> <span> [<a href="https://arxiv.org/pdf/2406.18167">pdf</a>, <a href="https://arxiv.org/format/2406.18167">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"> H.E.S.S. observations of the 2021 periastron passage of PSR B1259-63/LS 2883 </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=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=Aschersleben%2C+J">J. Aschersleben</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=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</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=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bouyahiaoui%2C+M">M. Bouyahiaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+C">C. Burger-Scheidlin</a>, <a href="/search/astro-ph?searchtype=author&query=Caroff%2C+S">S. Caroff</a>, <a href="/search/astro-ph?searchtype=author&query=Casanova%2C+S">S. Casanova</a> , et al. (119 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.18167v1-abstract-short" style="display: inline;"> PSR B1259-63 is a gamma-ray binary system that hosts a pulsar in an eccentric orbit, with a 3.4 year period, around an O9.5Ve star. At orbital phases close to periastron passages, the system radiates bright and variable non-thermal emission. We report on an extensive VHE observation campaign conducted with the High Energy Stereoscopic System, comprised of ~100 hours of data taken from $t_p-24$ day… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.18167v1-abstract-full').style.display = 'inline'; document.getElementById('2406.18167v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.18167v1-abstract-full" style="display: none;"> PSR B1259-63 is a gamma-ray binary system that hosts a pulsar in an eccentric orbit, with a 3.4 year period, around an O9.5Ve star. At orbital phases close to periastron passages, the system radiates bright and variable non-thermal emission. We report on an extensive VHE observation campaign conducted with the High Energy Stereoscopic System, comprised of ~100 hours of data taken from $t_p-24$ days to $t_p+127$ days around the system's 2021 periastron passage. We also present the timing and spectral analyses of the source. The VHE light curve in 2021 is consistent with the stacked light curve of all previous observations. Within the light curve, we report a VHE maximum at times coincident with the third X-ray peak first detected in the 2021 X-ray light curve. In the light curve -- although sparsely sampled in this time period -- we see no VHE enhancement during the second disc crossing. In addition, we see no correspondence to the 2021 GeV flare in the VHE light curve. The VHE spectrum obtained from the analysis of the 2021 dataset is best described by a power law of spectral index $螕= 2.65 \pm 0.04_{\text{stat}}$ $\pm 0.04_{\text{sys}}$, a value consistent with the previous H.E.S.S. observations of the source. We report spectral variability with a difference of $螖螕= 0.56 ~\pm~ 0.18_{\text{stat}}$ $~\pm~0.10_{\text{sys}}$ at 95% c.l., between sub-periods of the 2021 dataset. We also find a linear correlation between contemporaneous flux values of X-ray and TeV datasets, detected mainly after $t_p+25$ days, suggesting a change in the available energy for non-thermal radiation processes. We detect no significant correlation between GeV and TeV flux points, within the uncertainties of the measurements, from $\sim t_p-23$ days to $\sim t_p+126$ days. This suggests that the GeV and TeV emission originate from different electron populations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.18167v1-abstract-full').style.display = 'none'; document.getElementById('2406.18167v1-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted to A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.16802">arXiv:2403.16802</a> <span> [<a href="https://arxiv.org/pdf/2403.16802">pdf</a>, <a href="https://arxiv.org/format/2403.16802">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/10.1051/0004-6361/202348374">10.1051/0004-6361/202348374 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Unveiling extended gamma-ray emission around HESS J1813-178 </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Aschersleben%2C+J">J. Aschersleben</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=Baktash%2C+A">A. Baktash</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=Barnard%2C+J">J. Barnard</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</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=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bouyahiaoui%2C+M">M. Bouyahiaoui</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=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+C">C. Burger-Scheidlin</a> , et al. (126 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.16802v1-abstract-short" style="display: inline;"> HESS J1813$-$178 is a very-high-energy $纬$-ray source spatially coincident with the young and energetic pulsar PSR J1813$-$1749 and thought to be associated with its pulsar wind nebula (PWN). Recently, evidence for extended high-energy emission in the vicinity of the pulsar has been revealed in the Fermi Large Area Telescope (LAT) data. This motivates revisiting the HESS J1813$-$178 region, taking… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.16802v1-abstract-full').style.display = 'inline'; document.getElementById('2403.16802v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.16802v1-abstract-full" style="display: none;"> HESS J1813$-$178 is a very-high-energy $纬$-ray source spatially coincident with the young and energetic pulsar PSR J1813$-$1749 and thought to be associated with its pulsar wind nebula (PWN). Recently, evidence for extended high-energy emission in the vicinity of the pulsar has been revealed in the Fermi Large Area Telescope (LAT) data. This motivates revisiting the HESS J1813$-$178 region, taking advantage of improved analysis methods and an extended data set. Using data taken by the High Energy Stereoscopic System (H.E.S.S.) experiment and the Fermi-LAT, we aim to describe the $纬$-ray emission in the region with a consistent model, to provide insights into its origin. We performed a likelihood-based analysis on 32 hours of H.E.S.S. data and 12 years of Fermi-LAT data and fit a spectro-morphological model to the combined datasets. These results allowed us to develop a physical model for the origin of the observed $纬$-ray emission in the region. In addition to the compact very-high-energy $纬$-ray emission centered on the pulsar, we find a significant yet previously undetected component along the Galactic plane. With Fermi-LAT data, we confirm extended high-energy emission consistent with the position and elongation of the extended emission observed with H.E.S.S. These results establish a consistent description of the emission in the region from GeV energies to several tens of TeV. This study suggests that HESS J1813$-$178 is associated with a $纬$-ray PWN powered by PSR J1813$-$1749. A possible origin of the extended emission component is inverse Compton emission from electrons and positrons that have escaped the confines of the pulsar and form a halo around the PWN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.16802v1-abstract-full').style.display = 'none'; document.getElementById('2403.16802v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13+5 pages, 13+11 figures. Accepted for publication in A&A. Corresponding authors: T.Wach, A.Mitchell, V.Joshi, P.Chamb茅ry</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 686, A149 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.12608">arXiv:2403.12608</a> <span> [<a href="https://arxiv.org/pdf/2403.12608">pdf</a>, <a href="https://arxiv.org/format/2403.12608">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/10.1051/0004-6361/202348651">10.1051/0004-6361/202348651 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spectrum and extension of the inverse-Compton emission of the Crab Nebula from a combined Fermi-LAT and H.E.S.S. analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Aschersleben%2C+J">J. Aschersleben</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=Baktash%2C+A">A. Baktash</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=Batzofin%2C+R">R. Batzofin</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=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bradascio%2C+F">F. Bradascio</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=Brown%2C+A">A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+C">C. Burger-Scheidlin</a> , et al. (137 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.12608v2-abstract-short" style="display: inline;"> The Crab Nebula is a unique laboratory for studying the acceleration of electrons and positrons through their non-thermal radiation. Observations of very-high-energy $纬$ rays from the Crab Nebula have provided important constraints for modelling its broadband emission. We present the first fully self-consistent analysis of the Crab Nebula's $纬$-ray emission between 1 GeV and $\sim$100 TeV, that is… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.12608v2-abstract-full').style.display = 'inline'; document.getElementById('2403.12608v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.12608v2-abstract-full" style="display: none;"> The Crab Nebula is a unique laboratory for studying the acceleration of electrons and positrons through their non-thermal radiation. Observations of very-high-energy $纬$ rays from the Crab Nebula have provided important constraints for modelling its broadband emission. We present the first fully self-consistent analysis of the Crab Nebula's $纬$-ray emission between 1 GeV and $\sim$100 TeV, that is, over five orders of magnitude in energy. Using the open-source software package Gammapy, we combined 11.4 yr of data from the Fermi Large Area Telescope and 80 h of High Energy Stereoscopic System (H.E.S.S.) data at the event level and provide a measurement of the spatial extension of the nebula and its energy spectrum. We find evidence for a shrinking of the nebula with increasing $纬$-ray energy. Furthermore, we fitted several phenomenological models to the measured data, finding that none of them can fully describe the spatial extension and the spectral energy distribution at the same time. Especially the extension measured at TeV energies appears too large when compared to the X-ray emission. Our measurements probe the structure of the magnetic field between the pulsar wind termination shock and the dust torus, and we conclude that the magnetic field strength decreases with increasing distance from the pulsar. We complement our study with a careful assessment of systematic uncertainties. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.12608v2-abstract-full').style.display = 'none'; document.getElementById('2403.12608v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18+6 pages, 15+2 figures. Accepted for publication in A&A. Corresponding authors: M. Meyer, L. Mohrmann, T. Unbehaun. v2: after A&A language editing</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 686, A308 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.16019">arXiv:2401.16019</a> <span> [<a href="https://arxiv.org/pdf/2401.16019">pdf</a>, <a href="https://arxiv.org/format/2401.16019">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.adi2048">10.1126/science.adi2048 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Acceleration and transport of relativistic electrons in the jets of the microquasar SS 433 </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Aschersleben%2C+J">J. Aschersleben</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=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</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=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bouyahiaou%2C+M">M. Bouyahiaou</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhau%2C+M">M. Breuhau</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+M">A. M. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+C">C. Burger-Scheidlin</a>, <a href="/search/astro-ph?searchtype=author&query=Caroff%2C+S">S. Caroff</a> , et al. (140 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="2401.16019v1-abstract-short" style="display: inline;"> SS 433 is a microquasar, a stellar binary system with collimated relativistic jets. We observed SS 433 in gamma rays using the High Energy Stereoscopic System (H.E.S.S.), finding an energy-dependent shift in the apparent position of the gamma-ray emission of the parsec-scale jets. These observations trace the energetic electron population and indicate the gamma rays are produced by inverse-Compton… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.16019v1-abstract-full').style.display = 'inline'; document.getElementById('2401.16019v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.16019v1-abstract-full" style="display: none;"> SS 433 is a microquasar, a stellar binary system with collimated relativistic jets. We observed SS 433 in gamma rays using the High Energy Stereoscopic System (H.E.S.S.), finding an energy-dependent shift in the apparent position of the gamma-ray emission of the parsec-scale jets. These observations trace the energetic electron population and indicate the gamma rays are produced by inverse-Compton scattering. Modelling of the energy-dependent gamma-ray morphology constrains the location of particle acceleration and requires an abrupt deceleration of the jet flow. We infer the presence of shocks on either side of the binary system at distances of 25 to 30 parsecs and conclude that self-collimation of the precessing jets forms the shocks, which then efficiently accelerate electrons. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.16019v1-abstract-full').style.display = 'none'; document.getElementById('2401.16019v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted 20th Apr. 2023, published 25th January 2024 (accepted version)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Science383,402-406(2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.07071">arXiv:2401.07071</a> <span> [<a href="https://arxiv.org/pdf/2401.07071">pdf</a>, <a href="https://arxiv.org/format/2401.07071">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"> TeV flaring activity of the AGN PKS 0625-354 in November 2018 </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=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=Aschersleben%2C+J">J. Aschersleben</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=Baktash%2C+A">A. Baktash</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=Barnard%2C+J">J. Barnard</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</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=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bradascio%2C+F">F. Bradascio</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=Brown%2C+A">A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+B">B. Bruno</a> , et al. (117 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="2401.07071v1-abstract-short" style="display: inline;"> Most $纬$-ray detected active galactic nuclei are blazars with one of their relativistic jets pointing towards the Earth. Only a few objects belong to the class of radio galaxies or misaligned blazars. Here, we investigate the nature of the object PKS 0625-354, its $纬$-ray flux and spectral variability and its broad-band spectral emission with observations from H.E.S.S., Fermi-LAT, Swift-XRT, and U… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.07071v1-abstract-full').style.display = 'inline'; document.getElementById('2401.07071v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.07071v1-abstract-full" style="display: none;"> Most $纬$-ray detected active galactic nuclei are blazars with one of their relativistic jets pointing towards the Earth. Only a few objects belong to the class of radio galaxies or misaligned blazars. Here, we investigate the nature of the object PKS 0625-354, its $纬$-ray flux and spectral variability and its broad-band spectral emission with observations from H.E.S.S., Fermi-LAT, Swift-XRT, and UVOT taken in November 2018. The H.E.S.S. light curve above 200 GeV shows an outburst in the first night of observations followed by a declining flux with a halving time scale of 5.9h. The $纬纬$-opacity constrains the upper limit of the angle between the jet and the line of sight to $\sim10^\circ$. The broad-band spectral energy distribution shows two humps and can be well fitted with a single-zone synchrotron self Compton emission model. We conclude that PKS 0625-354, as an object showing clear features of both blazars and radio galaxies, can be classified as an intermediate active galactic nuclei. Multi-wavelength studies of such intermediate objects exhibiting features of both blazars and radio galaxies are sparse but crucial for the understanding of the broad-band emission of $纬$-ray detected active galactic nuclei in general. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.07071v1-abstract-full').style.display = 'none'; document.getElementById('2401.07071v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 6 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/2310.06181">arXiv:2310.06181</a> <span> [<a href="https://arxiv.org/pdf/2310.06181">pdf</a>, <a href="https://arxiv.org/format/2310.06181">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/10.1038/s41550-023-02052-3">10.1038/s41550-023-02052-3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of a Radiation Component from the Vela Pulsar Reaching 20 Teraelectronvolts </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=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=Aschersleben%2C+J">J. Aschersleben</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=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</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=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bradascio%2C+F">F. Bradascio</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=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+C">C. Burger-Scheidlin</a> , et al. (157 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.06181v1-abstract-short" style="display: inline;"> Gamma-ray observations have established energetic isolated pulsars as outstanding particle accelerators and antimatter factories in the Galaxy. There is, however, no consensus regarding the acceleration mechanisms and the radiative processes at play, nor the locations where these take place. The spectra of all observed gamma-ray pulsars to date show strong cutoffs or a break above energies of a fe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06181v1-abstract-full').style.display = 'inline'; document.getElementById('2310.06181v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.06181v1-abstract-full" style="display: none;"> Gamma-ray observations have established energetic isolated pulsars as outstanding particle accelerators and antimatter factories in the Galaxy. There is, however, no consensus regarding the acceleration mechanisms and the radiative processes at play, nor the locations where these take place. The spectra of all observed gamma-ray pulsars to date show strong cutoffs or a break above energies of a few gigaelectronvolt (GeV). Using the H.E.S.S. array of Cherenkov telescopes, we discovered a novel radiation component emerging beyond this generic GeV cutoff in the Vela pulsar's broadband spectrum. The extension of gamma-ray pulsation energies up to at least 20 teraelectronvolts (TeV) shows that Vela pulsar can accelerate particles to Lorentz factors higher than $4\times10^7$. This is an order of magnitude larger than in the case of the Crab pulsar, the only other pulsar detected in the TeV energy range. Our results challenge the state-of-the-art models for high-energy emission of pulsars while providing a new probe, i.e. the energetic multi-TeV component, for constraining the acceleration and emission processes in their extreme energy limit. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06181v1-abstract-full').style.display = 'none'; document.getElementById('2310.06181v1-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 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">38 pages, 6 figures. This preprint has not undergone peer review or any post-submission improvements or corrections. The Version of Record of this article is published in Nature Astronomy, Nat Astron (2023), and is available online at https://doi.org/10.1038/s41550-023-02052-3</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.16699">arXiv:2308.16699</a> <span> [<a href="https://arxiv.org/pdf/2308.16699">pdf</a>, <a href="https://arxiv.org/format/2308.16699">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"> H.E.S.S. realtime follow-ups of IceCube high-energy neutrino alerts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bradascio%2C+F">Federica Bradascio</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">Halim Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Borowska%2C+J">Jowita Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Mbarubucyeye%2C+J+D">Jean Damascene Mbarubucyeye</a>, <a href="/search/astro-ph?searchtype=author&query=Oukacha%2C+E">Enzo Oukacha</a>, <a href="/search/astro-ph?searchtype=author&query=Sch%C3%BCssler%2C+F">Fabian Sch眉ssler</a>, <a href="/search/astro-ph?searchtype=author&query=Suzuki%2C+H">Hiromasa Suzuki</a>, <a href="/search/astro-ph?searchtype=author&query=Wierzcholska%2C+A">Alicja Wierzcholska</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="2308.16699v1-abstract-short" style="display: inline;"> The evidence for multi-messenger photon and neutrino emission from the blazar TXS 0506+056 has demonstrated the importance of realtime follow-up of neutrino events by various ground- and space-based facilities. The effort of H.E.S.S. and other experiments in coordinating observations to obtain quasi-simultaneous multiwavelength flux and spectrum measurements has been critical in measuring the chan… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.16699v1-abstract-full').style.display = 'inline'; document.getElementById('2308.16699v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.16699v1-abstract-full" style="display: none;"> The evidence for multi-messenger photon and neutrino emission from the blazar TXS 0506+056 has demonstrated the importance of realtime follow-up of neutrino events by various ground- and space-based facilities. The effort of H.E.S.S. and other experiments in coordinating observations to obtain quasi-simultaneous multiwavelength flux and spectrum measurements has been critical in measuring the chance coincidence with the high-energy neutrino event IC-170922A and constraining theoretical models. For about a decade, the H.E.S.S. transient program has included a search for gamma-ray emission associated with high-energy neutrino alerts, looking for gamma-ray activity from known sources and newly detected emitters consistent with the neutrino location. In this contribution, we present an overview of follow-up activities for realtime neutrino alerts with H.E.S.S. in 2021 and 2022. Our analysis includes both public IceCube neutrino alerts and alerts exchanged as part of a joint H.E.S.S.-IceCube program. We focus on interesting coincidences observed with gamma-ray sources, particularly highlighting the significant detection of PKS 0625-35, an AGN previously detected by H.E.S.S., and three IceCube neutrinos. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.16699v1-abstract-full').style.display = 'none'; document.getElementById('2308.16699v1-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Presented at the 38th International Cosmic Ray Conference (ICRC2023). See arXiv:2307.13047 for all IceCube contributions</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> PoS-ICRC2023-1546 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.01692">arXiv:2307.01692</a> <span> [<a href="https://arxiv.org/pdf/2307.01692">pdf</a>, <a href="https://arxiv.org/format/2307.01692">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/10.3847/2041-8213/ace3c0">10.3847/2041-8213/ace3c0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The vanishing of the primary emission region in PKS 1510-089 </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Aschersleben%2C+J">J. Aschersleben</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=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Barnard%2C+J">J. Barnard</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</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=Bernloehr%2C+K">K. Bernloehr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</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=Boettcher%2C+M">M. Boettcher</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=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bouyahiaoui%2C+M">M. Bouyahiaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Bradascio%2C+F">F. Bradascio</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=Brown%2C+A+M">A. M. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a> , et al. (130 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="2307.01692v1-abstract-short" style="display: inline;"> In July 2021, PKS 1510-089 exhibited a significant flux drop in the high-energy gamma-ray (by a factor 10) and optical (by a factor 5) bands and remained in this low state throughout 2022. Similarly, the optical polarization in the source vanished, resulting in the optical spectrum being fully explained through the steady flux of the accretion disk and the broad-line region. Unlike the aforementio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.01692v1-abstract-full').style.display = 'inline'; document.getElementById('2307.01692v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.01692v1-abstract-full" style="display: none;"> In July 2021, PKS 1510-089 exhibited a significant flux drop in the high-energy gamma-ray (by a factor 10) and optical (by a factor 5) bands and remained in this low state throughout 2022. Similarly, the optical polarization in the source vanished, resulting in the optical spectrum being fully explained through the steady flux of the accretion disk and the broad-line region. Unlike the aforementioned bands, the very-high-energy gamma-ray and X-ray fluxes did not exhibit a significant flux drop from year to year. This suggests that the steady-state very-high-energy gamma-ray and X-ray fluxes originate from a different emission region than the vanished parts of the high-energy gamma-ray and optical jet fluxes. The latter component has disappeared through either a swing of the jet away from the line-of-sight or a significant drop in the photon production efficiency of the jet close to the black hole. Either change could become visible in high-resolution radio images. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.01692v1-abstract-full').style.display = 'none'; document.getElementById('2307.01692v1-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 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 4 figures, 6 tables; accepted for publication in ApJ Letters; corresponding authors: Joleen Barnard, Markus Boettcher, Hester Schutte, Michael Zacharias</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.17819">arXiv:2306.17819</a> <span> [<a href="https://arxiv.org/pdf/2306.17819">pdf</a>, <a href="https://arxiv.org/format/2306.17819">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"> Multiwavelength Observations of the Blazar PKS 0735+178 in Spatial and Temporal Coincidence with an Astrophysical Neutrino Candidate IceCube-211208A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C+B">C. B. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Archer%2C+A">A. Archer</a>, <a href="/search/astro-ph?searchtype=author&query=Bangale%2C+P">P. Bangale</a>, <a href="/search/astro-ph?searchtype=author&query=Bartkoske%2C+J+T">J. T. Bartkoske</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+P">P. Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">W. Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Brill%2C+A">A. Brill</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=Christiansen%2C+J+L">J. L. Christiansen</a>, <a href="/search/astro-ph?searchtype=author&query=Chromey%2C+A+J">A. J. Chromey</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=Foote%2C+G+M">G. M. Foote</a>, <a href="/search/astro-ph?searchtype=author&query=Fortson%2C+L">L. Fortson</a>, <a href="/search/astro-ph?searchtype=author&query=Furniss%2C+A">A. Furniss</a>, <a href="/search/astro-ph?searchtype=author&query=Gallagher%2C+G">G. Gallagher</a>, <a href="/search/astro-ph?searchtype=author&query=Hanlon%2C+W">W. Hanlon</a>, <a href="/search/astro-ph?searchtype=author&query=Hanna%2C+D">D. Hanna</a>, <a href="/search/astro-ph?searchtype=author&query=Hervet%2C+O">O. Hervet</a>, <a href="/search/astro-ph?searchtype=author&query=Hinrichs%2C+C+E">C. E. Hinrichs</a>, <a href="/search/astro-ph?searchtype=author&query=Hoang%2C+J">J. Hoang</a>, <a href="/search/astro-ph?searchtype=author&query=Holder%2C+J">J. Holder</a>, <a href="/search/astro-ph?searchtype=author&query=Humensky%2C+T+B">T. B. Humensky</a> , et al. (185 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="2306.17819v1-abstract-short" style="display: inline;"> We report on multiwavelength target-of-opportunity observations of the blazar PKS 0735+178, located 2.2$^\circ$ away from the best-fit position of the IceCube neutrino event IceCube-211208A detected on December 8, 2021. The source was in a high-flux state in the optical, ultraviolet, X-ray, and GeV gamma-ray bands around the time of the neutrino event, exhibiting daily variability in the soft X-ra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.17819v1-abstract-full').style.display = 'inline'; document.getElementById('2306.17819v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.17819v1-abstract-full" style="display: none;"> We report on multiwavelength target-of-opportunity observations of the blazar PKS 0735+178, located 2.2$^\circ$ away from the best-fit position of the IceCube neutrino event IceCube-211208A detected on December 8, 2021. The source was in a high-flux state in the optical, ultraviolet, X-ray, and GeV gamma-ray bands around the time of the neutrino event, exhibiting daily variability in the soft X-ray flux. The X-ray data from Swift-XRT and NuSTAR characterize the transition between the low-energy and high-energy components of the broadband spectral energy distribution (SED), and the gamma-ray data from Fermi -LAT, VERITAS, and H.E.S.S. require a spectral cut-off near 100 GeV. Both X-ray and gamma-ray measurements provide strong constraints on the leptonic and hadronic models. We analytically explore a synchrotron self-Compton model, an external Compton model, and a lepto-hadronic model. Models that are entirely based on internal photon fields face serious difficulties in matching the observed SED. The existence of an external photon field in the source would instead explain the observed gamma-ray spectral cut-off in both leptonic and lepto-hadronic models and allow a proton jet power that marginally agrees with the Eddington limit in the lepto-hadronic model. We show a numerical lepto-hadronic model with external target photons that reproduces the observed SED and is reasonably consistent with the neutrino event despite requiring a high jet power. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.17819v1-abstract-full').style.display = 'none'; document.getElementById('2306.17819v1-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> 30 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 3 figures, 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/2305.09607">arXiv:2305.09607</a> <span> [<a href="https://arxiv.org/pdf/2305.09607">pdf</a>, <a href="https://arxiv.org/format/2305.09607">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/10.1051/0004-6361/202346056">10.1051/0004-6361/202346056 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraining the cosmic-ray pressure in the inner Virgo Cluster using H.E.S.S. observations of M 87 </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=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=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</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=Batzofin%2C+R">R. Batzofin</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=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bradascio%2C+F">F. Bradascio</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=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+C">C. Burger-Scheidlin</a>, <a href="/search/astro-ph?searchtype=author&query=Bylund%2C+T">T. Bylund</a> , et al. (139 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="2305.09607v1-abstract-short" style="display: inline;"> The origin of the gamma-ray emission from M87 is currently a matter of debate. This work aims to localize the VHE (100 GeV-100 TeV) gamma-ray emission from M87 and probe a potential extended hadronic emission component in the inner Virgo Cluster. The search for a steady and extended gamma-ray signal around M87 can constrain the cosmic-ray energy density and the pressure exerted by the cosmic rays… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.09607v1-abstract-full').style.display = 'inline'; document.getElementById('2305.09607v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.09607v1-abstract-full" style="display: none;"> The origin of the gamma-ray emission from M87 is currently a matter of debate. This work aims to localize the VHE (100 GeV-100 TeV) gamma-ray emission from M87 and probe a potential extended hadronic emission component in the inner Virgo Cluster. The search for a steady and extended gamma-ray signal around M87 can constrain the cosmic-ray energy density and the pressure exerted by the cosmic rays onto the intra-cluster medium, and allow us to investigate the role of the cosmic rays in the active galactic nucleus feedback as a heating mechanism in the Virgo Cluster. H.E.S.S. telescopes are sensitive to VHE gamma rays and have been utilized to observe M87 since 2004. We utilized a Bayesian block analysis to identify M87 emission states with H.E.S.S. observations from 2004 until 2021, dividing them into low, intermediate, and high states. Because of the causality argument, an extended ($\gtrsim$kpc) signal is allowed only in steady emission states. Hence, we fitted the morphology of the 120h low state data and found no significant gamma-ray extension. Therefore, we derived for the low state an upper limit of 58"(corresponding to $\approx$4.6kpc) in the extension of a single-component morphological model described by a rotationally symmetric 2D Gaussian model at 99.7% confidence level. Our results exclude the radio lobes ($\approx$30 kpc) as the principal component of the VHE gamma-ray emission from the low state of M87. The gamma-ray emission is compatible with a single emission region at the radio core of M87. These results, with the help of two multiple-component models, constrain the maximum cosmic-ray to thermal pressure ratio $X_{CR,max.}$$\lesssim$$0.32$ and the total energy in cosmic-ray protons (CRp) to $U_{CR}$$\lesssim$5$\times10^{58}$ erg in the inner 20kpc of the Virgo Cluster for an assumed CRp power-law distribution in momentum with spectral index $伪_{p}$=2.1. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.09607v1-abstract-full').style.display = 'none'; document.getElementById('2305.09607v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 7 figures. Accepted for publication in A&A. Corresponding authors: Victor Barbosa Martins, Stefan Ohm, Cornelia Arcaro, Natalia 呕ywucka, Mathieu de Naurois</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 675, A138 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.04796">arXiv:2304.04796</a> <span> [<a href="https://arxiv.org/pdf/2304.04796">pdf</a>, <a href="https://arxiv.org/ps/2304.04796">ps</a>, <a href="https://arxiv.org/format/2304.04796">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/10.1088/1538-3873/acd8f0">10.1088/1538-3873/acd8f0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Large Array Survey Telescope -- System Overview and Performances </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ofek%2C+E+O">E. O. Ofek</a>, <a href="/search/astro-ph?searchtype=author&query=Ben-Ami%2C+S">S. Ben-Ami</a>, <a href="/search/astro-ph?searchtype=author&query=Polishook%2C+D">D. Polishook</a>, <a href="/search/astro-ph?searchtype=author&query=Segre%2C+E">E. Segre</a>, <a href="/search/astro-ph?searchtype=author&query=Blumenzweig%2C+A">A. Blumenzweig</a>, <a href="/search/astro-ph?searchtype=author&query=Strotjohann%2C+N+L">N. L. Strotjohann</a>, <a href="/search/astro-ph?searchtype=author&query=Yaron%2C+O">O. Yaron</a>, <a href="/search/astro-ph?searchtype=author&query=Shani%2C+Y+M">Y. M. Shani</a>, <a href="/search/astro-ph?searchtype=author&query=Nachshon%2C+S">S. Nachshon</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Y. Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Hershko%2C+O">O. Hershko</a>, <a href="/search/astro-ph?searchtype=author&query=Engel%2C+M">M. Engel</a>, <a href="/search/astro-ph?searchtype=author&query=Segre%2C+M">M. Segre</a>, <a href="/search/astro-ph?searchtype=author&query=Segev%2C+N">N. Segev</a>, <a href="/search/astro-ph?searchtype=author&query=Zimmerman%2C+E">E. Zimmerman</a>, <a href="/search/astro-ph?searchtype=author&query=Nir%2C+G">G. Nir</a>, <a href="/search/astro-ph?searchtype=author&query=Judkovsky%2C+Y">Y. Judkovsky</a>, <a href="/search/astro-ph?searchtype=author&query=Gal-Yam%2C+A">A. Gal-Yam</a>, <a href="/search/astro-ph?searchtype=author&query=Zackay%2C+B">B. Zackay</a>, <a href="/search/astro-ph?searchtype=author&query=Waxman%2C+E">E. Waxman</a>, <a href="/search/astro-ph?searchtype=author&query=Kushnir%2C+D">D. Kushnir</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+P">P. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Azaria%2C+R">R. Azaria</a>, <a href="/search/astro-ph?searchtype=author&query=Manulis%2C+I">I. Manulis</a>, <a href="/search/astro-ph?searchtype=author&query=Diner%2C+O">O. Diner</a> , et al. (16 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.04796v1-abstract-short" style="display: inline;"> The Large Array Survey Telescope (LAST) is a wide-field visible-light telescope array designed to explore the variable and transient sky with a high cadence. LAST will be composed of 48, 28-cm f/2.2 telescopes (32 already installed) equipped with full-frame backside-illuminated cooled CMOS detectors. Each telescope provides a field of view (FoV) of 7.4 deg^2 with 1.25 arcsec/pix, while the system… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.04796v1-abstract-full').style.display = 'inline'; document.getElementById('2304.04796v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.04796v1-abstract-full" style="display: none;"> The Large Array Survey Telescope (LAST) is a wide-field visible-light telescope array designed to explore the variable and transient sky with a high cadence. LAST will be composed of 48, 28-cm f/2.2 telescopes (32 already installed) equipped with full-frame backside-illuminated cooled CMOS detectors. Each telescope provides a field of view (FoV) of 7.4 deg^2 with 1.25 arcsec/pix, while the system FoV is 355 deg^2 in 2.9 Gpix. The total collecting area of LAST, with 48 telescopes, is equivalent to a 1.9-m telescope. The cost-effectiveness of the system (i.e., probed volume of space per unit time per unit cost) is about an order of magnitude higher than most existing and under-construction sky surveys. The telescopes are mounted on 12 separate mounts, each carrying four telescopes. This provides significant flexibility in operating the system. The first LAST system is under construction in the Israeli Negev Desert, with 32 telescopes already deployed. We present the system overview and performances based on the system commissioning data. The Bp 5-sigma limiting magnitude of a single 28-cm telescope is about 19.6 (21.0), in 20 s (20x20 s). Astrometric two-axes precision (rms) at the bright-end is about 60 (30)\,mas in 20\,s (20x20 s), while absolute photometric calibration, relative to GAIA, provides ~10 millimag accuracy. Relative photometric precision, in a single 20 s (320 s) image, at the bright-end measured over a time scale of about 60 min is about 3 (1) millimag. We discuss the system science goals, data pipelines, and the observatory control system in companion publications. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.04796v1-abstract-full').style.display = 'none'; document.getElementById('2304.04796v1-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 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to PASP, 15pp</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.02631">arXiv:2304.02631</a> <span> [<a href="https://arxiv.org/pdf/2304.02631">pdf</a>, <a href="https://arxiv.org/format/2304.02631">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/10.1051/0004-6361/202245776">10.1051/0004-6361/202245776 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Detection of extended gamma-ray emission around the Geminga pulsar 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=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=Aschersleben%2C+J">J. Aschersleben</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=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</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=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bouyahiaoui%2C+M">M. Bouyahiaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Bradascio%2C+F">F. Bradascio</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=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Scheidlin%2C+C+B">C. Burger Scheidlin</a>, <a href="/search/astro-ph?searchtype=author&query=Cangemi%2C+F">F. Cangemi</a> , et al. (143 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="2304.02631v1-abstract-short" style="display: inline;"> Geminga is an enigmatic radio-quiet gamma-ray pulsar located at a mere 250 pc distance from Earth. Extended very-high-energy gamma-ray emission around the pulsar was discovered by Milagro and later confirmed by HAWC, which are both water Cherenkov detector-based experiments. However, evidence for the Geminga pulsar wind nebula in gamma rays has long evaded detection by imaging atmospheric Cherenko… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.02631v1-abstract-full').style.display = 'inline'; document.getElementById('2304.02631v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.02631v1-abstract-full" style="display: none;"> Geminga is an enigmatic radio-quiet gamma-ray pulsar located at a mere 250 pc distance from Earth. Extended very-high-energy gamma-ray emission around the pulsar was discovered by Milagro and later confirmed by HAWC, which are both water Cherenkov detector-based experiments. However, evidence for the Geminga pulsar wind nebula in gamma rays has long evaded detection by imaging atmospheric Cherenkov telescopes (IACTs) despite targeted observations. The detection of gamma-ray emission on angular scales > 2 deg poses a considerable challenge for the background estimation in IACT data analysis. With recent developments in understanding the complementary background estimation techniques of water Cherenkov and atmospheric Cherenkov instruments, the H.E.S.S. IACT array can now confirm the detection of highly extended gamma-ray emission around the Geminga pulsar with a radius of at least 3 deg in the energy range 0.5-40 TeV. We find no indications for statistically significant asymmetries or energy-dependent morphology. A flux normalisation of $(2.8\pm0.7)\times10^{-12}$ cm$^{-2}$s$^{-1}$TeV$^{-1}$ at 1 TeV is obtained within a 1 deg radius region around the pulsar. To investigate the particle transport within the halo of energetic leptons around the pulsar, we fitted an electron diffusion model to the data. The normalisation of the diffusion coefficient obtained of $D_0 = 7.6^{+1.5}_{-1.2} \times 10^{27}$ cm$^2$s$^{-1}$, at an electron energy of 100 TeV, is compatible with values previously reported for the pulsar halo around Geminga, which is considerably below the Galactic average. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.02631v1-abstract-full').style.display = 'none'; document.getElementById('2304.02631v1-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 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 15 figures, 7 tables. 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 673, A148 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.12855">arXiv:2303.12855</a> <span> [<a href="https://arxiv.org/pdf/2303.12855">pdf</a>, <a href="https://arxiv.org/format/2303.12855">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/10.1088/1475-7516/2023/04/040">10.1088/1475-7516/2023/04/040 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for the evaporation of primordial black holes 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=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=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Boettcher%2C+M">M. Boettcher</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</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=Batzo%2C+R">R. Batzo</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=Bi%2C+B">B. Bi</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=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bradascio%2C+F">F. Bradascio</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=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+C">C. Burger-Scheidlin</a>, <a href="/search/astro-ph?searchtype=author&query=Caro%2C+S">S. Caro</a>, <a href="/search/astro-ph?searchtype=author&query=Casanova%2C+S">S. Casanova</a>, <a href="/search/astro-ph?searchtype=author&query=Celic%2C+J">J. Celic</a> , et al. (124 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="2303.12855v1-abstract-short" style="display: inline;"> Primordial Black Holes (PBHs) are hypothetical black holes predicted to have been formed from density fluctuations in the early Universe. PBHs with an initial mass around $10^{14}-10^{15}$g are expected to end their evaporation at present times in a burst of particles and very-high-energy (VHE) gamma rays. Those gamma rays may be detectable by the High Energy Stereoscopic System (H.E.S.S.), an arr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.12855v1-abstract-full').style.display = 'inline'; document.getElementById('2303.12855v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.12855v1-abstract-full" style="display: none;"> Primordial Black Holes (PBHs) are hypothetical black holes predicted to have been formed from density fluctuations in the early Universe. PBHs with an initial mass around $10^{14}-10^{15}$g are expected to end their evaporation at present times in a burst of particles and very-high-energy (VHE) gamma rays. Those gamma rays may be detectable by the High Energy Stereoscopic System (H.E.S.S.), an array of imaging atmospheric Cherenkov telescopes. This paper reports on the search for evaporation bursts of VHE gamma rays with H.E.S.S., ranging from 10 to 120 seconds, as expected from the final stage of PBH evaporation and using a total of 4816 hours of observations. The most constraining upper limit on the burst rate of local PBHs is $2000$ pc$^{-3}$ yr$^{-1}$ for a burst interval of 120 seconds, at the 95\% confidence level. The implication of these measurements for PBH dark matter are also discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.12855v1-abstract-full').style.display = 'none'; document.getElementById('2303.12855v1-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 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in JCAP, corresponding authors: F.Brun, J-F. Glicenstein, V. Marandon, T. Tavernier</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.10558">arXiv:2303.10558</a> <span> [<a href="https://arxiv.org/pdf/2303.10558">pdf</a>, <a href="https://arxiv.org/format/2303.10558">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/acc405">10.3847/2041-8213/acc405 <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. follow-up observations of GRB221009A </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=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=Aschersleben%2C+J">J. Aschersleben</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=Baktash%2C+A">A. Baktash</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=Batzofin%2C+R">R. Batzofin</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=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bouyahiaoui%2C+M">M. Bouyahiaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Bradascio%2C+F">F. Bradascio</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=Bruno%2C+B">B. Bruno</a> , et al. (138 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="2303.10558v1-abstract-short" style="display: inline;"> GRB221009A is the brightest gamma-ray burst ever detected. To probe the very-high-energy (VHE, $>$\!100 GeV) emission, the High Energy Stereoscopic System (H.E.S.S.) began observations 53 hours after the triggering event, when the brightness of the moonlight no longer precluded observations. We derive differential and integral upper limits using H.E.S.S. data from the third, fourth, and ninth nigh… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.10558v1-abstract-full').style.display = 'inline'; document.getElementById('2303.10558v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.10558v1-abstract-full" style="display: none;"> GRB221009A is the brightest gamma-ray burst ever detected. To probe the very-high-energy (VHE, $>$\!100 GeV) emission, the High Energy Stereoscopic System (H.E.S.S.) began observations 53 hours after the triggering event, when the brightness of the moonlight no longer precluded observations. We derive differential and integral upper limits using H.E.S.S. data from the third, fourth, and ninth nights after the initial GRB detection, after applying atmospheric corrections. The combined observations yield an integral energy flux upper limit of $桅_\mathrm{UL}^{95\%} = 9.7 \times 10^{-12}~\mathrm{erg\,cm^{-2}\,s^{-1}}$ above $E_\mathrm{thr} = 650$ GeV. The constraints derived from the H.E.S.S. observations complement the available multiwavelength data. The radio to X-ray data are consistent with synchrotron emission from a single electron population, with the peak in the SED occurring above the X-ray band. Compared to the VHE-bright GRB190829A, the upper limits for GRB221009A imply a smaller gamma-ray to X-ray flux ratio in the afterglow. Even in the absence of a detection, the H.E.S.S. upper limits thus contribute to the multiwavelength picture of GRB221009A, effectively ruling out an IC dominated scenario. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.10558v1-abstract-full').style.display = 'none'; document.getElementById('2303.10558v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 4 figures. Accepted for publication in APJL. Corresponding authors: J. Damascene Mbarubucyeye, H. Ashkar, S. J. Zhu, B. Reville, F. Sch眉ssler</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.13663">arXiv:2302.13663</a> <span> [<a href="https://arxiv.org/pdf/2302.13663">pdf</a>, <a href="https://arxiv.org/format/2302.13663">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/10.1051/0004-6361/202245459">10.1051/0004-6361/202245459 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HESS J1809$-$193: a halo of escaped electrons around a pulsar wind nebula? </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=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=Aschersleben%2C+J">J. Aschersleben</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=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</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=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=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bouyahiaoui%2C+M">M. Bouyahiaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Bradascio%2C+F">F. Bradascio</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=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+C">C. Burger-Scheidlin</a>, <a href="/search/astro-ph?searchtype=author&query=Bylund%2C+T">T. Bylund</a>, <a href="/search/astro-ph?searchtype=author&query=Caroff%2C+S">S. Caroff</a> , et al. (130 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.13663v1-abstract-short" style="display: inline;"> Context. HESS J1809$-$193 is an unassociated very-high-energy $纬$-ray source located on the Galactic plane. While it has been connected to the nebula of the energetic pulsar PSR J1809$-$1917, supernova remnants and molecular clouds present in the vicinity also constitute possible associations. Recently, the detection of $纬$-ray emission up to energies of $\sim$100 TeV with the HAWC observatory has… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.13663v1-abstract-full').style.display = 'inline'; document.getElementById('2302.13663v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.13663v1-abstract-full" style="display: none;"> Context. HESS J1809$-$193 is an unassociated very-high-energy $纬$-ray source located on the Galactic plane. While it has been connected to the nebula of the energetic pulsar PSR J1809$-$1917, supernova remnants and molecular clouds present in the vicinity also constitute possible associations. Recently, the detection of $纬$-ray emission up to energies of $\sim$100 TeV with the HAWC observatory has led to renewed interest in HESS J1809$-$193. Aims. We aim to understand the origin of the $纬$-ray emission of HESS J1809$-$193. Methods. We analysed 93.2 h of data taken on HESS J1809$-$193 above 0.27 TeV with the High Energy Stereoscopic System (H.E.S.S.), using a multi-component, three-dimensional likelihood analysis. In addition, we provide a new analysis of 12.5 yr of Fermi-LAT data above 1 GeV within the region of HESS J1809$-$193. The obtained results are interpreted in a time-dependent modelling framework. Results. For the first time, we were able to resolve the emission detected with H.E.S.S. into two components: an extended component that exhibits a spectral cut-off at $\sim$13 TeV, and a compact component that is located close to PSR J1809$-$1917 and shows no clear spectral cut-off. The Fermi-LAT analysis also revealed extended $纬$-ray emission, on scales similar to that of the extended H.E.S.S. component. Conclusions. Our modelling indicates that based on its spectrum and spatial extent, the extended H.E.S.S. component is likely caused by inverse Compton emission from old electrons that form a halo around the pulsar wind nebula. The compact component could be connected to either the pulsar wind nebula or the supernova remnant and molecular clouds. Due to its comparatively steep spectrum, modelling the Fermi-LAT emission together with the H.E.S.S. components is not straightforward. (abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.13663v1-abstract-full').style.display = 'none'; document.getElementById('2302.13663v1-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 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 10 figures. Accepted for publication in A&A. Corresponding authors: Vikas Joshi, Lars Mohrmann</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 672, A103 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.05933">arXiv:2111.05933</a> <span> [<a href="https://arxiv.org/pdf/2111.05933">pdf</a>, <a href="https://arxiv.org/format/2111.05933">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/10.3847/1538-4357/ac63c9">10.3847/1538-4357/ac63c9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> COMAP Early Science: VII. Prospects for CO Intensity Mapping at Reionization </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Breysse%2C+P+C">Patrick C. Breysse</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+D+T">Dongwoo T. Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Cleary%2C+K+A">Kieran A. Cleary</a>, <a href="/search/astro-ph?searchtype=author&query=Ihle%2C+H+T">H氓vard T. Ihle</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabhan%2C+H">Hamsa Padmanabhan</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+M+B">Marta B. Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J. Richard Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Borowska%2C+J">Jowita Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Catha%2C+M">Morgan Catha</a>, <a href="/search/astro-ph?searchtype=author&query=Church%2C+S+E">Sarah E. Church</a>, <a href="/search/astro-ph?searchtype=author&query=Dunne%2C+D+A">Delaney A. Dunne</a>, <a href="/search/astro-ph?searchtype=author&query=Eriksen%2C+H+K">Hans Kristian Eriksen</a>, <a href="/search/astro-ph?searchtype=author&query=Foss%2C+M+K">Marie Kristine Foss</a>, <a href="/search/astro-ph?searchtype=author&query=Gaier%2C+T">Todd Gaier</a>, <a href="/search/astro-ph?searchtype=author&query=Gundersen%2C+J+O">Joshua Ott Gundersen</a>, <a href="/search/astro-ph?searchtype=author&query=Harris%2C+A+I">Andrew I. Harris</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+R">Richard Hobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Keating%2C+L">Laura Keating</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+J+W">James W. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Lawrence%2C+C+R">Charles R. Lawrence</a>, <a href="/search/astro-ph?searchtype=author&query=Lunde%2C+J+G+S">Jonas G. S. Lunde</a>, <a href="/search/astro-ph?searchtype=author&query=Murray%2C+N">Norman Murray</a>, <a href="/search/astro-ph?searchtype=author&query=Pearson%2C+T+J">Timothy J. Pearson</a>, <a href="/search/astro-ph?searchtype=author&query=Philip%2C+L">Liju Philip</a>, <a href="/search/astro-ph?searchtype=author&query=Rasmussen%2C+M">Maren Rasmussen</a> , et al. (7 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="2111.05933v2-abstract-short" style="display: inline;"> We introduce COMAP-EoR, the next generation of the Carbon Monoxide Mapping Array Project aimed at extending CO intensity mapping to the Epoch of Reionization. COMAP-EoR supplements the existing 30 GHz COMAP Pathfinder with two additional 30 GHz instruments and a new 16 GHz receiver. This combination of frequencies will be able to simultaneously map CO(1--0) and CO(2--1) at reionization redshifts (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05933v2-abstract-full').style.display = 'inline'; document.getElementById('2111.05933v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.05933v2-abstract-full" style="display: none;"> We introduce COMAP-EoR, the next generation of the Carbon Monoxide Mapping Array Project aimed at extending CO intensity mapping to the Epoch of Reionization. COMAP-EoR supplements the existing 30 GHz COMAP Pathfinder with two additional 30 GHz instruments and a new 16 GHz receiver. This combination of frequencies will be able to simultaneously map CO(1--0) and CO(2--1) at reionization redshifts ($z\sim5-8$) in addition to providing a significant boost to the $z\sim3$ sensitivity of the Pathfinder. We examine a set of existing models of the EoR CO signal, and find power spectra spanning several orders of magnitude, highlighting our extreme ignorance about this period of cosmic history and the value of the COMAP-EoR measurement. We carry out the most detailed forecast to date of an intensity mapping cross-correlation, and find that five out of the six models we consider yield signal to noise ratios (S/N) $\gtrsim20$ for COMAP-EoR, with the brightest reaching a S/N above 400. We show that, for these models, COMAP-EoR can make a detailed measurement of the cosmic molecular gas history from $z\sim2-8$, as well as probe the population of faint, star-forming galaxies predicted by these models to be undetectable by traditional surveys. We show that, for the single model that does not predict numerous faint emitters, a COMAP-EoR-type measurement is required to rule out their existence. We briefly explore prospects for a third-generation Expanded Reionization Array (COMAP-ERA) capable of detecting the faintest models and characterizing the brightest signals in extreme detail. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05933v2-abstract-full').style.display = 'none'; document.getElementById('2111.05933v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 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">Paper 7 of 7 in series. 19 pages, 10 figures, to be 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/2111.05932">arXiv:2111.05932</a> <span> [<a href="https://arxiv.org/pdf/2111.05932">pdf</a>, <a href="https://arxiv.org/format/2111.05932">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> </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/ac63c8">10.3847/1538-4357/ac63c8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> COMAP Early Science: VI. A First Look at the COMAP Galactic Plane Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rennie%2C+T+J">Thomas J. Rennie</a>, <a href="/search/astro-ph?searchtype=author&query=Harper%2C+S+E">Stuart E. Harper</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+C">Clive Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Philip%2C+L">Liju Philip</a>, <a href="/search/astro-ph?searchtype=author&query=Cleary%2C+K+A">Kieran A. Cleary</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+R+J">Richard J. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Borowska%2C+J">Jowita Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Breysse%2C+P+C">Patrick C. Breysse</a>, <a href="/search/astro-ph?searchtype=author&query=Catha%2C+M">Morgan Catha</a>, <a href="/search/astro-ph?searchtype=author&query=Cepeda-Arroita%2C+R">Roke Cepeda-Arroita</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+D+T">Dongwoo T. Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Church%2C+S+E">Sarah E. Church</a>, <a href="/search/astro-ph?searchtype=author&query=Dunne%2C+D+A">Delaney A. Dunne</a>, <a href="/search/astro-ph?searchtype=author&query=Eriksen%2C+H+K">Hans Kristian Eriksen</a>, <a href="/search/astro-ph?searchtype=author&query=Foss%2C+M+K">Marie Kristine Foss</a>, <a href="/search/astro-ph?searchtype=author&query=Gaier%2C+T">Todd Gaier</a>, <a href="/search/astro-ph?searchtype=author&query=Gunderson%2C+J+O">Joshua Ott Gunderson</a>, <a href="/search/astro-ph?searchtype=author&query=Harris%2C+A+I">Andrew I. Harris</a>, <a href="/search/astro-ph?searchtype=author&query=Hensley%2C+B">Brandon Hensley</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+R">Richard Hobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Ihle%2C+H+T">H氓vard T. Ihle</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+J+W">James W. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Lawrence%2C+C+R">Charles R. Lawrence</a>, <a href="/search/astro-ph?searchtype=author&query=Lunde%2C+J+G+S">Jonas G. S. Lunde</a>, <a href="/search/astro-ph?searchtype=author&query=Paladini%2C+R">Roberta Paladini</a> , et al. (7 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="2111.05932v6-abstract-short" style="display: inline;"> We present early results from the COMAP Galactic Plane Survey conducted between June 2019 and April 2021, spanning $20^\circ<\ell<40^\circ$ in Galactic longitude and $|b|<1.\!\!^{\circ}5$ in Galactic latitude with an angular resolution of $4.5^{\prime}$. The full survey will span $\ell \sim 20^{\circ}$- $220^{\circ}$ and will be the first large-scale radio continuum survey at $30$ GHz with sub-deg… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05932v6-abstract-full').style.display = 'inline'; document.getElementById('2111.05932v6-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.05932v6-abstract-full" style="display: none;"> We present early results from the COMAP Galactic Plane Survey conducted between June 2019 and April 2021, spanning $20^\circ<\ell<40^\circ$ in Galactic longitude and $|b|<1.\!\!^{\circ}5$ in Galactic latitude with an angular resolution of $4.5^{\prime}$. The full survey will span $\ell \sim 20^{\circ}$- $220^{\circ}$ and will be the first large-scale radio continuum survey at $30$ GHz with sub-degree resolution. We present initial results from the first part of the survey, including diffuse emission and spectral energy distributions (SEDs) of HII regions and supernova remnants. Using low and high frequency surveys to constrain free-free and thermal dust emission contributions, we find evidence of excess flux density at $30\,$GHz in six regions that we interpret as anomalous microwave emission. Furthermore we model UCHII contributions using data from the $5\,$GHz CORNISH catalogue and reject this as the cause of the $30\,$GHz excess. Six known supernova remnants (SNR) are detected at $30\,$GHz, and we measure spectral indices consistent with the literature or show evidence of steepening. The flux density of the SNR W44 at $30\,$GHz is consistent with a power-law extrapolation from lower frequencies with no indication of spectral steepening in contrast with recent results from the Sardinia Radio Telescope. We also extract five hydrogen radio recombination lines to map the warm ionized gas, which can be used to estimate electron temperatures or to constrain continuum free-free emission. The full COMAP Galactic plane survey, to be released in 2023/2024, will be an invaluable resource for Galactic astrophysics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05932v6-abstract-full').style.display = 'none'; document.getElementById('2111.05932v6-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 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">Paper 6 of 7 in series. 28 pages, 10 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/2111.05931">arXiv:2111.05931</a> <span> [<a href="https://arxiv.org/pdf/2111.05931">pdf</a>, <a href="https://arxiv.org/format/2111.05931">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/10.3847/1538-4357/ac63c7">10.3847/1538-4357/ac63c7 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> COMAP Early Science: V. Constraints and Forecasts at $z \sim 3$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chung%2C+D+T">Dongwoo T. Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Breysse%2C+P+C">Patrick C. Breysse</a>, <a href="/search/astro-ph?searchtype=author&query=Cleary%2C+K+A">Kieran A. Cleary</a>, <a href="/search/astro-ph?searchtype=author&query=Ihle%2C+H+T">H氓vard T. Ihle</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabhan%2C+H">Hamsa Padmanabhan</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+M+B">Marta B. Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J. Richard Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Borowska%2C+J">Jowita Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Catha%2C+M">Morgan Catha</a>, <a href="/search/astro-ph?searchtype=author&query=Church%2C+S+E">Sarah E. Church</a>, <a href="/search/astro-ph?searchtype=author&query=Dunne%2C+D+A">Delaney A. Dunne</a>, <a href="/search/astro-ph?searchtype=author&query=Eriksen%2C+H+K">Hans Kristian Eriksen</a>, <a href="/search/astro-ph?searchtype=author&query=Foss%2C+M+K">Marie Kristine Foss</a>, <a href="/search/astro-ph?searchtype=author&query=Gaier%2C+T">Todd Gaier</a>, <a href="/search/astro-ph?searchtype=author&query=Gundersen%2C+J+O">Joshua Ott Gundersen</a>, <a href="/search/astro-ph?searchtype=author&query=Harper%2C+S+E">Stuart E. Harper</a>, <a href="/search/astro-ph?searchtype=author&query=Harris%2C+A+I">Andrew I. Harris</a>, <a href="/search/astro-ph?searchtype=author&query=Hensley%2C+B">Brandon Hensley</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+R">Richard Hobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Keating%2C+L+C">Laura C. Keating</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+J">Junhan Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+J+W">James W. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Lawrence%2C+C+R">Charles R. Lawrence</a>, <a href="/search/astro-ph?searchtype=author&query=Lunde%2C+J+G+S">Jonas Gahr Sturtzel Lunde</a>, <a href="/search/astro-ph?searchtype=author&query=Murray%2C+N">Norman Murray</a> , et al. (12 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="2111.05931v3-abstract-short" style="display: inline;"> We present the current state of models for the $z\sim3$ carbon monoxide (CO) line-intensity signal targeted by the CO Mapping Array Project (COMAP) Pathfinder in the context of its early science results. Our fiducial model, relating dark matter halo properties to CO luminosities, informs parameter priors with empirical models of the galaxy-halo connection and previous CO(1-0) observations. The Pat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05931v3-abstract-full').style.display = 'inline'; document.getElementById('2111.05931v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.05931v3-abstract-full" style="display: none;"> We present the current state of models for the $z\sim3$ carbon monoxide (CO) line-intensity signal targeted by the CO Mapping Array Project (COMAP) Pathfinder in the context of its early science results. Our fiducial model, relating dark matter halo properties to CO luminosities, informs parameter priors with empirical models of the galaxy-halo connection and previous CO(1-0) observations. The Pathfinder early science data spanning wavenumbers $k=0.051$-$0.62\,$Mpc$^{-1}$ represent the first direct 3D constraint on the clustering component of the CO(1-0) power spectrum. Our 95% upper limit on the redshift-space clustering amplitude $A_{\rm clust}\lesssim70\,渭$K$^2$ greatly improves on the indirect upper limit of $420\,渭$K$^2$ reported from the CO Power Spectrum Survey (COPSS) measurement at $k\sim1\,$Mpc$^{-1}$. The COMAP limit excludes a subset of models from previous literature, and constrains interpretation of the COPSS results, demonstrating the complementary nature of COMAP and interferometric CO surveys. Using line bias expectations from our priors, we also constrain the squared mean line intensity-bias product, $\langle{Tb}\rangle^2\lesssim50\,渭$K$^2$, and the cosmic molecular gas density, $蟻_\text{H2}<2.5\times10^8\,M_\odot\,$Mpc$^{-3}$ (95% upper limits). Based on early instrument performance and our current CO signal estimates, we forecast that the five-year Pathfinder campaign will detect the CO power spectrum with overall signal-to-noise of 9-17. Between then and now, we also expect to detect the CO-galaxy cross-spectrum using overlapping galaxy survey data, enabling enhanced inferences of cosmic star-formation and galaxy-evolution history. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05931v3-abstract-full').style.display = 'none'; document.getElementById('2111.05931v3-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 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 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">Paper 5 of 7 in series. 17 pages + appendix and bibliography (30 pages total); 15 figures, 6 tables; accepted for publication in ApJ; v3 reflects the accepted version with minor changes and additions to text</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ, 933, 186 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.05930">arXiv:2111.05930</a> <span> [<a href="https://arxiv.org/pdf/2111.05930">pdf</a>, <a href="https://arxiv.org/format/2111.05930">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/10.3847/1538-4357/ac63c5">10.3847/1538-4357/ac63c5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> COMAP Early Science: IV. Power Spectrum Methodology and Results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ihle%2C+H+T">H氓vard T. Ihle</a>, <a href="/search/astro-ph?searchtype=author&query=Borowska%2C+J">Jowita Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Cleary%2C+K+A">Kieran A. Cleary</a>, <a href="/search/astro-ph?searchtype=author&query=Eriksen%2C+H+K">Hans Kristian Eriksen</a>, <a href="/search/astro-ph?searchtype=author&query=Foss%2C+M+K">Marie K. Foss</a>, <a href="/search/astro-ph?searchtype=author&query=Harper%2C+S+E">Stuart E. Harper</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+J">Junhan Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lunde%2C+J+G+S">Jonas G. S. Lunde</a>, <a href="/search/astro-ph?searchtype=author&query=Philip%2C+L">Liju Philip</a>, <a href="/search/astro-ph?searchtype=author&query=Rasmussen%2C+M">Maren Rasmussen</a>, <a href="/search/astro-ph?searchtype=author&query=Stutzer%2C+N">Nils-Ole Stutzer</a>, <a href="/search/astro-ph?searchtype=author&query=Uzgil%2C+B+D">Bade D. Uzgil</a>, <a href="/search/astro-ph?searchtype=author&query=Watts%2C+D+J">Duncan J. Watts</a>, <a href="/search/astro-ph?searchtype=author&query=Wehus%2C+I+K">Ingunn Kathrine Wehus</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J. Richard Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Breysse%2C+P+C">Patrick C. Breysse</a>, <a href="/search/astro-ph?searchtype=author&query=Catha%2C+M">Morgan Catha</a>, <a href="/search/astro-ph?searchtype=author&query=Church%2C+S+E">Sarah E. Church</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+D+T">Dongwoo T. Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+C">Clive Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Dunne%2C+D+A">Delaney A. Dunne</a>, <a href="/search/astro-ph?searchtype=author&query=Gaier%2C+T">Todd Gaier</a>, <a href="/search/astro-ph?searchtype=author&query=Gundersen%2C+J+O">Joshua Ott Gundersen</a>, <a href="/search/astro-ph?searchtype=author&query=Harris%2C+A+I">Andrew I. Harris</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+R">Richard Hobbs</a> , et al. (8 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.05930v3-abstract-short" style="display: inline;"> We present the power spectrum methodology used for the first-season COMAP analysis, and assess the quality of the current data set. The main results are derived through the Feed-feed Pseudo-Cross-Spectrum (FPXS) method, which is a robust estimator with respect to both noise modeling errors and experimental systematics. We use effective transfer functions to take into account the effects of instrum… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05930v3-abstract-full').style.display = 'inline'; document.getElementById('2111.05930v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.05930v3-abstract-full" style="display: none;"> We present the power spectrum methodology used for the first-season COMAP analysis, and assess the quality of the current data set. The main results are derived through the Feed-feed Pseudo-Cross-Spectrum (FPXS) method, which is a robust estimator with respect to both noise modeling errors and experimental systematics. We use effective transfer functions to take into account the effects of instrumental beam smoothing and various filter operations applied during the low-level data processing. The power spectra estimated in this way have allowed us to identify a systematic error associated with one of our two scanning strategies, believed to be due to residual ground or atmospheric contamination. We omit these data from our analysis and no longer use this scanning technique for observations. We present the power spectra from our first season of observing and demonstrate that the uncertainties are integrating as expected for uncorrelated noise, with any residual systematics suppressed to a level below the noise. Using the FPXS method, and combining data on scales $k=0.051-0.62 \,\mathrm{Mpc}^{-1}$ we estimate $P_\mathrm{CO}(k) = -2.7 \pm 1.7 \times 10^4渭\textrm{K}^2\mathrm{Mpc}^3$, the first direct 3D constraint on the clustering component of the CO(1-0) power spectrum in the literature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05930v3-abstract-full').style.display = 'none'; document.getElementById('2111.05930v3-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 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">Paper 4 of 7 in series. 18 pages, 11 figures, as accepted 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/2111.05929">arXiv:2111.05929</a> <span> [<a href="https://arxiv.org/pdf/2111.05929">pdf</a>, <a href="https://arxiv.org/format/2111.05929">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.3847/1538-4357/ac63ca">10.3847/1538-4357/ac63ca <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> COMAP Early Science: III. CO Data Processing </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Foss%2C+M+K">Marie K. Foss</a>, <a href="/search/astro-ph?searchtype=author&query=Ihle%2C+H+T">H氓vard T. Ihle</a>, <a href="/search/astro-ph?searchtype=author&query=Borowska%2C+J">Jowita Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Cleary%2C+K+A">Kieran A. Cleary</a>, <a href="/search/astro-ph?searchtype=author&query=Eriksen%2C+H+K">Hans Kristian Eriksen</a>, <a href="/search/astro-ph?searchtype=author&query=Harper%2C+S+E">Stuart E. Harper</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+J">Junhan Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+J+W">James W. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Lunde%2C+J+G+S">Jonas G. S. Lunde</a>, <a href="/search/astro-ph?searchtype=author&query=Philip%2C+L">Liju Philip</a>, <a href="/search/astro-ph?searchtype=author&query=Rasmussen%2C+M">Maren Rasmussen</a>, <a href="/search/astro-ph?searchtype=author&query=Stutzer%2C+N">Nils-Ole Stutzer</a>, <a href="/search/astro-ph?searchtype=author&query=Uzgil%2C+B+D">Bade D. Uzgil</a>, <a href="/search/astro-ph?searchtype=author&query=Watts%2C+D+J">Duncan J. Watts</a>, <a href="/search/astro-ph?searchtype=author&query=Wehus%2C+I+K">Ingunn K. Wehus</a>, <a href="/search/astro-ph?searchtype=author&query=Woody%2C+D+P">David P. Woody</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J. Richard Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Breysse%2C+P+C">Patrick C. Breysse</a>, <a href="/search/astro-ph?searchtype=author&query=Catha%2C+M">Morgan Catha</a>, <a href="/search/astro-ph?searchtype=author&query=Church%2C+S+E">Sarah E. Church</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+D+T">Dongwoo T. Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+C">Clive Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Dunne%2C+D+A">Delaney A. Dunne</a>, <a href="/search/astro-ph?searchtype=author&query=Gaier%2C+T">Todd Gaier</a>, <a href="/search/astro-ph?searchtype=author&query=Gundersen%2C+J+O">Joshua Ott Gundersen</a> , et al. (8 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.05929v3-abstract-short" style="display: inline;"> We describe the first season COMAP analysis pipeline that converts raw detector readouts to calibrated sky maps. This pipeline implements four main steps: gain calibration, filtering, data selection, and map-making. Absolute gain calibration relies on a combination of instrumental and astrophysical sources, while relative gain calibration exploits real-time total-power variations. High efficiency… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05929v3-abstract-full').style.display = 'inline'; document.getElementById('2111.05929v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.05929v3-abstract-full" style="display: none;"> We describe the first season COMAP analysis pipeline that converts raw detector readouts to calibrated sky maps. This pipeline implements four main steps: gain calibration, filtering, data selection, and map-making. Absolute gain calibration relies on a combination of instrumental and astrophysical sources, while relative gain calibration exploits real-time total-power variations. High efficiency filtering is achieved through spectroscopic common-mode rejection within and across receivers, resulting in nearly uncorrelated white noise within single-frequency channels. Consequently, near-optimal but biased maps are produced by binning the filtered time stream into pixelized maps; the corresponding signal bias transfer function is estimated through simulations. Data selection is performed automatically through a series of goodness-of-fit statistics, including $蠂^2$ and multi-scale correlation tests. Applying this pipeline to the first-season COMAP data, we produce a dataset with very low levels of correlated noise. We find that one of our two scanning strategies (the Lissajous type) is sensitive to residual instrumental systematics. As a result, we no longer use this type of scan and exclude data taken this way from our Season 1 power spectrum estimates. We perform a careful analysis of our data processing and observing efficiencies and take account of planned improvements to estimate our future performance. Power spectrum results derived from the first-season COMAP maps are presented and discussed in companion papers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05929v3-abstract-full').style.display = 'none'; document.getElementById('2111.05929v3-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> 30 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 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">Paper 3 of 7 in series. 26 pages, 23 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/2111.05928">arXiv:2111.05928</a> <span> [<a href="https://arxiv.org/pdf/2111.05928">pdf</a>, <a href="https://arxiv.org/format/2111.05928">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.3847/1538-4357/ac63c6">10.3847/1538-4357/ac63c6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> COMAP Early Science: II. Pathfinder Instrument </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+J+W">James W. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Cleary%2C+K+A">Kieran A. Cleary</a>, <a href="/search/astro-ph?searchtype=author&query=Woody%2C+D+P">David P. Woody</a>, <a href="/search/astro-ph?searchtype=author&query=Catha%2C+M">Morgan Catha</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+D+T">Dongwoo T. Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Gundersen%2C+J+O">Joshua Ott Gundersen</a>, <a href="/search/astro-ph?searchtype=author&query=Harper%2C+S+E">Stuart E. Harper</a>, <a href="/search/astro-ph?searchtype=author&query=Harris%2C+A+I">Andrew I. Harris</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+R">Richard Hobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Ihle%2C+H+T">H氓vard T. Ihle</a>, <a href="/search/astro-ph?searchtype=author&query=Kocz%2C+J">Jonathon Kocz</a>, <a href="/search/astro-ph?searchtype=author&query=Pearson%2C+T+J">Timothy J. Pearson</a>, <a href="/search/astro-ph?searchtype=author&query=Philip%2C+L">Liju Philip</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+T+W">Travis W. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Basoalto%2C+L">Lilian Basoalto</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J. Richard Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Borowska%2C+J">Jowita Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Breysse%2C+P+C">Patrick C. Breysse</a>, <a href="/search/astro-ph?searchtype=author&query=Church%2C+S+E">Sarah E. Church</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+C">Clive Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Dunne%2C+D+A">Delaney A. Dunne</a>, <a href="/search/astro-ph?searchtype=author&query=Eriksen%2C+H+K">Hans Kristian Eriksen</a>, <a href="/search/astro-ph?searchtype=author&query=Foss%2C+M+K">Marie Kristine Foss</a>, <a href="/search/astro-ph?searchtype=author&query=Gaier%2C+T">Todd Gaier</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+J">Junhan Kim</a> , et al. (10 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.05928v3-abstract-short" style="display: inline;"> Line intensity mapping (LIM) is a new technique for tracing the global properties of galaxies over cosmic time. Detection of the very faint signals from redshifted carbon monoxide (CO), a tracer of star formation, pushes the limits of what is feasible with a total-power instrument. The CO Mapping Project (COMAP) Pathfinder is a first-generation instrument aiming to prove the concept and develop th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05928v3-abstract-full').style.display = 'inline'; document.getElementById('2111.05928v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.05928v3-abstract-full" style="display: none;"> Line intensity mapping (LIM) is a new technique for tracing the global properties of galaxies over cosmic time. Detection of the very faint signals from redshifted carbon monoxide (CO), a tracer of star formation, pushes the limits of what is feasible with a total-power instrument. The CO Mapping Project (COMAP) Pathfinder is a first-generation instrument aiming to prove the concept and develop the technology for future experiments, as well as delivering early science products. With 19 receiver channels in a hexagonal focal plane arrangement on a 10.4 m antenna, and an instantaneous 26-34 GHz frequency range with 2 MHz resolution, it is ideally suited to measuring CO($J$=1-0) from $z\sim3$. In this paper we discuss strategies for designing and building the Pathfinder and the challenges that were encountered. The design of the instrument prioritized LIM requirements over those of ancillary science. After a couple of years of operation, the instrument is well understood, and the first year of data is already yielding useful science results. Experience with this Pathfinder will drive the design of the next generations of experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05928v3-abstract-full').style.display = 'none'; document.getElementById('2111.05928v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 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">Paper 2 of 7 in series. 27 pages, 28 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/2111.05927">arXiv:2111.05927</a> <span> [<a href="https://arxiv.org/pdf/2111.05927">pdf</a>, <a href="https://arxiv.org/format/2111.05927">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/10.3847/1538-4357/ac63cc">10.3847/1538-4357/ac63cc <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> COMAP Early Science: I. Overview </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cleary%2C+K+A">Kieran A. Cleary</a>, <a href="/search/astro-ph?searchtype=author&query=Borowska%2C+J">Jowita Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Breysse%2C+P+C">Patrick C. Breysse</a>, <a href="/search/astro-ph?searchtype=author&query=Catha%2C+M">Morgan Catha</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+D+T">Dongwoo T. Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Church%2C+S+E">Sarah E. Church</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+C">Clive Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Eriksen%2C+H+K">Hans Kristian Eriksen</a>, <a href="/search/astro-ph?searchtype=author&query=Foss%2C+M+K">Marie Kristine Foss</a>, <a href="/search/astro-ph?searchtype=author&query=Gundersen%2C+J+O">Joshua Ott Gundersen</a>, <a href="/search/astro-ph?searchtype=author&query=Harper%2C+S+E">Stuart E. Harper</a>, <a href="/search/astro-ph?searchtype=author&query=Harris%2C+A+I">Andrew I. Harris</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+R">Richard Hobbs</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%A5vard"> H氓vard</a>, <a href="/search/astro-ph?searchtype=author&query=Ihle%2C+T">T. Ihle</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+J">Junhan Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kocz%2C+J">Jonathon Kocz</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+J+W">James W. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Lunde%2C+J+G+S">Jonas G. S. Lunde</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabhan%2C+H">Hamsa Padmanabhan</a>, <a href="/search/astro-ph?searchtype=author&query=Pearson%2C+T+J">Timothy J. Pearson</a>, <a href="/search/astro-ph?searchtype=author&query=Philip%2C+L">Liju Philip</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+T+W">Travis W. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Rasmussen%2C+M">Maren Rasmussen</a>, <a href="/search/astro-ph?searchtype=author&query=Readhead%2C+A+C+S">Anthony C. S. Readhead</a> , et al. (18 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="2111.05927v3-abstract-short" style="display: inline;"> The CO Mapping Array Project (COMAP) aims to use line intensity mapping of carbon monoxide (CO) to trace the distribution and global properties of galaxies over cosmic time, back to the Epoch of Reionization (EoR). To validate the technologies and techniques needed for this goal, a Pathfinder instrument has been constructed and fielded. Sensitive to CO(1-0) emission from $z=2.4$-$3.4$ and a fainte… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05927v3-abstract-full').style.display = 'inline'; document.getElementById('2111.05927v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.05927v3-abstract-full" style="display: none;"> The CO Mapping Array Project (COMAP) aims to use line intensity mapping of carbon monoxide (CO) to trace the distribution and global properties of galaxies over cosmic time, back to the Epoch of Reionization (EoR). To validate the technologies and techniques needed for this goal, a Pathfinder instrument has been constructed and fielded. Sensitive to CO(1-0) emission from $z=2.4$-$3.4$ and a fainter contribution from CO(2-1) at $z=6$-8, the Pathfinder is surveying $12$ deg$^2$ in a 5-year observing campaign to detect the CO signal from $z\sim3$. Using data from the first 13 months of observing, we estimate $P_\mathrm{CO}(k) = -2.7 \pm 1.7 \times 10^4渭\mathrm{K}^2 \mathrm{Mpc}^3$ on scales $k=0.051-0.62 \mathrm{Mpc}^{-1}$ - the first direct 3D constraint on the clustering component of the CO(1-0) power spectrum. Based on these observations alone, we obtain a constraint on the amplitude of the clustering component (the squared mean CO line temperature-bias product) of $\langle Tb\rangle^2<49$ $渭$K$^2$ - nearly an order-of-magnitude improvement on the previous best measurement. These constraints allow us to rule out two models from the literature. We forecast a detection of the power spectrum after 5 years with signal-to-noise ratio (S/N) 9-17. Cross-correlation with an overlapping galaxy survey will yield a detection of the CO-galaxy power spectrum with S/N of 19. We are also conducting a 30 GHz survey of the Galactic plane and present a preliminary map. Looking to the future of COMAP, we examine the prospects for future phases of the experiment to detect and characterize the CO signal from the EoR. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05927v3-abstract-full').style.display = 'none'; document.getElementById('2111.05927v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 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">Paper 1 of 7 in series. 18 pages, 16 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/2104.11171">arXiv:2104.11171</a> <span> [<a href="https://arxiv.org/pdf/2104.11171">pdf</a>, <a href="https://arxiv.org/format/2104.11171">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/10.3847/1538-4357/ac2a35">10.3847/1538-4357/ac2a35 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A model of spectral line broadening in signal forecasts for line-intensity mapping experiments </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chung%2C+D+T">Dongwoo T. Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Breysse%2C+P+C">Patrick C. Breysse</a>, <a href="/search/astro-ph?searchtype=author&query=Ihle%2C+H+T">H氓vard Tveit Ihle</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabhan%2C+H">Hamsa Padmanabhan</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+M+B">Marta B. Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J. Richard Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Borowska%2C+J">Jowita Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Cleary%2C+K+A">Kieran A. Cleary</a>, <a href="/search/astro-ph?searchtype=author&query=Eriksen%2C+H+K">Hans Kristian Eriksen</a>, <a href="/search/astro-ph?searchtype=author&query=Foss%2C+M+K">Marie Kristine Foss</a>, <a href="/search/astro-ph?searchtype=author&query=Gundersen%2C+J+O">Joshua Ott Gundersen</a>, <a href="/search/astro-ph?searchtype=author&query=Keating%2C+L+C">Laura C. Keating</a>, <a href="/search/astro-ph?searchtype=author&query=Lunde%2C+J+G+S">Jonas Gahr Sturtzel Lunde</a>, <a href="/search/astro-ph?searchtype=author&query=Philip%2C+L">Liju Philip</a>, <a href="/search/astro-ph?searchtype=author&query=Stutzer%2C+N">Nils-Ole Stutzer</a>, <a href="/search/astro-ph?searchtype=author&query=Viero%2C+M+P">Marco P. Viero</a>, <a href="/search/astro-ph?searchtype=author&query=Watts%2C+D+J">Duncan J. Watts</a>, <a href="/search/astro-ph?searchtype=author&query=Wehus%2C+I+K">Ingunn Kathrine Wehus</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="2104.11171v2-abstract-short" style="display: inline;"> Line-intensity mapping observations will find fluctuations of integrated line emission are attenuated by varying degrees at small scales due to the width of the line emission profiles. This attenuation may significantly impact estimates of astrophysical or cosmological quantities derived from measurements. We consider a theoretical treatment of the effect of line broadening on both the clustering… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.11171v2-abstract-full').style.display = 'inline'; document.getElementById('2104.11171v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.11171v2-abstract-full" style="display: none;"> Line-intensity mapping observations will find fluctuations of integrated line emission are attenuated by varying degrees at small scales due to the width of the line emission profiles. This attenuation may significantly impact estimates of astrophysical or cosmological quantities derived from measurements. We consider a theoretical treatment of the effect of line broadening on both the clustering and shot-noise components of the power spectrum of a generic line-intensity power spectrum using a halo model. We then consider possible simplifications to allow easier application in analysis, particularly in the context of inferences that require numerous, repeated, fast computations of model line-intensity signals across a large parameter space. For the CO Mapping Array Project (COMAP) and the CO(1-0) line-intensity field at $z\sim3$ serving as our primary case study, we expect a $\sim10\%$ attenuation of the spherically averaged power spectrum on average at relevant scales of $k\approx0.2$-$0.3$ Mpc$^{-1}$, compared to $\sim25\%$ for the interferometric Millimetre-wave Intensity Mapping Experiment (mmIME) targeting shot noise from CO lines at $z\sim1$-$5$ at scales of $k\gtrsim1$ Mpc$^{-1}$. We also consider the nature and amplitude of errors introduced by simplified treatments of line broadening, and find that while an approximation using a single effective velocity scale is sufficient for spherically-averaged power spectra, a more careful treatment is necessary when considering other statistics such as higher multipoles of the anisotropic power spectrum or the voxel intensity distribution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.11171v2-abstract-full').style.display = 'none'; document.getElementById('2104.11171v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">24 pages + appendix and bibliography (33 pages total), 16 figures, 2 tables; accepted for publication in ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ, 923, 188 (2021) </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg> <a href="https://info.arxiv.org/help/contact.html"> Contact</a> </li> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>subscribe to arXiv mailings</title><desc>Click here to subscribe</desc><path d="M476 3.2L12.5 270.6c-18.1 10.4-15.8 35.6 2.2 43.2L121 358.4l287.3-253.2c5.5-4.9 13.3 2.6 8.6 8.3L176 407v80.5c0 23.6 28.5 32.9 42.5 15.8L282 426l124.6 52.2c14.2 6 30.4-2.9 33-18.2l72-432C515 7.8 493.3-6.8 476 3.2z"/></svg> <a href="https://info.arxiv.org/help/subscribe"> Subscribe</a> </li> </ul> </div> </div> </div>   <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/license/index.html">Copyright</a></li> <li><a href="https://info.arxiv.org/help/policies/privacy_policy.html">Privacy Policy</a></li> </ul> </div> <div class="column sorry-app-links"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/web_accessibility.html">Web Accessibility Assistance</a></li> <li> <p class="help"> <a class="a11y-main-link" href="https://status.arxiv.org" target="_blank">arXiv Operational Status <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 256 512" class="icon filter-dark_grey" role="presentation"><path d="M224.3 273l-136 136c-9.4 9.4-24.6 9.4-33.9 0l-22.6-22.6c-9.4-9.4-9.4-24.6 0-33.9l96.4-96.4-96.4-96.4c-9.4-9.4-9.4-24.6 0-33.9L54.3 103c9.4-9.4 24.6-9.4 33.9 0l136 136c9.5 9.4 9.5 24.6.1 34z"/></svg></a><br> Get status notifications via <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/email/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg>email</a> or <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/slack/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 448 512" class="icon filter-black" role="presentation"><path d="M94.12 315.1c0 25.9-21.16 47.06-47.06 47.06S0 341 0 315.1c0-25.9 21.16-47.06 47.06-47.06h47.06v47.06zm23.72 0c0-25.9 21.16-47.06 47.06-47.06s47.06 21.16 47.06 47.06v117.84c0 25.9-21.16 47.06-47.06 47.06s-47.06-21.16-47.06-47.06V315.1zm47.06-188.98c-25.9 0-47.06-21.16-47.06-47.06S139 32 164.9 32s47.06 21.16 47.06 47.06v47.06H164.9zm0 23.72c25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06H47.06C21.16 243.96 0 222.8 0 196.9s21.16-47.06 47.06-47.06H164.9zm188.98 47.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06h-47.06V196.9zm-23.72 0c0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06V79.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06V196.9zM283.1 385.88c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06v-47.06h47.06zm0-23.72c-25.9 0-47.06-21.16-47.06-47.06 0-25.9 21.16-47.06 47.06-47.06h117.84c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06H283.1z"/></svg>slack</a> </p> </li> </ul> </div> </div> </div>  </div> </footer> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/member_acknowledgement.js"></script> </body> </html>

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