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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.19874">arXiv:2412.19874</a> <span> [<a href="https://arxiv.org/pdf/2412.19874">pdf</a>, <a href="https://arxiv.org/format/2412.19874">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 Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epja/s10050-025-01490-z">10.1140/epja/s10050-025-01490-z <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Felsenkeller shallow-underground laboratory for nuclear astrophysics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bemmerer%2C+D">Daniel Bemmerer</a>, <a href="/search/physics?searchtype=author&query=Boeltzig%2C+A">Axel Boeltzig</a>, <a href="/search/physics?searchtype=author&query=Grieger%2C+M">Marcel Grieger</a>, <a href="/search/physics?searchtype=author&query=Gudat%2C+K">Katharina Gudat</a>, <a href="/search/physics?searchtype=author&query=Hensel%2C+T">Thomas Hensel</a>, <a href="/search/physics?searchtype=author&query=Masha%2C+E">Eliana Masha</a>, <a href="/search/physics?searchtype=author&query=Osswald%2C+M">Max Osswald</a>, <a href="/search/physics?searchtype=author&query=Poser%2C+B">Bruno Poser</a>, <a href="/search/physics?searchtype=author&query=R%C3%BCmmler%2C+S">Simon R眉mmler</a>, <a href="/search/physics?searchtype=author&query=Schmidt%2C+K">Konrad Schmidt</a>, <a href="/search/physics?searchtype=author&query=Ta%C3%ADn%2C+J+L">Jos茅 Luis Ta铆n</a>, <a href="/search/physics?searchtype=author&query=Tarife%C3%B1o-Saldivia%2C+A">Ariel Tarife帽o-Saldivia</a>, <a href="/search/physics?searchtype=author&query=Turkat%2C+S">Steffen Turkat</a>, <a href="/search/physics?searchtype=author&query=Yadav%2C+A">Anup Yadav</a>, <a href="/search/physics?searchtype=author&query=Zuber%2C+K">Kai Zuber</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="2412.19874v1-abstract-short" style="display: inline;"> In the Felsenkeller shallow-underground site, protected from cosmic muons by a 45 m thick rock overburden, a research laboratory including a 5 MV Pelletron ion accelerator and a number of radioactivity-measurement setups is located. The laboratory and its installations are described in detail. The background radiation has been studied, finding suppression factors of 40 for cosmic-ray muons, 200 fo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.19874v1-abstract-full').style.display = 'inline'; document.getElementById('2412.19874v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.19874v1-abstract-full" style="display: none;"> In the Felsenkeller shallow-underground site, protected from cosmic muons by a 45 m thick rock overburden, a research laboratory including a 5 MV Pelletron ion accelerator and a number of radioactivity-measurement setups is located. The laboratory and its installations are described in detail. The background radiation has been studied, finding suppression factors of 40 for cosmic-ray muons, 200 for ambient neutrons, and 100 for the background in germanium $纬$-ray detectors. Using an additional active muon veto, typically the background is just twice as high as in very deep underground laboratories. The properties of the accelerator including its external and internal ion sources and beam line are given. For the radioactivity counting setup, detection limits in the 10$^{-4}$ Bq range have been obtained. Practical aspects for the usage of the laboratory by outside scientific users are discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.19874v1-abstract-full').style.display = 'none'; document.getElementById('2412.19874v1-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to Eur. Phys. J. A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. A 61, 19 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.05053">arXiv:2411.05053</a> <span> [<a href="https://arxiv.org/pdf/2411.05053">pdf</a>, <a href="https://arxiv.org/format/2411.05053">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 Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.nima.2021.165081">10.1016/j.nima.2021.165081 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characterization of the LUNA neutron detector array for the measurement of the 13C(a,n)16O reaction </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Csedreki%2C+L">L. Csedreki</a>, <a href="/search/physics?searchtype=author&query=Ciani%2C+G+F">G. F. Ciani</a>, <a href="/search/physics?searchtype=author&query=Balibrea-Correa%2C+J">J. Balibrea-Correa</a>, <a href="/search/physics?searchtype=author&query=Best%2C+A">A. Best</a>, <a href="/search/physics?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/physics?searchtype=author&query=Barile%2C+F">F. Barile</a>, <a href="/search/physics?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/physics?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/physics?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+C+G">C. G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/physics?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/physics?searchtype=author&query=Chillery%2C+T">T. Chillery</a>, <a href="/search/physics?searchtype=author&query=Colombetti%2C+P">P. Colombetti</a>, <a href="/search/physics?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/physics?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/physics?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/physics?searchtype=author&query=Di+Leva%2C+A">A. Di Leva</a>, <a href="/search/physics?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/physics?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/physics?searchtype=author&query=Fiore%2C+E+M">E. M. Fiore</a>, <a href="/search/physics?searchtype=author&query=Formicola%2C+A">A. Formicola</a>, <a href="/search/physics?searchtype=author&query=Fulop%2C+Z">Zs. Fulop</a>, <a href="/search/physics?searchtype=author&query=Gervino%2C+G">G. Gervino</a>, <a href="/search/physics?searchtype=author&query=Guglielmetti%2C+A">A. Guglielmetti</a> , et al. (24 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="2411.05053v1-abstract-short" style="display: inline;"> We introduce the LUNA neutron detector array developed for the investigation of the 13C(a,n)16O reaction towards its astrophysical s-process Gamow peak in the low-background environment of the Laboratori Nazionali del Gran Sasso (LNGS). Eighteen 3He counters are arranged in two different configurations (in a vertical and a horizontal orientation) to optimize neutron detection effciency, target han… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.05053v1-abstract-full').style.display = 'inline'; document.getElementById('2411.05053v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.05053v1-abstract-full" style="display: none;"> We introduce the LUNA neutron detector array developed for the investigation of the 13C(a,n)16O reaction towards its astrophysical s-process Gamow peak in the low-background environment of the Laboratori Nazionali del Gran Sasso (LNGS). Eighteen 3He counters are arranged in two different configurations (in a vertical and a horizontal orientation) to optimize neutron detection effciency, target handling and target cooling over the investigated energy range Ea;lab = 300 - 400 keV (En = 2.2 - 2.6 MeV in emitted neutron energy). As a result of the deep underground location, the passive shielding of the setup and active background suppression using pulse shape discrimination, we reached a total background rate of 1.23 +- 0.12 counts/hour. This resulted in an improvement of two orders of magnitude over the state of the art allowing a direct measurement of the 13C(a,n)16O cross-section down to Ea;lab = 300 keV. The absolute neutron detection efficiency of the setup was determined using the 51V(p,n)51Cr reaction and an AmBe radioactive source, and completed with a Geant4 simulation. We determined a (34+-3) % and (38+-3) % detection efficiency for the vertical and horizontal configurations, respectively, for En = 2.4 MeV neutrons. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.05053v1-abstract-full').style.display = 'none'; document.getElementById('2411.05053v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 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">8 pages, 5 figures, to be published in NIMA</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nuclear Inst. and Methods in Physics Research, A 994 (2021) 165081 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.03905">arXiv:2301.03905</a> <span> [<a href="https://arxiv.org/pdf/2301.03905">pdf</a>, <a href="https://arxiv.org/format/2301.03905">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 Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.astropartphys.2023.102816">10.1016/j.astropartphys.2023.102816 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A new ultra low-level HPGe activity counting setup in the Felsenkeller shallow-underground laboratory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Turkat%2C+S">S. Turkat</a>, <a href="/search/physics?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/physics?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/physics?searchtype=author&query=Domula%2C+A+R">A. R. Domula</a>, <a href="/search/physics?searchtype=author&query=Koch%2C+J">J. Koch</a>, <a href="/search/physics?searchtype=author&query=Lossin%2C+T">T. Lossin</a>, <a href="/search/physics?searchtype=author&query=Osswald%2C+M">M. Osswald</a>, <a href="/search/physics?searchtype=author&query=Schmidt%2C+K">K. Schmidt</a>, <a href="/search/physics?searchtype=author&query=Zuber%2C+K">K. Zuber</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="2301.03905v2-abstract-short" style="display: inline;"> A new ultra low-level counting setup has been installed in the shallow-underground laboratory Felsenkeller in Dresden, Germany. It includes a high-purity germanium detector (HPGe) of 163\% relative efficiency within passive and active shields. The passive shield consists of 45m rock overburden (140 meters water equivalent), 40 cm of low-activity concrete, and a lead and copper castle enclosed by a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.03905v2-abstract-full').style.display = 'inline'; document.getElementById('2301.03905v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.03905v2-abstract-full" style="display: none;"> A new ultra low-level counting setup has been installed in the shallow-underground laboratory Felsenkeller in Dresden, Germany. It includes a high-purity germanium detector (HPGe) of 163\% relative efficiency within passive and active shields. The passive shield consists of 45m rock overburden (140 meters water equivalent), 40 cm of low-activity concrete, and a lead and copper castle enclosed by an anti-radon box. The passive shielding alone is found to reduce the background rate to rates comparable to other shallow-underground laboratories. An additional active veto is given by five large plastic scintillation panels surrounding the setup. It further reduces the background rate by more than one order of magnitude down to 116$\pm$1 kg$^{-1}$ d$^{-1}$ in an energy interval of 40-2700 keV. This low background rate is unprecedented for shallow-underground laboratories and close to deep underground laboratories. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.03905v2-abstract-full').style.display = 'none'; document.getElementById('2301.03905v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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 Astroparticle Physics; corrected typo in abstract</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astropart. Phys. 148 (2023) 102816 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.00002">arXiv:2005.00002</a> <span> [<a href="https://arxiv.org/pdf/2005.00002">pdf</a>, <a href="https://arxiv.org/format/2005.00002">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 Detectors">physics.ins-det</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="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epja/s10050-020-00149-1">10.1140/epja/s10050-020-00149-1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Setup commissioning for an improved measurement of the D(p,gamma)3He cross section at Big Bang Nucleosynthesis energies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Mossa%2C+V">V. Mossa</a>, <a href="/search/physics?searchtype=author&query=St%C3%B6ckel%2C+K">K. St枚ckel</a>, <a href="/search/physics?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/physics?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/physics?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/physics?searchtype=author&query=Barile%2C+F">F. Barile</a>, <a href="/search/physics?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/physics?searchtype=author&query=Best%2C+A">A. Best</a>, <a href="/search/physics?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/physics?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+C+G">C. G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/physics?searchtype=author&query=Csedreki%2C+L">L. Csedreki</a>, <a href="/search/physics?searchtype=author&query=Chillery%2C+T">T. Chillery</a>, <a href="/search/physics?searchtype=author&query=Ciani%2C+G+F">G. F. Ciani</a>, <a href="/search/physics?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/physics?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/physics?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/physics?searchtype=author&query=Di+Leva%2C+A">A. Di Leva</a>, <a href="/search/physics?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/physics?searchtype=author&query=Fiore%2C+E+M">E. M. Fiore</a>, <a href="/search/physics?searchtype=author&query=Formicola%2C+A">A. Formicola</a>, <a href="/search/physics?searchtype=author&query=F%C3%BCl%C3%B6p%2C+Z">Zs. F眉l枚p</a>, <a href="/search/physics?searchtype=author&query=Gervino%2C+G">G. Gervino</a>, <a href="/search/physics?searchtype=author&query=Guglielmetti%2C+A">A. Guglielmetti</a> , et al. (22 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2005.00002v1-abstract-short" style="display: inline;"> Among the reactions involved in the production and destruction of deuterium during Big Bang Nucleosynthesis, the deuterium-burning D(p,gamma)3He reaction has the largest uncertainty and limits the precision of theoretical estimates of primordial deuterium abundance. Here we report the results of a careful commissioning of the experimental setup used to measure the cross-section of the D(p,gamma)3H… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.00002v1-abstract-full').style.display = 'inline'; document.getElementById('2005.00002v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.00002v1-abstract-full" style="display: none;"> Among the reactions involved in the production and destruction of deuterium during Big Bang Nucleosynthesis, the deuterium-burning D(p,gamma)3He reaction has the largest uncertainty and limits the precision of theoretical estimates of primordial deuterium abundance. Here we report the results of a careful commissioning of the experimental setup used to measure the cross-section of the D(p,gamma)3He reaction at the Laboratory for Underground Nuclear Astrophysics of the Gran Sasso Laboratory (Italy). The commissioning was aimed at minimising all sources of systematic uncertainty in the measured cross sections. The overall systematic error achieved (< 3 %) will enable improved predictions of BBN deuterium abundance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.00002v1-abstract-full').style.display = 'none'; document.getElementById('2005.00002v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 11 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.08744">arXiv:2001.08744</a> <span> [<a href="https://arxiv.org/pdf/2001.08744">pdf</a>, <a href="https://arxiv.org/ps/2001.08744">ps</a>, <a href="https://arxiv.org/format/2001.08744">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 Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epja/s10050-020-00077-0">10.1140/epja/s10050-020-00077-0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A new approach to monitor 13C-targets degradation in situ for 13C(alpha,n)16O cross-section measurements at LUNA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Ciani%2C+G+F">G. F. Ciani</a>, <a href="/search/physics?searchtype=author&query=Csedreki%2C+L">L. Csedreki</a>, <a href="/search/physics?searchtype=author&query=Balibrea-Correa%2C+J">J. Balibrea-Correa</a>, <a href="/search/physics?searchtype=author&query=Best%2C+A">A. Best</a>, <a href="/search/physics?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/physics?searchtype=author&query=Barile%2C+F">F. Barile</a>, <a href="/search/physics?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/physics?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/physics?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+C+G">C. G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/physics?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/physics?searchtype=author&query=Chillery%2C+T">T. Chillery</a>, <a href="/search/physics?searchtype=author&query=Colombetti%2C+P">P. Colombetti</a>, <a href="/search/physics?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/physics?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/physics?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/physics?searchtype=author&query=Di+Leva%2C+A">A. Di Leva</a>, <a href="/search/physics?searchtype=author&query=Di+Paolo%2C+L">L. Di Paolo</a>, <a href="/search/physics?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/physics?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/physics?searchtype=author&query=Fiore%2C+E+M">E. M. Fiore</a>, <a href="/search/physics?searchtype=author&query=Formicola%2C+A">A. Formicola</a>, <a href="/search/physics?searchtype=author&query=Fulop%2C+Z">Zs. Fulop</a>, <a href="/search/physics?searchtype=author&query=Gervino%2C+G">G. Gervino</a> , et al. (24 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="2001.08744v2-abstract-short" style="display: inline;"> Direct measurements of reaction cross-sections at astrophysical energies often require the use of solid targets able to withstand high ion beam currents for extended periods of time. Thus, monitoring target thickness, isotopic composition, and target stoichiometry during data taking is critical to account for possible target modifications and to reduce uncertainties in the final cross-section resu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.08744v2-abstract-full').style.display = 'inline'; document.getElementById('2001.08744v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.08744v2-abstract-full" style="display: none;"> Direct measurements of reaction cross-sections at astrophysical energies often require the use of solid targets able to withstand high ion beam currents for extended periods of time. Thus, monitoring target thickness, isotopic composition, and target stoichiometry during data taking is critical to account for possible target modifications and to reduce uncertainties in the final cross-section results. A common technique used for these purposes is the Nuclear Resonant Reaction Analysis (NRRA), which however requires that a narrow resonance be available inside the dynamic range of the accelerator used. In cases when this is not possible, as for example the 13C(alpha,n)16O reaction recently studied at low energies at the Laboratory for Underground Nuclear Astrophysics (LUNA) in Italy, alternative approaches must be found. Here, we present a new application of the shape analysis of primary gamma rays emitted by the 13C(p,g)14N radiative capture reaction. This approach was used to monitor 13C target degradation {\em in situ} during the 13C(alpha,n)16O data taking campaign. The results obtained are in agreement with evaluations subsequently performed at Atomki (Hungary) using the NRRA method. A preliminary application for the extraction of the 13C(alpha,n)16O reaction cross-section at one beam energy is also reported. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.08744v2-abstract-full').style.display = 'none'; document.getElementById('2001.08744v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 6 figures, to be published in EPJ A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The European Physical Journal A volume 56, Article number: 75 (2020) </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 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