Astroparticle Physics最新文献

{"title":"Sibyll★","authors":"Felix Riehn ,&nbsp;Anatoli Fedynitch ,&nbsp;Ralph Engel","doi":"10.1016/j.astropartphys.2024.102964","DOIUrl":"https://doi.org/10.1016/j.astropartphys.2024.102964","url":null,"abstract":"<div><p>In the last decade, an increasing number of datasets have revealed a consistent discrepancy between the number of muons measured in ultra-high-energy extensive air showers (EAS) and the numbers predicted by simulations. This gap persists despite incorporating Large Hadron Collider (LHC) data into the tuning of current hadronic interaction models, leading to the phenomenon often termed the “muon puzzle”. To gain a deeper understanding of the potential origins of this muon puzzle, we have developed Sibyll<span><math><msup><mrow></mrow><mrow><mo>★</mo></mrow></msup></math></span>, a series of phenomenologically modified versions of Sibyll 2.3d. In these models, we have increased muon production by altering <span><math><msup><mrow><mi>ρ</mi></mrow><mrow><mn>0</mn></mrow></msup></math></span>, baryon–antibaryon pair, or kaon production in hadronic multiparticle production processes. These variants remain within bounds from provided by accelerator measurements, including those from the LHC and fixed-target experiments, notably NA49 and NA61, showing a level of consistency comparable to Sibyll 2.3d. Our findings show that these modifications can increase the muon count in EAS by up to 35%, while minimally affecting the depth of shower maximum (<span><math><msub><mrow><mi>X</mi></mrow><mrow><mi>max</mi></mrow></msub></math></span>) and other shower variables. Additionally, we assess the impact of these modifications on various observables, including inclusive muon and neutrino fluxes and the multiplicities of muon bundles in deep underground and water/ice Cherenkov detectors. We aim for at least one of these model variants to offer a more accurate representation of EAS data at the highest energies, thereby enhancing the quality of Monte Carlo predictions used in training neural networks. This improvement is crucial for achieving more reliable data analyses and interpretations.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"160 ","pages":"Article 102964"},"PeriodicalIF":3.5,"publicationDate":"2024-03-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140348008","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Observations of the Crab Nebula with MACE (Major Atmospheric Cherenkov Experiment)","authors":"Borwankar C. ,&nbsp;Sharma M. ,&nbsp;Hariharan J. ,&nbsp;Venugopal K. ,&nbsp;Godambe S. ,&nbsp;Mankuzhyil N. ,&nbsp;Chandra P. ,&nbsp;Khurana M. ,&nbsp;Pathania A. ,&nbsp;Chouhan N. ,&nbsp;Dhar V.K. ,&nbsp;Thubstan R. ,&nbsp;Norlha S. ,&nbsp;Keshavanand ,&nbsp;Sarkar D. ,&nbsp;Dar Z.A. ,&nbsp;Kotwal S.V. ,&nbsp;Godiyal S. ,&nbsp;Kushwaha C.P. ,&nbsp;Singh K.K. ,&nbsp;Yadav K.K.","doi":"10.1016/j.astropartphys.2024.102960","DOIUrl":"10.1016/j.astropartphys.2024.102960","url":null,"abstract":"<div><p>The Major Atmospheric Cherenkov Experiment (MACE) is a large size (21 m) Imaging Atmospheric Cherenkov Telescope (IACT) installed at an altitude of 4270 m above sea level at Hanle, Ladakh in northern India. Here we report the detection of Very High Energy (VHE) <span><math><mi>γ</mi></math></span>-ray emission from Crab Nebula above 80 GeV. We analyzed <span><math><mo>∼</mo></math></span> 15 h of data collected at low zenith angle between November 2022 and February 2023. The energy spectrum is well described by a log-parabola function with a flux of <span><math><mrow><mo>∼</mo><mrow><mo>(</mo><mn>3</mn><mo>.</mo><mn>46</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>2</mn><msub><mrow><mn>6</mn></mrow><mrow><mi>s</mi><mi>t</mi><mi>a</mi><mi>t</mi></mrow></msub><mo>)</mo></mrow><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>10</mn></mrow></msup></mrow></math></span> <span><math><mrow><msup><mrow><mi>TeV</mi></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup><msup><mrow><mi>cm</mi></mrow><mrow><mo>−</mo><mn>2</mn></mrow></msup><msup><mrow><mi>s</mi></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></mrow></math></span>, at 400 GeV with spectral index of <span><math><mrow><mn>2</mn><mo>.</mo><mn>09</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>0</mn><msub><mrow><mn>6</mn></mrow><mrow><mi>s</mi><mi>t</mi><mi>a</mi><mi>t</mi></mrow></msub></mrow></math></span> and a curvature parameter of <span><math><mrow><mn>0</mn><mo>.</mo><mn>08</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>0</mn><msub><mrow><mn>7</mn></mrow><mrow><mi>s</mi><mi>t</mi><mi>a</mi><mi>t</mi></mrow></msub></mrow></math></span>. The <span><math><mi>γ</mi></math></span>-rays are detected in an energy range spanning from 80<!--> <!-->GeV to <span><math><mo>∼</mo></math></span>5<!--> <!-->TeV. The energy resolution improves from <span><math><mo>∼</mo></math></span> 34% at an analysis energy threshold of 80<!--> <!-->GeV to <span><math><mo>∼</mo></math></span> 21% above 1<!--> <!-->TeV. The daily light curve and the spectral energy distribution obtained for the Crab Nebula is in agreement with previous measurements, considering statistical and systematic uncertainties.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"159 ","pages":"Article 102960"},"PeriodicalIF":3.5,"publicationDate":"2024-03-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140282874","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Curvature Quantization based on the Ehrenfest Paradox in the Bohr Atomic Model","authors":"Fima Ardianto Putra ,&nbsp;Ahmad Khalil Yaqubi ,&nbsp;Riza Ibnu Adam ,&nbsp;Vandan Wiliyanti ,&nbsp;Puzi Anigrahawati","doi":"10.1016/j.astropartphys.2024.102950","DOIUrl":"10.1016/j.astropartphys.2024.102950","url":null,"abstract":"<div><p>Ehrenfest Paradox has been studied in the Bohr Atomic Model as a theoretical procedure for expressing the atomic coordinate curvature in the term of electromagnetic fine structure/coupling constant α = 1/137. The strength of the curvature corresponding to the gravitational aspect depends on the principal quantum number via a new constant <span><math><mrow><mfrac><mrow><mn>16</mn><msup><mrow><mi>α</mi></mrow><mn>2</mn></msup></mrow><msubsup><mi>a</mi><mn>0</mn><mn>2</mn></msubsup></mfrac><mo>=</mo><mn>3</mn><mo>,</mo><mn>0348</mn><mspace></mspace><mo>×</mo><msup><mrow><mn>10</mn></mrow><mn>17</mn></msup><msup><mrow><mi>m</mi></mrow><mrow><mo>−</mo><mn>2</mn></mrow></msup></mrow></math></span>, which shows that the value of the curvature is quantised. For instance <em>n</em> = 1, the value is 3, 0349  × 10¹⁷ <em>m</em>⁻². The curvature value in the Bohr atomic model can be used as a standard to compare how strong the curvatures of all systems are. This procedure can also be generalized to the strong and weak interactions in such a way that the value of the curvature can be represented by their own coupling constants. In the real situation, we can take the case of the atom near supermassive objects such as: blackhole, neutron star, white dwarf, etc. In this case, the atom is in the curved space-time, while the space-time curvature is quantized by the atom. Principally, the idea of the curvature and quantization are correlated. The excitation (the change of the state) of the atom or the atomic nuclei will generate the change of the space-time curvature Δ<em>G</em>_μν(α)_<em>n</em> that manifests a quantized curvature propagation (curvaton) through the space-time coordinate in the form of quantum stress tensor <span><math><mrow><mstyle><mi>Δ</mi></mstyle><msubsup><mi>T</mi><mrow><mi>μ</mi><mi>ν</mi></mrow><mrow><mo>(</mo><mrow><mi>q</mi><mn>2</mn><mi>B</mi></mrow><mo>)</mo></mrow></msubsup><mo>=</mo><mi>ℏ</mi><mstyle><mi>Δ</mi></mstyle><msub><mi>σ</mi><mi>n</mi></msub><mstyle><mi>Δ</mi></mstyle><msub><mi>G</mi><mrow><mi>μ</mi><mi>ν</mi></mrow></msub><msub><mrow><mo>(</mo><mi>α</mi><mo>)</mo></mrow><mi>n</mi></msub></mrow></math></span>. It can be viewed as a unit of moving curvature reduced to a gravitational wave. This theory can be considered to expand the unification between quantum mechanics and gravitation.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"159 ","pages":"Article 102950"},"PeriodicalIF":3.5,"publicationDate":"2024-03-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140149663","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The exact solution approach to warm inflation","authors":"Oem Trivedi","doi":"10.1016/j.astropartphys.2024.102951","DOIUrl":"https://doi.org/10.1016/j.astropartphys.2024.102951","url":null,"abstract":"<div><p>The theory of cosmic inflation has received a great amount of deserved attention in recent years due to it’s stunning predictions about the early universe. Alongside the usual cold inflation paradigm, warm inflation has garnered a huge amount of interest in modern inflationary studies. It’s peculiar features and specifically different predictions from cold inflation have led to a substantial amount of literature about it. Various modified cosmological scenarios have also been studied in the warm inflationary regime. In this work, we introduce the exact solution approach for warm inflation. This approach allows one to directly study warm inflationary regime in a variety of modified cosmological scenarios. We begin by outlining our method and show that it generalizes the modified Friedmann approach of Del Campo, and reduces to the well known Hamilton–Jacobi formalism for inflation in particular limits. We also find the perturbation spectra for cosmological and tensor perturbations in the early universe, and then apply our method to study warm inflation in a Tsallis entropy modified Friedmann universe. We end our paper with some concluding remarks on the domain of applicability of our work.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"158 ","pages":"Article 102951"},"PeriodicalIF":3.5,"publicationDate":"2024-02-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140024007","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Analyses of continuous measurements of cosmic ray induced-neutrons spectra at the Concordia Antarctic Station from 2016 to 2024","authors":"G. Hubert","doi":"10.1016/j.astropartphys.2024.102949","DOIUrl":"10.1016/j.astropartphys.2024.102949","url":null,"abstract":"<div><p>This paper presents analyses of cosmic-ray-induced neutron measurements spanning from 2016 to 2023 at the Concordia Antarctic high-altitude station. Environmental and systematic effects are meticulously considered in both long-term and short-term perspectives. The study delves into space weather cases, focusing on solar events in September 2017 and October 2021, along with a specific examination of the impact of the Atmospheric River in March 2022. The paper explores the valuable contribution of modeling to data analyses, particularly its capacity to infer solar modulation from neutron spectra. All analyses integrate modulations of the neutron spectrum, with a specific emphasis on short-term events, representing the principal contribution of the spectral measurements.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"159 ","pages":"Article 102949"},"PeriodicalIF":3.5,"publicationDate":"2024-02-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140008178","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The performance of generalised Davies–Cotton optical systems with infinitesimal mirror facets","authors":"S. Fegan","doi":"10.1016/j.astropartphys.2024.102948","DOIUrl":"10.1016/j.astropartphys.2024.102948","url":null,"abstract":"<div><p>This paper presents Taylor expansions for the imaging and timing characteristics of spherical optical systems with infinitesimal mirror facets, sometimes referred to as “modified Davies–Cotton” telescopes. Such a system comprises a discontinuous spherical mirror surface whose curvature radius is different from its focal length, and whose mirrors are aligned to suppress spherical aberration. Configurations that range between two “optima” are, one of which minimises tangential comatic aberration and the other that minimises timing dispersion.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"158 ","pages":"Article 102948"},"PeriodicalIF":3.5,"publicationDate":"2024-02-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S0927650524000252/pdfft?md5=c1fa59dd4cd5a9fd0e314cec6e91052e&pid=1-s2.0-S0927650524000252-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139924579","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The cosmic ray energetics and mass for the international space station (ISS-CREAM) instrument","authors":"Y.S. Yoon ,&nbsp;Y. Amare ,&nbsp;D. Angelaszek ,&nbsp;N. Anthony ,&nbsp;K. Cheryian ,&nbsp;G.H. Choi ,&nbsp;M. Copley ,&nbsp;S. Coutu ,&nbsp;L. Derome ,&nbsp;L. Eraud ,&nbsp;L. Hagenau ,&nbsp;J.H. Han ,&nbsp;H.G. Huh ,&nbsp;Y.S. Hwang ,&nbsp;H.J. Hyun ,&nbsp;S. Im ,&nbsp;H.B. Jeon ,&nbsp;J.A. Jeon ,&nbsp;S. Jeong ,&nbsp;S.C. Kang ,&nbsp;H.G. Zhang","doi":"10.1016/j.astropartphys.2024.102947","DOIUrl":"10.1016/j.astropartphys.2024.102947","url":null,"abstract":"<div><p>The ISS-CREAM instrument is the modified version of the Cosmic Ray Energetics And Mass (CREAM) experiment, which was flown on balloons multiple times over Antarctica and later installed on the International Space Station (ISS). Its primary objective is to measure the energy spectra of individual cosmic-ray elements for the charge range of <em>Z</em> = 1 to <em>Z</em> = 26, in the energy range of ∼ 10¹² to ∼ 10¹⁵ eV. The instrument comprises a tungsten/scintillator calorimeter and a pixelated silicon charge detector as primary detectors to determine the energy and charge of cosmic rays. Additionally, it includes top and bottom scintillator counting detectors and a boronated scintillator detector to differentiate between electrons and hadrons for multi-TeV electron measurements. The ISS-CREAM instrument was installed on the ISS in August 2017 and operated until February 2019. This paper provides an overview of the instrument, focusing on its detectors, trigger systems, common electronics, and power systems. The paper highlights the modifications made to these components to optimize their performance for ISS operations.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"158 ","pages":"Article 102947"},"PeriodicalIF":3.5,"publicationDate":"2024-02-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139874753","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Machine learning-based discrimination of bulk and surface events of germanium detectors for light dark matter detection","authors":"P. Zhang ,&nbsp;H. Ma ,&nbsp;L. Yang ,&nbsp;Z. Zeng ,&nbsp;Q. Yue ,&nbsp;J. Cheng","doi":"10.1016/j.astropartphys.2024.102946","DOIUrl":"10.1016/j.astropartphys.2024.102946","url":null,"abstract":"<div><p>Surface events that exhibit incomplete charge collection are an essential background source in the light dark matter detection experiments with p-type point-contact germanium detectors. We propose a machine learning-based algorithm to identify bulk and surface events according to their pulse shape features. We construct the training and test set with part of the <span><math><mi>γ</mi></math></span>-source calibration data and use the rising edge of the waveform as the model input. This method is verified with the test set and another part of the <span><math><mi>γ</mi></math></span>-source calibration data. Results show that this method performs well on both datasets, and presents robustness against the bulk events’ proportion and the dataset size. Compared with the previous approach, the uncertainty is reduced by 16% near the energy threshold on the physics data of CDEX-1B. In addition, the key pattern identified in the waveform is verified to be consistent with its physical nature by digging into this algorithm.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"158 ","pages":"Article 102946"},"PeriodicalIF":3.5,"publicationDate":"2024-02-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139832980","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Systematic effects on a Compton polarimeter at the focus of an X-ray mirror","authors":"M. Aoyagi ,&nbsp;R.G. Bose ,&nbsp;S. Chun ,&nbsp;E. Gau ,&nbsp;K. Hu ,&nbsp;K. Ishiwata ,&nbsp;N.K. Iyer ,&nbsp;F. Kislat ,&nbsp;M. Kiss ,&nbsp;K. Klepper ,&nbsp;H. Krawczynski ,&nbsp;L. Lisalda ,&nbsp;Y. Maeda ,&nbsp;F. af Malmborg ,&nbsp;H. Matsumoto ,&nbsp;A. Miyamoto ,&nbsp;T. Miyazawa ,&nbsp;M. Pearce ,&nbsp;B.F. Rauch ,&nbsp;N. Rodriguez Cavero ,&nbsp;M. Yoshimoto","doi":"10.1016/j.astropartphys.2024.102944","DOIUrl":"10.1016/j.astropartphys.2024.102944","url":null,"abstract":"<div><p>XL-Calibur is a balloon-borne Compton polarimeter for X-rays in the <span><math><mo>∼</mo></math></span>15–80 keV range. Using an X-ray mirror with a 12 m focal length for collecting photons onto a beryllium scattering rod surrounded by CZT detectors, a minimum-detectable polarization as low as <span><math><mo>∼</mo></math></span>3% is expected during a 24-hour on-target observation of a 1 Crab source at 45° elevation.</p><p>Systematic effects alter the reconstructed polarization as the mirror focal spot moves across the beryllium scatterer, due to pointing offsets, mechanical misalignment or deformation of the carbon-fiber truss supporting the mirror and the polarimeter. Unaddressed, this can give rise to a spurious polarization signal for an unpolarized flux, or a change in reconstructed polarization fraction and angle for a polarized flux. Using bench-marked Monte-Carlo simulations and an accurate mirror point-spread function characterized at synchrotron beam-lines, systematic effects are quantified, and mitigation strategies discussed. By recalculating the scattering site for a shifted beam, systematic errors can be reduced from several tens of percent to the few-percent level for any shift within the scattering element. The treatment of these systematic effects will be important for any polarimetric instrument where a focused X-ray beam is impinging on a scattering element surrounded by counting detectors.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"158 ","pages":"Article 102944"},"PeriodicalIF":3.5,"publicationDate":"2024-02-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S0927650524000215/pdfft?md5=ffe1e03456d8bdcd4b3e6321fe3442d4&pid=1-s2.0-S0927650524000215-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139892564","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Alpha backgrounds in NaI(Tl) crystals of COSINE-100","authors":"G. Adhikari ,&nbsp;N. Carlin ,&nbsp;D.F.F.S. Cavalcante ,&nbsp;J.Y. Cho ,&nbsp;J.J. Choi ,&nbsp;S. Choi ,&nbsp;A.C. Ezeribe ,&nbsp;L.E. França ,&nbsp;C. Ha ,&nbsp;I.S. Hahn ,&nbsp;S.J. Hollick ,&nbsp;E.J. Jeon ,&nbsp;H.W. Joo ,&nbsp;W.G. Kang ,&nbsp;M. Kauer ,&nbsp;B.H. Kim ,&nbsp;H.J. Kim ,&nbsp;J. Kim ,&nbsp;K.W. Kim ,&nbsp;S.H. Kim ,&nbsp;G.H. Yu","doi":"10.1016/j.astropartphys.2024.102945","DOIUrl":"https://doi.org/10.1016/j.astropartphys.2024.102945","url":null,"abstract":"<div><p>COSINE-100 is a dark matter direct detection experiment with 106<!--> <!-->kg NaI(Tl) as the target material. ²¹⁰Pb and daughter isotopes are a dominant background in the WIMP region of interest and are detected via <span><math><mi>β</mi></math></span> decay and <span><math><mi>α</mi></math></span> decay. Analysis of the <span><math><mi>α</mi></math></span> channel complements the background model as observed in the <span><math><mi>β</mi></math></span>/<span><math><mi>γ</mi></math></span> channel. We present the measurement of the quenching factors and Monte Carlo simulation results and activity quantification of the <span><math><mi>α</mi></math></span> decay components of the COSINE-100 NaI(Tl) crystals. The data strongly indicate that the <span><math><mi>α</mi></math></span> decays probabilistically undergo two possible quenching factors but require further investigation. The fitted results are consistent with independent measurements and improve the overall understanding of the COSINE-100 backgrounds. Furthermore, the half-life of ²¹⁶Po has been measured to be <span><math><mrow><mn>143</mn><mo>.</mo><mn>4</mn><mspace></mspace><mo>±</mo><mspace></mspace><mn>1</mn><mo>.</mo><mn>2</mn></mrow></math></span> <!--> <!-->ms, which is consistent with and more precise than most current measurements.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"158 ","pages":"Article 102945"},"PeriodicalIF":3.5,"publicationDate":"2024-02-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139726414","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}