Astroparticle Physics最新文献

{"title":"High redshift constraints on extended logotropic models","authors":"Hachemi B. Benaoum ,&nbsp;Pierre-Henri Chavanis ,&nbsp;Orlando Luongo ,&nbsp;Marco Muccino ,&nbsp;Hernando Quevedo","doi":"10.1016/j.astropartphys.2023.102852","DOIUrl":"10.1016/j.astropartphys.2023.102852","url":null,"abstract":"<div><p><span>A single logotropic fluid, responsible for the existence of the whole dark sector, is here extensively revised at intermediate redshifts. In particular, by investigating possible generalizations that conceptually overcome previous issues of standard logotropic scenarios, we fix bound over classes of logotropic models that exhibit additional terms in the equation of state. Employing </span><span><math><msub><mrow><mi>σ</mi></mrow><mrow><mn>8</mn></mrow></msub></math></span><span> measurements combined with low redshift data sets of Supernovae<span><span> and Hubble observational data, we show the statistical significance of those extensions and their departure from the standard cosmological model. Evidences against generalized versions of logotropic models are, in particular, prompted. Our outcomes definitively show that any departure from the original logotropic model, including the Anton–Schmidt </span>dark energy, are clearly disfavored at the level of perturbations and/or background cosmology. This indicates that, in order to have a logotropic fluid, plausible generalized versions of it would point out to reduce the complexity of the fluid itself, instead of adding extra terms.</span></span></p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"151 ","pages":"Article 102852"},"PeriodicalIF":3.5,"publicationDate":"2023-09-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"45738930","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":"Phenomenological implications of sterile neutrinos in the μνSSM and dark matter","authors":"Paulina Knees ,&nbsp;Daniel E. López-Fogliani ,&nbsp;Carlos Muñoz","doi":"10.1016/j.astropartphys.2023.102865","DOIUrl":"https://doi.org/10.1016/j.astropartphys.2023.102865","url":null,"abstract":"<div><p>We analyze the role of sterile neutrinos in the framework of the <span><math><mrow><mi>μ</mi><mi>ν</mi></mrow></math></span>SSM, where the presence of right-handed neutrinos provides a simultaneous solution to <span><math><mi>μ</mi></math></span>- and <span><math><mi>ν</mi></math></span><span>-problems in supersymmetry<span>. We adopt a minimalistic approach, reproducing light neutrino masses and mixing angles at tree-level using just two right-handed neutrinos as part of the seesaw mechanism. A third right-handed neutrino does not contribute significantly to the mass of the three active ones, behaving as a sterile neutrino with a mass in the range keV-MeV. Furthermore, a sterile neutrino of about 10 keV can be a good candidate for dark matter with a lifetime larger than the age of the Universe. In particular, the three-body decay to active neutrinos gives the dominant contribution to its lifetime. The one-loop decay to gamma and active neutrino is subdominant, but relevant for observations such as astrophysical X-rays. We find regions of the parameter space of the </span></span><span><math><mrow><mi>μ</mi><mi>ν</mi></mrow></math></span>SSM, with different values of the sterile neutrino mass, fulfilling not only these constraints but also collider constraints from the Higgs sector.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"151 ","pages":"Article 102865"},"PeriodicalIF":3.5,"publicationDate":"2023-09-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"49733360","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 energy spectrum of cosmic rays measured by the Telescope Array using 10 years of fluorescence detector data","authors":"R.U. Abbasi ,&nbsp;Y. Abe ,&nbsp;T. Abu-Zayyad ,&nbsp;M. Allen ,&nbsp;Y. Arai ,&nbsp;R. Arimura ,&nbsp;E. Barcikowski ,&nbsp;J.W. Belz ,&nbsp;D.R. Bergman ,&nbsp;S.A. Blake ,&nbsp;I. Buckland ,&nbsp;B.G. Cheon ,&nbsp;M. Chikawa ,&nbsp;A. Fedynitch ,&nbsp;T. Fujii ,&nbsp;K. Fujisue ,&nbsp;K. Fujita ,&nbsp;R. Fujiwara ,&nbsp;M. Fukushima ,&nbsp;G. Furlich ,&nbsp;Z. Zundel","doi":"10.1016/j.astropartphys.2023.102864","DOIUrl":"10.1016/j.astropartphys.2023.102864","url":null,"abstract":"<div><p><span>The Telescope Array (TA) Cosmic Ray Observatory is the largest cosmic ray detector in the northern hemisphere. TA was built to study ultra-high-energy cosmic rays (UHECRs), cosmic rays with energies above </span><span><math><mrow><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>18</mn></mrow></msup><mspace></mspace><mi>eV</mi></mrow></math></span><span>. TA is a hybrid detector, employing two distinct detection methods: a surface detector array and a set of fluorescence telescopes. We will present a measurement of the cosmic ray energy spectrum for energies above </span><span><math><mrow><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>17</mn><mo>.</mo><mn>5</mn></mrow></msup><mspace></mspace><mi>eV</mi></mrow></math></span> using only the fluorescence telescopes. A novel weather classification scheme using machine learning was used to select data parts with good weather to ensure the quality of the fluorescence data. The data from the Black Rock Mesa (BRM) and Long Ridge (LR) fluorescence telescope sites were analyzed separately in monocular mode, with the calculated fluxes combined into a single spectrum. The 10-year monocular combined cosmic ray energy spectrum is observed to be in excellent agreement with previous measurements from the northern hemisphere. We present fits of the combined spectrum to a series of broken power law models. The thrice-broken power law was observed to be the best fit considering the Poisson deviance per degrees of freedom. The three breaks suggest an additional feature of the spectrum between the previously observed Ankle feature at <span><math><mrow><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>18</mn><mo>.</mo><mn>7</mn></mrow></msup><mspace></mspace><mi>eV</mi></mrow></math></span> and the GZK suppression at <span><math><mrow><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>19</mn><mo>.</mo><mn>8</mn></mrow></msup><mspace></mspace><mi>eV</mi></mrow></math></span>.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"151 ","pages":"Article 102864"},"PeriodicalIF":3.5,"publicationDate":"2023-09-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"44000411","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":"Bracketing the direct detection exclusion plot for a WIMP of spin one half in non-relativistic effective theory","authors":"Sunghyun Kang,&nbsp;Injun Jeong,&nbsp;Stefano Scopel","doi":"10.1016/j.astropartphys.2023.102854","DOIUrl":"10.1016/j.astropartphys.2023.102854","url":null,"abstract":"&lt;div&gt;&lt;p&gt;&lt;span&gt;Assuming a standard Maxwellian velocity distribution for the WIMPs in the halo of our Galaxy we use the null results of an exhaustive set of 9 direct detection experiments to calculate the maximal variation of the exclusion plot for each Wilson coefficient of the most general Galilean–invariant effective Hamiltonian for a WIMP of spin one half due to interferences. We consider 56 Wilson coefficients &lt;/span&gt;&lt;span&gt;&lt;math&gt;&lt;msubsup&gt;&lt;mrow&gt;&lt;mi&gt;c&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;i&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;p&lt;/mi&gt;&lt;mo&gt;,&lt;/mo&gt;&lt;mi&gt;n&lt;/mi&gt;&lt;/mrow&gt;&lt;/msubsup&gt;&lt;/math&gt;&lt;/span&gt; and &lt;span&gt;&lt;math&gt;&lt;msubsup&gt;&lt;mrow&gt;&lt;mi&gt;α&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;i&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;n&lt;/mi&gt;&lt;mo&gt;,&lt;/mo&gt;&lt;mi&gt;p&lt;/mi&gt;&lt;/mrow&gt;&lt;/msubsup&gt;&lt;/math&gt;&lt;/span&gt; for WIMP–proton and WIMP–neutron contact interactions &lt;span&gt;&lt;math&gt;&lt;msubsup&gt;&lt;mrow&gt;&lt;mi&gt;O&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;i&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;p&lt;/mi&gt;&lt;mo&gt;,&lt;/mo&gt;&lt;mi&gt;n&lt;/mi&gt;&lt;/mrow&gt;&lt;/msubsup&gt;&lt;/math&gt;&lt;/span&gt; and the corresponding long range interaction &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;msubsup&gt;&lt;mrow&gt;&lt;mi&gt;O&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;i&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;p&lt;/mi&gt;&lt;mo&gt;,&lt;/mo&gt;&lt;mi&gt;n&lt;/mi&gt;&lt;/mrow&gt;&lt;/msubsup&gt;&lt;mo&gt;/&lt;/mo&gt;&lt;msup&gt;&lt;mrow&gt;&lt;mi&gt;q&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;2&lt;/mn&gt;&lt;/mrow&gt;&lt;/msup&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt;, parameterized by a massless propagator &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;mo&gt;/&lt;/mo&gt;&lt;msup&gt;&lt;mrow&gt;&lt;mi&gt;q&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;2&lt;/mn&gt;&lt;/mrow&gt;&lt;/msup&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt;. For each coupling we provide a different exclusion plot when the following set of operators is allowed to interfere: proton–neutron, i.e. &lt;span&gt;&lt;math&gt;&lt;msubsup&gt;&lt;mrow&gt;&lt;mi&gt;c&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;i&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;p&lt;/mi&gt;&lt;/mrow&gt;&lt;/msubsup&gt;&lt;/math&gt;&lt;/span&gt;–&lt;span&gt;&lt;math&gt;&lt;msubsup&gt;&lt;mrow&gt;&lt;mi&gt;c&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;i&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;n&lt;/mi&gt;&lt;/mrow&gt;&lt;/msubsup&gt;&lt;/math&gt;&lt;/span&gt; or &lt;span&gt;&lt;math&gt;&lt;msubsup&gt;&lt;mrow&gt;&lt;mi&gt;α&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;i&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;p&lt;/mi&gt;&lt;/mrow&gt;&lt;/msubsup&gt;&lt;/math&gt;&lt;/span&gt;–&lt;span&gt;&lt;math&gt;&lt;msubsup&gt;&lt;mrow&gt;&lt;mi&gt;α&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;i&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;n&lt;/mi&gt;&lt;/mrow&gt;&lt;/msubsup&gt;&lt;/math&gt;&lt;/span&gt;; contact–contact or long range–long range, i.e. &lt;span&gt;&lt;math&gt;&lt;msubsup&gt;&lt;mrow&gt;&lt;mi&gt;c&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;i&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;p&lt;/mi&gt;&lt;mo&gt;,&lt;/mo&gt;&lt;mi&gt;n&lt;/mi&gt;&lt;/mrow&gt;&lt;/msubsup&gt;&lt;/math&gt;&lt;/span&gt;–&lt;span&gt;&lt;math&gt;&lt;msubsup&gt;&lt;mrow&gt;&lt;mi&gt;c&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;j&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;p&lt;/mi&gt;&lt;mo&gt;,&lt;/mo&gt;&lt;mi&gt;n&lt;/mi&gt;&lt;/mrow&gt;&lt;/msubsup&gt;&lt;/math&gt;&lt;/span&gt; or &lt;span&gt;&lt;math&gt;&lt;msubsup&gt;&lt;mrow&gt;&lt;mi&gt;α&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;i&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;p&lt;/mi&gt;&lt;mo&gt;,&lt;/mo&gt;&lt;mi&gt;n&lt;/mi&gt;&lt;/mrow&gt;&lt;/msubsup&gt;&lt;/math&gt;&lt;/span&gt;–&lt;span&gt;&lt;math&gt;&lt;msubsup&gt;&lt;mrow&gt;&lt;mi&gt;α&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;j&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;p&lt;/mi&gt;&lt;mo&gt;,&lt;/mo&gt;&lt;mi&gt;n&lt;/mi&gt;&lt;/mrow&gt;&lt;/msubsup&gt;&lt;/math&gt;&lt;/span&gt;; contact– long range, i.e. &lt;span&gt;&lt;math&gt;&lt;msubsup&gt;&lt;mrow&gt;&lt;mi&gt;c&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;i&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;p&lt;/mi&gt;&lt;mo&gt;,&lt;/mo&gt;&lt;mi&gt;n&lt;/mi&gt;&lt;/mrow&gt;&lt;/msubsup&gt;&lt;/math&gt;&lt;/span&gt;–&lt;span&gt;&lt;math&gt;&lt;msubsup&gt;&lt;mrow&gt;&lt;mi&gt;α&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;j&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;p&lt;/mi&gt;&lt;mo&gt;,&lt;/mo&gt;&lt;mi&gt;n&lt;/mi&gt;&lt;/mrow&gt;&lt;/msubsup&gt;&lt;/math&gt;&lt;/span&gt;. For each of the 56 Wilson coefficients &lt;span&gt;&lt;math&gt;&lt;msubsup&gt;&lt;mrow&gt;&lt;mi&gt;c&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;i&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;p&lt;/mi&gt;&lt;mo&gt;,&lt;/mo&gt;&lt;mi&gt;n&lt;/mi&gt;&lt;/mrow&gt;&lt;/msubsup&gt;&lt;/math&gt;&lt;/span&gt; and &lt;span&gt;&lt;math&gt;&lt;msubsup&gt;&lt;m","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"151 ","pages":"Article 102854"},"PeriodicalIF":3.5,"publicationDate":"2023-09-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"48222015","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":"Analytic approach to axion-like-particle emission in core-collapse supernovae","authors":"Ana Luisa Foguel ,&nbsp;Eduardo S. Fraga","doi":"10.1016/j.astropartphys.2023.102855","DOIUrl":"10.1016/j.astropartphys.2023.102855","url":null,"abstract":"<div><p><span>We investigate the impact of a presumed axion-like-particle (ALP) emission in a core-collapse supernova explosion on neutrino luminosities and mean energies employing a relatively simple analytic description. We compute the nuclear Bremsstrahlung and Primakoff axion luminosities as functions of the protoneutron star (PNS) parameters and discuss how the ALP luminosities compete with the neutrino emission, modifying the total PNS thermal energy dissipation. Our results are publicly available in the python package </span><span>ARtiSANS</span>, which can be used to compute the neutrino and axion observables for different choices of parameters.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"151 ","pages":"Article 102855"},"PeriodicalIF":3.5,"publicationDate":"2023-09-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"45670573","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 MIGDAL experiment: Measuring a rare atomic process to aid the search for dark matter","authors":"H.M. Araújo ,&nbsp;S.N. Balashov ,&nbsp;J.E. Borg ,&nbsp;F.M. Brunbauer ,&nbsp;C. Cazzaniga ,&nbsp;C.D. Frost ,&nbsp;F. Garcia ,&nbsp;A.C. Kaboth ,&nbsp;M. Kastriotou ,&nbsp;I. Katsioulas ,&nbsp;A. Khazov ,&nbsp;H. Kraus ,&nbsp;V.A. Kudryavtsev ,&nbsp;S. Lilley ,&nbsp;A. Lindote ,&nbsp;D. Loomba ,&nbsp;M.I. Lopes ,&nbsp;E. Lopez Asamar ,&nbsp;P. Luna Dapica ,&nbsp;P.A. Majewski ,&nbsp;R. Veenhof","doi":"10.1016/j.astropartphys.2023.102853","DOIUrl":"10.1016/j.astropartphys.2023.102853","url":null,"abstract":"<div><p>We present the Migdal In Galactic Dark mAtter expLoration (MIGDAL) experiment aiming at the unambiguous observation and study of the so-called Migdal effect induced by fast-neutron scattering. It is hoped that this elusive atomic process can be exploited to enhance the reach of direct dark matter search experiments to lower masses, but it is still lacking experimental confirmation. Our goal is to detect the predicted atomic electron emission which is thought to accompany nuclear scattering with low, but calculable, probability, by deploying an Optical Time Projection Chamber filled with a low-pressure gas based on CF<span><math><msub><mrow></mrow><mrow><mn>4</mn></mrow></msub></math></span>. Initially, pure CF<span><math><msub><mrow></mrow><mrow><mn>4</mn></mrow></msub></math></span> will be used, and then in mixtures containing other elements employed by leading dark matter search technologies — including noble species, plus Si and Ge. High resolution track images generated by a Gas Electron Multiplier stack, together with timing information from scintillation and ionisation readout, will be used for 3D reconstruction of the characteristic event topology expected for this process — an arrangement of two tracks sharing a common vertex, with one belonging to a Migdal electron and the other to a nuclear recoil. Different energy-loss rate distributions along both tracks will be used as a powerful discrimination tool against background events. In this article we present the design of the experiment, informed by extensive particle and track simulations and detailed estimations of signal and background rates. In pure CF<span><math><msub><mrow></mrow><mrow><mn>4</mn></mrow></msub></math></span> we expect to observe 8.9 (29.3) Migdal events per calendar day of exposure to an intense D–D (D–T) neutron generator beam at the NILE facility located at the Rutherford Appleton Laboratory (UK). With our nominal assumptions, 5<span><math><mi>σ</mi></math></span> median discovery significance can be achieved in under one day with either generator.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"151 ","pages":"Article 102853"},"PeriodicalIF":3.5,"publicationDate":"2023-09-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"44587819","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":"Detection of high energy X-ray radiation following muon captures on Pb","authors":"S. Ilić ,&nbsp;M. Krmar ,&nbsp;D. Knežević ,&nbsp;D. Maletić ,&nbsp;N. Jovančević","doi":"10.1016/j.astropartphys.2023.102889","DOIUrl":"10.1016/j.astropartphys.2023.102889","url":null,"abstract":"<div><p>Low background HPGe detector, shielded by lead, was used to collect background gamma spectra for more than 180 days. Three lines, originating from transitions of muons captured in orbitals of lead atoms were for the first time recognized in background spectra. Relative intensities of detected transitions were calculated and compared with the theoretical prediction.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"153 ","pages":"Article 102889"},"PeriodicalIF":3.5,"publicationDate":"2023-08-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"47860785","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":"Sensitivities for coherent elastic scattering of solar and supernova neutrinos with future NaI(Tl) dark matter search detectors of COSINE-200/1T","authors":"Young Ju Ko ,&nbsp;Hyun Su Lee","doi":"10.1016/j.astropartphys.2023.102890","DOIUrl":"10.1016/j.astropartphys.2023.102890","url":null,"abstract":"<div><p>We investigate the prospects for measuring the coherent elastic neutrino–nucleus scattering of solar and supernova neutrinos in future NaI(Tl) dark matter detection experiments. Considering the reduced background and improved light yield of the recently developed NaI(Tl) crystals, more than 3<span><math><mi>σ</mi></math></span><span><span> observation sensitivities of the supernova neutrino within the </span>Milky Way are demonstrated. In the case of the solar neutrino, approximately 3</span><span><math><mi>σ</mi></math></span> observations are marginal with a 1<!--> <span>ton NaI(Tl) experiment assuming an order of magnitude reduced background, five photoelectron thresholds, and 5-year data exposure.</span></p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"153 ","pages":"Article 102890"},"PeriodicalIF":3.5,"publicationDate":"2023-08-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"45119683","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":"Sensitivity of the Cherenkov Telescope Array to spectral signatures of hadronic PeVatrons with application to Galactic Supernova Remnants","authors":"Cherenkov Telescope Array Consortium,&nbsp;F. Acero ,&nbsp;A. Acharyya ,&nbsp;R. Adam ,&nbsp;A. Aguasca-Cabot ,&nbsp;I. Agudo ,&nbsp;A. Aguirre-Santaella ,&nbsp;J. Alfaro ,&nbsp;R. Aloisio ,&nbsp;N. Álvarez Crespo ,&nbsp;R. Alves Batista ,&nbsp;L. Amati ,&nbsp;E. Amato ,&nbsp;G. Ambrosi ,&nbsp;E.O. Angüner ,&nbsp;C. Aramo ,&nbsp;C. Arcaro ,&nbsp;T. Armstrong ,&nbsp;K. Asano ,&nbsp;Y. Ascasibar ,&nbsp;M. Z̆ivec","doi":"10.1016/j.astropartphys.2023.102850","DOIUrl":"10.1016/j.astropartphys.2023.102850","url":null,"abstract":"<div><p><span>The local Cosmic Ray (CR) energy spectrum<span> exhibits a spectral softening at energies around 3 PeV. Sources which are capable of accelerating hadrons<span> to such energies are called hadronic PeVatrons. However, hadronic PeVatrons have not yet been firmly identified within the Galaxy. Several source classes, including Galactic Supernova Remnants (SNRs), have been proposed as PeVatron candidates. The potential to search for hadronic PeVatrons with the Cherenkov Telescope Array (CTA) is assessed. The focus is on the usage of very high energy </span></span></span><span><math><mi>γ</mi></math></span><span>-ray spectral signatures<span> for the identification of PeVatrons. Assuming that SNRs can accelerate CRs up to knee energies, the number of Galactic SNRs which can be identified as PeVatrons with CTA is estimated within a model for the evolution of SNRs. Additionally, the potential of a follow-up observation strategy under moonlight conditions for PeVatron searches is investigated. Statistical methods<span> for the identification of PeVatrons are introduced, and realistic Monte-Carlo simulations of the response of the CTA observatory to the emission spectra from hadronic PeVatrons are performed. Based on simulations of a simplified model for the evolution for SNRs, the detection of a </span></span></span><span><math><mi>γ</mi></math></span>-ray signal from in average 9 Galactic PeVatron SNRs is expected to result from the scan of the Galactic plane with CTA after 10 h of exposure. CTA is also shown to have excellent potential to confirm these sources as PeVatrons in deep observations with <span><math><mrow><mi>O</mi><mrow><mo>(</mo><mn>100</mn><mo>)</mo></mrow></mrow></math></span> hours of exposure per source.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"150 ","pages":"Article 102850"},"PeriodicalIF":3.5,"publicationDate":"2023-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"41451062","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":"Low-mass extension of direct detection bounds on WIMP-quark and WIMP-gluon effective interactions using the Migdal effect","authors":"Gaurav Tomar ,&nbsp;Sunghyun Kang ,&nbsp;Stefano Scopel","doi":"10.1016/j.astropartphys.2023.102851","DOIUrl":"10.1016/j.astropartphys.2023.102851","url":null,"abstract":"<div><p><span>Updating a previous analysis where we used elastic nuclear recoils we study the Migdal effect to extend to low WIMP<span> masses the direct detection bounds to operators up to dimension 7 of the relativistic effective field theory<span> describing WIMP interactions with quarks and gluons. To this aim we include in our analysis the data of the XENON1T, SuperCDMS, COSINE-100, and DarkSide-50 experiments and assume a standard Maxwellian for the WIMP velocity distribution. We find that the bounds can reach down to a WIMP mass </span></span></span><span><math><mo>≃</mo></math></span>20 MeV, although in the case of higher-dimension operators the energy scale of the ensuing constraints may be inconsistent with the validity of the effective theory.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"150 ","pages":"Article 102851"},"PeriodicalIF":3.5,"publicationDate":"2023-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"46134606","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}