IceCube-Gen2-Optical is a planned, large-scale upgrade to the existing IceCube Neutrino Observatory. This ∼ 8 cubic kilometer in-ice detector is optimized for point-source science, yielding integer-factor improvementstoangularresolution, andincreasedsensitivitytohigherenergies. Here, itsimpactonfuture study of the diffuse astrophysical spectrum is considered. New analyses of up-going muon neutrino tracks and of all-sky cascade events are performed by adapting standard IceCube selection and analysis methods to this proposed configuration. Improvements to sensitivity of both analyses are presented, along with the combined result. The all-sky cascade analysis excludes a majority of the parameter space allowed by the same period of IceCube observation. The work explores the impact of leading atmospheric systematics on IceCube-Gen2 diffuse sensitivity, and on that of similar, future experiments. A characterization of the Gen2-Optical diffuse program, and implications for our understanding of astrophysical sources in this coming era of next-generation, volumetric neutrino experiments, are provided.
{"title":"Forecasted Sensitivity of IceCube-Gen2 to the Astrophysical Diffuse Spectrum","authors":"A. Kochocki","doi":"10.22323/1.423.0100","DOIUrl":"https://doi.org/10.22323/1.423.0100","url":null,"abstract":"IceCube-Gen2-Optical is a planned, large-scale upgrade to the existing IceCube Neutrino Observatory. This ∼ 8 cubic kilometer in-ice detector is optimized for point-source science, yielding integer-factor improvementstoangularresolution, andincreasedsensitivitytohigherenergies. Here, itsimpactonfuture study of the diffuse astrophysical spectrum is considered. New analyses of up-going muon neutrino tracks and of all-sky cascade events are performed by adapting standard IceCube selection and analysis methods to this proposed configuration. Improvements to sensitivity of both analyses are presented, along with the combined result. The all-sky cascade analysis excludes a majority of the parameter space allowed by the same period of IceCube observation. The work explores the impact of leading atmospheric systematics on IceCube-Gen2 diffuse sensitivity, and on that of similar, future experiments. A characterization of the Gen2-Optical diffuse program, and implications for our understanding of astrophysical sources in this coming era of next-generation, volumetric neutrino experiments, are provided.","PeriodicalId":375543,"journal":{"name":"Proceedings of 27th European Cosmic Ray Symposium — PoS(ECRS)","volume":"81 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-02-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"122100896","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"Gamma ray bursts detection capabilities of a sudden ionospheric disturbance SID detector.","authors":"D. Sapundjiev","doi":"10.22323/1.423.0058","DOIUrl":"https://doi.org/10.22323/1.423.0058","url":null,"abstract":"","PeriodicalId":375543,"journal":{"name":"Proceedings of 27th European Cosmic Ray Symposium — PoS(ECRS)","volume":"44 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-02-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"116917481","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
This paper reviews recent progress in the field of direct measurements of Galactic cosmic rays. High-statistic measurements of cosmic ray energy spectra, chemical and isotopic composition, and the rare antimatter components have been made using large particle physics experiments operating in space. The recent results are discussed in relation to our understanding of the origin of cosmic rays, the open questions, and the challenges for future experiments of direct detection.
{"title":"Direct Measurements of Galactic Cosmic Rays","authors":"N. Tomassetti","doi":"10.22323/1.423.0007","DOIUrl":"https://doi.org/10.22323/1.423.0007","url":null,"abstract":"This paper reviews recent progress in the field of direct measurements of Galactic cosmic rays. High-statistic measurements of cosmic ray energy spectra, chemical and isotopic composition, and the rare antimatter components have been made using large particle physics experiments operating in space. The recent results are discussed in relation to our understanding of the origin of cosmic rays, the open questions, and the challenges for future experiments of direct detection.","PeriodicalId":375543,"journal":{"name":"Proceedings of 27th European Cosmic Ray Symposium — PoS(ECRS)","volume":"10 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-01-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"131686057","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Q. Luce, D. Schmidt, O. Deligny, I. Lhenry-Yvon, M. Roth, A. Watson
When analysing data from air-shower arrays, it has become common practice to use the signal at a considerable distance from the shower axis ($r_text{opt}$) as a surrogate for the size of the shower. This signal, $S(r_text{opt}$), can then be related to the primary energy in a variety of ways. After a brief review of the reasons behind the introduction of $r_text{opt}$ laid out in a seminal paper by Hillas in 1969, it will be shown that $r_text{opt}$, is a more effective tool when detectors are laid out on a triangular grid than when detectors are deployed on a square grid. This result may have implications for explaining the differences between the flux observed by the Auger and Telescope collaborations above 10,EeV and should be kept in mind when designing new shower arrays.
{"title":"The Use of the Signal at an Optimal Distance from the Shower Core as a Surrogate for Shower Size","authors":"Q. Luce, D. Schmidt, O. Deligny, I. Lhenry-Yvon, M. Roth, A. Watson","doi":"10.22323/1.423.0078","DOIUrl":"https://doi.org/10.22323/1.423.0078","url":null,"abstract":"When analysing data from air-shower arrays, it has become common practice to use the signal at a considerable distance from the shower axis ($r_text{opt}$) as a surrogate for the size of the shower. This signal, $S(r_text{opt}$), can then be related to the primary energy in a variety of ways. After a brief review of the reasons behind the introduction of $r_text{opt}$ laid out in a seminal paper by Hillas in 1969, it will be shown that $r_text{opt}$, is a more effective tool when detectors are laid out on a triangular grid than when detectors are deployed on a square grid. This result may have implications for explaining the differences between the flux observed by the Auger and Telescope collaborations above 10,EeV and should be kept in mind when designing new shower arrays.","PeriodicalId":375543,"journal":{"name":"Proceedings of 27th European Cosmic Ray Symposium — PoS(ECRS)","volume":"42 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-01-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"121724862","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Understanding the origins of ultrahigh energy cosmic rays (UHECRs) - which reach energies in excess of $10^{20}~{rm eV}$ - stretches particle acceleration physics to its very limits. In this review, we discuss how such energies can be reached, using general arguments that can often be derived on the back of an envelope. We explore possible particle acceleration mechanisms, with special attention paid to shock acceleration. Informed by the arguments derived, we discuss where UHECRs might come from and which classes of powerful astrophysical objects could be UHECR sources; generally, we favour radio galaxies, GRB afterglows and other sources which are not too compact and dissipate prodigious amounts of energy on large scales, allowing them to generate large products $beta B R$ without the CRs undergoing restrictive losses. Finally, we discuss when UHECRs are accelerated by highlighting the importance of source variability, and explore the intriguing possibility that the UHECR arrival directions are partly a result of"echoes"from magnetic structures in the local Universe.
{"title":"How, where and when do cosmic rays reach ultrahigh energies?","authors":"J. Matthews, A. M. Taylor","doi":"10.22323/1.423.0010","DOIUrl":"https://doi.org/10.22323/1.423.0010","url":null,"abstract":"Understanding the origins of ultrahigh energy cosmic rays (UHECRs) - which reach energies in excess of $10^{20}~{rm eV}$ - stretches particle acceleration physics to its very limits. In this review, we discuss how such energies can be reached, using general arguments that can often be derived on the back of an envelope. We explore possible particle acceleration mechanisms, with special attention paid to shock acceleration. Informed by the arguments derived, we discuss where UHECRs might come from and which classes of powerful astrophysical objects could be UHECR sources; generally, we favour radio galaxies, GRB afterglows and other sources which are not too compact and dissipate prodigious amounts of energy on large scales, allowing them to generate large products $beta B R$ without the CRs undergoing restrictive losses. Finally, we discuss when UHECRs are accelerated by highlighting the importance of source variability, and explore the intriguing possibility that the UHECR arrival directions are partly a result of\"echoes\"from magnetic structures in the local Universe.","PeriodicalId":375543,"journal":{"name":"Proceedings of 27th European Cosmic Ray Symposium — PoS(ECRS)","volume":"1 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-01-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"130162797","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Sofia Grusovin, G. Consolati, A. Angelis, C. Arcaro, F. Bisconti, A. Chiavassa, M. Doro, F. Guarino, M. Mariotti, E. Prandini
The Southern Wide-field Gamma-ray Observatory (SWGO) is an international collaboration working on realizing a next-generation observatory located in the Southern hemisphere, which offers a privileged view of our galactic center. We are working on the construction of a prototype water Cherenkov detector at Politecnico di Milano using a flexible testing facility for several candidate light sensors and configurations. A structure able to hold different types of detectors in multiple configurations has been designed, built and tested in Politecnico's labs. Furthermore, an analytical study of muons and electrons showers has been carried out using the SWGO observatory simulation software to examine the correlation between the detection capabilities of the prototype tank and its water level.
南方宽视场伽玛射线天文台(SWGO)是一项国际合作，致力于实现位于南半球的下一代天文台，它提供了我们银河系中心的特权视图。我们正在米兰理工大学(Politecnico di Milano)建造一个水切伦科夫探测器的原型，使用一个灵活的测试设备来测试几种候选的光传感器和配置。一种能够容纳多种配置的不同类型探测器的结构已经在巴黎理工大学的实验室中设计、制造和测试。此外，利用SWGO天文台模拟软件进行了介子和电子阵雨的分析研究，以检验原型水箱的探测能力与其水位之间的相关性。
{"title":"A prototype tank for the SWGO detector","authors":"Sofia Grusovin, G. Consolati, A. Angelis, C. Arcaro, F. Bisconti, A. Chiavassa, M. Doro, F. Guarino, M. Mariotti, E. Prandini","doi":"10.22323/1.423.0150","DOIUrl":"https://doi.org/10.22323/1.423.0150","url":null,"abstract":"The Southern Wide-field Gamma-ray Observatory (SWGO) is an international collaboration working on realizing a next-generation observatory located in the Southern hemisphere, which offers a privileged view of our galactic center. We are working on the construction of a prototype water Cherenkov detector at Politecnico di Milano using a flexible testing facility for several candidate light sensors and configurations. A structure able to hold different types of detectors in multiple configurations has been designed, built and tested in Politecnico's labs. Furthermore, an analytical study of muons and electrons showers has been carried out using the SWGO observatory simulation software to examine the correlation between the detection capabilities of the prototype tank and its water level.","PeriodicalId":375543,"journal":{"name":"Proceedings of 27th European Cosmic Ray Symposium — PoS(ECRS)","volume":"40 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-01-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"131315702","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The Pierre Auger Observatory is the largest astroparticle experiment in operation. Complementary to the measurements of the charged ultra-high energy (UHE) cosmic rays, it provides a very good sensitivity to the detection of UHE photons and neutrinos. Since the photon and neutrino fluxes are correlated to the acceleration mechanisms of charged particles, searches for these neutral particles enhance the multi-messenger understanding of UHE cosmic-ray sources and of transient astrophysical phenomena. In addition, searches for diffuse fluxes may bring information about exotic scenarios such as the decay of hypothetical super-heavy dark matter in the Galactic halo. In this contribution, we present an overview of the current UHE photon and neutrino searches at the Observatory and discuss the most recent results. We report on stringent limits to the UHE photon and neutrino diffuse and point-like fluxes above 1017 eV, which lead to strong constraints on theoretical models describing the nature of dark matter candidates and the sources of the most energetic particles in the Universe.
{"title":"Searches for ultra-high energy photons and neutrinos with the Pierre Auger Observatory","authors":"N. Gonz'alez","doi":"10.22323/1.423.0089","DOIUrl":"https://doi.org/10.22323/1.423.0089","url":null,"abstract":"The Pierre Auger Observatory is the largest astroparticle experiment in operation. Complementary to the measurements of the charged ultra-high energy (UHE) cosmic rays, it provides a very good sensitivity to the detection of UHE photons and neutrinos. Since the photon and neutrino fluxes are correlated to the acceleration mechanisms of charged particles, searches for these neutral particles enhance the multi-messenger understanding of UHE cosmic-ray sources and of transient astrophysical phenomena. In addition, searches for diffuse fluxes may bring information about exotic scenarios such as the decay of hypothetical super-heavy dark matter in the Galactic halo. In this contribution, we present an overview of the current UHE photon and neutrino searches at the Observatory and discuss the most recent results. We report on stringent limits to the UHE photon and neutrino diffuse and point-like fluxes above 1017 eV, which lead to strong constraints on theoretical models describing the nature of dark matter candidates and the sources of the most energetic particles in the Universe.","PeriodicalId":375543,"journal":{"name":"Proceedings of 27th European Cosmic Ray Symposium — PoS(ECRS)","volume":"67 12","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-12-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"120969583","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
High-redshift primordial galaxies have recently been found with evolved stellar populations and complex star-formation histories reaching back to 250 Myr after the Big Bang. Their intense bursts of star-formation appear to be interspersed with sustained periods of strong quenching, however the processes underlying this evolutionary behaviour remain unclear. Unlike later epochs, galaxies in the early Universe are not located in large associations like clusters. Instead, they co-evolve with their developing circumgalactic halo as relatively isolated ecosystems. Thus, the mechanisms that could bring about the downfall of their star-formation are presumably intrinsic, and feedback processes associated with their intense starburst episodes likely play an important role. Cosmic rays are a viable agent to deliver this feedback, and could account for the star-formation histories inferred for these systems. The cosmic ray impact on galaxies may be investigated using the wealth of multi-wavelength data soon to be obtained with the armada of new and upcoming facilities. Complementary approaches to probe their action across the electromagnetic spectrum can be arranged into a distance ladder of cosmic ray feedback signatures. With a clear understanding of how cosmic ray activity in primordial systems can be traced, it will be possible to extend this ladder to high redshifts and map-out the role played by cosmic rays in shaping galaxy evolution over cosmic time.
{"title":"Cosmic rays as a feedback agent in primordial galactic ecosystems","authors":"E. Owen","doi":"10.22323/1.423.0136","DOIUrl":"https://doi.org/10.22323/1.423.0136","url":null,"abstract":"High-redshift primordial galaxies have recently been found with evolved stellar populations and complex star-formation histories reaching back to 250 Myr after the Big Bang. Their intense bursts of star-formation appear to be interspersed with sustained periods of strong quenching, however the processes underlying this evolutionary behaviour remain unclear. Unlike later epochs, galaxies in the early Universe are not located in large associations like clusters. Instead, they co-evolve with their developing circumgalactic halo as relatively isolated ecosystems. Thus, the mechanisms that could bring about the downfall of their star-formation are presumably intrinsic, and feedback processes associated with their intense starburst episodes likely play an important role. Cosmic rays are a viable agent to deliver this feedback, and could account for the star-formation histories inferred for these systems. The cosmic ray impact on galaxies may be investigated using the wealth of multi-wavelength data soon to be obtained with the armada of new and upcoming facilities. Complementary approaches to probe their action across the electromagnetic spectrum can be arranged into a distance ladder of cosmic ray feedback signatures. With a clear understanding of how cosmic ray activity in primordial systems can be traced, it will be possible to extend this ladder to high redshifts and map-out the role played by cosmic rays in shaping galaxy evolution over cosmic time.","PeriodicalId":375543,"journal":{"name":"Proceedings of 27th European Cosmic Ray Symposium — PoS(ECRS)","volume":"150 12 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"130890942","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The transport of charged particles in various astrophysical environments permeated by magnetic fields is described in terms of a diffusion process, which relies on diffusion-tensor parameters generally inferred from Monte-Carlo simulations. Based on a red-noise approximation to model the two-point correlation function of the magnetic field experienced by charged particles between two successive times, the diffusion-tensor coefficients were previously derived in the case of pure turbulence. In this contribution to ECRS2022, the derivation is extended to the case of a mean field on top of the turbulence. The results are applicable to a variety of astrophysical environments in regimes where the Larmor radius of the particles is resonant with the power spectrum of the turbulence wavelength (gyro-resonant regime), or where the Larmor radius is greater than the largest turbulence wavelength (high-rigidity regime).
{"title":"Theoretical derivation of diffusion-tensor coefficients for the transport of charged particles in magnetic fields","authors":"O. Deligny","doi":"10.22323/1.423.0139","DOIUrl":"https://doi.org/10.22323/1.423.0139","url":null,"abstract":"The transport of charged particles in various astrophysical environments permeated by magnetic fields is described in terms of a diffusion process, which relies on diffusion-tensor parameters generally inferred from Monte-Carlo simulations. Based on a red-noise approximation to model the two-point correlation function of the magnetic field experienced by charged particles between two successive times, the diffusion-tensor coefficients were previously derived in the case of pure turbulence. In this contribution to ECRS2022, the derivation is extended to the case of a mean field on top of the turbulence. The results are applicable to a variety of astrophysical environments in regimes where the Larmor radius of the particles is resonant with the power spectrum of the turbulence wavelength (gyro-resonant regime), or where the Larmor radius is greater than the largest turbulence wavelength (high-rigidity regime).","PeriodicalId":375543,"journal":{"name":"Proceedings of 27th European Cosmic Ray Symposium — PoS(ECRS)","volume":"37 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-12-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"126654336","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The IceCube Neutrino Observatory is a multi-component detector embedded deep within the South-Pole Ice. This proceeding will discuss an analysis from an integrated operation of IceCube and its surface array, IceTop, to estimate cosmic-ray composition. The work will describe a novel graph neural network based approach for estimating the mass of primary cosmic rays, that takes advantage of signal-footprint information and reconstructed cosmic-ray air shower parameters. In addition, the work will also introduce new composition-sensitive parameters for improving the estimation of cosmic-ray composition, with the potential of improving our understanding of the high-energy muon content in cosmic-ray air showers.
{"title":"Cosmic-Ray Composition analysis at IceCube using Graph Neural Networks","authors":"P. Koundal","doi":"10.22323/1.423.0085","DOIUrl":"https://doi.org/10.22323/1.423.0085","url":null,"abstract":"The IceCube Neutrino Observatory is a multi-component detector embedded deep within the South-Pole Ice. This proceeding will discuss an analysis from an integrated operation of IceCube and its surface array, IceTop, to estimate cosmic-ray composition. The work will describe a novel graph neural network based approach for estimating the mass of primary cosmic rays, that takes advantage of signal-footprint information and reconstructed cosmic-ray air shower parameters. In addition, the work will also introduce new composition-sensitive parameters for improving the estimation of cosmic-ray composition, with the potential of improving our understanding of the high-energy muon content in cosmic-ray air showers.","PeriodicalId":375543,"journal":{"name":"Proceedings of 27th European Cosmic Ray Symposium — PoS(ECRS)","volume":"25 4","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-11-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"120997234","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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