P. Klimov, B. Khrenov, N. Kalmykov, S. Sharakin, M. Zotov
TUS (Tracking Ultraviolet Set-up) was the world’s first orbital detector aimed at testing the principle of observing ultra-high energy cosmic rays (UHECRs) with a space-based fluorescence telescope. TUS was launched into orbit on 28th April 2016 as a part of the scientific payload of the Lomonosov satellite, and itsmission continued for 1.5 years. During this time, its exposure reached ∼ 1550 km2 sr yr for primary energy & 400 EeV, and a number of extensive air showers-like events were registered. The shape and kinematics of the signal in these events closely resembled those expected fromUHECRs but amplitudes of the signal and some other features were in contradiction with this assumption. A detailed analysis of one of EAS-like events (TUS161003) revealed that a primary cosmic ray would need to have an energy & 1 ZeV in order to produce a light curve of the observed amplitude, which is incompatible with the cosmic ray spectrum obtained with ground-based experiments. More than this, the slant depth of the shower maximum be the signal produced by a cosmic particle, was estimated as . 500 g/cm2, which corresponds to cosmic rays around 1 PeV. We present a preliminary discussion of a hypothesis that the TUS161003 event and perhaps some other bright EAS-like events could be produced by relativistic dust grains, which were considered a possible component of the cosmic ray flux beyond the GZK cut-off some time ago.
{"title":"Relativistic dust grains: a new subject of research with orbital fluorescence detectors","authors":"P. Klimov, B. Khrenov, N. Kalmykov, S. Sharakin, M. Zotov","doi":"10.22323/1.395.0315","DOIUrl":"https://doi.org/10.22323/1.395.0315","url":null,"abstract":"TUS (Tracking Ultraviolet Set-up) was the world’s first orbital detector aimed at testing the principle of observing ultra-high energy cosmic rays (UHECRs) with a space-based fluorescence telescope. TUS was launched into orbit on 28th April 2016 as a part of the scientific payload of the Lomonosov satellite, and itsmission continued for 1.5 years. During this time, its exposure reached ∼ 1550 km2 sr yr for primary energy & 400 EeV, and a number of extensive air showers-like events were registered. The shape and kinematics of the signal in these events closely resembled those expected fromUHECRs but amplitudes of the signal and some other features were in contradiction with this assumption. A detailed analysis of one of EAS-like events (TUS161003) revealed that a primary cosmic ray would need to have an energy & 1 ZeV in order to produce a light curve of the observed amplitude, which is incompatible with the cosmic ray spectrum obtained with ground-based experiments. More than this, the slant depth of the shower maximum be the signal produced by a cosmic particle, was estimated as . 500 g/cm2, which corresponds to cosmic rays around 1 PeV. We present a preliminary discussion of a hypothesis that the TUS161003 event and perhaps some other bright EAS-like events could be produced by relativistic dust grains, which were considered a possible component of the cosmic ray flux beyond the GZK cut-off some time ago.","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"42 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-08-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"76328066","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}
Liam David, F. Fraschetti, J. Giacalone, R. Wimmer–Schweingruber, L. Berger, D. Lario
Lunar & Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA Center for Astrophysics | Harvard & Smithsonian, Cambridge, MA, 02138, USA Institute of Experimental and Applied Physics, Kiel University, Kiel, Germany National Space Science Center, Chinese Academy of Sciences, Beijing, China Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA E-mail: liamdavid@email.arizona.edu
{"title":"Energy Balance at Interplanetary Shocks: In-situ Measurement of the Fraction in Supra-thermal and Energetic Ions with ACE and Wind","authors":"Liam David, F. Fraschetti, J. Giacalone, R. Wimmer–Schweingruber, L. Berger, D. Lario","doi":"10.22323/1.395.1311","DOIUrl":"https://doi.org/10.22323/1.395.1311","url":null,"abstract":"Lunar & Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA Center for Astrophysics | Harvard & Smithsonian, Cambridge, MA, 02138, USA Institute of Experimental and Applied Physics, Kiel University, Kiel, Germany National Space Science Center, Chinese Academy of Sciences, Beijing, China Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA E-mail: liamdavid@email.arizona.edu","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"522 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-08-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"86885137","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 Large-Sized Telescopes (LSTs) of Cherenkov TelescopeArray (CTA) are designed for gammaray studies focusing on low energy threshold, high flux sensitivity, rapid telescope repositioning speed and a large field of view. Once the CTA array is complete, the LSTs will be dominating the CTA performance between 20 GeV and 150 GeV. During most of the CTA Observatory construction phase, however, the LSTs will be dominating the array performance until several TeVs. In this presentation we will report on the status of the LST-1 telescope inaugurated in La Palma, Canary islands, Spain in 2018. We will show the progress of the telescope commissioning, compare the expectations with the achieved performance, and give a glance of the first physics results.
{"title":"Status and results of the prototype LST of CTA","authors":"D. Mazin","doi":"10.22323/1.395.0872","DOIUrl":"https://doi.org/10.22323/1.395.0872","url":null,"abstract":"The Large-Sized Telescopes (LSTs) of Cherenkov TelescopeArray (CTA) are designed for gammaray studies focusing on low energy threshold, high flux sensitivity, rapid telescope repositioning speed and a large field of view. Once the CTA array is complete, the LSTs will be dominating the CTA performance between 20 GeV and 150 GeV. During most of the CTA Observatory construction phase, however, the LSTs will be dominating the array performance until several TeVs. In this presentation we will report on the status of the LST-1 telescope inaugurated in La Palma, Canary islands, Spain in 2018. We will show the progress of the telescope commissioning, compare the expectations with the achieved performance, and give a glance of the first physics results.","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"18 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-08-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"83342165","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}
Cosmic rays are messengers from highly energetic events in the Universe. These rare ultra-highenergy particles can be detected efficiently and in an affordable way using large arrays of radio antennas. Linearly polarized geomagnetic emission is the dominant emission mechanism produced when charged particles in air showers get deflected in the Earth’s magnetic field. The sub-dominant Askaryan emission is radially polarized and produced due to the time-varying negative-charge excess in the shower front. The relative amplitude of these two emission components depends on various air shower parameters, such as the arrival direction and the depth of the shower maximum. We studied these dependencies using CoREAS simulations of the radio emission from air showers at the South Pole using a star-shaped antenna layout. On the one hand, the parametrization of the Askaryan-to-geomagnetic ratio can be used as input for a more accurate reconstruction of the shower energy. On the other hand, if measured precisely enough, this ratio may provide a new method to reconstruct the atmospheric depth of the shower maximum.
{"title":"Parametrization of the Relative Amplitude of Geomagnetic and Askaryan Radio Emission from Cosmic-Ray Air Showers using CORSIKA/CoREAS Simulations","authors":"E. Paudel, A. Coleman, F. Schroeder","doi":"10.22323/1.395.0429","DOIUrl":"https://doi.org/10.22323/1.395.0429","url":null,"abstract":"Cosmic rays are messengers from highly energetic events in the Universe. These rare ultra-highenergy particles can be detected efficiently and in an affordable way using large arrays of radio antennas. Linearly polarized geomagnetic emission is the dominant emission mechanism produced when charged particles in air showers get deflected in the Earth’s magnetic field. The sub-dominant Askaryan emission is radially polarized and produced due to the time-varying negative-charge excess in the shower front. The relative amplitude of these two emission components depends on various air shower parameters, such as the arrival direction and the depth of the shower maximum. We studied these dependencies using CoREAS simulations of the radio emission from air showers at the South Pole using a star-shaped antenna layout. On the one hand, the parametrization of the Askaryan-to-geomagnetic ratio can be used as input for a more accurate reconstruction of the shower energy. On the other hand, if measured precisely enough, this ratio may provide a new method to reconstruct the atmospheric depth of the shower maximum.","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"232 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-08-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"77076548","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}
Department of Astronomy, Peking University, 5 Yiheyuan Rd, Beijing, China The Kavli Institute for Astronomy and Astrophysics, Peking University, 5 Yiheyuan Rd, Beijing, China Tsung-Dao Lee Institute, Shanghai Jiao Tong University, 800 Dongchuan Rd, Shanghai, China School of Physics and Astronomy, Shanghai Jiao Tong University, 800 Dongchuan Rd, Shanghai, China E-mail: fan_hu@pke.edu.cn, zhuo.li@pku.edu.cn, donglianxu@sjtu.edu.cn
{"title":"Exploring a PMT+SiPM hybrid optical module for next generation neutrino telescopes","authors":"F. Hu, Zhuo Li, Donglian Xu","doi":"10.22323/1.395.1043","DOIUrl":"https://doi.org/10.22323/1.395.1043","url":null,"abstract":"Department of Astronomy, Peking University, 5 Yiheyuan Rd, Beijing, China The Kavli Institute for Astronomy and Astrophysics, Peking University, 5 Yiheyuan Rd, Beijing, China Tsung-Dao Lee Institute, Shanghai Jiao Tong University, 800 Dongchuan Rd, Shanghai, China School of Physics and Astronomy, Shanghai Jiao Tong University, 800 Dongchuan Rd, Shanghai, China E-mail: fan_hu@pke.edu.cn, zhuo.li@pku.edu.cn, donglianxu@sjtu.edu.cn","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"32 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-08-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"88346329","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}
M. Blank, M. Tluczykont, A. Awad, D. Horns, A. Porelli, I. Astapov, P. Bezyazeekov, E. Bonvech, A. Borodin, A. Bulan, M. Brueckner, N. Budnev, A. Chiavassa, D. Chernov, A. Dyachok, A. Gafarov, A. Garmash, V. Grebenyuk, O. Gress, E. Gress, T. Gress, O. Grishin, A. Grinyuk, N. Kalmykov, V. Kindin, S. Kiryuhin, R. Kokoulin, K. Kompaniets, E. Korosteleva, V. Kozhin, E. Kravchenko, A. Kryukov, L. Kuzmichev, A. Lagutin, M. Lavrova, B. Lubsandorzhiev, N. Lubsandorzhiev, A. Lukanov, D. Lukyantsev, R. Mirgazov, R. Mirzoyan, R. Monkhoev, E. Osipova, A. Pakhorukov, A. Pan, L. Pankov, A. Panov, A. Petrukhin, D. Podgrudkov, V. Poleschuk, M. Popesku, E. Popova, E. Postnikov, V. Prosin, V. Ptuskin, A. Pushnin, R. Raikin, A. Razumov, G. Rubtsov, E. Ryabov, Y. Sagan, V. Samoliga, A. Silaev, A. S. Junior, A. Sidorenkov, A. Skurikhin, M. Slunečka, A. Sokolov, L. Sveshnikova, V. Tabolenko, B. Tarashansky, L. Tkachev, R. Togoo, N. Ushakov, A. Vaidyanathan, P. Volchugov, N. Volkov, D. Voronin, R. Wischnewski, A. Zagorodnikov,
The TAIGA-experiment aims to implement a hybrid detection technique of Extensive Air Showers (EAS) at TeV to PeV energies, combining the wide angle Cherenkov timing array HiSCORE with Imaging Air Cherenkov Telescopes (IACTs). The detector currently consists of 89 HiSCORE stations and two IACTs, distributed over an area of about 1 km2. Our goal is to introduce a new reconstruction technique, combining the good angular and shower core resolution of HiSCORE with the gamma-hadron separation power of the imaging telescopes. With the second IACT in operation, three different event types can be explored: IACT stereo, full hybrid (IACT stereo + stations) and mono hybrid (IACT mono + HiSCORE), the latter being the operational goal of TAIGA. The status of the development of the full hybrid reconstruction and its verification using real data and simulation are presented.
{"title":"Development of hybrid reconstruction techniques for TAIGA","authors":"M. Blank, M. Tluczykont, A. Awad, D. Horns, A. Porelli, I. Astapov, P. Bezyazeekov, E. Bonvech, A. Borodin, A. Bulan, M. Brueckner, N. Budnev, A. Chiavassa, D. Chernov, A. Dyachok, A. Gafarov, A. Garmash, V. Grebenyuk, O. Gress, E. Gress, T. Gress, O. Grishin, A. Grinyuk, N. Kalmykov, V. Kindin, S. Kiryuhin, R. Kokoulin, K. Kompaniets, E. Korosteleva, V. Kozhin, E. Kravchenko, A. Kryukov, L. Kuzmichev, A. Lagutin, M. Lavrova, B. Lubsandorzhiev, N. Lubsandorzhiev, A. Lukanov, D. Lukyantsev, R. Mirgazov, R. Mirzoyan, R. Monkhoev, E. Osipova, A. Pakhorukov, A. Pan, L. Pankov, A. Panov, A. Petrukhin, D. Podgrudkov, V. Poleschuk, M. Popesku, E. Popova, E. Postnikov, V. Prosin, V. Ptuskin, A. Pushnin, R. Raikin, A. Razumov, G. Rubtsov, E. Ryabov, Y. Sagan, V. Samoliga, A. Silaev, A. S. Junior, A. Sidorenkov, A. Skurikhin, M. Slunečka, A. Sokolov, L. Sveshnikova, V. Tabolenko, B. Tarashansky, L. Tkachev, R. Togoo, N. Ushakov, A. Vaidyanathan, P. Volchugov, N. Volkov, D. Voronin, R. Wischnewski, A. Zagorodnikov, ","doi":"10.22323/1.395.0757","DOIUrl":"https://doi.org/10.22323/1.395.0757","url":null,"abstract":"The TAIGA-experiment aims to implement a hybrid detection technique of Extensive Air Showers (EAS) at TeV to PeV energies, combining the wide angle Cherenkov timing array HiSCORE with Imaging Air Cherenkov Telescopes (IACTs). The detector currently consists of 89 HiSCORE stations and two IACTs, distributed over an area of about 1 km2. Our goal is to introduce a new reconstruction technique, combining the good angular and shower core resolution of HiSCORE with the gamma-hadron separation power of the imaging telescopes. With the second IACT in operation, three different event types can be explored: IACT stereo, full hybrid (IACT stereo + stations) and mono hybrid (IACT mono + HiSCORE), the latter being the operational goal of TAIGA. The status of the development of the full hybrid reconstruction and its verification using real data and simulation are presented.","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"33 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-08-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"76887095","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}
C. Hill, Max Meier, R. Nagai, K. Kin, N. Shimizu, A. Ishihara, S. Yoshida, T. Anderson, J. Braun, A. Fienberg, Jeff Weber
New optical sensors called the “D-Egg” have been developed for cost-effective instrumentation for the IceCube Upgrade. With two 8-inch high quantum efficient photomultiplier tubes (PMTs), they offer increased effective photocathode area while retaining as much of the successful IceCube Digital Optical Module design as possible. Mass production of D-Eggs has started in 2020. By the end of 2021, there will be 310 D-Eggs produced with 288 deployed in the IceCube Upgrade. The D-Egg readout system uses advanced technologies in electronics and computing power. Each of the two PMT signals is digitised using ultra-low-power 14-bit ADCs with a sampling frequency of 240 MSPS, enabling seamless and lossless event recording from single-photon signals to signals exceeding 200 PE within 10 ns, as well as flexible event triggering. In this paper, we report the single photon detection performance as well as the multiple photon recording capability of D-Eggs from the mass production line which have been evaluated with the built-in data acquisition system.
{"title":"Performance of the D-Egg optical sensor for the IceCube-Upgrade","authors":"C. Hill, Max Meier, R. Nagai, K. Kin, N. Shimizu, A. Ishihara, S. Yoshida, T. Anderson, J. Braun, A. Fienberg, Jeff Weber","doi":"10.22323/1.395.1042","DOIUrl":"https://doi.org/10.22323/1.395.1042","url":null,"abstract":"New optical sensors called the “D-Egg” have been developed for cost-effective instrumentation for the IceCube Upgrade. With two 8-inch high quantum efficient photomultiplier tubes (PMTs), they offer increased effective photocathode area while retaining as much of the successful IceCube Digital Optical Module design as possible. Mass production of D-Eggs has started in 2020. By the end of 2021, there will be 310 D-Eggs produced with 288 deployed in the IceCube Upgrade. The D-Egg readout system uses advanced technologies in electronics and computing power. Each of the two PMT signals is digitised using ultra-low-power 14-bit ADCs with a sampling frequency of 240 MSPS, enabling seamless and lossless event recording from single-photon signals to signals exceeding 200 PE within 10 ns, as well as flexible event triggering. In this paper, we report the single photon detection performance as well as the multiple photon recording capability of D-Eggs from the mass production line which have been evaluated with the built-in data acquisition system.","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"43 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-08-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"75107789","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}
V. Yurovsky, I. Kudryashov, F. Gasratov, Vasiliy Latonov
The description of the inhomogeneity of the cosmic ray spectrum in the region of 10 TV, which is observed in experimental data, in terms of isotropic diffusion from a single close source is considered. It is shown that such a description is possible, the area of possible localization of the source in space and time, its energy is found. The method of penalty functions is used to account for the data on the spectrum of all particles. nhe calculation of the anisotropy of the diffusion tensor for the energy range of interest in the galactic magnetic field is also shown
{"title":"Interpretation of the spectral inhomogeneity in the 10TV region in terms of a close source","authors":"V. Yurovsky, I. Kudryashov, F. Gasratov, Vasiliy Latonov","doi":"10.22323/1.395.0166","DOIUrl":"https://doi.org/10.22323/1.395.0166","url":null,"abstract":"The description of the inhomogeneity of the cosmic ray spectrum in the region of 10 TV, which is observed in experimental data, in terms of isotropic diffusion from a single close source is considered. It is shown that such a description is possible, the area of possible localization of the source in space and time, its energy is found. The method of penalty functions is used to account for the data on the spectrum of all particles. nhe calculation of the anisotropy of the diffusion tensor for the energy range of interest in the galactic magnetic field is also shown","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"22 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-08-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"84115752","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}
V.A. Allakhverdyan,a A.D. Avrorin,b A.V. Avrorin,b V.M. Aynutdinov,b R. Bannasch,c Z. Bardačová,d I.A. Belolaptikov,a I.V. Borina,a V.B. Brudanin,a,1 N.M. Budnev,e V.Y. Dik,a G.V. Domogatsky,b A.A. Doroshenko,b R. Dvornický,a,d A.N. Dyachok,e Zh.-A.M. Dzhilkibaev,b E. Eckerová,d T.V. Elzhov,a L. Fajt, f S.V. Fialkovski,g,1 A.R. Gafarov,e K.V. Golubkov,b N.S. Gorshkov,a T.I. Gress,e M.S. Katulin,a K.G. Kebkal,c O.G. Kebkal,c E.V. Khramov,a M.M. Kolbin,a K.V. Konischev,a K.A. Kopański,h A.V. Korobchenko,a A.P. Koshechkin,b V.A. Kozhin,i M.V. Kruglov,a M.K. Kryukov,b V.F. Kulepov, Pa. Malecki,h Y.M. Malyshkin,a M.B. Milenin,b R.R. Mirgazov,e D.V. Naumov,a V. Nazari,a W. Noga,h D.P. Petukhov,b E.N. Pliskovsky,a M.I. Rozanov, j V.D. Rushay,a E.V. Ryabov,e G.B. Safronov,b B.A. Shaybonov,a M.D. Shelepov,b F. Šimkovic,a,d, f A.E. Sirenko,a A.V. Skurikhin,i A.G. Solovjev,a M.N. Sorokovikov,a I. Štekl, f A.P. Stromakov,b E.O. Sushenok,a O.V. Suvorova,b V.A. Tabolenko,e B.A. Tarashansky,e Y.V. Yablokova,a S.A. Yakovlevc and D.N. Zaborovb,∗ Joint Institute for Nuclear Research, Dubna, Russia Institute for Nuclear Research, Russian Academy of Sciences, Moscow, Russia EvoLogics GmbH, Berlin, Germany Comenius University, Bratislava, Slovakia Irkutsk State University, Irkutsk, Russia Czech Technical University in Prague, Prague, Czech Republic Nizhny Novgorod State Technical University, Nizhny Novgorod, Russia Institute of Nuclear Physics of Polish Academy of Sciences (IFJ PAN), Kraków, Poland Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow, Russia St. Petersburg State Marine Technical University, St.Petersburg, Russia
{"title":"Observations of track-like neutrino events with Baikal-GVD","authors":"D. Zaborov","doi":"10.22323/1.395.1177","DOIUrl":"https://doi.org/10.22323/1.395.1177","url":null,"abstract":"V.A. Allakhverdyan,a A.D. Avrorin,b A.V. Avrorin,b V.M. Aynutdinov,b R. Bannasch,c Z. Bardačová,d I.A. Belolaptikov,a I.V. Borina,a V.B. Brudanin,a,1 N.M. Budnev,e V.Y. Dik,a G.V. Domogatsky,b A.A. Doroshenko,b R. Dvornický,a,d A.N. Dyachok,e Zh.-A.M. Dzhilkibaev,b E. Eckerová,d T.V. Elzhov,a L. Fajt, f S.V. Fialkovski,g,1 A.R. Gafarov,e K.V. Golubkov,b N.S. Gorshkov,a T.I. Gress,e M.S. Katulin,a K.G. Kebkal,c O.G. Kebkal,c E.V. Khramov,a M.M. Kolbin,a K.V. Konischev,a K.A. Kopański,h A.V. Korobchenko,a A.P. Koshechkin,b V.A. Kozhin,i M.V. Kruglov,a M.K. Kryukov,b V.F. Kulepov, Pa. Malecki,h Y.M. Malyshkin,a M.B. Milenin,b R.R. Mirgazov,e D.V. Naumov,a V. Nazari,a W. Noga,h D.P. Petukhov,b E.N. Pliskovsky,a M.I. Rozanov, j V.D. Rushay,a E.V. Ryabov,e G.B. Safronov,b B.A. Shaybonov,a M.D. Shelepov,b F. Šimkovic,a,d, f A.E. Sirenko,a A.V. Skurikhin,i A.G. Solovjev,a M.N. Sorokovikov,a I. Štekl, f A.P. Stromakov,b E.O. Sushenok,a O.V. Suvorova,b V.A. Tabolenko,e B.A. Tarashansky,e Y.V. Yablokova,a S.A. Yakovlevc and D.N. Zaborovb,∗ Joint Institute for Nuclear Research, Dubna, Russia Institute for Nuclear Research, Russian Academy of Sciences, Moscow, Russia EvoLogics GmbH, Berlin, Germany Comenius University, Bratislava, Slovakia Irkutsk State University, Irkutsk, Russia Czech Technical University in Prague, Prague, Czech Republic Nizhny Novgorod State Technical University, Nizhny Novgorod, Russia Institute of Nuclear Physics of Polish Academy of Sciences (IFJ PAN), Kraków, Poland Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow, Russia St. Petersburg State Marine Technical University, St.Petersburg, Russia","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"15 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-08-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"90088511","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}
A. Bulgarelli, S. Caroff, A. Addis, P. Aubert, L. Baroncelli, G. D. Cesare, A. DiPiano, V. Fioretti, E. García, G. Maurin, N. Parmiggiani, T. Vuillaume, I. Oya, C. Hoischen
The Cherenkov Telescope Array (CTA) Observatory, with dozens of telescopes located in both the Northern and Southern Hemispheres, will be the largest ground-based gamma-ray observatory and will provide broad energy coverage from 20 GeV to 300 TeV. The large effective area and field-of-view, coupled with the fast slewing capability and unprecedented sensitivity, make CTA a crucial instrument for the future of ground-based gamma-ray astronomy. To maximise the scientific return, the array will send alerts on transients and variable phenomena (e.g. gamma-ray burst, active galactic nuclei, gamma-ray binaries, serendipitous sources). Rapid and effective communication to the community requires a reliable and automated system to detect and issue candidate science alerts. This automation will be accomplished by the Science Alert Generation (SAG) pipeline, a key system of the CTA Observatory. SAG is part of the Array Control and Data Acquisition (ACADA) working group. The SAG working group develops the pipelines to perform data reconstruction, data quality monitoring, science monitoring and real-time alert issuing during observations to the Transients Handler functionality of ACADA. SAG is the system that performs the first real-time scientific analysis after the data acquisition. The system performs analysis on multiple time scales (from seconds to hours). SAG must issue candidate science alerts within 20 seconds from the data taking and with sensitivity at least half of the CTA nominal sensitivity. These challenging requirements must be fulfilled by managing trigger rates of tens of kHz from the arrays. Dedicated and highly optimised software and hardware architecture must thus be designed and tested. In this work, we present the general architecture of the ACADA-SAG system.
{"title":"The Science Alert Generation system of the Cherenkov Telescope Array Observatory.","authors":"A. Bulgarelli, S. Caroff, A. Addis, P. Aubert, L. Baroncelli, G. D. Cesare, A. DiPiano, V. Fioretti, E. García, G. Maurin, N. Parmiggiani, T. Vuillaume, I. Oya, C. Hoischen","doi":"10.22323/1.395.0937","DOIUrl":"https://doi.org/10.22323/1.395.0937","url":null,"abstract":"The Cherenkov Telescope Array (CTA) Observatory, with dozens of telescopes located in both the Northern and Southern Hemispheres, will be the largest ground-based gamma-ray observatory and will provide broad energy coverage from 20 GeV to 300 TeV. The large effective area and field-of-view, coupled with the fast slewing capability and unprecedented sensitivity, make CTA a crucial instrument for the future of ground-based gamma-ray astronomy. To maximise the scientific return, the array will send alerts on transients and variable phenomena (e.g. gamma-ray burst, active galactic nuclei, gamma-ray binaries, serendipitous sources). Rapid and effective communication to the community requires a reliable and automated system to detect and issue candidate science alerts. This automation will be accomplished by the Science Alert Generation (SAG) pipeline, a key system of the CTA Observatory. SAG is part of the Array Control and Data Acquisition (ACADA) working group. The SAG working group develops the pipelines to perform data reconstruction, data quality monitoring, science monitoring and real-time alert issuing during observations to the Transients Handler functionality of ACADA. SAG is the system that performs the first real-time scientific analysis after the data acquisition. The system performs analysis on multiple time scales (from seconds to hours). SAG must issue candidate science alerts within 20 seconds from the data taking and with sensitivity at least half of the CTA nominal sensitivity. These challenging requirements must be fulfilled by managing trigger rates of tens of kHz from the arrays. Dedicated and highly optimised software and hardware architecture must thus be designed and tested. In this work, we present the general architecture of the ACADA-SAG system.","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"31 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-08-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"79166684","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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