M. Ribó, A. Fattorini, K. Satalecka, E. Bernardini
{"title":"MAGIC as a Neutrino Follow-Up Instrument","authors":"M. Ribó, A. Fattorini, K. Satalecka, E. Bernardini","doi":"10.22323/1.357.0066","DOIUrl":"https://doi.org/10.22323/1.357.0066","url":null,"abstract":"","PeriodicalId":257968,"journal":{"name":"Proceedings of The New Era of Multi-Messenger Astrophysics — PoS(Asterics2019)","volume":"27 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2019-08-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"124453211","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 discovery of a diffuse flux of high energy neutrinos has opened a new era in the field of neutrino astronomy. Up to now only one high energy neutrino has an identified astrophysical counterpart, the blazar TXS 0506+056. However the origin of the diffuse neutrino flux remains still a mystery, even if many possible explanations have been proposed in the last few years. The most natural hypothesis was that high energy neutrinos are produced by blazars, since these powerful objects dominate the γ -ray sky above 100 TeV. However the IceCube stacking limit shows that resolved blazars cannot contribute more than 20%. Other natural sources are the ones rich of gas, in which the proton-proton interaction dominates. In this scenario an issue would be the over-production of γ -rays associated to neutrinos, if the neutrino spectrum were too soft. In this work we summarize the present knowledge and we discuss the role of low luminosity BL Lacs, showing that it is still possible to power the sub-PeV neutrino flux with blazars. Moreover we also discuss the role of pp sources, showing that they are still into the game and they can saturate the sub-PeV neutrino emission, giving also a contribution larger than 50% in the energy range between 10 TeV and 100 TeV.
{"title":"On the sources of high energy neutrinos","authors":"A. Palladino","doi":"10.22323/1.357.0058","DOIUrl":"https://doi.org/10.22323/1.357.0058","url":null,"abstract":"The discovery of a diffuse flux of high energy neutrinos has opened a new era in the field of neutrino astronomy. Up to now only one high energy neutrino has an identified astrophysical counterpart, the blazar TXS 0506+056. However the origin of the diffuse neutrino flux remains still a mystery, even if many possible explanations have been proposed in the last few years. The most natural hypothesis was that high energy neutrinos are produced by blazars, since these powerful objects dominate the γ -ray sky above 100 TeV. However the IceCube stacking limit shows that resolved blazars cannot contribute more than 20%. Other natural sources are the ones rich of gas, in which the proton-proton interaction dominates. In this scenario an issue would be the over-production of γ -rays associated to neutrinos, if the neutrino spectrum were too soft. In this work we summarize the present knowledge and we discuss the role of low luminosity BL Lacs, showing that it is still possible to power the sub-PeV neutrino flux with blazars. Moreover we also discuss the role of pp sources, showing that they are still into the game and they can saturate the sub-PeV neutrino emission, giving also a contribution larger than 50% in the energy range between 10 TeV and 100 TeV.","PeriodicalId":257968,"journal":{"name":"Proceedings of The New Era of Multi-Messenger Astrophysics — PoS(Asterics2019)","volume":"11 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2019-08-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"128081033","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}
Gamma-ray bursts (GRBs) are transients associated with the formation of compact objects. It had long been theorised that mergers of two neutron stars leading to the formation of a heavier neutron star or a black hole are the progenitors of the so-called ‘short’ GRBs. The merger is associated with the emission of gravitational waves (GWs) that are detectable on earth, and this association was proved empirically with the detection of a short GRB and other electromagnetic emission of the GW source 170817. It is important to make statistical predictions of the number of sGRBs detectable by a GRB monitor in the sky. Here I present predictions of the event rate of the AstroSat-CZTI via careful studies of the luminosity function of short GRBs. Using the maximum distance to which the GW networks are sensitive in the past, present and future runs, stringent lower limits are placed on the rate of binary neutron star mergers (BNSMs). It is shown that the number will go up significantly in the next observing runs of aLIGO/VIRGO. Comparison of the short GRB rate with the BNSM rate calculated independently from the single source statistics of GW170817 reveals the presence of a slight tension that can have significant implications on the physics of the merger ejecta; however the scenario that each BNSM indeed produces a short GRB, cannot be ruled out.
{"title":"The binary neutron star merger rate via the modelled rate of short gamma-ray bursts","authors":"D. Paul","doi":"10.22323/1.357.0059","DOIUrl":"https://doi.org/10.22323/1.357.0059","url":null,"abstract":"Gamma-ray bursts (GRBs) are transients associated with the formation of compact objects. It had long been theorised that mergers of two neutron stars leading to the formation of a heavier neutron star or a black hole are the progenitors of the so-called ‘short’ GRBs. The merger is associated with the emission of gravitational waves (GWs) that are detectable on earth, and this association was proved empirically with the detection of a short GRB and other electromagnetic emission of the GW source 170817. It is important to make statistical predictions of the number of sGRBs detectable by a GRB monitor in the sky. Here I present predictions of the event rate of the AstroSat-CZTI via careful studies of the luminosity function of short GRBs. Using the maximum distance to which the GW networks are sensitive in the past, present and future runs, stringent lower limits are placed on the rate of binary neutron star mergers (BNSMs). It is shown that the number will go up significantly in the next observing runs of aLIGO/VIRGO. Comparison of the short GRB rate with the BNSM rate calculated independently from the single source statistics of GW170817 reveals the presence of a slight tension that can have significant implications on the physics of the merger ejecta; however the scenario that each BNSM indeed produces a short GRB, cannot be ruled out.","PeriodicalId":257968,"journal":{"name":"Proceedings of The New Era of Multi-Messenger Astrophysics — PoS(Asterics2019)","volume":"240 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2019-08-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"116424640","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":"Data and Software Preservation through Containerisation in KM3NeT","authors":"T. Gál","doi":"10.22323/1.357.0027","DOIUrl":"https://doi.org/10.22323/1.357.0027","url":null,"abstract":"","PeriodicalId":257968,"journal":{"name":"Proceedings of The New Era of Multi-Messenger Astrophysics — PoS(Asterics2019)","volume":"104 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2019-08-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"127332409","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":"The ASTERICS project: developing a new era of Multi-messenger astrophysics","authors":"C. Jackson, G. Cimò, R. Meer","doi":"10.22323/1.357.0037","DOIUrl":"https://doi.org/10.22323/1.357.0037","url":null,"abstract":"","PeriodicalId":257968,"journal":{"name":"Proceedings of The New Era of Multi-Messenger Astrophysics — PoS(Asterics2019)","volume":"4 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2019-08-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"126579909","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}
S. Stellacci, B. Spisso, C. Pellegrino, C. Bozza, T. Chiarusi, R. Coniglione, E. Giorgio, Paolo Lo Re, P. Migliozzi, A. Martini
{"title":"CORELib: COsmic Ray Event Library","authors":"S. Stellacci, B. Spisso, C. Pellegrino, C. Bozza, T. Chiarusi, R. Coniglione, E. Giorgio, Paolo Lo Re, P. Migliozzi, A. Martini","doi":"10.22323/1.357.0079","DOIUrl":"https://doi.org/10.22323/1.357.0079","url":null,"abstract":"","PeriodicalId":257968,"journal":{"name":"Proceedings of The New Era of Multi-Messenger Astrophysics — PoS(Asterics2019)","volume":"24 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2019-08-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"125554795","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}
B. Miller, A. Adamson, J. Blakeslee, A. Stephens, J. Thomas-Osip, Arturo Núñez
Gemini Observatory will be an important facility for following up time-domain discoveries in the multi-messenger era. Gemini has a variety of time allocation processes in order to accommodate a broad range of project needs and timescales. Time is allocated by regular participant TACs, a common large program TAC, and by proposer peer review for "fast-turnaround" proposals. Queue observing allows Gemini to easily execute target-of-opportunity (ToO) observations and this capability will be very important for transient follow-up. Instrumentation includes optical and near-infrared imagers and spectrographs at both sites. New facility instruments and systems are under development including GHOST (high-resolution optical spectrograph), SCORPIO (the broad-wavelength follow-up workhorse), and a new multi-conjugate AO system for Gemini North. Visitor instruments are also highly encouraged. All new facility instruments will be delivered with data reduction pipelines and the data are delivered via a cloud-based science archive. Finally, we summarize planned changes to our operations software to handle the expected increased volume of ToO triggers and to incorporate Gemini into the developing time-domain follow-up infrastructure. These changes will include new interfaces, more programmatic access, a real-time scheduler, and automated data reduction.
{"title":"Gemini Operations for Multi-Messenger Astronomy","authors":"B. Miller, A. Adamson, J. Blakeslee, A. Stephens, J. Thomas-Osip, Arturo Núñez","doi":"10.22323/1.357.0050","DOIUrl":"https://doi.org/10.22323/1.357.0050","url":null,"abstract":"Gemini Observatory will be an important facility for following up time-domain discoveries in the multi-messenger era. Gemini has a variety of time allocation processes in order to accommodate a broad range of project needs and timescales. Time is allocated by regular participant TACs, a common large program TAC, and by proposer peer review for \"fast-turnaround\" proposals. Queue observing allows Gemini to easily execute target-of-opportunity (ToO) observations and this capability will be very important for transient follow-up. Instrumentation includes optical and near-infrared imagers and spectrographs at both sites. New facility instruments and systems are under development including GHOST (high-resolution optical spectrograph), SCORPIO (the broad-wavelength follow-up workhorse), and a new multi-conjugate AO system for Gemini North. Visitor instruments are also highly encouraged. All new facility instruments will be delivered with data reduction pipelines and the data are delivered via a cloud-based science archive. Finally, we summarize planned changes to our operations software to handle the expected increased volume of ToO triggers and to incorporate Gemini into the developing time-domain follow-up infrastructure. These changes will include new interfaces, more programmatic access, a real-time scheduler, and automated data reduction.","PeriodicalId":257968,"journal":{"name":"Proceedings of The New Era of Multi-Messenger Astrophysics — PoS(Asterics2019)","volume":"55 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2019-08-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"127847364","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}
J. Lightfoot, J. Colomé, M. Kettenis, Dave Morris, M. Timmer
{"title":"A Platform for Multi-Messenger Observing","authors":"J. Lightfoot, J. Colomé, M. Kettenis, Dave Morris, M. Timmer","doi":"10.22323/1.357.0045","DOIUrl":"https://doi.org/10.22323/1.357.0045","url":null,"abstract":"","PeriodicalId":257968,"journal":{"name":"Proceedings of The New Era of Multi-Messenger Astrophysics — PoS(Asterics2019)","volume":"37 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2019-08-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"117066087","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}
Open Science is the combination of Open Data and Open Access leading to interoperability of resources for science production. Fostering new science through interoperability is the goal of the International Virtual Observatory Alliance (IVOA), whose standards provide the framework to allow Open Science in Astronomy and Astrophysics. Data Access, Discovery and Interoperability (DADI) is the ASTERICS work package dealing with the dissemination of the Virtual Observatory (VO) standards and technologies, gathering needs from the scientific community and ESFRIs requirements related to interoperability, and stirring them into updates or additions to the VO scenario. Within DADI, networking and discussion forums and training events for the ESFRI partners (as well as for the general data providers) have been held, to put together the thinking heads of the research infrastructure (RI) projects and the staff having VO knowledge. These events initially brought the interoperability perspective to the large scientific collaborations and later allowed to feel the pulse of how much of the VO technology was welcomed, used and investigated by the RIs. During the events, requirements and perspective on the open science scenario were brought in by the projects and collaborations and discussed with VO knowledgeable people. This contribution tries to summarise what was discussed in such a context, in terms of how useful and practical resource interoperability is when a large collaboration has to intertwine it with project requests.
{"title":"ESFRIs & VO: networking and discussing","authors":"M. Molinaro, F. Pasian","doi":"10.22323/1.357.0052","DOIUrl":"https://doi.org/10.22323/1.357.0052","url":null,"abstract":"Open Science is the combination of Open Data and Open Access leading to interoperability of resources for science production. Fostering new science through interoperability is the goal of the International Virtual Observatory Alliance (IVOA), whose standards provide the framework to allow Open Science in Astronomy and Astrophysics. Data Access, Discovery and Interoperability (DADI) is the ASTERICS work package dealing with the dissemination of the Virtual Observatory (VO) standards and technologies, gathering needs from the scientific community and ESFRIs requirements related to interoperability, and stirring them into updates or additions to the VO scenario. Within DADI, networking and discussion forums and training events for the ESFRI partners (as well as for the general data providers) have been held, to put together the thinking heads of the research infrastructure (RI) projects and the staff having VO knowledge. These events initially brought the interoperability perspective to the large scientific collaborations and later allowed to feel the pulse of how much of the VO technology was welcomed, used and investigated by the RIs. During the events, requirements and perspective on the open science scenario were brought in by the projects and collaborations and discussed with VO knowledgeable people. This contribution tries to summarise what was discussed in such a context, in terms of how useful and practical resource interoperability is when a large collaboration has to intertwine it with project requests.","PeriodicalId":257968,"journal":{"name":"Proceedings of The New Era of Multi-Messenger Astrophysics — PoS(Asterics2019)","volume":"29 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2019-08-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"122878940","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}
T. P. A. C. P. Abreu, M. Aglietta, I. Allekotte, K. A. Cheminant, A. Almela, J. Alvarez-Muñiz, J. A. Yebra, G. A. Anastasi, L. Anchordoqui, B. Andrada, S. Andringa, C. Aramo, P. Ferreira, E. Arnone, J. C. A. Vel'azquez, Hernán Asorey, P. Assis, G. Avila, E. Avocone, A. Badescu, A. Bakalová, A. Bălăceanu, F. Barbato, J. Bellido, C. Bérat, M. Bertaina, G. Bhatta, P. Biermann, V. Binet, K. Bismark, T. Bister, J. Biteau, J. Blazek, C. Bleve, J. Blumer, M. Boh'avcov'a, D. Boncioli, C. Bonifazi, L. Arbeletche, N. Borodai, J. Brack, T. Bretz, P. G. B. Orchera, F. Briechle, P. Buchholz, A. Bueno, S. Buitink, M. Buscemi, M. Busken, A. Bwembya, K. Caballero-Mora, L. Caccianiga, I. Caracas, R. Caruso, A. Castellina, F. Catalani, G. Cataldi, L. Cazon, M. Cerda, J. Chinellato, J. Chudoba, L. Chytka, R. Clay, A. Cerutti, R. Colalillo, A. Coleman, M. Coluccia, R. Conceiccao, A. Condorelli, G. Consolati, F. Contreras, F. Convenga, D. D. Santos, C. Covault, M. Cristinziani, S. Dasso, K. Daumiller, B. Dawson, R. M. Almeida
One of the key challenges in astroparticle physics is identifying the sources of cosmic rays at the highest energies (above 10^18 eV). In this context, the search for ultra-high energy photons is of high interest. Observing photons of such energies would impact astrophysics and particle physics as well as fundamental physics and would be an important contribution to multimessenger astronomy. The Pierre Auger Observatory near Malargue, Argentina, is the largest air-shower experiment for the detection of ultra-high energy cosmic rays. It consists of an array of about 1660 water Cherenkov detectors arranged on a triangular grid which covers an area of more than 3000 km^2. 27 fluorescence telescopes at four sites overlooking the detector array provide an independent and complementary method for air-shower detection. In the contribution, the various activities at the Pierre Auger Observatory concerning searches for ultra-high energy photons will be presented and the current results will be summarized.
{"title":"Searches for ultra-high-energy photons at the Pierre Auger Observatory","authors":"T. P. A. C. P. Abreu, M. Aglietta, I. Allekotte, K. A. Cheminant, A. Almela, J. Alvarez-Muñiz, J. A. Yebra, G. A. Anastasi, L. Anchordoqui, B. Andrada, S. Andringa, C. Aramo, P. Ferreira, E. Arnone, J. C. A. Vel'azquez, Hernán Asorey, P. Assis, G. Avila, E. Avocone, A. Badescu, A. Bakalová, A. Bălăceanu, F. Barbato, J. Bellido, C. Bérat, M. Bertaina, G. Bhatta, P. Biermann, V. Binet, K. Bismark, T. Bister, J. Biteau, J. Blazek, C. Bleve, J. Blumer, M. Boh'avcov'a, D. Boncioli, C. Bonifazi, L. Arbeletche, N. Borodai, J. Brack, T. Bretz, P. G. B. Orchera, F. Briechle, P. Buchholz, A. Bueno, S. Buitink, M. Buscemi, M. Busken, A. Bwembya, K. Caballero-Mora, L. Caccianiga, I. Caracas, R. Caruso, A. Castellina, F. Catalani, G. Cataldi, L. Cazon, M. Cerda, J. Chinellato, J. Chudoba, L. Chytka, R. Clay, A. Cerutti, R. Colalillo, A. Coleman, M. Coluccia, R. Conceiccao, A. Condorelli, G. Consolati, F. Contreras, F. Convenga, D. D. Santos, C. Covault, M. Cristinziani, S. Dasso, K. Daumiller, B. Dawson, R. M. Almeida","doi":"10.22323/1.357.0068","DOIUrl":"https://doi.org/10.22323/1.357.0068","url":null,"abstract":"One of the key challenges in astroparticle physics is identifying the sources of cosmic rays at the highest energies (above 10^18 eV). In this context, the search for ultra-high energy photons is of high interest. Observing photons of such energies would impact astrophysics \u0000and particle physics as well as fundamental physics and would be an important contribution to multimessenger astronomy. The Pierre Auger Observatory near Malargue, Argentina, is the largest air-shower experiment for the detection of ultra-high energy cosmic rays. It consists of an array of about 1660 water Cherenkov detectors arranged on a triangular grid which covers an area of more than 3000 km^2. 27 fluorescence telescopes at four sites overlooking the detector array provide an independent and complementary method for air-shower detection. \u0000In the contribution, the various activities at the Pierre Auger Observatory concerning searches for ultra-high energy photons will be presented and the current results will be summarized.","PeriodicalId":257968,"journal":{"name":"Proceedings of The New Era of Multi-Messenger Astrophysics — PoS(Asterics2019)","volume":"52 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2019-08-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"132420380","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}
京公网安备 11010802042870号
京ICP备2023020795号-1
扫码关注我们
求助内容：
应助结果提醒方式：