1,376 research outputs found
Recent Advances in Chromospheric and Coronal Polarization Diagnostics
I review some recent advances in methods to diagnose polarized radiation with
which we may hope to explore the magnetism of the solar chromosphere and
corona. These methods are based on the remarkable signatures that the
radiatively induced quantum coherences produce in the emergent spectral line
polarization and on the joint action of the Hanle and Zeeman effects. Some
applications to spicules, prominences, active region filaments, emerging flux
regions and the quiet chromosphere are discussed.Comment: Review paper to appear in "Magnetic Coupling between the Interior and
the Atmosphere of the Sun", eds. S. S. Hasan and R. J. Rutten, Astrophysics
and Space Science Proceedings, Springer-Verlag, 200
Corrigendum: COVID-19 Confinement and Health Risk Behaviors in Spain
In the original article, the reference for Chen et al. (2009) was incorrectly written as “Chen, P., Mao, L., Nassis, G. P., Harmer, P., Ainsworth, B. E., and Li, F. (2009). Wuhan coronavirus (2019-nCoV): the need to maintain regular physical activity while taking precautions. J. Sport Health Sci. 9, 103–104. doi: 10.1016/j.jshs.2020.02.001”. It should be “Chen, P., Mao, L., Nassis, G. P., Harmer, P., Ainsworth, B. E., and Li, F. (2020). Coronavirus disease (COVID-19): The need to maintain regular physical activity while taking precautions. J. Sport Health Sci. 9, 103–104. doi: 10.1016/j.jshs.2020.02.001”. The authors apologize for this error and state that this does not change the scientific conclusions of the article in any way. The original article has been updated
Aspects of N-partite information in conformal field theories
We present several new results for the -partite information, , of
spatial regions in the ground state of -dimensional conformal field
theories. First, we show that can be written in terms of a single
-point function of twist operators. Using this, we argue that in the limit
in which all mutual separations are much greater than the regions sizes, the
-partite information scales as , where is the
typical distance between pairs of regions and is the lowest primary
scaling dimension. In the case of spherical entangling surfaces, we obtain a
completely explicit formula for the in terms of 2-, 3- and 4-point
functions of the lowest-dimensional primary. Then, we consider a
three-dimensional scalar field in the lattice. We verify the predicted
long-distance scaling and provide strong evidence that is always positive
for general regions and arbitrary for that theory. For the , we find
excellent numerical agreement between our general formula and the lattice
result for disk regions. We also perform lattice calculations of the mutual
information for more general regions and general separations both for a free
scalar and a free fermion, and conjecture that, normalized by the corresponding
disk entanglement entropy coefficients, the scalar result is always greater
than the fermion one. Finally, we verify explicitly the equality between the
-partite information of bulk and boundary fields in holographic theories for
spherical entangling surfaces in general dimensions.Comment: 39 pages + appendices, 12 figure
Deep-learning based reconstruction of the shower maximum Xmax using the water-Cherenkov detectors of the Pierre Auger Observatory
The successful installation, commissioning, and operation of the Pierre Auger Observatory would not have been possible without the strong commitment and effort from the technical and administrative staff in Malargue. We are very grateful to the following agencies and organizations for financial support.
Argentina - Comision Nacional de Energia Atomica; Agencia Nacional de Promocion Cientifica y Tecnologica (ANPCyT); Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET); Gobierno de la Provincia de Mendoza; Municipalidad de Malargue; NDM Holdings and Valle Las Lenas; in gratitude for their continuing cooperation over land access; Australia -the Australian Research Council; Brazil - Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq); Financiadora de Estudos e Projetos (FINEP); Fundacao de Amparo a Pesquisa do Estado de Rio de Janeiro (FAPERJ); Sao Paulo Research Foundation (FAPESP) Grants No. 2019/10151-2, No. 2010/07359-6 and No. 1999/05404-3; Ministerio da Ciencia, Tecnologia, Inovacoes e Comunicacoes (MCTIC); Czech Republic Grant No. MSMT CR LTT18004, LM2015038, LM2018102, CZ.02.1.01/0.0/0.0/16_013/0001402, CZ.02.1.01/0.0/0.0/18_046/0016010 and CZ.02.1.01/0.0/0.0/17_049/0008422; France -Centre de Calcul IN2P3/CNRS; Centre National de la Recherche Scientifique (CNRS); Conseil Regional Ile-de-France; Departement Physique Nucleaire et Corpusculaire (PNC-IN2P3/CNRS); Departement Sciences de l'Univers (SDU-INSU/CNRS); Institut Lagrange de Paris (ILP) Grant No. LABEX ANR-10-LABX-63 within the Investissements d'Avenir Programme Grant No. ANR-11-IDEX-0004-02; Germany-Bundesministerium fur Bildung und Forschung (BMBF); Deutsche Forschungsgemeinschaft (DFG); Finanzministerium Baden-Wurttemberg; Helmholtz Alliance for Astroparticle Physics (HAP); Helmholtz-Gemeinschaft Deutscher Forschungszentren (HGF); Ministerium fur Innovation, Wissenschaft und Forschung des Landes Nordrhein-Westfalen; Ministerium fur Wissenschaft, Forschung und Kunst des Landes Baden-Wurttemberg; Italy - Istituto Nazionale di Fisica Nucleare (INFN); Istituto Nazionale di Astrofisica (INAF); Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR); CETEMPS Center of Excellence; Ministero degli Affari Esteri (MAE); Mexico-Consejo Nacional de Ciencia y Tecnologia (CONACYT) No. 167733; Universidad Nacional Autonoma de Mexico (UNAM); PAPIIT DGAPA-UNAM; The Netherlands - Ministry of Education, Culture and Science; Netherlands Organisation for Scientific Research (NWO); Dutch national e-infrastructure with the support of SURF Cooperative; Poland - Ministry of Science and Higher Education, grant No. DIR/WK/2018/11; National Science Centre, Grants No. 2013/08/M/ST9/00322, No. 2016/23/B/ST9/01635 and No. HARMONIA 5-2013/10/M/ST9/00062, UMO-2016/22/M/ST9/00198; Portugal - Portuguese national funds and FEDER funds within Programa Operacional Factores de Competitividade through Fundacao para a Ciencia e a Tecnologia (COMPETE); Romania-Romanian Ministry of Education and Research, the Program Nucleu within MCI (PN19150201/16N/2019 and PN-19060102) and project PNIII-P1-1.2-PCCDI-2017-0839/19PCCDI/2018 within PNCDI III; Slovenia - Slovenian Research Agency, grants P1-0031, P1-0385, I0-0033, N1-0111; Spain - Ministerio de Economia, Industria y Competitividad (FPA2017-85114-P and PID2019-104676GB-C32, Xunta de Galicia (ED431C 2017/07), Junta de Andalucia (SOMM17/6104/UGR, P18-FR-4314) Feder Funds, RENATA Red Nacional Tematica de Astroparticulas (FPA2015-68783-REDT) and Maria de Maeztu Unit of Excellence (MDM-2016-0692); USA -Department of Energy, Contracts No. DE-AC02-07CH11359, No. DE-FR02-04ER41300, No. DE-FG02-99ER41107 and No. DE-SC0011689; National Science Foundation, Grant No. 0450696; The Grainger Foundation; Marie Curie-IRSES/EPLANET; European Particle Physics Latin American Network; and UNESCO.The atmospheric depth of the air shower maximum X-max is an observable commonly used for the determination of the nuclear mass composition of ultra-high energy cosmic rays. Direct measurements of X-max are performed using observations of the longitudinal shower development with fluorescence telescopes. At the same time, several methods have been proposed for an indirect estimation of X-max from the characteristics of the shower particles registered with surface detector arrays. In this paper, we present a deep neural network (DNN) for the estimation of X-max The reconstruction relies on the signals induced by shower particles in the ground based water-Cherenkov detectors of the Pierre Auger Observatory. The network architecture features recurrent long short-term memory layers to process the temporal structure of signals and hexagonal convolutions to exploit the symmetry of the surface detector array. We evaluate the performance of the network using air showers simulated with three different hadronic interaction models. Thereafter, we account for long-term detector effects and calibrate the reconstructed X-max using fluorescence measurements. Finally, we show that the event-by-event resolution in the reconstruction of the shower maximum improves with increasing shower energy and reaches less than 25 g/cm(2) at energies above 2x10(19) eV.United States Department of Energy (DOE) DE-AC02-07CH11359 - DE-FR02-04ER41300 - DE- FG02-99ER41107 - DE-SC0011689Argentina - Comision Nacional de Energia AtomicaArgentina - Agencia Nacional de Promocion Cientifica y Tecnologica (ANPCyT)Argentina - Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET)Argentina - Gobierno de la Provincia de MendozaArgentina - Municipalidad de MalargueAustralian Research CouncilConselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPQ)
Fundacao de Apoio a Pesquisa do Distrito Federal (FAPDF)Brazil - Financiadora de Estudos e Projetos (FINEP)Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio De Janeiro (FAPERJ)Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) 2019/10151-2-2010/07359-6-1999/05404-3Brazil - Ministerio da Ciencia, Tecnologia, Inovacoes e Comunicacoes (MCTIC)Czech Republic Grant MSMT CR LTT18004 - LM2015038 - LM2018102 - CZ.02.1.01/0.0/0.0/16_013/0001402 - CZ.02.1.01/0.0/0.0/18_046/0016010 - CZ.02.1.01/0.0/0.0/17_049/0008422France - Centre de Calcul IN2P3/CNRSCentre National de la Recherche Scientifique (CNRS)France - Conseil Regional Ile-de-FranceFrance - Departement Physique Nucleaire et Corpusculaire (PNC-IN2P3/CNRS)France - Departement Sciences de l'Univers (SDU-INSU/CNRS)French National Research Agency (ANR) LABEX ANR-10-LABX-63 - ANR-11-IDEX-0004-02Federal Ministry of Education & Research (BMBF)German Research Foundation (DFG)Germany-Finanzministerium Baden-WurttembergGermany-Helmholtz Alliance for Astroparticle Physics (HAP)Germany-Helmholtz-Gemeinschaft Deutscher Forschungszentren (HGF)Germany-Ministerium fur Innovation, Wissenschaft und Forschung des Landes Nordrhein-WestfalenGermany-Ministerium fur Wissenschaft, Forschung und Kunst des Landes Baden-WurttembergItaly - Istituto Nazionale di Fisica Nucleare (INFN)Italy - Istituto Nazionale di Astrofisica (INAF)Italy - Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR)Italy - CETEMPS Center of ExcellenceItaly - Ministero degli Affari Esteri (MAE)Consejo Nacional de Ciencia y Tecnologia (CONACyT) 167733Mexico-Universidad Nacional Autonoma de Mexico (UNAM)Mexico-PAPIIT DGAPA-UNAMThe Netherlands - Ministry of Education, Culture and ScienceNetherlands Organization for Scientific Research (NWO)The Netherlands - SURF CooperativePoland - Ministry of Science and Higher Education DIR/WK/2018/11Poland - National Science Centre 2013/08/M/ST9/00322 - 2016/23/B/ST9/01635 -HARMONIA 5-2013/10/M/ST9/00062 - UMO-2016/22/M/ST9/00198Portugal - Portuguese national fundsPortugal - FEDER funds within Programa Operacional Factores de Competitividade through Fundacao para a Ciencia e a Tecnologia (COMPETE)Romania-Romanian Ministry of Education and ResearchRomania-Program Nucleu within MCI PN19150201/16N/2019 - PN-19060102Romania-PNCDI III PNIII-P1-1.2-PCCDI-2017-0839/19PCCDI/2018Slovenian Research Agency - Slovenia P1-0031 - P1-0385 - I0-0033 - N1-0111Spain - Ministerio de Economia, Industria y Competitividad FPA2017-85114-P - PID2019-104676GB-C32Spain - Xunta de Galicia ED431C 2017/07Junta de Andalucia SOMM17/6104/UGR - P18-FR-4314Spain - RENATA Red Nacional Tematica de Astroparticulas FPA2015-68783-REDTSpain - Maria de Maeztu Unit of Excellence MDM-2016-0692National Science Foundation (NSF) 0450696USA - Grainger FoundationUSA - Marie Curie-IRSES/EPLANETUSA - European Particle Physics Latin American NetworkUSA - UNESCOArgentina - NDM Holdings and Valle Las LenasThe Netherlands - Dutch national e-infrastructureSpain - Feder Fund
Design and implementation of the AMIGA embedded system for data acquisition
The successful installation, commissioning, and operation of the Pierre Auger Observatory would not have been possible without the strong commitment and effort from the technical and admin-istrative staff in Malargtie. We are very grateful to the following agencies and organizations for financial support: Comision Nacional de Energla Atomica, Agencia Nacional de Promocion Cientffica y Tec-nologica (ANPCyT) , Consejo Nacional de Investigaciones Cientfficas y Tecnicas (CONICET) , Gobierno de la Provincia de Mendoza, Municipalidad de Malargtie, NDM Holdings and Valle Las Leilas, in gratitude for their continuing cooperation over land access, Argentina; the Australian Research Council; Conselho Nacional de Desenvolvimento Cientffico e Tecnologico (CNPq) , Fi-nanciadora de Estudos e Projetos (FINEP) , FundagAo de Amparo a Pesquisa do Estado de Rio de Janeiro (FAPERJ) , SAo Paulo Research Foundation (FAPESP) Grants No. 2010/07359-6 and No. 1999/05404-3, Ministerio de Ciencia e Tecnologia (MCT) , Brazil; Grant No.MSMT CR LG15014, LO1305 and LM2015038 and the Czech Science Foundation Grant No. 14-17501S, Czech Republic; Centre de Calcul IN2P3/CNRS, Centre National de la Recherche Scientifique (CNRS) , Conseil Regional Ile-de-France, Departement Physique Nucleaire et Corpusculaire (PNC-IN2P3/CNRS) , Departement Sciences de l'Univers (SDU-INSU/CNRS) , Institut Lagrange de Paris (ILP) Grant No. LABEX ANR-10-LABX-63, within the Investissements d'Avenir Programme Grant No. ANR-11-IDEX-0004-02, France; Bundesministerium fur Bildung und Forschung (BMBF) , Deutsche Forschungsgemeinschaft (DFG) , Finanzministerium Baden-Wurttemberg, Helmholtz Al-liance for Astroparticle Physics (HAP) , Helmholtz-Gemeinschaft Deutscher Forschungszentren (HGF) , Ministerium fur Wissenschaft und Forschung, Nordrhein Westfalen, Ministerium fur Wis-senschaft, Forschung und Kunst, Baden-Wurttemberg, Germany; Istituto Nazionale di Fisica Nu-cleare (INFN) ,Istituto Nazionale di Astrofisica (INAF) , Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR) , Gran Sasso Center for Astroparticle Physics (CFA) , CETEMPS Cen-ter of Excellence, Ministero degli Affari Esteri (MAE) , Italy; Consejo Nacional de Ciencia y Tecnologia (CONACYT) No. 167733, Mexico; Universidad Nacional Autonoma de Mexico (UNAM) , PAPIIT DGAPA-UNAM, Mexico; Ministerie van Onderwijs, Cultuur en Wetenschap, Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO) , Stichting voor Fundamenteel Onderzoek der Materie (FOM) , Netherlands; National Centre for Research and Development, Grants No. ERA-NET-ASPERA/01/11 and No. ERA-NET-ASPERA/02/11, National Science Cen-tre, Grants No. 2013/08/M/ST9/00322, No. 2013/08/M/ST9/00728 and No. HARMONIA 5 - 2013/10/M/ST9/00062, Poland; Portuguese national funds and FEDER funds within Programa Operacional Factores de Competitividade through Fundagdo para a Ciencia e a Tecnologia (COM-PETE) , Portugal; Romanian Authority for Scientific Research ANCS, CNDI-UEFISCDI partner-ship projects Grants No. 20/2012 and No.194/2012 and PN 16 42 01 02; Slovenian Research Agency, Slovenia; Comunidad de Madrid, Fondo Europeo de Desarrollo Regional (FEDER) funds, Ministerio de Economia y Competitividad, Xunta de Galicia, European Community 7th Frame-work Program, Grant No. FP7-PEOPLE-2012-IEF-328826, Spain; Science and Technology Fa-cilities Council, United Kingdom; Department of Energy, Contracts No. DE-AC02-07CH11359, No. DE-FR02-04ER41300, No. DE-FG02-99ER41107 and No. DE-SC0011689, National Science Foundation, Grant No. 0450696, The Grainger Foundation, U.S.A.
; NAFOSTED, Vietnam; Marie Curie-IRSES/EPLANET, European Particle Physics Latin American Network, European Union 7th Framework Program, Grant No. PIRSES-2009-GA-246806; and UNESCO.The Auger Muon Infill Ground Array (AMIGA) is part of the AugerPrime upgrade of
the Pierre Auger Observatory. It consists of particle counters buried 2.3m underground next to the
water-Cherenkov stations that form the 23.5 km2 large infilled array. The reduced distance between
detectors in this denser area allows the lowering of the energy threshold for primary cosmic ray
reconstruction down to about 1017 eV. At the depth of 2.3m the electromagnetic component of
cosmic ray showers is almost entirely absorbed so that the buried scintillators provide an independent
and direct measurement of the air showers muon content. This work describes the design
and implementation of the AMIGA embedded system, which provides centralized control, data
acquisition and environment monitoring to its detectors. The presented system was firstly tested in
the engineering array phase ended in 2017, and lately selected as the final design to be installed in
all new detectors of the production phase. The system was proven to be robust and reliable and has
worked in a stable manner since its first deployment.Comision Nacional de Energla AtomicaANPCyTConsejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET)Gobierno de la Provincia de MendozaMunicipalidad de MalargtieNDM HoldingsAustralian Research CouncilConselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPQ)Financiadora de Inovacao e Pesquisa (Finep)Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) 2010/07359-6
1999/05404-3Ministerio de Ciencia e Tecnologia (MCT) , BrazilGrant Agency of the Czech Republic
Czech Republic Government 14-17501SCentre de Calcul IN2P3/CNRSCentre National de la Recherche Scientifique (CNRS)
Region Ile-de-France
Departement Physique Nucleaire et Corpusculaire PNC-IN2P3/CNRS
Departement Sciences de l'Univers (SDU-INSU/CNRS)
French National Research Agency (ANR) LABEX ANR-10-LABX-63
ANR-11-IDEX-0004-02Federal Ministry of Education & Research (BMBF)German Research Foundation (DFG)
Finanzministerium Baden-Wurttemberg, Helmholtz Al-liance for Astroparticle Physics (HAP)
Helmholtz Association
Ministerium fur Wissenschaft und Forschung, Nordrhein Westfalen
Ministerium fur Wis-senschaft, Forschung und Kunst, Baden-Wurttemberg, GermanyIstituto Nazionale di Fisica Nucleare (INFN)
Istituto Nazionale Astrofisica (INAF)Ministry of Education, Universities and Research (MIUR)Gran Sasso Center for Astroparticle Physics (CFA)CETEMPS Cen-ter of ExcellenceMinistry of Foreign Affairs and International Cooperation (Italy)Consejo Nacional de Ciencia y Tecnologia (CONACyT) 167733Mexico; Universidad Nacional Autonoma de Mexico (UNAM)Programa de Apoyo a Proyectos de Investigacion e Innovacion Tecnologica (PAPIIT)Universidad Nacional Autonoma de MexicoMinisterie van Onderwijs, Cultuur en Wetenschap
Netherlands Organization for Scientific Research (NWO)
FOM (The Netherlands)
Netherlands GovernmentNational Centre for Research & Development, Poland ERA-NET-ASPERA/01/11
ERA-NET-ASPERA/02/11National Science Centre, Poland 2013/08/M/ST9/00322
2013/08/M/ST9/00728
HARMONIA 5 - 2013/10/M/ST9/00062Portuguese national fundsFEDER funds within Programa Operacional Factores de Competitividade through Fundagdo para a Ciencia e a Tecnologia (COM-PETE) , PortugalRomanian Authority for Scientific Research ANCSConsiliul National al Cercetarii Stiintifice (CNCS)
Unitatea Executiva pentru Finantarea Invatamantului Superior, a Cercetarii, Dezvoltarii si Inovarii (UEFISCDI) 20/2012
194/2012
PN 16 42 01 02Slovenian Research Agency - SloveniaComunidad de MadridFondo Europeo de Desarrollo Regional (FEDER) funds, Ministerio de Economia y Competitividad,Xunta de Galicia ,European Community 7th Frame-work Program FP7-PEOPLE-2012-IEF-328826UK Research & Innovation (UKRI)Science & Technology Facilities Council (STFC)United States Department of Energy (DOE) DE-FG02-99ER41107
DE-SC0011689National Science Foundation (NSF) 0450696Grainger Foundation, U.S.ANational Foundation for Science & Technology Development (NAFOSTED)Marie Curie-IRSES/EPLANETEuropean Particle Physics Latin American Network
European Commission PIRSES-2009-GA-246806UNESCOMSMT CR LG15014
LO1305
LM201503
Design, upgrade and characterization of the silicon photomultiplier front-end for the AMIGA detector at the Pierre Auger Observatory
The successful installation, commissioning, and operation of the Pierre Auger Observatory would not have been possible without the strong commitment and effort from the technical and administrative staff in Malargue. We are very grateful to the following agencies and organizations for financial support:
Argentina -Comision Nacional de Energia Atomica; Agencia Nacional de Promocion Cientifica y Tecnologica (ANPCyT); Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET); Gobierno de la Provincia de Mendoza; Municipalidad de Malargue; NDM Holdings and Valle Las Lenas; in gratitude for their continuing cooperation over land access; Australia -the Australian Research Council; Brazil -Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq); Financiadora de Estudos e Projetos (FINEP); Fundacao de Amparo a Pesquisa do Estado de Rio de Janeiro (FAPERJ); Sao Paulo Research Foundation (FAPESP) Grants No. 2019/10151-2, No. 2010/07359-6 and No. 1999/05404-3; Ministerio da Ciencia, Tecnologia, Inovacoes e Comunicacoes (MCTIC); Czech Republic Grant No. MSMT CR LTT18004, LM2015038, LM2018102, CZ.02.1.01/0.0/0.0/16_013/0001402, CZ.02.1.01/0.0/0.0/18_046/0016010 and CZ.02.1.01/0.0/0.0/17_049/0008422; France -Centre de Calcul IN2P3/CNRS; Centre National de la Recherche Scientifique (CNRS); Conseil Regional Ile-de-France; Departement Physique Nucleaire et Corpusculaire (PNC-IN2P3/CNRS); Departement Sciences de l'Univers (SDU-INSU/CNRS); Institut Lagrange de Paris (ILP) Grant No. LABEX ANR-10-LABX-63 within the Investissements d'Avenir Programme Grant No. ANR-11-IDEX-0004-02; Germany-Bundesministerium fur Bildung und Forschung (BMBF); Deutsche Forschungsgemeinschaft (DFG); Finanzministerium Baden-Wurttemberg; Helmholtz Alliance for Astroparticle Physics (HAP); Helmholtz-Gemeinschaft Deutscher Forschungszentren (HGF); Ministerium fur Innovation, Wissenschaft und Forschung des Landes Nordrhein-Westfalen; Ministerium fur Wissenschaft, Forschung und Kunst des Landes Baden-Wurttemberg; Italy-Istituto Nazionale di Fisica Nucleare (INFN); Istituto Nazionale di Astrofisica (INAF); Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR); CETEMPS Center of Excellence; Ministero degli Affari Esteri (MAE); Mexico-Consejo Nacional de Ciencia y Tecnologia (CONACYT) No. 167733; Universidad Nacional Autonoma de Mexico (UNAM); PAPIIT DGAPA-UNAM; The Netherlands -Ministry of Education, Culture and Science; Netherlands Organisation for Scientific Research (NWO); Dutch national e-infrastructure with the support of SURF Cooperative; Poland-Ministry of Science and Higher Education, grant No. DIR/WK/2018/11; National Science Centre, Grants No. 2013/08/M/ST9/00322, No. 2016/23/B/ST9/01635 and No. HARMONIA 5-2013/10/M/ST9/00062, UMO-2016/22/M/ST9/00198; Portugal -Portuguese national funds and FEDER funds within Programa Operacional Factores de Competitividade through Fundacao para a Ciencia e a Tecnologia (COMPETE); Romania-Romanian Ministry of Education and Research, the Program Nucleu within MCI(PN19150201/16N/2019 and PN19060102) and project PN-III-P1-1.2-PCCDI-2017-0839/19PCCDI/2018 within PNCDI III; Slovenia -Slovenian Research Agency, grants P1-0031, P1-0385, I0-0033, N1-0111; Spain-Ministerio de Economia, Industria y Competitividad (FPA2017-85114-P and FPA2017-85197-P), Xunta de Galicia (ED431C 2017/07), Junta de Andalucia (SOMM17/6104/UGR), Feder Funds, RENATA Red Nacional Tematica de Astroparticulas (FPA2015-68783-REDT) and Maria de Maeztu Unit of Excellence (MDM-2016-0692); U.S.A. -Department of Energy, Contracts No. DE-AC02-07CH11359, No. DE-FR02-04ER41300, No. DE-FG02-99ER41107 and No. DE-SC0011689; National Science Foundation, Grant No. 0450696; The Grainger Foundation; Marie Curie-IRSES/EPLANET; European Particle Physics Latin American Network; and UNESCO.AMIGA (Auger Muons and Infill for the Ground Array) is an upgrade of the Pierre Auger Observatory to complement the study of ultra-high-energy cosmic rays (UHECR) by measuring the muon content of extensive air showers (EAS). It consists of an array of 61 water Cherenkov detectors on a denser spacing in combination with underground scintillation detectors used for muon density measurement. Each detector is composed of three scintillation modules, with 10 m(2) detection area per module, buried at 2.3 m depth, resulting in a total detection area of 30 m(2). Silicon photomultiplier sensors (SiPM) measure the amount of scintillation light generated by charged particles traversing the modules. In this paper, the design of the front-end electronics to process the signals of those SiPMs and test results from the laboratory and from the Pierre Auger Observatory are described. Compared to our previous prototype, the new electronics shows a higher performance, higher efficiency and lower power consumption, and it has a new acquisition system with increased dynamic range that allows measurements closer to the shower core. The new acquisition system is based on the measurement of the total charge signal that the muonic component of the cosmic ray shower generates in the detector.Argentina - Comision Nacional de Energia AtomicaArgentina - Agencia Nacional de Promocion Cientifica y Tecnologica (ANPCyT)Argentina - Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET)Argentina - Gobierno de la Provincia de MendozaArgentina - Municipalidad de MalargueArgentina - NDM HoldingsArgentina - Valle Las LenasAustralian Research CouncilConselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPQ)
Fundacao de Apoio a Pesquisa do Distrito Federal (FAPDF)
Brazil - Financiadora de Estudos e Projetos (FINEP)Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio De Janeiro (FAPERJ)Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) 2019/10151-2
2010/07359-6
1999/05404-3Brazil - Ministerio da Ciencia, Tecnologia, Inovacoes e Comunicacoes (MCTIC)Brazil - Czech Republic Grant MSMT CR LTT18004
LM2015038
LM2018102
CZ.02.1.01/0.0/0.0/16_013/0001402
CZ.02.1.01/0.0/0.0/18_046/0016010
CZ.02.1.01/0.0/0.0/17_049/0008422France - Centre de Calcul IN2P3/CNRSCentre National de la Recherche Scientifique (CNRS)France - Conseil Regional Ile-de-FranceFrance - Departement Physique Nucleaire et Corpusculaire (PNC-IN2P3/CNRS)France - Departement Sciences de l'Univers (SDU-INSU/CNRS)French National Research Agency (ANR) LABEX ANR-10-LABX-63Institut Lagrange de Paris (ILP) within the Investissements d'Avenir Programme
ANR-11-IDEX-0004-02Federal Ministry of Education & Research (BMBF)Bundesministerium fur Bildung und Forschung (BMBF)German Research Foundation (DFG)Germany - Finanzministerium Baden-WurttembergGermany - Helmholtz Alliance for Astroparticle Physics (HAP)Germany - Helmholtz-Gemeinschaft Deutscher Forschungszentren (HGF)Germany - Ministerium fur Innovation, Wissenschaft und Forschung des Landes Nordrhein-WestfalenGermany - Ministerium fur Wissenschaft, Forschung und Kunst des Landes Baden-WurttembergItaly - Istituto Nazionale di Fisica Nucleare (INFN)Italy - Istituto Nazionale di Astrofisica (INAF)Italy - Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR)Italy - CETEMPS Center of ExcellenceConsejo Nacional de Ciencia y Tecnologia (CONACyT) 167733Mexico - Universidad Nacional Autonoma de Mexico (UNAM)Mexico - PAPIIT DGAPA-UNAMNetherlands - Ministry of Education, Culture and ScienceNetherlands Organization for Scientific Research (NWO)Netherlands Organisation for Scientific Research (NWO)The Netherlands - SURF CooperativePoland - Ministry of Science and Higher Education DIR/WK/2018/11
Poland - National Science Centre 2013/08/M/ST9/00322
2016/23/B/ST9/01635
HARMONIA 5-2013/10/M/ST9/00062
UMO-2016/22/M/ST9/00198Portugal - Portuguese national funds
Portugal - FEDER funds within Programa Operacional Factores de Competitividade through Fundacao para a Ciencia e a Tecnologia (COMPETE)Romania - Romanian Ministry of Education and Research
Romania - Program Nucleu within MCI PN19150201/16N/2019
PN19060102
Romania - PNCDI III PN-III-P1-1.2-PCCDI-2017-0839/19PCCDI/2018Slovenian Research Agency - Slovenia P1-0031
P1-0385
I0-0033
N1-0111Spain - Ministerio de Economia, Industria y Competitividad FPA2017-85114-P
FPA2017-85197-PSpain - Xunta de Galicia ED431C 2017/07Junta de Andalucia SOMM17/6104/UGRSpain - Feder FundsSpain - RENATA Red Nacional Tematica de Astroparticulas FPA2015-68783-REDTSpain - Maria de Maeztu Unit of Excellence MDM-2016-0692United States Department of Energy (DOE) DE-AC02-07CH11359National Science Foundation (NSF) 0450696U.S.A. - Grainger Foundation
U.S.A. - Marie Curie-IRSES/EPLANET
U.S.A. - European Particle Physics Latin American Network
U.S.A. - UNESCOItaly - Ministero degli Affari Esteri (MAE)The Netherlands - Dutch national e-infrastructur
Anomalous circular polarization profiles in the He I 1083.0 nm multiplet from solar spicules
We report Stokes vector observations of solar spicules and a prominence in
the He I 1083 nm multiplet carried out with the Tenerife Infrared Polarimeter.
The observations show linear polarization profiles that are produced by
scattering processes in the presence of a magnetic field. After a careful data
reduction, we demonstrate the existence of extremely asymmetric Stokes V
profiles in the spicular material that we are able to model with two magnetic
components along the line of sight, and under the presence of atomic
orientation in the energy levels that give rise to the multiplet. We discuss
some possible scenarios that can generate the atomic orientation in spicules.
We stress the importance of spectropolarimetric observations across the limb to
distinguish such signals from observational artifacts.Comment: accepted for publication in Ap
Systematic identification of phenotypically enriched loci using a patient network of genomic disorders
Background
Network medicine is a promising new discipline that combines systems biology approaches and network science to understand the complexity of pathological phenotypes. Given the growing availability of personalized genomic and phenotypic profiles, network models offer a robust integrative framework for the analysis of "omics" data, allowing the characterization of the molecular aetiology of pathological processes underpinning genetic diseases.
Methods
Here we make use of patient genomic data to exploit different network-based analyses to study genetic and phenotypic relationships between individuals. For this method, we analyzed a dataset of structural variants and phenotypes for 6,564 patients from the DECIPHER database, which encompasses one of the most comprehensive collections of pathogenic Copy Number Variations (CNVs) and their associated ontology-controlled phenotypes. We developed a computational strategy that identifies clusters of patients in a synthetic patient network according to their genetic overlap and phenotype enrichments.
Results
Many of these clusters of patients represent new genotype-phenotype associations, suggesting the identification of newly discovered phenotypically enriched loci (indicative of potential novel syndromes) that are currently absent from reference genomic disorder databases such as ClinVar, OMIM or DECIPHER itself.
Conclusions
We provide a high-resolution map of pathogenic phenotypes associated with their respective significant genomic regions and a new powerful tool for diagnosis of currently uncharacterized mutations leading to deleterious phenotypes and syndromes
Removal of Spectro-Polarimetric Fringes by 2D Pattern Recognition
We present a pattern-recognition based approach to the problem of removal of
polarized fringes from spectro-polarimetric data. We demonstrate that 2D
Principal Component Analysis can be trained on a given spectro-polarimetric map
in order to identify and isolate fringe structures from the spectra. This
allows us in principle to reconstruct the data without the fringe component,
providing an effective and clean solution to the problem. The results presented
in this paper point in the direction of revising the way that science and
calibration data should be planned for a typical spectro-polarimetric observing
run.Comment: ApJ, in pres
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