96 research outputs found
Cerenkov Events Seen by The TALE Air Fluorescence Detector
The Telescope Array Low-Energy Extension (TALE) is a hybrid, Air Fluorescence
Detector (FD) / Scintillator Array, designed to study cosmic ray initiated
showers at energies above eV. Located in the western Utah
desert, the TALE FD is comprised of 10 telescopes which cover the elevation
range 31-58 in addition to 14 telescopes with elevation coverage of
3-31.
As with all other FD's, a subset of the shower events recorded by TALE are
ones for which the Cerenkov light produced by the shower particles dominates
the total observed light signal. In fact, for the telescopes with higher
elevation coverage, low energy Cerenkov events form the vast majority of
triggered cosmic ray events. In the typical FD data analysis procedure, this
subset of events is discarded and only events for which the majority of signal
photons come from air fluorescence are kept.
In this talk, I will report on a study to reconstruct the "Cerenkov Events"
seen by the high elevation viewing telescopes of TALE. Monte Carlo studies and
a first look at real events observed by TALE look very promising. Even as a
monocular detector, the geometrical reconstruction method employed in this
analysis allows for a pointing accuracy on the order of a degree. Preliminary
Monte Carlo studies indicate that, the expected energy resolution is better
than 25. It may be possible to extend the low energy reach of TALE to below
eV. This would be the first time a detector designed specifically as
an air fluorescence detector is used as an imaging Cerenkov detector.Comment: Presentation at the DPF 2013 Meeting of the American Physical Society
Division of Particles and Fields, Santa Cruz, California, August 13-17, 2013.
5 pages, 2 figure
Search for Spatial Correlations of Neutrinos with Ultra-high-energy Cosmic Rays
For several decades, the origin of ultra-high-energy cosmic rays (UHECRs) has been an unsolved question of high-energy astrophysics. One approach for solving this puzzle is to correlate UHECRs with high-energy neutrinos, since neutrinos are a direct probe of hadronic interactions of cosmic rays and are not deflected by magnetic fields. In this paper, we present three different approaches for correlating the arrival directions of neutrinos with the arrival directions of UHECRs. The neutrino data are provided by the IceCube Neutrino Observatory and ANTARES, while the UHECR data with energies above similar to 50 EeV are provided by the Pierre Auger Observatory and the Telescope Array. All experiments provide increased statistics and improved reconstructions with respect to our previous results reported in 2015. The first analysis uses a high-statistics neutrino sample optimized for point-source searches to search for excesses of neutrino clustering in the vicinity of UHECR directions. The second analysis searches for an excess of UHECRs in the direction of the highest-energy neutrinos. The third analysis searches for an excess of pairs of UHECRs and highest-energy neutrinos on different angular scales. None of the analyses have found a significant excess, and previously reported overfluctuations are reduced in significance. Based on these results, we further constrain the neutrino flux spatially correlated with UHECRs
CPT and Lorentz violation in the electroweak sector
Long ago, Carroll, Field and Jackiw introduced CPT-violation in the photon sector by adding a dimension-3 gauge-invariant term parametrized by a constant four-vector parameter k(AF) to the usual (Maxwell) Lagrangian, deriving an ultra-tight bound from astrophysical data. Here, we will discuss recent work studying the extension of this term to the full electroweak gauge sector of the Standard Model. In the context of the Standard Model Extension, CPT and Lorentz violation arises from two gauge-invariant terms parametrized by the four vectors k(1) and k(2). First we will show how upon spontaneous breaking of the electroweak gauge symmetry these two terms yield Lorentz-violating terms for the photon and the W and Z bosons. As it turns out, the resulting modified dispersion relations for the W bosons yield spacelike momentum for one of its propagating modes at sufficiently large energy. This in turn allows for the possibility of Cherenkov-like W-boson emission by high-energy fermions such as protons, provoking their decay. Analysis of ultra-high-energy cosmic ray data allows for bounding the previously unbound parameter k(2), and, by combination with the ultra-tight bound on k(AF), the parameter k(1).Portuguese Fundacao para a Ciencia e a Tecnologia (FCT) - SFRH/BPD/101403/2014program POPH/FSE
New College of Floridainfo:eu-repo/semantics/publishedVersio
Search for Spatial Correlations of Neutrinos with Ultra-high-energy Cosmic Rays
For several decades, the origin of ultra-high-energy cosmic rays (UHECRs) has been an unsolved question of highenergy
astrophysics. One approach for solving this puzzle is to correlate UHECRs with high-energy neutrinos,
since neutrinos are a direct probe of hadronic interactions of cosmic rays and are not deflected by magnetic fields.
In this paper, we present three different approaches for correlating the arrival directions of neutrinos with the
arrival directions of UHECRs. The neutrino data are provided by the IceCube Neutrino Observatory and
ANTARES, while the UHECR data with energies above âŒ50 EeV are provided by the Pierre Auger Observatory
and the Telescope Array. All experiments provide increased statistics and improved reconstructions with respect to
our previous results reported in 2015. The first analysis uses a high-statistics neutrino sample optimized for pointsource
searches to search for excesses of neutrino clustering in the vicinity of UHECR directions. The second
analysis searches for an excess of UHECRs in the direction of the highest-energy neutrinos. The third analysis
searches for an excess of pairs of UHECRs and highest-energy neutrinos on different angular scales. None of the analyses have found a significant excess, and previously reported overfluctuations are reduced in significance.
Based on these results, we further constrain the neutrino flux spatially correlated with UHECRs.Centre National
de la Recherche Scientifique (CNRS), Commissariat Ă lâĂ©nergie
atomique et aux Ă©nergies alternatives (CEA), Commission
Européenne (FEDER fund and Marie Curie Program), Institut
Universitaire de France (IUF), LabEx UnivEarthS (ANR-10-
LABX-0023 and ANR-18-IDEX-0001), RĂ©gion IÌle-de-France
(DIM-ACAV), RĂ©gion Alsace (contrat CPER), RĂ©gion Provence-
Alpes-CĂŽte dâAzur, DĂ©partement du Var and Ville de La
Seyne-sur-Mer, FranceBundesministerium fĂŒr Bildung und
Forschung (BMBF), GermanyIstituto Nazionale di Fisica
Nucleare (INFN), ItalyNederlandse organisatie voor
Wetenschappelijk Onderzoek (NWO), the NetherlandsCouncil
of the President of the Russian Federation for young
scientists and leading scientific schools supporting grants,
RussiaExecutive Unit for Financing Higher Education,
Research, Development and Innovation (UEFISCDI), RomaniaMinisterio de Ciencia, InnovaciĂłn, InvestigaciĂłn y
Universidades (MCIU): Programa Estatal de GeneraciĂłn de
Conocimiento (refs. PGC2018-096663-B-C41, -A-C42, -BC43,
-B-C44) (MCIU/FEDER), Generalitat Valenciana: Prometeo
(PROMETEO/2020/019), GrisolĂa (refs. GRISOLIA/
2018/119, /2021/192) and GenT (refs. CIDEGENT/2018/
034, /2019/043, /2020/049, /2021/023) programs, Junta de
AndalucĂa (ref. A-FQM-053-UGR18), La Caixa Foundation
(ref. LCF/BQ/IN17/11620019), EU: MSC program (ref.
101025085), SpainMinistry of Higher Education, Scientific
Research and Innovation, Morocco, and the Arab Fund for
Economic and Social Development, KuwaitU.S. National Science Foundation-Office of
Polar Programs, U.S. National Science Foundation-Physics
Division, U.S. National Science Foundation-EPSCoR, Wisconsin
Alumni Research Foundation, Center for High Throughput
Computing (CHTC) at the University of WisconsinâMadison,
Open Science Grid (OSG), Extreme Science and Engineering
Discovery Environment (XSEDE), Frontera computing project at
the Texas Advanced Computing Center, U.S. Department of
EnergyâNational Energy Research Scientific Computing Center,
Particle astrophysics research computing center at the University
of Maryland, Institute for Cyber-Enabled Research at Michigan
State University, and Astroparticle physics computational facility
at Marquette UniversityBelgiumâFunds for Scientific Research
(FRS-FNRS and FWO), FWO Odysseus and Big Science
programmes, and Belgian Federal Science Policy Office (Belspo)GermanyâBundesministerium fĂŒr Bildung und Forschung
(BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz
Alliance for Astroparticle Physics (HAP), Initiative and Networking
Fund of the Helmholtz Association, Deutsches Elektronen
Synchrotron (DESY), and High Performance Computing cluster
of the RWTH AachenSwedenâSwedish Research Council,
Swedish Polar Research Secretariat, Swedish National Infrastructure
for Computing (SNIC), and Knut and Alice Wallenberg
FoundationAustraliaâAustralian Research CouncilCanadaâ
Natural Sciences and Engineering Research Council of Canada,
Calcul Québec, Compute Ontario, Canada Foundation for
Innovation, WestGrid, and Compute CanadaDenmarkâVillum
Fonden and Carlsberg FoundationNew ZealandâMarsden
FundJapanâJapan Society for Promotion of Science (JSPS)
and Institute for Global Prominent Research (IGPR) of Chiba
UniversityKoreaâNational Research Foundation of Korea
(NRF)SwitzerlandâSwiss National Science Foundation
(SNSF)United KingdomâDepartment of Physics, University
of OxfordArgentinaâComisiĂłn Nacional de EnergĂa AtĂłmica; Agencia
Nacional de PromociĂłn CientĂfica y TecnolĂłgica (ANPCyT);
Consejo Nacional de Investigaciones CientĂficas y TĂ©cnicas
(CONICET); Gobierno de la Provincia de Mendoza; Municipalidad
de MalargĂŒe; NDM Holdings and Valle Las Leñas; in
gratitude for their continuing cooperation over land access;
Australiaâthe Australian Research Council;BelgiumâFonds de
la Recherche Scientifique (FNRS); Research Foundation Flanders
(FWO)BrazilâConselho Nacional de Desenvolvimento CientĂfico
e TecnolĂłgico (CNPq)Financiadora de Estudos e Projetos
(FINEP)Fundação de Amparo à Pesquisa do Estado de Rio de
Janeiro (FAPERJ); SĂŁo Paulo Research Foundation (FAPESP)
Grants No. 2019/10151-2, No. 2010/07359-6 and No. 1999/
05404-3; MinistĂ©rio da CiĂȘncia, Tecnologia, InovaçÔes e
ComunicaçÔes (MCTIC)Czech RepublicâGrant 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_049/0008422FranceâCentre de Calcul
IN2P3/CNRSCentre National de la Recherche Scientifique
(CNRS); Conseil RĂ©gional Ile-de-France; DĂ©partement Physique
Nucléaire et Corpusculaire (PNC-IN2P3/CNRS); Département
Sciences de lâUnivers (SDU-INSU/CNRS); Institut Lagrange de
Paris (ILP) Grant No. LABEX ANR-10-LABX-63 within the
Investissements dâAvenir Programme Grant No. ANR-11-IDEX-
0004-02GermanyâBundesministerium fĂŒr Bildung und Forschung
(BMBF); Deutsche Forschungsgemeinschaft (DFG);
Finanzministerium Baden-WĂŒrttemberg; Helmholtz Alliance for
Astroparticle Physics (HAP); Helmholtz-Gemeinschaft Deutscher
Forschungszentren (HGF); Ministerium fĂŒr Innovation, Wissenschaft
und Forschung des Landes Nordrhein-Westfalen;
Ministerium fĂŒr Wissenschaft, Forschung und Kunst des Landes
Baden-WĂŒrttembergItalyâIstituto Nazionale di Fisica Nucleare (INFN); Istituto Nazionale di Astrofisica (INAF); Ministero
dellâIstruzione, dellâUniversitĂĄ e della Ricerca (MIUR);
CETEMPS Center of Excellence; Ministero degli Affari Esteri
(MAE)MĂ©xicoâConsejo Nacional de Ciencia y TecnologĂa
(CONACYT) No. 167733; Universidad Nacional AutĂłnoma de
MĂ©xico (UNAM)PAPIIT DGAPA-UNAMThe Netherlandsâ
Ministry of Education, Culture and Science; Netherlands
Organisation for Scientific Research (NWO); Dutch national
e-infrastructure with the support of SURF CooperativePoland
âMinistry of Education and Science, grant No. DIR/WK/
2018/11National Science Centre, Grants No. 2016/22/M/
ST9/00198, 2016/23/B/ST9/01635, and 2020/39/B/ST9/
01398PortugalâPortuguese national funds and FEDER funds
within Programa Operacional Factores de Competitividade
through Fundação para a CiĂȘncia e a Tecnologia (COMPETE)RomaniaâMinistry of Research, Innovation and Digitization,
CNCS/CCCDIâUEFISCDI, projects PN19150201/16N/
2019, PN1906010, TE128 and PED289, within PNCDI IIISloveniaâSlovenian Research Agency, grants P1-0031, P1-
0385, I0-0033, N1-0111SpainâMinisterio de EconomĂa,
Industria y Competitividad (FPA2017-85114-P and PID2019-
104676GB-C32), Xunta de Galicia (ED431C 2017/07), Junta
de AndalucĂa (SOMM17/6104/UGR, P18-FR-4314) Feder
Funds, RENATA Red Nacional TemĂĄtica de AstropartĂculas
(FPA2015-68783-REDT) and MarĂa de Maeztu Unit of
Excellence (MDM-2016-0692)USAâDepartment of Energy,
Contracts No. DE-AC02-07CH11359, No. DE-FR02-04ER41
300, 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.Japan
Society for the Promotion of Science (JSPS) through Grants-in-
Aid for Priority Area 431, for Specially Promoted Research
JP21000002, for Scientific Research (S) JP19104006, for
Specially Promoted Research JP15H05693, for Scientific
Research (S) JP15H05741, for Science Research (A)
JP18H03705, for Young Scientists (A) JPH26707011, and for
Fostering Joint International Research (B) JP19KK0074, by the
joint research program of the Institute for Cosmic Ray Research
(ICRR), The University of Tokyo; by the Pioneering Program of
RIKEN for the Evolution of Matter in the Universe (r-EMU)U.S. National Science Foundation awards PHY-1404495,
PHY-1404502, PHY-1607727, PHY-1712517, PHY-1806797,
PHY-2012934, and PHY-2112904National Research
Foundation of Korea (2017K1A4A3015188, 2020R1A2C1
008230, and 2020R1A2C2102800)Ministry of Science
and Higher Education of the Russian Federation under the
contract 075-15-2020-778, IISN project No. 4.4501.18Belgian Science Policy under IUAP VII/37 (ULB
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