000570294 001__ 570294
000570294 005__ 20230219005323.0
000570294 0247_ $$2INSPIRETeX$$aBlank:2023dxn
000570294 0247_ $$2inspire$$ainspire:2626781
000570294 0247_ $$2arXiv$$aarXiv:2301.11002
000570294 0247_ $$2altmetric$$aaltmetric:141824564
000570294 037__ $$aPUBDB-2023-00657
000570294 041__ $$aEnglish
000570294 082__ $$a520
000570294 088__ $$2arXiv$$aarXiv:2301.11002
000570294 1001_ $$aBlank, M.$$b0
000570294 245__ $$aDetection of the Crab Nebula using a Random Forest Analysis of the first TAIGA IACT Data
000570294 260__ $$c2023
000570294 3367_ $$0PUB:(DE-HGF)25$$2PUB:(DE-HGF)$$aPreprint$$bpreprint$$mpreprint$$s1676298728_29393
000570294 3367_ $$2ORCID$$aWORKING_PAPER
000570294 3367_ $$028$$2EndNote$$aElectronic Article
000570294 3367_ $$2DRIVER$$apreprint
000570294 3367_ $$2BibTeX$$aARTICLE
000570294 3367_ $$2DataCite$$aOutput Types/Working Paper
000570294 500__ $$a8 pages, 9 figures, accepted by MNRAS  10.1093/mnras/stad276
000570294 520__ $$aThe Tunka Advanced Instrument for Gamma- and cosmic-ray Astronomy (TAIGA) is a multicomponent experiment for the measurement of TeV to PeV gamma- and cosmic rays. Our goal is to establish a novel hybrid direct air shower technique, sufficient to access the energy domain of the long-sought Pevatrons. The hybrid air Cherenkov light detection technique combines the strengths of the HiSCORE shower front sampling array, and two $\thicksim$4 m class, $\sim$9.6 deg field of view Imaging Air Cherenkov Telescopes (IACTs). The HiSCORE array provides good angular and shower core position resolution, while the IACTs provide the image shape and orientation for gamma-hadron separation. In future, an additional muon detector will be used for hadron tagging at $\ge$ 100 TeV energies. Here, only data from the first IACT of the TAIGA experiment are used. A random forest algorithm was trained using Monte Carlo (MC) simulations and real data, and applied to 85 h of selected observational data tracking the Crab Nebula at a mean zenith angle of 33.5 deg, resulting in a threshold energy of 6 TeV for this dataset. The analysis was performed using the gammapy package. A total of 163.5 excess events were detected, with a statistical significance of 8.5 sigma. The observed spectrum of the Crab Nebula is best fit with a power law above 6 TeV with a flux normalisation of $(3.20\pm0.42)\cdot10^{-10} TeV^{-1} cm^{-2} s^{-1})$ at a reference energy of 13 TeV and a spectral index of $-2.74\pm0.16$.
000570294 536__ $$0G:(DE-HGF)POF4-613$$a613 - Matter and Radiation from the Universe (POF4-613)$$cPOF4-613$$fPOF IV$$x0
000570294 588__ $$aDataset connected to CrossRef, INSPIRE, Journals: bib-pubdb1.desy.de
000570294 650_7 $$2INSPIRE$$aradiation, Cherenkov
000570294 650_7 $$2INSPIRE$$aenergy, threshold
000570294 650_7 $$2INSPIRE$$ashowers, atmosphere
000570294 650_7 $$2INSPIRE$$amuon, detector
000570294 650_7 $$2INSPIRE$$aTeV
000570294 650_7 $$2INSPIRE$$aair
000570294 650_7 $$2INSPIRE$$acosmic radiation
000570294 650_7 $$2INSPIRE$$ahybrid
000570294 650_7 $$2INSPIRE$$apower spectrum
000570294 650_7 $$2INSPIRE$$aMonte Carlo
000570294 650_7 $$2INSPIRE$$aCherenkov counter
000570294 650_7 $$2INSPIRE$$aflux
000570294 650_7 $$2INSPIRE$$aspatial resolution
000570294 650_7 $$2INSPIRE$$aimaging
000570294 650_7 $$2INSPIRE$$astatistical
000570294 650_7 $$2INSPIRE$$ahadron
000570294 693__ $$0EXP:(DE-H253)TAIGA-20190101$$5EXP:(DE-H253)TAIGA-20190101$$eTunka Advanced Instrument for cosmic ray physics and Gamma Astronomy$$x0
000570294 7001_ $$0P:(DE-H253)PIP1006705$$aTluczykont, M.$$b1
000570294 7001_ $$0P:(DE-H253)PIP1017590$$aPorelli, A.$$b2
000570294 7001_ $$0R.Mirzoyan.1$$aMirzoyan, R.$$b3
000570294 7001_ $$0P:(DE-H253)PIP1003748$$aWischnewski, R.$$b4
000570294 7001_ $$0A.K.Awad.1$$aAwad, A. K.$$b5
000570294 7001_ $$0P:(DE-H253)PIP1016618$$aBrueckner, M.$$b6$$eCorresponding author
000570294 8564_ $$uhttps://bib-pubdb1.desy.de/record/570294/files/2301.11002v1.pdf$$yRestricted
000570294 8564_ $$uhttps://bib-pubdb1.desy.de/record/570294/files/2301.11002v1.pdf?subformat=pdfa$$xpdfa$$yRestricted
000570294 909CO $$ooai:bib-pubdb1.desy.de:570294$$pVDB
000570294 9101_ $$0I:(DE-HGF)0$$6P:(DE-H253)PIP1006705$$aExternal Institute$$b1$$kExtern
000570294 9101_ $$0I:(DE-588b)2008985-5$$6P:(DE-H253)PIP1017590$$aDeutsches Elektronen-Synchrotron$$b2$$kDESY
000570294 9101_ $$0I:(DE-588b)2008985-5$$6P:(DE-H253)PIP1003748$$aDeutsches Elektronen-Synchrotron$$b4$$kDESY
000570294 9101_ $$0I:(DE-HGF)0$$6P:(DE-H253)PIP1016618$$aExternal Institute$$b6$$kExtern
000570294 9131_ $$0G:(DE-HGF)POF4-613$$1G:(DE-HGF)POF4-610$$2G:(DE-HGF)POF4-600$$3G:(DE-HGF)POF4$$4G:(DE-HGF)POF$$aDE-HGF$$bForschungsbereich Materie$$lMatter and the Universe$$vMatter and Radiation from the Universe$$x0
000570294 9141_ $$y2023
000570294 9201_ $$0I:(DE-H253)Z_GA-20210408$$kZ_GA$$lGammaastronomie$$x0
000570294 980__ $$apreprint
000570294 980__ $$aVDB
000570294 980__ $$aI:(DE-H253)Z_GA-20210408
000570294 980__ $$aUNRESTRICTED