Joint analysis of the energy spectrum of ultra-high-energy cosmic rays as measured at the Pierre Auger Observatory and the Telescope Array
Y. TsunesadaRasha AbbasiT. Abu‐ZayyadMonica AllenYuto AraiRyuhei ArimuraE. BarcikowskiJohn BelzD. R. BergmanSamuel BlakeR. CadyByongGu CheonJyunsei ChibaMichiyuki ChikawaToshihiro FujiiKozo FujisueK. FujitaRyota FujiwaraM. FukushimaRyota FukushimaGreg FurlichRicardo GonzálezW. HanlonMotoki HayashiN. HayashidaK. HibinoRyo HiguchiKen HondaD. IkedaTaichi InadomiNaoya InoueTakaaki IshiiHirotaka ItoD. IvanovHirokazu IwakuraAoi IwasakiHyoming JeongSoomin JeongCharlie JuiK. KadotaF. KakimotoO. KalashevK. KasaharaSaori KasamiHideyuki KawaiS. KawakamiS. KawanaKatsumasa KawataIvan KharukE. KidoHangBae KimJihee KimJihyun KimMin Hyo KimSang‐Woo KimYusuke KimuraShoichi KishigamiYuto KubotaShinnosuke KurisuVladim KuzminM. KuznetsovYoungjoon KwonKwang‐Ho LeeBayarJon Paul LubsandorzhievJon Paul LundquistKazuhiro MachidaHiroyuki MatsumiyaToshio MatsuyamaJ. N. MatthewsR. MaytaM. MinaminoKeijiro MukaiI. MyersShigehiro NagatakiKei NakaiRyo NakamuraToru NakamuraTomoyuki NakamuraYuya NakamuraArata NakazawaEiji NishioT. NonakaHiroyuki OdaS. OgioM. OhnishiH. OhokaYuya OkuTakeshi OkudaYugo OmuraM. OnoR. OnogiA. OshimaS. OzawaIl Hung ParkMatt PottsМ. С. ПширковJackson RemingtonDoug RodriguezГ. РубцовDongsu RyuHiroyuki SagawaRyosuke SaharaYasunori SaitoН. СакакиT. SakoN. SakuraiKengo SanoKoki SatoT. SekiKoichi SekinoP. D. ShahYuma ShibasakiF. ShibataNorimichi ShibataT. ShibataHideaki ShimodairaBokkyun ShinHeungsu ShinDaiki ShintoJeremy SmithP. SokolskyNaohiro SoneBen StokesTom StromanYoshinori TakagiYuichi TakahashiMai TakamuraMasahiro TakedaRyuji TakeishiA. TaketaMasato TakitaY. TamedaHideki TanakaKoichi TanakaM. TanakaYuta TanoueS. B. ThomasGordon ThomsonPetr TinyakovI. TkachevHisono TokunoTaka TomidaS. TroitskyRyosuke TsudaYukio UchihoriShigeharu UdoTakafumi UehamaF. UrbanTiffany WongKohei YadaMashu YamamotoK. YamazakiJongmann YangK. YashiroFugo YoshidaTsubasa YoshiokaYana ZhezherZach Zundel
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The measurement of the energy spectrum of ultra-high-energy cosmic rays (UHECRs) is of crucial importance to clarify their origin and acceleration mechanisms. The Pierre Auger Observatory in Argentina and the Telescope Array (TA) in the US have reported their measurements of UHECR energy spectra observed in the southern and northern hemisphere, respectively. The region of the sky accessible to both Observatories ($[-15,+24]$ degrees in declination) can be used to cross-calibrate the two spectra. The Auger-TA energy spectrum working group was organized in 2012 and has been working to understand the uncertainties in energy scale in both experiments, their systematic differences, and differences in the shape of the spectra. In previous works, we reported that there was an overall agreement of the energy spectra measured by the two observatories below 10 EeV while at higher energies, a remaining significant difference was observed in the common declination band. We revisit this issue to understand its origin by examining the systematic uncertainties, statistical effects, and other possibilities. We will also discuss the differences in the spectra in different declination bands and a new feature in the spectrum recently reported by the Auger Collaboration.Keywords:
Pierre Auger Observatory
Right ascension
The goal of the Pierre Auger Observatory is to determine the still unknown nature and origin of ultra-high energy cosmic rays. The study of these elusive particles probes astrophysical sites of particle acceleration as well as fundamental interactions at energies unattainable in accelerator facilities. Auger combines two observational techniques, a large surface array and air fluorescence detectors, to observe the extended air showers generated in the atmosphere by cosmic rays. This hybrid observation yields an excellent resolution and allows for important cross-checks. The Auger South site, located in Mendoza (Argentina), is now nearing completion, with 60% of its surface array and three out of its four fluorescence detectors in operation. First results on the energy spectrum measurement, the search for anisotropies in arrival directions and the upper limit on the photon fraction are discussed.
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Variation (astronomy)
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Data are given for 205 LTT stars found on 23 areas, covering 25 squares degrees each, south of declination -40° and right ascension between 04 h 30 m and 16 h 00 m. Four stars present differences in proper motion ≥0.10″, three present differences in position angle >20° and one presents those differences in both values
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Astrolabe
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Representation
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Right ascension for α Scorpii A and right ascension and declination for 9 Sagittarii obtained with the astrolabe of Santiago are given in the FK5 system. The average precision is 0.07″ in right ascension and 0.15″ in declination. Other results are given for these radio stars for comparison. Some remarks are made on the declination of 9 Sgr as obtained with the astrolabe
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A method based on weighted least squares surface fitting was studied,which was used for astronomical observation space target.This method can be used in celestial positioning of high-precision and large data quantity,and it is also very simple.Through observing the real sky,the star maps continuously were calculated.The results show that the fitting mean square errors are all less than 4″in the direction of ascension and declination.The positioning accuracy in the direction of declination is better than that of ascension,the max positioning error of the observed stars are 5.13″and 1.74″in the direction of ascension and declination.It's demonstrated that the effects of star centroid errors are reduced,and the match up errors are also removed.The utilization of observed data and the precision of celestial positioning is improved.The method is well suited for application.
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The goal of the Pierre Auger Observatory is to determine the still unknown nature and origin of ultra-high energy cosmic rays. The study of these elusive particles probes astrophysical sites of particle acceleration as well as fundamental interactions at energies unattainable in accelerator facilities. Auger combines two observational techniques, a large surface array and air fluorescence detectors, to observe the extended air showers generated in the atmosphere by cosmic rays. This hybrid observation yields an excellent resolution and allows for important cross-checks. The Auger South site, located in Mendoza (Argentina), is now nearing completion, with 60% of its surface array and three out of its four fluorescence detectors in operation. First results on the energy spectrum measurement, the search for anisotropies in arrival directions and the upper limit on the photon fraction are discussed.
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Right ascension
Data Reduction
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Those that are curious in observing the Heavenly Motions, and particularly myself, whose Business it is, are greatly obliged to the late Signior Cassini , for his Thought of applying Threads at half Right Angles in the common Focus of a Telescope, to determine thereby the differences of Right Ascension and Declination of any two Stars, whose situation is such, that by their diurnal Motion they follow each other through the Aperture of the Telescope,
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