K. Mitsui

A 4-inch silicon/tungsten calorimeter for p-p collider experiments

Abstract A 4-inch diameter silicon/tungsten sandwich calorimeter with 64 cm 2 in active area and 18 radiation lengths in depth has been constructed. The performance has been investigated for incoming electrons of 500 MeV to 4.5 GeV. The calorimeter shows a good linearity over the electron energy region and the energy resolution is well expressed by σ (rms)/ E = 17√ t / E %, where t represents the unit sampling thickness in radiation lengths and E the incident electron energy in GeV. The agreement between these results and a Monte Carlo simulation is quite satisfactory. The center of shower has been determined with the accuracy of better than 2 mm at energies exceeding 1 GeV.

A Si(Li)-Pb shower calorimeter for p-p collider experiments

Abstract A silicon/lead sandwich calorimeter with 38 cm 2 in active area and 10 radiation lengths in depth has been constructed. The performance has been investigated for incoming electrons of 250 to 750 MeV. The calorimeter shows a good linearity over the electron energy region and the energy resolution was well expressed by σ (rms)/ E = (16.5 ± 0.5)/√ E (GeV) %. Also, it is shown that the deposited energy and energy resolution do not change greatly even when the incident beam position is very close to the detector edge. The agreement between these results and a Monte Carlo simulation is quite satisfactory.

Angular resolution of the Ohya air shower detector

Accurate measurements of the total number of muons in an air shower are important for the discrimination of showers produced by astronomical gamma rays from those produced by protons. In order to perform this discrimination, muon detectors with a total area of about 400 m2 have been constructed in the Ohya stone mine. At ground level, scintillation detectors have been distributed for determining the total number of electrons in the air shower. The arrival direction of the air shower determined by usual timing information was examined using independent data on the arrival direction determined by muons in the shower. The angular resolution thus obtained at the shower maximum is 1.7° in the south-north plane and 2° in the east-west plane. The difference of the resolution is due to the asymmetric arrangement of scintillation detectors.

The trigger system of mutron, a cosmic ray magnetic spectrometer

Abstract A large magnetic spectrometer for cosmic-ray studies has been built at Cosmic Ray Laboratory, University of Tokyo, which consists of two 400 t solid iron magnets, multiwire proportional chambers (MWPC), wire spark chambers and a calorimeter. In this paper the trigger system will be described whose geometrical acceptance is about 1300 cm 2 sr including the magnets. The trigger system consists of twenty large area MWPCs. The trigger selection is made up of the momentum selection, which excludes low momentum muons, and the particle-number selection limiting the number of particles hitting the trigger detectors simultaneously. This combination for trigger reduces the background level and improves the ratio of muons to background. The trigger rate is about 1.0 per minute in the usual operation.

Cosmic-ray muon spectrum derived from the transferred energy spectrum of bursts observed by the mutron calorimeter

SummaryMeasurements of the energy transfer,E′, of bursts produced in a calorimeter are calibrated with the momenta of the incoming and outgoing muons measured by the Mutron magnet spectrometers. The relation between energy transferE′ and momentum difference Δpc was obtained in the energy range from 30 GeV to 1 TeV as follows:E′=(0.85±0.16) Δpc. Using this calibrated calorimeter, we observed distributions of the energy transfer of bursts produced in the calorimeter up to 6 TeV by the magnet spectrometer plus calorimeter triggers, as well as by the calorimeter trigger alone. From the observed burst spectrum, we have derived the muon energy spectrum at sea-level. The differential pion production spectrum combined with the data using composite triggers gives an exponentγ=2.58±0.19 in the muon energy region from 200 GeV to 6 TeV and 2.74±0.19 in the region from 1 TeV to 6 TeV. The muon energy spectrum thus obtained is compared with the direct measurement of the muon spectrum by the Mutron magnet spectrometers. It is thus established that measurements of the transferred energy spectrum of bursts are available for the derivation of the muon energy spectrum beyond the energy region measured by the magnet spectrometer.RiassuntoSi calibrano le misure del trasferimento d’energiaE′ di scrosci prodotti in un calorimetro con gl’impulsi dei muoni in entrata e in uscita misurati dagli spettrometri a magneti Mutron. Si ottiene la relazione tra il trasferimento di energiaE′ e la differenza d’impulsi Δpc nell’intervallo di energia da 30 GeV a 1 TeV come segue:E′=(0.85±0.16)Δpc. Usando questo calorimetro calibrato, sono state osservate le distribuzioni del trasferimento d’energia di scrosci prodotti nel calorimetro fino a 6 TeV sia mediante l’innesco dello spettrometro a magneti piú quello del calorimetro, che solamente con quello del calorimetro. Dallo spettro degli scrosci osservato, è stato derivato lo spettro d’energia dei muoni a livello del mare. Lo spettro differenziale di produzione di pioni combinato con i dati ottenuti usando inneschi composti dà un esponenteγ=2.58±0.19 nella regione d’energia muonica da 200 GeV a 6 TeV e 2.74±0.19 nella regione da 1 TeV a 6 TeV. Lo spettro d’energia muonica cosí ottenuto è confrontato con la misura diretta dello spettro muonico degli spettrometri a magneti Mutron. Si stabilisce cosí che le misure dello spettro d’energia trasferita degli scoppi permettono di derivare lo spettro d’energia muonica al di là della regione d’energia misurata dallo spettrometro a magneti.

Electromagnetic interactions of cosmic-ray muons up to 10 TeV (pair productions and bremsstrahlung)

SummaryElectromagnetic interactions (excluding nuclear interactions) of cosmic-ray muons were investigated by a combined arrangement of the Mutron magnet spectrometer and calorimeter. The interactions covered their transferred energies ranging from 1 GeV to several TeV produced by muons with energies up to 10 TeV. There is reasonable agreement between the experimental results and the theoretical predictions. For transferred energies less than 10 GeV, however, the observed number of events produced by muons around 1 TeV may be somewhat smaller than theoretically expected. The probability of accompaniment of a muon emerging from thick iron plates is also studied. The data are very useful for the measurement of the muon momentum by the magnet spectrometer. The ratio of the interaction probability for positive muons to that for negative muons is 0.94±0.02 for interactions with energy transfers over 1 GeV. However, by considering the measured accuracy of the value ±0.05 used for the charge ratio of incident muons, there is no evidence to support any suggestion that the interaction cross-sections of positive and negative muons for energy transfers above 1 GeV differ in the range from 100 GeV to 10 TeV.RiassuntoSono state studiate le interazioni elettromagnetiche (escludendo le interazioni nucleari) dei muoni dei raggi cosmici mediante una disposizione combinata dello spettrometro a magneti Mutron e del calorimetro. Le interazioni riguardano le energie trasferite che vanno da 1 GeV a qualche TeV prodotte da muoni con energie fino a 10 TeV. Si trova un discreto accordo tra i risultati sperimentali e le previsioni teoriche. Per energie trasferite minori di 10 GeV, comunque, il numero osservato di eventi prodotti da muoni a circa 1 TeV può essere un po’ piú piccolo di quanto previsto teoricamente. Si studia anche la probabilità di accompagnamento di un muone uscente da spesse piastre di ferro. I dati sono molto utili per misurare l’impulso del muone con lo spettrometro a magneti. Il rapporto tra la probabilità d’interazione per muoni positivi e quella per muoni negativi è di 0.94±0.02 per interazioni con trasferimenti di energia al di sopra di 1 GeV. Comunque, considerando l’accuratezza misurata del valore ±0.05 usato per il rapporto di carica dei muoni incidenti, non c’è nessuna prova che sostenga l’ipotesi che le sezioni d’urto d’interazione tra muoni positivi e negativi per trasferimento d’energia al di sopra di 1 GeV differiscano nell’intervallo da 100 GeV a 10 TeV.

A calorimeter to study cosmic ray muon interactions

Abstract A calorimeter with a volume of 3.6×4×2.4 m 3 has been built in the Institute for Cosmic Ray Research, University of Tokyo to study the interactions of cosmic ray muons of known momenta. The calorimeter is located between the two magnets of MUTRON, a magnet spectrometer built by the same laboratory to measure muon momenta up to a maximum of 17 TeV c −1 . In this article, the design of the calorimeter is described and the characteristics of the counters used are reported. The expected number of the interactions and the accuracy of energy determinations by the calorimeter are also discussed.

New limit on the flux of slowly moving magnetic monopoles

A search for slowly moving superheavy magnetic monopoles has been performed using a combination of scintillation counters and proportional chambers which are situated on the ground near sea level. The minimum threshold threshold of the energy loss is set at 1/20 of the minimum ionisation. An upper flux limit of 1.8*10-12 cm-2 sr-1 s-1 for magnetic monopoles was obtained over a wide velocity range from 2.5*10-4 c to 1.0*10-1 c at the 90% confidence level. The velocity range for the trigger system was set from 10-4 c to 10-1 c.

Energy Spectrum of Cosmic-Ray Neutrinos in the Atmosphere.

SummaryThe energy spectrum of cosmic-ray neutrinos in the atmosphere has been calculated for the neutrino energy from 0.2 GeV to 108 GeV by taking into account the results of p-p collision, p-nucleus collision, nucleus-nucleus collision, the energy spectrum of primary cosmic rays, momentum spectrum and charge ratio of cosmic-ray muons measured by MUTRON, and the production of prompt neutrinos in the decay of charmed particles. Our result on neutrino intensity is in good agreement with the result of Osborneet al. for the horizontal direction if their muon spectrum has been corrected, and also with the result of Volkova for the vertical direction except for the lower energies. For the horizontal direction the intensity of prompt muon-neutrinos exceeds that of muonneutrinos from the conventional processes at the neutrino energy of 106 GeV and also the intensity of prompt electron-neutrinos exceeds that of electron-neutrinos from the conventional processes at the energy of 105 GeV. The corresponding values for the vertical direction are 105 GeV and 104 GeV, respectively. In the energy region from 0.3 GeV to 3 GeV, the expected value for the ratio of intensity of electron-neutrino to that of muon-neutrino is obtained as 0.42±0.08 and this is excellent agreement with the experimental value 0.36±0.13 of NUSEX group.RiassuntoÈ stato calcolato lo spettro d’energia dei neutrini dei raggi cosmici nell’atmosfera per un’energia neutrinica da 0.2 a 108 GeV tenendo conto dei risultati delle collisioni p-p, p-nucleo, nucleo-nucleo, dello spettro d’energia dei raggi cosmici primari, dello spettro dell’impulso e del rapporto di carica dei muoni dei raggi cosmici misurato da MUTRON e dalla produzione di neutrini pronti nel decadimento di particelle con charm. Il nostro risultato sull’intensità dei neutrini è in buon accordo con il risultato di Osborneet al. per la direzione orizzontale se il loro spettro muonico viene corretto, ed anche con il risultato di Volkova per la direzione verticale tranne che per le energie piú basse. Per la direzione orizzontale l’intensità dei neutrini muonici pronti è maggiore di quella dei neutrini muonici che derivano dai processi convenzionali ad energia neutrinica di 106 GeV ed anche l’intensità dei neutrini elettronici pronti è maggiore di quella dei neutrini elettronici che derivano dai processi convenzionali all’energia di 105 GeV. I valori corrispondenti per la direzione verticale sono rispettivamente 105 e 104 GeV. Nella regione d’energia tra 0.3 e 3 GeV, il valore atteso ottenuto per il rapporto tra l’intensità dei neutrini elettronici e quella dei neutrini muonici è 0.42±0.08 e questo è in accordo eccellente con il valore sperimentale 0.36±0.13 del gruppo NUSEX.РезюмеВычисляется Энергетический спектр нейтрино космических лучей в атмосфере для Энергий нейтрино от 0.2 ГЭВ до 108 ГЭВ, учитывая р-р соударения, р-ядерные соударения, ядерно-ядерные соударения, Энергетический спектр первичных космических лучей, импульсный спектр и зарядовое отнощение мюонов космических лучей, измеренных с помошью МUTRON, и образование нейтрино в распадах очарованных частиц. Нащ результат для интенсивности нейтрино хорощо согласуется с результатом Осборна и др. для горизонтального направления, если их мюонный спектр является правильным, а также с результатом Волковой для вертикального направления, за исключением низких Энергий. Для горизонтального направления интенсивность мгновенных мюонных нейтрино превыщает интенсивность мюон-ных нейтрино из обычных процессов при Энергиях нейтрино 106 ГЭВ. Йнтенсивность мгновенных Электронных нейтрино превыщает интенсивность Электронных нейтрино из обычных процессов при Энергии 105 ГЭВ. Соответствуюшие величины для вертикального направления соответственно равны 105 ГЭВ и ДО4 ГЭВ. В области Энергий от 0.3 ГЭВ до 3 ГЭВ ожидаемая величина отнощения интенсивностей Электронных нейтрино к интенсивности мюонных нейтрино составляет 0.42±0.08. Ёта величина прекрасно согласуется с Экспериментальным результатом 0.36±0.13, полученным группой

The observation of Cherenkov light from the decay of 40K

Abstract In the observation of Cherenkov light produced by cosmic rays in the ocean, illuminations produced by 40 K should be considered as a background to a photomultiplier. We have measured the pulse height distribution and the counting rate of Cherenkov light from 40 K using a solution with a higher concentration of potassium salts than sea water and compared them with expected values.