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94 results on '"Haines, TJ"'

1. Search for n-n ¯ oscillation in Super-Kamiokande SEARCH FOR n-n ¯ OSCILLATION IN SUPER-⋯ K. ABE et al.

Author

Abe, K, Hayato, Y, Iida, T, Ishihara, K, Kameda, J, Koshio, Y, Minamino, A, Mitsuda, C, Miura, M, Moriyama, S, Nakahata, M, Obayashi, Y, Ogawa, H, Sekiya, H, Shiozawa, M, Suzuki, Y, Takeda, A, Takeuchi, Y, Ueshima, K, Watanabe, H, Higuchi, I, Ishihara, C, Ishitsuka, M, Kajita, T, Kaneyuki, K, Mitsuka, G, Nakayama, S, Nishino, H, Okumura, K, Saji, C, Takenaga, Y, Clark, S, Desai, S, Dufour, F, Herfurth, A, Kearns, E, Likhoded, S, Litos, M, Raaf, JL, Stone, JL, Sulak, LR, Wang, W, Goldhaber, M, Casper, D, Cravens, JP, Dunmore, J, Griskevich, J, Kropp, WR, Liu, DW, Mine, S, Regis, C, Smy, MB, Sobel, HW, Vagins, MR, Ganezer, KS, Hartfiel, B, Hill, J, Keig, WE, Jang, JS, Jeoung, IS, Kim, JY, Lim, IT, Scholberg, K, Tanimoto, N, Walter, CW, Wendell, R, Ellsworth, RW, Tasaka, S, Guillian, G, Learned, JG, Matsuno, S, Messier, MD, Ichikawa, AK, Ishida, T, Ishii, T, Iwashita, T, Kobayashi, T, Nakadaira, T, Nakamura, K, Nishikawa, K, Nitta, K, Oyama, Y, Suzuki, AT, Hasegawa, M, Maesaka, H, Nakaya, T, Sasaki, T, Sato, H, Tanaka, H, Yamamoto, S, Yokoyama, M, Haines, TJ, Dazeley, S, Hatakeyama, S, Svoboda, R, Sullivan, GW, Gran, R, Habig, A, Fukuda, Y, and Itow, Y

Subjects
hep-ex, Nuclear & Particles Physics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Quantum Physics, Atomic, Molecular, Nuclear, Particle and Plasma Physics
Abstract

A search for neutron-antineutron (n-n¯) oscillation was undertaken in Super-Kamiokande using the 1489 live-day or 2.45×1034 neutron-year exposure data. This process violates both baryon and baryon minus lepton numbers by an absolute value of two units and is predicted by a large class of hypothetical models where the seesaw mechanism is incorporated to explain the observed tiny neutrino masses and the matter-antimatter asymmetry in the Universe. No evidence for n-n¯ oscillation was found; the lower limit of the lifetime for neutrons bound in O16, in an analysis that included all of the significant sources of experimental uncertainties, was determined to be 1.9×1032years at the 90% confidence level. The corresponding lower limit for the oscillation time of free neutrons was calculated to be 2.7×108s using a theoretical value of the nuclear suppression factor of 0.517×1023s-1 and its uncertainty.

Published
2015

2. Search for n−n¯ oscillation in Super-Kamiokande

Author

Abe, K, Hayato, Y, Iida, T, Ishihara, K, Kameda, J, Koshio, Y, Minamino, A, Mitsuda, C, Miura, M, Moriyama, S, Nakahata, M, Obayashi, Y, Ogawa, H, Sekiya, H, Shiozawa, M, Suzuki, Y, Takeda, A, Takeuchi, Y, Ueshima, K, Watanabe, H, Higuchi, I, Ishihara, C, Ishitsuka, M, Kajita, T, Kaneyuki, K, Mitsuka, G, Nakayama, S, Nishino, H, Okumura, K, Saji, C, Takenaga, Y, Clark, S, Desai, S, Dufour, F, Herfurth, A, Kearns, E, Likhoded, S, Litos, M, Raaf, JL, Stone, JL, Sulak, LR, Wang, W, Goldhaber, M, Casper, D, Cravens, JP, Dunmore, J, Griskevich, J, Kropp, WR, Liu, DW, Mine, S, Regis, C, Smy, MB, Sobel, HW, Vagins, MR, Ganezer, KS, Hartfiel, B, Hill, J, Keig, WE, Jang, JS, Jeoung, IS, Kim, JY, Lim, IT, Scholberg, K, Tanimoto, N, Walter, CW, Wendell, R, Ellsworth, RW, Tasaka, S, Guillian, G, Learned, JG, Matsuno, S, Messier, MD, Ichikawa, AK, Ishida, T, Ishii, T, Iwashita, T, Kobayashi, T, Nakadaira, T, Nakamura, K, Nishikawa, K, Nitta, K, Oyama, Y, Suzuki, AT, Hasegawa, M, Maesaka, H, Nakaya, T, Sasaki, T, Sato, H, Tanaka, H, Yamamoto, S, Yokoyama, M, Haines, TJ, Dazeley, S, Hatakeyama, S, Svoboda, R, Sullivan, GW, Gran, R, Habig, A, Fukuda, Y, and Itow, Y

Subjects
Nuclear and Plasma Physics, Particle and High Energy Physics, Physical Sciences, hep-ex, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Quantum Physics, Nuclear & Particles Physics, Mathematical physics, Astronomical sciences, Particle and high energy physics
Abstract

A search for neutron-antineutron (n-n¯) oscillation was undertaken in Super-Kamiokande using the 1489 live-day or 2.45×1034 neutron-year exposure data. This process violates both baryon and baryon minus lepton numbers by an absolute value of two units and is predicted by a large class of hypothetical models where the seesaw mechanism is incorporated to explain the observed tiny neutrino masses and the matter-antimatter asymmetry in the Universe. No evidence for n-n¯ oscillation was found; the lower limit of the lifetime for neutrons bound in O16, in an analysis that included all of the significant sources of experimental uncertainties, was determined to be 1.9×1032years at the 90% confidence level. The corresponding lower limit for the oscillation time of free neutrons was calculated to be 2.7×108s using a theoretical value of the nuclear suppression factor of 0.517×1023s-1 and its uncertainty.

Published
2015

3. First results of a study of TeV emission from GRBs in Milagrito

Author

McEnery, JE, Atkins, R, Benbow, W, Berley, D, Chen, ML, Coyne, DG, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, McConnell, M, McCullough, JF, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Shen, B, Shoup, A, Sinnis, C, Smith, AJ, Sullivan, GW, Tumer, T, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Subjects
astro-ph
Abstract

Milagrito, a detector sensitive to gamma-rays at TeV energies, monitored thenorthern sky during the period February 1997 through May 1998. With a largefield of view and high duty cycle, this instrument was used to perform a searchfor TeV counterparts to gamma-ray bursts. Within the Milagrito field of view 54gamma-ray bursts at keV energies were observed by the Burst And TransientSatellite Experiment (BATSE) aboard the Compton Gamma-Ray Observatory. Thispaper describes the results of a preliminary analysis to search for TeVemission correlated with BATSE detected bursts. Milagrito detected an excess ofevents coincident both spatially and temporally with GRB 970417a, with chanceprobability $2.8 \times 10^{-5}$ within the BATSE error radius. No othersignificant correlations were detected. Since 54 bursts were examined thechance probability of observing an excess with this significance in any ofthese bursts is $1.5 \times 10^{-3}$. The statistical aspects and physicalimplications of this result are discussed.

Published
2000

4. First results of a study of TeV emission from GRBs in Milagrito

Author

Miller, RS, Atkins, R, Benbow, W, Berley, D, Chen, ML, Coyne, DG, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, McConnell, M, McCullough, JF, McEnery, JE, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Shen, B, Shoup, A, Sinnis, C, Smith, AJ, Sullivan, GW, Tumer, T, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Subjects
astro-ph
Abstract

Milagrito, a detector sensitive to gamma-rays at TeV energies, monitored thenorthern sky during the period February 1997 through May 1998. With a largefield of view and high duty cycle, this instrument was used to perform a searchfor TeV counterparts to gamma-ray bursts. Within the Milagrito field of view 54gamma-ray bursts at keV energies were observed by the Burst And TransientSatellite Experiment (BATSE) aboard the Compton Gamma-Ray Observatory. Thispaper describes the results of a preliminary analysis to search for TeVemission correlated with BATSE detected bursts. Milagrito detected an excess ofevents coincident both spatially and temporally with GRB 970417a, with chanceprobability $2.8 \times 10^{-5}$ within the BATSE error radius. No othersignificant correlations were detected. Since 54 bursts were examined thechance probability of observing an excess with this significance in any ofthese bursts is $1.5 \times 10^{-3}$. The statistical aspects and physicalimplications of this result are discussed.

Published
2000

5. Instrumented Water Tanks can Improve Air Shower Detector Sensitivity

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Subjects
astro-ph
Abstract

Previous works have shown that water Cherenkov detectors have superiorsensitivity to those of scintillation counters as applied to detectingextensive air showers (EAS). This is in large part due to their much highersensitivity to EAS photons which are more than five times more numerous thanEAS electrons. Large area water Cherenkov detectors can be constructedrelatively cheaply and operated reliably. A sparse detector array has beendesigned which uses these types of detectors to substantially increase the areaover which the Milagro Gamma Ray Observatory collects EAS information.Improvements to the Milagro detector's performance characteristics andsensitivity derived from this array and preliminary results from a prototypearray currently installed near the Milagro detector will be presented.

Published
1999

6. Calibration of the Milagro Cosmic Ray Telescope

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Subjects
astro-ph
Abstract

The Milagro detector is an air shower array which uses the water Cherenkovtechnique and is capable of continuously monitoring the sky at energies near 1TeV. The detector consists of 20000 metric tons of pure water instrumented with723 photo-multiplier tubes (PMTs). The PMTs are arranged in a two-layerstructure on a lattice of 3 m spacing covering 5000 $m^2$ area. The directionof the shower is determined from the relative timing of the PMT signals,necessitating a common time reference and amplitude slewing corrections toimprove the time resolution. The calibration system to provide these consistsof a pulsed laser driving 30 diffusing light sources deployed in the pond toallow cross-calibration of the PMTs. The system is capable of calibrating timesand the pulse-heights from the PMTs using the time-over-threshold technique.The absolute energy scale is provided using single muons passing through thedetector. The description of the calibration system of the Milagro detector andits prototype Milagrito will be presented.

Published
1999

7. Status of the Milagro Gamma Ray Observatory

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Subjects
astro-ph
Abstract

The Milagro Gamma Ray Observatory is the world's first large-area waterCherenkov detector capable of continuously monitoring the sky at TeV energies.Located in northern New Mexico, Milagro will perform an all sky survey of theNorthern Hemisphere at energies between ~250 GeV and 50 TeV. With a high dutycycle, large detector area (~5000 square meters), and a wide field-of-view (~1sr), Milagro is uniquely capable of searching for transient and DC sources ofhigh-energy gamma-ray emission. Milagro has been operating since February,1999. The current status of the Milagro Observatory and initial results will bediscussed.

Published
1999

8. Study of the Shadows of the Moon and the Sun with VHE Cosmic Rays

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Subjects
astro-ph
Abstract

Milagrito, a prototype for the Milagro detector, operated for 15 months in1997-8 and collected 8.9 billion events. It was the first extensive air shower(EAS) array sensitive to showers intiated by primaries with energy below 1 TeV.The shadows of the sun and moon observed with cosmic rays can be used to studysystematic pointing shifts and measure the angular resolution of EAS arrays.Below a few TeV, the paths of cosmic rays coming toward the earth are bent bythe helio- and geo-magnetic fields. This is expected to distort and displacethe shadows of the sun and the moon. The moon shadow, offset from the nominal(undeflected) position, has been observed with high statistical significance inMilagrito. This can be used to establish energy calibrations, as well as tosearch for the anti-matter content of the VHE cosmic ray flux. The shadow ofthe sun has also been observed with high significance.

Published
1999

9. Search for Short Duration Bursts of TeV Gamma Rays with the Milagrito Telescope

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Subjects
astro-ph
Abstract

The Milagrito water Cherenkov telescope operated for over a year. The mostprobable gamma-ray energy was ~1 TeV and the trigger rate was as high as 400Hz. We have developed an efficient technique for searching the entire sky forshort duration bursts of TeV photons. Such bursts may result from "traditional"gamma-ray bursts that were not in the field-of-view of any other instruments,the evaporation of primordial black holes, or some as yet undiscoveredphenomenon. We have begun to search the Milagrito data set for bursts ofduration 10 seconds. Here we will present the technique and the expectedresults. Final results will be presented at the conference.

Published
1999

10. Detection of 6 November 1997 Ground Level Event by Milagrito

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Subjects
astro-ph
Abstract

Solar Energetic Particles from the 6 November 1997 solar flare/CME(coronalmass ejection) with energies exceeding 10 GeV have been detected by Milagrito,a prototype of the Milagro Gamma Ray Observatory. While particle accelerationbeyond 1 GeV at the Sun is well established, few data exist for protons or ionsbeyond 10 GeV. The Milagro observatory, a ground based water Cherenkov detectordesigned for observing very high energy gamma ray sources, can also be used tostudy the Sun. Milagrito, which operated for approximately one year in 1997/98,was sensitive to solar proton and neutron fluxes above ~5- 10 GeV. Milagritooperated in a scaler mode, which was primarily sensitive to muons, low energyphotons, and electrons, and the detector operated in a mode sensitive toshowers and high zenith angle muons. In its scaler mode, Milagrito registered arate increase coincident with the 6 November 1997 ground level event observedby Climax and other neutron monitors. A preliminary analysis suggests thepresence of >10 GeV particles.

Published
1999

11. Milagrito Detection of TeV Emission from Mrk 501

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Subjects
astro-ph
Abstract

The Milagro water Cherenkov detector near Los Alamos, New Mexico, has beenoperated as a sky monitor at energies of a few TeV between February 1997 andApril 1998. Serving as a test run for the full Milagro detector, Milagrito hastaken data during the strong and long-lasting 1997 flare of Mrk 501. We presentresults from the analysis of Mrk 501 and compare the excess and backgroundrates with expectations from the detector simulations.

Published
1999

12. Search for a TeV Component of GRBs using the Milagrito Detector

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Subjects
astro-ph
Abstract

Observing gamma ray bursts (GRBs) in the TeV energy range can be extremelyvaluable in providing insight to GRB radiation mechanisms and in constrainingsource distances. The Milagrito detector was an air shower array which used thewater Cherenkov technique to search for TeV sources. Data from this detectorwas analyzed to look for a TeV component of GRBs coincident with low energy-rays detected by the BATSE instrument on the Compton Gamma Ray Observatory. Asample of 54 BATSE GRBs which were in the field of view of the Milagritodetector during its lifetime (February 1997 to May 1998) was used.

Published
1999

13. An All-Sky Search for Steady VHE Gamma-Ray Sources

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Subjects
astro-ph
Abstract

The Milagrito water Cherenkov detector in the Jemez Mountains near LosAlamos, New Mexico took data from February 1997 to April 1998. Milagrito servedas a prototype for the larger Milagro detector, which has just begunoperations. Milagrito was the first large-aperture gamma-ray detector withsensitivity to gamma rays below 1 TeV. We report here on a search for steadyemission from point sources over most of the northern sky using data fromMilagrito.

Published
1999

14. An All-Sky Search for Steady VHE Gamma-Ray Sources

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, Yodh, GB, Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Abstract

The Milagrito water Cherenkov detector in the Jemez Mountains near Los Alamos, New Mexico took data from February 1997 to April 1998. Milagrito served as a prototype for the larger Milagro detector, which has just begun operations. Milagrito was the first large-aperture gamma-ray detector with sensitivity to gamma rays below 1 TeV. We report here on a search for steady emission from point sources over most of the northern sky using data from Milagrito.

Published
2017

15. Study of the Shadows of the Moon and the Sun with VHE Cosmic Rays

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, Yodh, GB, Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Abstract

Milagrito, a prototype for the Milagro detector, operated for 15 months in 1997-8 and collected 8.9 billion events. It was the first extensive air shower (EAS) array sensitive to showers intiated by primaries with energy below 1 TeV. The shadows of the sun and moon observed with cosmic rays can be used to study systematic pointing shifts and measure the angular resolution of EAS arrays. Below a few TeV, the paths of cosmic rays coming toward the earth are bent by the helio- and geo-magnetic fields. This is expected to distort and displace the shadows of the sun and the moon. The moon shadow, offset from the nominal (undeflected) position, has been observed with high statistical significance in Milagrito. This can be used to establish energy calibrations, as well as to search for the anti-matter content of the VHE cosmic ray flux. The shadow of the sun has also been observed with high significance.

Published
2017

16. Search for Short Duration Bursts of TeV Gamma Rays with the Milagrito Telescope

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, Yodh, GB, Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Abstract

The Milagrito water Cherenkov telescope operated for over a year. The most probable gamma-ray energy was ~1 TeV and the trigger rate was as high as 400 Hz. We have developed an efficient technique for searching the entire sky for short duration bursts of TeV photons. Such bursts may result from "traditional" gamma-ray bursts that were not in the field-of-view of any other instruments, the evaporation of primordial black holes, or some as yet undiscovered phenomenon. We have begun to search the Milagrito data set for bursts of duration 10 seconds. Here we will present the technique and the expected results. Final results will be presented at the conference.

Published
2017

17. Instrumented Water Tanks can Improve Air Shower Detector Sensitivity

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, Yodh, GB, Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Abstract

Previous works have shown that water Cherenkov detectors have superior sensitivity to those of scintillation counters as applied to detecting extensive air showers (EAS). This is in large part due to their much higher sensitivity to EAS photons which are more than five times more numerous than EAS electrons. Large area water Cherenkov detectors can be constructed relatively cheaply and operated reliably. A sparse detector array has been designed which uses these types of detectors to substantially increase the area over which the Milagro Gamma Ray Observatory collects EAS information. Improvements to the Milagro detector's performance characteristics and sensitivity derived from this array and preliminary results from a prototype array currently installed near the Milagro detector will be presented.

Published
2017

18. Search for a TeV Component of GRBs using the Milagrito Detector

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, Yodh, GB, Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Abstract

Observing gamma ray bursts (GRBs) in the TeV energy range can be extremely valuable in providing insight to GRB radiation mechanisms and in constraining source distances. The Milagrito detector was an air shower array which used the water Cherenkov technique to search for TeV sources. Data from this detector was analyzed to look for a TeV component of GRBs coincident with low energy -rays detected by the BATSE instrument on the Compton Gamma Ray Observatory. A sample of 54 BATSE GRBs which were in the field of view of the Milagrito detector during its lifetime (February 1997 to May 1998) was used.

Published
2017

19. Milagrito Detection of TeV Emission from Mrk 501

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, Yodh, GB, Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Abstract

The Milagro water Cherenkov detector near Los Alamos, New Mexico, has been operated as a sky monitor at energies of a few TeV between February 1997 and April 1998. Serving as a test run for the full Milagro detector, Milagrito has taken data during the strong and long-lasting 1997 flare of Mrk 501. We present results from the analysis of Mrk 501 and compare the excess and background rates with expectations from the detector simulations.

Published
2017

20. Calibration of the Milagro Cosmic Ray Telescope

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, Yodh, GB, Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Abstract

The Milagro detector is an air shower array which uses the water Cherenkov technique and is capable of continuously monitoring the sky at energies near 1 TeV. The detector consists of 20000 metric tons of pure water instrumented with 723 photo-multiplier tubes (PMTs). The PMTs are arranged in a two-layer structure on a lattice of 3 m spacing covering 5000 $m^2$ area. The direction of the shower is determined from the relative timing of the PMT signals, necessitating a common time reference and amplitude slewing corrections to improve the time resolution. The calibration system to provide these consists of a pulsed laser driving 30 diffusing light sources deployed in the pond to allow cross-calibration of the PMTs. The system is capable of calibrating times and the pulse-heights from the PMTs using the time-over-threshold technique. The absolute energy scale is provided using single muons passing through the detector. The description of the calibration system of the Milagro detector and its prototype Milagrito will be presented.

Published
2017

21. Status of the Milagro Gamma Ray Observatory

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, Yodh, GB, Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Abstract

The Milagro Gamma Ray Observatory is the world's first large-area water Cherenkov detector capable of continuously monitoring the sky at TeV energies. Located in northern New Mexico, Milagro will perform an all sky survey of the Northern Hemisphere at energies between ~250 GeV and 50 TeV. With a high duty cycle, large detector area (~5000 square meters), and a wide field-of-view (~1 sr), Milagro is uniquely capable of searching for transient and DC sources of high-energy gamma-ray emission. Milagro has been operating since February, 1999. The current status of the Milagro Observatory and initial results will be discussed.

Published
2017

22. Search for diffuse astrophysical neutrino flux using ultra-high-energy upward-going muons in Super-Kamiokande I

Author

Swanson, Mec, Abe, K., Hosaka, J., Iida, T., Ishihara, K., Kameda, J., Koshio, Y., Minamino, A., Mitsuda, C., Miura, M., Moriyama, S., Nakahata, M., Obayashi, Y., Ogawa, H., Shiozawa, M., Suzuki, Y., Takeda, A., Takeuchi, Y., Ueshima, K., Higuchi, I., Ishihara, C., Ishitsuka, M., Kajita, T., Kaneyuki, K., Mitsuka, G., Nakayama, S., Nishino, H., Okada, A., Okumura, K., Saji, C., Takenaga, Y., Clark, S., Desai, S., Dufour, F., Kearns, E., Likhoded, S., Litos, M., Raaf, Jl, Stone, Jl, Sulak, Lr, Wang, W., Goldhaber, M., Casper, D., Cravens, Jp, Dunmore, J., Kropp, Wr, Liu, Dw, Mine, S., Regis, C., Smy, Mb, Sobel, Hw, Vagins, MR, Ganezer, Ks, Hill, Je, Keig, We, Jang, Js, Kim, Jy, Lim, It, Scholberg, K., Tanimoto, N., Walter, Cw, Wendell, R., Ellsworth, Rw, Tasaka, S., Guillian, G., Learned, Jg, Matsuno, S., Messier, Md, Hayato, Y., Ichikawa, Ak, Ishida, T., Ishii, T., Iwashita, T., Kobayashi, T., Nakadaira, T., Nakamura, K., Nitta, K., Oyama, Y., Totsuka, Y., Suzuki, At, Hasegawa, M., Hiraide, K., Kato, I., Maesaka, H., Nakaya, T., Nishikawa, K., Sasaki, T., Sato, H., Yamamoto, S., Masashi Yokoyama, Haines, Tj, Dazeley, S., Hatakeyama, S., Svoboda, R., Sullivan, Gw, Turcan, D., Cooley, J., Mahn, Kbm, Habig, A., Fukuda, Y., Sato, T., Itow, Y., Koike, T., Jung, Ck, Kato, T., Kobayashi, K., Malek, M., Mcgrew, C., Sarrat, A., Terri, R., Yanagisawa, C., Tamura, N., Sakuda, M., Sugihara, M., Kuno, Y., Yoshida, M., Kim, Sb, Yang, Bs, Yoo, J., Ishizuka, T., Okazawa, H., Choi, Y., Seo, Hk, Gando, Y., Hasegawa, T., Inoue, K., Ishii, H., Nishijima, K., Ishino, H., Watanabe, Y., Koshiba, M., Kielczewska, D., Zalipska, J., Berns, Hg, Gran, R., Shiraishi, Kk, Stachyra, A., Thrane, E., Washburn, K., and Wilkes, Rj

23. Search for supernova neutrino bursts at super-kamiokande

Author

Ikeda, M., Takeda, A., Fukuda, Y., Vagins, MR, Abe, K., Iida, T., Ishihara, K., Kameda, J., Koshio, Y., Minamino, A., Mitsuda, C., Miura, M., Moriyama, S., Nakahata, M., Obayashi, Y., Ogawa, H., Sekiya, H., Shiozawa, M., Suzuki, Y., Yasuo Takeuchi, Ueshima, K., Watanabe, H., Yamada, S., Higuchi, I., Ishihara, C., Ishitsuka, M., Kajita, T., Kaneyuki, K., Mitsuka, G., Nakayama, S., Nishino, H., Okumura, K., Saji, C., Takenaga, Y., Clark, S., Desai, S., Dufour, F., Kearns, E., Likhoded, S., Litos, M., Raaf, Jl, Stone, Jl, Sulak, Lr, Wang, W., Goldhaber, M., Casper, D., Cravens, Jp, Dunmore, J., Kropp, Wr, Liu, Dw, Mine, S., Regis, C., Smy, Mb, Sobel, Hw, Ganezer, Ks, Hill, J., Keig, We, Jang, Js, Kim, Jy, Lim, It, Scholberg, K., Tanimoto, N., Walter, Cw, Wendell, R., Ellsworth, Rw, Tasaka, S., Guillian, G., Learned, Jg, Matsuno, S., Messier, Md, Hayato, Y., Ichikawa, Ak, Ishida, T., Ishii, T., Iwashita, T., Kobayashi, T., Nakadaira, T., Nakamura, K., Nitta, K., Oyama, Y., Totsuka, Y., Suzuki, At, Hasegawa, M., Hiraide, K., Maesaka, H., Nakaya, T., Nishikawa, K., Sasaki, T., Yamamoto, S., Yokoyama, M., Haines, Tj, Dazeley, S., Hatakeyama, S., Svoboda, R., Sullivan, Gw, Turcan, D., Habig, A., Sato, T., Itow, Y., Koike, T., Tanaka, T., Jung, Ck, Kato, T., Kobayashi, K., Malek, M., Mcgrew, C., Sarrat, A., Terri, R., Yanagisawa, C., Tamura, N., Idehara, Y., Sakuda, M., Sugihara, M., Kuno, Y., Yoshida, M., Kim, Sb, Yang, Bs, Yoo, J., Ishizuka, T., Okazawa, H., Choi, Y., Seo, Hk, Gando, Y., Hasegawa, T., Inoue, K., Furuse, Y., Ishii, H., Nishijima, K., Ishino, H., Watanabe, Y., Koshiba, M., Chen, S., Deng, Z., Liu, Y., Kielczewska, D., Zalipska, J., Berns, H., Gran, R., Shiraishi, Kk, Stachyra, A., Thrane, E., Washburn, K., and Wilkes, Rj

24. N-16 as a calibration source for Super-Kamiokande

Author

Blaufuss, E., Guillian, G., Fukuda, Y., Fukuda, S., Ishitsuka, M., Itow, Y., Kajita, T., Kameda, J., Kaneyuki, K., Kobayashi, K., Kobayashi, Y., Koshio, Y., Miura, M., Moriyama, S., Nakahata, M., Nakayama, S., Obayashi, Y., Okada, A., Okumura, K., Sakurai, N., Shiozawa, M., Suzuki, Y., Takeuchi, B., Yasuo Takeuchi, Toshito, T., Totsuka, Y., Yamada, S., Earl, M., Habig, A., Kearns, E., Messier, Md, Scholberg, K., Stone, Jl, Sulak, Lr, Walter, Cw, Goldhaber, M., Barszczak, T., Casper, D., Gajewski, W., Kropp, Wr, Mine, S., Price, Lr, Smy, M., Sobel, Hw, Vagins, MR, Ganezer, Ks, Keig, We, Ellsworth, Rw, Tasaka, S., Kibayashi, A., Learned, Jg, Matsuno, S., Takemori, D., Hayato, Y., Ishii, T., Kobayashi, T., Nakamura, K., Oyama, Y., Sakai, A., Sakuda, M., Sasaki, O., Echigo, S., Kohama, M., Suzuki, At, Inagaki, T., Nishikawa, K., Haines, Tj, Kim, Bk, Sanford, R., Svoboda, R., Chen, Ml, Goodman, Ja, Sullivan, Gw, Hill, J., Jung, Ck, Martens, K., Malek, M., Mauger, C., Mcgrew, C., Sharkey, E., Viren, B., Yanagisawa, C., Kirisawa, M., Inaba, S., Mitsuda, C., Miyano, K., Okazawa, H., Saji, C., Takahashi, M., Takahata, M., Nagashima, Y., Nitta, K., Takita, M., Yoshida, M., Kim, Sb, Etoh, M., Gando, Y., Hasegawa, T., Inoue, K., Ishihara, K., Maruyama, T., Shirai, J., Suzuki, A., Koshiba, M., Hatakeyama, Y., Ichikawa, Y., Koike, M., Nishijima, K., Fujiyasu, H., Ishino, H., Morii, M., Watanabe, Y., Golebiewska, U., Kielczewska, D., Boyd, Sc, Stachyra, Al, Wilkes, Rj, Young, Kk, and Super-Kamiokande Collaboration

25. Characterization of the Mercury pulsed power x-ray source spectrum using multichannel density aerogel Cherenkov detectors.

Author

Meaney KD, Kim Y, Herrmann HW, Young CY, Archuleta TA, Hamilton CE, Duke DL, Haines TJ, Corredor AC, Green JA, Fegenbush L, Kaufman MI, Malone RM, Baker SA, Richardson S, Zier J, Engelbrecht J, and Culver A

Abstract

The Aerogel Cherenkov Detector for Cygnus (ACD/C) is a time-dependent, x-ray spectral detector that uses SiO 2 aerogels spanning an index of refraction (n = 1.02-1.07) corresponding to a 1.1-2.3 MeV x-ray energy threshold. The ACD/C was developed for pulsed power x-ray sources like Cygnus located at the Nevada National Site and Mercury located at the Naval Research Laboratory (NRL). Aerogels sit between the measurement capabilities of gas (>2 MeV) and solids such as fused silica (>0.3 MeV). The detector uses an aluminum converter to Compton scatter incoming x-rays and create relativistic electrons, which produce Cherenkov light in an aerogel or a fused silica medium. The ACD/C was fielded at the NRL when Mercury was tuned to produce up to 4.8 MeV endpoint bremsstrahlung. Despite a high radiation and electromagnetic interference background, the ACD/C was able to achieve high signal over noise across five aerogel densities and fused silica, including a signal to noise for a 1.1 MeV aerogel threshold. Previous experiments at Cygnus observed a signal that was comparable to the noise (1×) at the same threshold. The ACD/C observed time-resolved rise and fall times for different energy thresholds of the photon spectrum. Monte Carlo simulations of the ACD/C's aerogel response curves were folded with a simulation of Mercury's photon energy spectrum and agree within the error to the observed result.

Published
2018
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26. Measurement of atmospheric neutrino flux consistent with tau neutrino appearance.

Author

Abe K, Hayato Y, Iida T, Ishihara K, Kameda J, Koshio Y, Minamino A, Mitsuda C, Miura M, Moriyama S, Nakahata M, Obayashi Y, Ogawa H, Shiozawa M, Suzuki Y, Takeda A, Takeuchi Y, Ueshima K, Higuchi I, Ishihara C, Ishitsuka M, Kajita T, Kaneyuki K, Mitsuka G, Nakayama S, Nishino H, Okumura K, Saji C, Takenaga Y, Totsuka Y, Clark S, Desai S, Dufour F, Kearns E, Likhoded S, Litos M, Raaf JL, Stone JL, Sulak LR, Wang W, Goldhaber M, Casper D, Cravens JP, Kropp WR, Liu DW, Mine S, Regis C, Smy MB, Sobel HW, Vagins MR, Ganezer KS, Hill JE, Keig WE, Jang JS, Kim JY, Lim IT, Scholberg K, Tanimoto N, Walter CW, Wendell R, Ellsworth RW, Tasaka S, Guillian E, Learned JG, Matsuno S, Messier MD, Ichikawa AK, Ishida T, Ishii T, Iwashita T, Kobayashi T, Nakadaira T, Nakamura K, Nitta K, Oyama Y, Suzuki AT, Hasegawa M, Kato I, Maesaka H, Nakaya T, Nishikawa K, Sasaki T, Sato H, Yamamoto S, Yokoyama M, Haines TJ, Dazeley S, Hatakeyama S, Svoboda R, Sullivan GW, Habig A, Gran R, Fukuda Y, Sato T, Itow Y, Koike T, Jung CK, Kato T, Kobayashi K, Malek M, McGrew C, Sarrat A, Terri R, Yanagisawa C, Tamura N, Sakuda M, Sugihara M, Kuno Y, Yoshida M, Kim SB, Yoo J, Ishizuka T, Okazawa H, Choi Y, Seo HK, Gando Y, Hasegawa T, Inoue K, Ishii H, Nishijima K, Ishino H, Watanabe Y, Koshiba M, Kielczewska D, Zalipska J, Berns HG, Shiraishi KK, Washburn K, and Wilkes RJ

Abstract

A search for the appearance of tau neutrinos from nu(mu) <--> nu(tau) oscillations in the atmospheric neutrinos has been performed using 1489.2 days of atmospheric neutrino data from the Super-Kamiokande-I experiment. A best fit tau neutrino appearance signal of 138+/-48(stat)-32(+15)(syst) events is obtained with an expectation of 78+/-26(syst). The hypothesis of no tau neutrino appearance is disfavored by 2.4 sigma.

Published
2006
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27. Evidence for TeV gamma-ray emission from a region of the galactic plane.

Author

Atkins R, Benbow W, Berley D, Blaufuss E, Coyne DG, DeYoung T, Dingus BL, Dorfan DE, Ellsworth RW, Fleysher L, Fleysher R, Gisler G, Gonzalez MM, Goodman JA, Haines TJ, Hays E, Hoffman CM, Kelley LA, Lansdell CP, Linnemann JT, McEnery JE, Miller RS, Mincer AI, Morales MF, Nemethy P, Noyes D, Ryan JM, Samuelson FW, Parkinson PM, Shoup A, Sinnis G, Smith AJ, Sullivan GW, Williams DA, Wilson ME, Xu XW, and Yodh GB

Abstract

Gamma-ray emission from a narrow band at the galactic equator has previously been detected up to 30 GeV. We report evidence for a TeV gamma-ray signal from a region of the galactic plane by Milagro, a large-field-of-view water Cherenkov detector for extensive air showers. An excess with a significance of 4.5 standard deviations has been observed from the region of galactic longitude l E (40 degrees, 100 degrees) and latitude /b/ < 5 degrees. Under the assumption of a simple power law spectrum, with no cutoff in the EGRET-Milagro energy range, the measured integral flux is phi gamma(>3.5 TeV) = (6.4 +/- 1.4 +/- 2.1) x 10(-11) cm(-2) s(-1) sr(-1). This flux is consistent with an extrapolation of the EGRET spectrum between 1 and 30 GeV in this galactic region.

Published
2005
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28. Evidence for an oscillatory signature in atmospheric neutrino oscillations.

Author

Ashie Y, Hosaka J, Ishihara K, Itow Y, Kameda J, Koshio Y, Minamino A, Mitsuda C, Miura M, Moriyama S, Nakahata M, Namba T, Nambu R, Obayashi Y, Shiozawa M, Suzuki Y, Takeuchi Y, Taki K, Yamada S, Ishitsuka M, Kajita T, Kaneyuki K, Nakayama S, Okada A, Okumura K, Ooyabu T, Saji C, Takenaga Y, Desai S, Kearns E, Likhoded S, Stone JL, Sulak LR, Walter CW, Wang W, Goldhaber M, Casper D, Cravens JP, Gajewski W, Kropp WR, Liu DW, Mine S, Smy MB, Sobel HW, Sterner CW, Vagins MR, Ganezer KS, Hill J, Keig WE, Jang JS, Kim JY, Lim IT, Ellsworth RW, Tasaka S, Guillian G, Kibayashi A, Learned JG, Matsuno S, Takemori D, Messier MD, Hayato Y, Ichikawa AK, Ishida T, Ishii T, Iwashita T, Kobayashi T, Maruyama T, Nakamura K, Nitta K, Oyama Y, Sakuda M, Totsuka Y, Suzuki AT, Hasegawa M, Hayashi K, Inagaki T, Kato I, Maesaka H, Morita T, Nakaya T, Nishikawa K, Sasaki T, Ueda S, Yamamoto S, Haines TJ, Dazeley S, Hatakeyama S, Svoboda R, Blaufuss E, Goodman JA, Sullivan GW, Turcan D, Scholberg K, Habig A, Fukuda Y, Jung CK, Kato T, Kobayashi K, Malek M, Mauger C, McGrew C, Sarrat A, Sharkey E, Yanagisawa C, Toshito T, Miyano K, Tamura N, Ishii J, Kuno Y, Nagashima Y, Takita M, Yoshida M, Kim SB, Yoo J, Okazawa H, Ishizuka T, Choi Y, Seo HK, Gando Y, Hasegawa T, Inoue K, Shirai J, Suzuki A, Koshiba M, Nakajima Y, Nishijima K, Harada T, Ishino H, Nishimura R, Watanabe Y, Kielczewska D, Zalipska J, Berns HG, Gran R, Shiraishi KK, Stachyra A, Washburn K, and Wilkes RJ

Abstract

Muon neutrino disappearance probability as a function of neutrino flight length L over neutrino energy E was studied. A dip in the L/E distribution was observed in the data, as predicted from the sinusoidal flavor transition probability of neutrino oscillation. The observed L/E distribution constrained nu(micro)<-->nu(tau) neutrino oscillation parameters; 1.9x10(-3)0.90 at 90% confidence level.

Published
2004
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29. Limits on the neutrino magnetic moment using 1496 days of Super-Kamiokande-I solar neutrino data.

Author

Liu DW, Ashie Y, Fukuda S, Fukuda Y, Ishihara K, Itow Y, Koshio Y, Minamino A, Miura M, Moriyama S, Nakahata M, Namba T, Nambu R, Obayashi Y, Sakurai N, Shiozawa M, Suzuki Y, Takeuchi H, Takeuchi Y, Yamada S, Ishitsuka M, Kajita T, Kaneyuki K, Nakayama S, Okada A, Ooyabu T, Saji C, Desai S, Earl M, Kearns E, Messier MD, Stone JL, Sulak LR, Walter CW, Wang W, Barszczak T, Casper D, Cravens JP, Gajewski W, Kropp WR, Mine S, Smy MB, Sobel HW, Sterner CW, Vagins MR, Ganezer KS, Hill J, Keig WE, Kim JY, Lim IT, Ellsworth RW, Tasaka S, Kibayashi A, Learned JG, Matsuno S, Takemori D, Hayato Y, Ichikawa AK, Ishida T, Ishii T, Iwashita T, Kameda J, Kobayashi T, Maruyama T, Nakamura K, Nitta K, Oyama Y, Sakuda M, Totsuka Y, Suzuki AT, Hasegawa M, Hayashi K, Inagaki T, Kato I, Maesaka H, Morita T, Nakaya T, Nishikawa K, Sasaki T, Ueda S, Yamamoto S, Haines TJ, Dazeley S, Hatakeyama S, Svoboda R, Blaufuss E, Goodman JA, Guillian G, Sullivan GW, Turcan D, Scholberg K, Habig A, Ackermann M, Jung CK, Kato T, Kobayashi K, Martens K, Malek M, Mauger C, McGrew C, Sharkey E, Viren B, Yanagisawa C, Toshito T, Mitsuda C, Miyano K, Shibata T, Ishii J, Kajiyama Y, Kuno Y, Nagashima Y, Takita M, Yoshida M, Kim HI, Kim SB, Yoo J, Okazawa H, Ishizuka T, Choi Y, Seo HK, Gando Y, Hasegawa T, Inoue K, Shirai J, Suzuki A, Koshiba M, Hashimoto T, Nakajima Y, Nishijima K, Ishino H, Morii M, Nishimura R, Watanabe Y, Kielczewska D, Zalipska J, Gran R, Shiraishi KK, Washburn K, and Wilkes RJ

Abstract

A search for a nonzero neutrino magnetic moment has been conducted using 1496 live days of solar neutrino data from Super-Kamiokande-I. Specifically, we searched for distortions to the energy spectrum of recoil electrons arising from magnetic scattering due to a nonzero neutrino magnetic moment. In the absence of a clear signal, we found micro(nu)

Published
2004
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30. Search for nu(e) from the sun at Super-Kamiokande-I.

Author

Gando Y, Fukuda S, Fukuda Y, Ishitsuka M, Itow Y, Kajita T, Kameda J, Kaneyuki K, Kobayashi K, Koshio Y, Miura M, Moriyama S, Nakahata M, Nakayama S, Namba T, Obayashi Y, Okada A, Ooyabu T, Saji C, Sakurai N, Shiozawa M, Suzuki Y, Takeuchi H, Takeuchi Y, Totsuka Y, Yamada S, Desai S, Earl M, Kearns E, Messier MD, Stone JL, Sulak LR, Walter CW, Goldhaber M, Barszczak T, Casper D, Gajewski W, Kropp WR, Mine S, Liu DW, Smy MB, Sobel HW, Vagins MR, Gago A, Ganezer KS, Hill J, Keig WE, Ellsworth RW, Tasaka S, Kibayashi A, Learned JG, Matsuno S, Takemori D, Hayato Y, Ichikawa AK, Ishii T, Kobayashi T, Maruyama T, Nakamura K, Oyama Y, Sakuda M, Yoshida M, Kohama M, Iwashita T, Suzuki AT, Inagaki T, Kato I, Nakaya T, Nishikawa K, Haines TJ, Dazeley S, Hatakeyama S, Svoboda R, Blaufuss E, Chen ML, Goodman JA, Guillian G, Sullivan GW, Turcan D, Scholberg K, Habig A, Ackermann M, Jung CK, Martens K, Malek M, Mauger C, McGrew C, Sharkey E, Viren B, Yanagisawa C, Toshito T, Mitsuda C, Miyano K, Shibata T, Kajiyama Y, Nagashima Y, Nitta K, Takita M, Kim HI, Kim SB, Yoo J, Okazawa H, Ishizuka T, Etoh M, Hasegawa T, Inoue K, Ishihara K, Shirai J, Suzuki A, Koshiba M, Hatakeyama Y, Ichikawa Y, Koike M, Nishijima K, Ishino H, Morii M, Nishimura R, Watanabe Y, Kielczewska D, Berns HG, Boyd SC, Stachyra AL, and Wilkes RJ

Abstract

We present the results of a search for low energy nu(e) from the Sun using 1496 days of data from Super-Kamiokande-I. We observe no significant excess of events and set an upper limit for the conversion probability to nu(e) of the 8B solar neutrino. This conversion limit is 0.8% (90% C.L.) of the standard solar model's neutrino flux for total energy=8-20 MeV. We also set a flux limit for monochromatic nu(e) for E(nu(e))=10-17 MeV.

Published
2003
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31. Search for supernova relic neutrinos at Super-Kamiokande.

Author

Malek M, Morii M, Fukuda S, Fukuda Y, Ishitsuka M, Itow Y, Kajita T, Kameda J, Kaneyuki K, Kobayashi K, Koshio Y, Miura M, Moriyama S, Nakahata M, Nakayama S, Namba T, Okada A, Ooyabu T, Saji C, Sakurai N, Shiozawa M, Suzuki Y, Takeuchi H, Takeuchi Y, Totsuka Y, Yamada S, Desai S, Earl M, Kearns E, Messier MD, Stone JL, Sulak LR, Walter CW, Goldhaber M, Barszczak T, Casper D, Gajewski W, Kropp WR, Mine S, Liu DW, Smy MB, Sobel HW, Vagins MR, Gago A, Ganezer KS, Keig WE, Ellsworth RW, Tasaka S, Kibayashi A, Learned JG, Matsuno S, Takemori D, Hayato Y, Ishii T, Kobayashi T, Maruyama T, Nakamura K, Obayashi Y, Oyama Y, Sakuda M, Yoshida M, Kohama M, Iwashita T, Suzuki AT, Ichikawa A, Inagaki T, Kato I, Nakaya T, Nishikawa K, Haines TJ, Dazeley S, Hatakeyama S, Svoboda R, Blaufuss E, Goodman JA, Guillian G, Sullivan GW, Turcan D, Scholberg K, Habig A, Ackermann M, Hill J, Jung CK, Martens K, Mauger C, McGrew C, Sharkey E, Viren B, Yanagisawa C, Toshito T, Mitsuda C, Miyano K, Shibata T, Kajiyama Y, Nagashima Y, Nitta K, Takita M, Kim HI, Kim SB, Yoo J, Okazawa H, Ishizuka T, Etoh M, Gando Y, Hasegawa T, Inoue K, Ishihara K, Shirai J, Suzuki A, Koshiba M, Hatakeyama Y, Ichikawa Y, Koike M, Nishijima K, Ishino H, Nishimura R, Watanabe Y, Kielczewska D, Berns HG, Boyd SC, Stachyra AL, and Wilkes RJ

Abstract

A search for the relic neutrinos from all past core-collapse supernovae was conducted using 1496 days of data from the Super-Kamiokande detector. This analysis looked for electron-type antineutrinos that had produced a positron with an energy greater than 18 MeV. In the absence of a signal, 90% C.L. upper limits on the total flux were set for several theoretical models; these limits ranged from 20 to 130 macro nu(e) cm(-2) s(-1). Additionally, an upper bound of 1.2 macro nu(e) cm(-2) s(-1) was set for the supernova relic neutrino flux in the energy region E(nu)>19.3 MeV.

Published
2003
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32. Constraints on neutrino oscillations using 1258 days of Super-Kamiokande solar neutrino data.

Author

Fukuda S, Fukuda Y, Ishitsuka M, Itow Y, Kajita T, Kameda J, Kaneyuki K, Kobayashi K, Koshio Y, Miura M, Moriyama S, Nakahata M, Nakayama S, Okada A, Sakurai N, Shiozawa M, Suzuki Y, Takeuchi H, Takeuchi Y, Toshito T, Totsuka Y, Yamada S, Desai S, Earl M, Kearns E, Messier MD, Scholberg K, Stone JL, Sulak LR, Walter CW, Goldhaber M, Barszczak T, Casper D, Gajewski W, Kropp WR, Mine S, Liu DW, Price LR, Smy MB, Sobel HW, Vagins MR, Ganezer KS, Keig WE, Ellsworth RW, Tasaka S, Kibayashi A, Learned JG, Matsuno S, Takemori D, Hayato Y, Ishii T, Kobayashi T, Nakamura K, Obayashi Y, Oyama Y, Sakai A, Sakuda M, Kohama M, Suzuki AT, Inagaki T, Nakaya T, Nishikawa K, Haines TJ, Blaufuss E, Dazeley S, Lee KB, Svoboda R, Goodman JA, Guillian G, Sullivan GW, Turcan D, Habig A, Hill J, Jung CK, Martens K, Malek M, Mauger C, McGrew C, Sharkey E, Viren B, Yanagisawa C, Mitsuda C, Miyano K, Saji C, Shibata T, Kajiyama Y, Nagashima Y, Nitta K, Takita M, Yoshida M, Kim HI, Kim SB, Yoo J, Okazawa H, Ishizuka T, Etoh M, Gando Y, Hasegawa T, Inoue K, Ishihara K, Maruyama T, Shirai J, Suzuki A, Koshiba M, Hatakeyama Y, Ichikawa Y, Koike M, Nishijima K, Fujiyasu H, Ishino H, Morii M, Watanabe Y, Golebiewska U, Kielczewska D, Boyd SC, Stachyra AL, Wilkes RJ, and Young KK

Abstract

We report the result of a search for neutrino oscillations using precise measurements of the recoil electron energy spectrum and zenith angle variations of the solar neutrino flux from 1258 days of neutrino-electron scattering data in Super-Kamiokande. The absence of significant zenith angle variation and spectrum distortion places strong constraints on neutrino mixing and mass difference in a flux-independent way. Using the Super-Kamiokande flux measurement in addition, two allowed regions at large mixing are found.

Published
2001
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33. Solar 8B and hep neutrino measurements from 1258 days of Super-Kamiokande data.

Author

Fukuda S, Fukuda Y, Ishitsuka M, Itow Y, Kajita T, Kameda J, Kaneyuki K, Kobayashi K, Koshio Y, Miura M, Moriyama S, Nakahata M, Nakayama S, Okada A, Sakurai N, Shiozawa M, Suzuki Y, Takeuchi H, Takeuchi Y, Toshito T, Totsuka Y, Yamada S, Desai S, Earl M, Kearns E, Messier MD, Scholberg K, Stone JL, Sulak LR, Walter CW, Goldhaber M, Barszczak T, Casper D, Gajewski W, Kropp WR, Mine S, Liu DW, Price LR, Smy MB, Sobel HW, Vagins MR, Ganezer KS, Keig WE, Ellsworth RW, Tasaka S, Kibayashi A, Learned JG, Matsuno S, Takemori D, Hayato Y, Ishii T, Kobayashi T, Nakamura K, Obayashi Y, Oyama Y, Sakai A, Sakuda M, Kohama M, Suzuki AT, Inagaki T, Nakaya T, Nishikawa K, Haines TJ, Blaufuss E, Dazeley S, Lee KB, Svoboda R, Goodman JA, Guillian G, Sullivan GW, Turcan D, Habig A, Hill J, Jung CK, Martens K, Malek M, Mauger C, McGrew C, Sharkey E, Viren B, Yanagisawa C, Mitsuda C, Miyano K, Saji C, Shibata T, Kajiyama Y, Nagashima Y, Nitta K, Takita M, Yoshida M, Kim HI, Kim SB, Yoo J, Okazawa H, Ishizuka T, Etoh M, Gando Y, Hasegawa T, Inoue K, Ishihara K, Maruyama T, Shirai J, Suzuki A, Koshiba M, Hatakeyama Y, Ichikawa Y, Koike M, Nishijima K, Fujiyasu H, Ishino H, Morii M, Watanabe Y, Golebiewska U, Kielczewska D, Boyd SC, Stachyra AL, Wilkes RJ, and Young KK

Abstract

Solar neutrino measurements from 1258 days of data from the Super-Kamiokande detector are presented. The measurements are based on recoil electrons in the energy range 5.0-20.0 MeV. The measured solar neutrino flux is 2.32+/-0.03(stat)+0.08-0.07(syst)x10(6) cm(-2) x s(-1), which is 45.1+/-0.5(stat)+1.6-1.4(syst)% of that predicted by the BP2000 SSM. The day vs night flux asymmetry (Phi(n)-Phi(d))/Phi(average) is 0.033+/-0.022(stat)+0.013-0.012(syst). The recoil electron energy spectrum is consistent with no spectral distortion. For the hep neutrino flux, we set a 90% C.L. upper limit of 40x10(3) cm(-2) x s(-1), which is 4.3 times the BP2000 SSM prediction.

Published
2001
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34. Evidence for TeV Emission from GRB 970417a.

Author

Atkins R, Benbow W, Berley D, Chen ML, Coyne DG, Dingus BL, Dorfan DE, Ellsworth RW, Evans D, Falcone A, Fleysher L, Fleysher R, Gisler G, Goodman JA, Haines TJ, Hoffman CM, Hugenberger S, Kelley LA, Leonor I I, McConnell M, McCullough JF, McEnery JE, Miller RS, Mincer AI, Morales MF, Nemethy P, Ryan JM, Shen B, Shoup A, Sinnis C, Smith AJ, Sullivan GW, Tumer T, Wang K, Wascko MO, Westerhoff S, Williams DA, Yang T, and Yodh GB

Abstract

Milagrito, a detector sensitive to very high energy gamma rays, monitored the northern sky from 1997 February through 1998 May. With a large field of view and a high duty cycle, this instrument was well suited to perform a search for TeV gamma-ray bursts (GRBs). We report on a search made for TeV counterparts to GRBs observed by BATSE. BATSE detected 54 GRBs within the field of view of Milagrito during this period. An excess of events coincident in time and space with one of these bursts, GRB 970417a, was observed by Milagrito. The excess has a chance probability of 2.8x10-5 of being a fluctuation of the background. The probability for observing an excess at least this large from any of the 54 bursts is 1.5x10-3. No significant correlations were detected from the other bursts.

Published
2000
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35. TeV Observations of Markarian 501 with the Milagrito Water Cerenkov Detector.

Author

Atkins R, Benbow W, Berley D, Chen ML, Coyne DG, Delay RS, Dingus BL, Dorfan DE, Ellsworth RW, Espinoza C, Evans D, Falcone A, Fleysher L, Fleysher R, Gisler G, Goodman JA, Haines TJ, Hoffman CM, Hugenberger S, Kelley LA, Leonor I I, McConnell M, McCullough JF, McEnery JE, Miller RS, Mincer AI, Morales MF, Murray MM, Nemethy P, Ryan JM, Schneider M, Shen B, Shoup A, Sinnis C, Smith AJ, Sullivan GW, Thompson TN, Tumer T, Wang K, Wascko MO, Westerhoff S, Williams DA, Yang T, and Yodh GB

Abstract

The Milagrito water Cerenkov detector near Los Alamos, New Mexico, was operated as a sky monitor at energies of a few TeV between 1997 February and 1998 May, including the period of the strong, long-lasting 1997 flare of Markarian 501. Milagrito served as a test run for the full Milagro detector. An event excess with a significance of 3.7 sigma from Markarian 501 was observed, in agreement with expectations.

Published
1999
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37. New limit on the rate-density of evaporating black holes.

Author

Alexandreas DE, Allen GE, Berley D, Biller S, Burman RL, Cavalli-Sforza M, Chang CY, Chen ML, Chumney P, Coyne D, Dion C, Dion GM, Dorfan D, Ellsworth RW, Goodman JA, Haines TJ, Harmon M, Hoffman CM, Kelley L, Klein S, Nagle DE, Schmidt DM, Schnee R, Sinnis C, Shoup A, Stark MJ, Weeks DD, Williams DA, Wu JP, Yang T, Yodh GB, and Zhang WP

Published
1993
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41. Measurement of atmospheric neutrino composition with the IMB-3 detector.

Author

Casper D, Becker-Szendy R, Bratton CB, Cady DR, Claus R, Dye ST, Gajewski W, Goldhaber M, Haines TJ, Halverson PG, Jones TW, Kielczewska D, Kropp WR, Learned JG, LoSecco JM, McGrew C, Matsuno S, Matthews J, Mudan MS, Price L, Reines F, Schultz J, Sinclair D, Sobel HW, Stone JL, Sulak LR, Svoboda R, Thornton G, and van der Velde JC

Published
1991
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44. Search for proton decay into e++ pi 0 in the IMB-3 detector.

Author

Becker-Szendy R, Bratton CB, Cady DR, Casper D, Claus R, Crouch M, Dye ST, Gajewski W, Goldhaber M, Haines TJ, Halverson PG, Jones TW, Kielczewska D, Kropp WR, Learned JG, LoSecco JM, McGrew C, Matsuno S, Mudan MS, Price L, Reines F, Schultz J, Sinclair D, Sobel HW, Stone JL, Sulak LR, Svoboda R, Thornton G, and van der Velde JC

Published
1990
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47. Experimental limits on the nucleon lifetime for two- and three-body decay modes.

Author

Park HS, Blewitt G, Cortez BG, Foster GW, Gajewski W, Haines TJ, Kielczewska D, LoSecco JM, Bionta RM, Bratton CB, Casper D, Chrysicopoulou P, Claus R, Errede S, Ganezer KS, Goldhaber M, Jones TW, Kropp WR, Learned JG, Lehmann E, Reines F, Schultz J, Seidel S, Shumard E, Sinclair D, Sobel HW, Stone JL, Sulak LR, Svoboda R, van der Velde JC, and Wuest C

Published
1985
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48. Search for multitrack nucleon decay.

Author

Seidel S, Bionta RM, Blewitt G, Bratton CB, Casper D, Ciocio A, Claus R, Dye ST, Errede S, Foster GW, Gajewski W, Ganezer KS, Goldhaber M, Haines TJ, Jones TW, Kielczewska D, Kropp WR, Learned JG, LoSecco JM, Matthews J, Park HS, Price L, Reines F, Schultz J, Shumard E, Sinclair D, Sobel HW, Stone JL, Sulak L, Svoboda R, Thornton G, van der Velde JC, and Wuest C

Published
1988
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49. Underground search for muons correlated with Cygnus X-3.

Author

Bionta RM, Blewitt G, Bratton CB, Casper D, Ciocio A, Claus R, Crouch M, Dye ST, Errede S, Foster GW, Gajewski W, Ganezer KS, Goldhaber M, Haines TJ, Jones TW, Kielczewska D, Kropp WR, Learned JG, LoSecco JM, Matthews J, Park HS, Price LR, Reines F, Schulz J, Seidel S, Shumard E, Sinclair D, Sobel HW, Stone JL, Sulak L, Svoboda R, Thornton G, van der Velde JC, and Wuest C

Published
1987
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50. Limits on the neutrino lifetime.

Author

LoSecco JM, Bionta RM, Blewitt G, Bratton CB, Casper D, Claus R, Cortez B, Errede S, Foster G, Gajewski W, Ganezer KS, Goldhaber M, Haines TJ, Jones TW, Kielczewska D, Kropp WR, Learned JG, Lehmann E, Park HS, Reines F, Schultz J, Seidel S, Shumard E, Sinclair D, Sobel HW, Stone JL, Sulak L, Svoboda R, Van der Velde JC, and Wuest C

Published
1987
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