Open Access. Powered by Scholars. Published by Universities.®
Physical Sciences and Mathematics Commons™
Open Access. Powered by Scholars. Published by Universities.®
Articles 1 - 22 of 22
Full-Text Articles in Physical Sciences and Mathematics
Three-Dimensional Imaging And Detection Efficiency Performance Of Orthogonal Coplanar Czt Strip Detectors, Mark L. Mcconnell, John R. Macri, James M. Ryan, K Larson, L A. Hamel, G Bernard, C Pomerleau, O Tousignant, Jean-Charles Leroux, V T. Jordanov
Three-Dimensional Imaging And Detection Efficiency Performance Of Orthogonal Coplanar Czt Strip Detectors, Mark L. Mcconnell, John R. Macri, James M. Ryan, K Larson, L A. Hamel, G Bernard, C Pomerleau, O Tousignant, Jean-Charles Leroux, V T. Jordanov
Space Science Center
We report on recent three-dimensional imaging performance and detection efficiency measurements obtained with 5 mm thick prototype CdZnTe detectors fabricated with orthogonal coplanar anode strips. In previous work, we have shown that detectors fabricated using this design achieve both very good energy resolution and sub-millimeter spatial resolution with fewer electronic channels than are required for pixel detectors. As electron-only devices, like pixel detectors, coplanar anode strip detectors can be fabricated in the thickness required to be effective imagers for photons with energies in excess of 500 keV. Unlike conventional double-sided strip detectors, the coplanar anode strip detectors require segmented contacts …
Analog Processing Of Signals From A Czt Strip Detector With Orthogonal Coplanar Anodes, K Larson, V T. Jordanov, Mark L. Mcconnell, John R. Macri, James M. Ryan, A Drake, L A. Hamel, O Tousignant
Analog Processing Of Signals From A Czt Strip Detector With Orthogonal Coplanar Anodes, K Larson, V T. Jordanov, Mark L. Mcconnell, John R. Macri, James M. Ryan, A Drake, L A. Hamel, O Tousignant
Space Science Center
We present the requirements, design, and performance of an analog circuit for processing the non-collecting anode strip signals from a cadmium zinc telluride (CZT) strip detector with orthogonal coplanar anodes. Detector signal simulations and measurements with a prototype are used to define the range of signal characteristics as a function of location of the gamma interaction in the detector. The signals from the non- collecting anode strip electrodes are used to define two of the three spatial coordinates including the depth of interaction, the z dimension. Analog signal processing options are discussed. A circuit to process the signals from the …
Mev Measurements Of Γ-Ray Bursts By Cgro-Comptel: Revised Catalog, A Connors, C A. Young, K Bennett, W Collmar, W Hermsen, R M. Kippen, L Kuiper, Mark L. Mcconnell, R S. Miller, James M. Ryan, V Schonfelder, O R. Williams, C Winkler
Mev Measurements Of Γ-Ray Bursts By Cgro-Comptel: Revised Catalog, A Connors, C A. Young, K Bennett, W Collmar, W Hermsen, R M. Kippen, L Kuiper, Mark L. Mcconnell, R S. Miller, James M. Ryan, V Schonfelder, O R. Williams, C Winkler
Space Science Center
The imaging COMPTEL telescope has accumulated 0.1–30 MeV spectra, time-histories, and positions of more than forty γ-ray bursts within its ∼3 sr field of view in the eight years since its launch. CGRO-COMPTEL measures in both imaging “telescope” and single detector “burst spectroscopy” mode. In an ongoing collaboration with BACODINE/GCN, bursts are imaged automatically, with localizations relayed to a global network of multiwavelength observers in near real time (∼10 minutes). We have updated our burst search procedure in two ways: 1) using more sensitive search algorithms; and 2) using data from more detectors. The first are double change-point algorithms. With …
The Spectral Variability Of Cygnus X-1 At Mev Energies, Mark L. Mcconnell, K Bennett, H Bloemen, W Collmar, W Hermsen, L Kuiper, B F. Phlips, James M. Ryan, V Schonfelder, H Steinle, A W. Strong
The Spectral Variability Of Cygnus X-1 At Mev Energies, Mark L. Mcconnell, K Bennett, H Bloemen, W Collmar, W Hermsen, L Kuiper, B F. Phlips, James M. Ryan, V Schonfelder, H Steinle, A W. Strong
Space Science Center
In previous work, we have used data from the first three years of the CGRO mission to assemble a broad-band γ-ray spectrum of the galactic black hole candidate Cygnus X-1. Contemporaneous data from the COMPTEL, OSSE and BATSE experiments on CGRO were selected on the basis of the hard X-ray flux (45–140 keV) as measured by BATSE. This provided a spectrum of Cygnus X-1 in its canonical low X-ray state (as measured at energies below 10 keV), covering the energy range from 50 keV to 5 MeV. Here we report on a comparison of this spectrum to a COMPTELOSSE spectrum …
Comptel 1.8 Mev All Sky Survey: The Cygnus Region, S Pluschke, R Diehl, V Schonfelder, G Weidenspointer, H Bloemen, W Hermsen, Mark L. Mcconnell, James M. Ryan, K Bennett, U Oberlack, J Knodlseder
Comptel 1.8 Mev All Sky Survey: The Cygnus Region, S Pluschke, R Diehl, V Schonfelder, G Weidenspointer, H Bloemen, W Hermsen, Mark L. Mcconnell, James M. Ryan, K Bennett, U Oberlack, J Knodlseder
Space Science Center
We present an updated version of COMPTEL’s 1.809 MeV sky survey. Based on eight years of observations we compare results from different imaging techniques using background from adjacent energy bands. We confirm the previously reported characteristics of the galactic 1.809 MeV emission, specifically an extended galactic ridge emission, mainly concentrated towards the inner galaxy, a peculiar emission feature in the Cygnus region, and a low-intensity ridge extending towards Carina and Vela. Because this gamma ray line is due to the decay of radioactive 26Al, predominantly synthesized in massive stars, one anticipates flux enhancements aligned with regions of recent star formation. …
The Comptel Instrumental-Line Background, G Weidenspointer, M Varendorff, U Oberlack, S Pluschke, D Morris, R Diehl, S C. Kappadath, Mark L. Mcconnell, James M. Ryan, V Schonfelder
The Comptel Instrumental-Line Background, G Weidenspointer, M Varendorff, U Oberlack, S Pluschke, D Morris, R Diehl, S C. Kappadath, Mark L. Mcconnell, James M. Ryan, V Schonfelder
Space Science Center
The instrumental-line background of the Compton telescope COMPTEL onboard the Compton Gamma-Ray Observatory is due to the activation and/or decay of a number of different isotopes. The major components of the COMPTEL instrumental-line background can be attributed to eight individual isotopes, namely 2D, 22Na, 24Na, 28Al, 40K, 52Mn, 57Ni, and 208Tl. In addition, evidence for the presence of 27Mg has been obtained in the search for gamma-ray lines from supernovae. The identification of the instrumental lines with specific isotopes is based on the line energies as well as on the variation of the activity with time, cosmic-ray intensity and deposited …
Spectra Of A Recent Bright Burst Measured By Cgro-Comptel: Grb 990123, C A. Young, A Connors, K Bennett, W Collmar, W Hermsen, R M. Kippen, E Kolaczyk, L Kuiper, Mark L. Mcconnell, R S. Miller, James M. Ryan, V Schonfelder, O R. Williams, C Winkler
Spectra Of A Recent Bright Burst Measured By Cgro-Comptel: Grb 990123, C A. Young, A Connors, K Bennett, W Collmar, W Hermsen, R M. Kippen, E Kolaczyk, L Kuiper, Mark L. Mcconnell, R S. Miller, James M. Ryan, V Schonfelder, O R. Williams, C Winkler
Space Science Center
CGRO-COMPTEL measures gamma-ray burst positions, time-histories and spectra in the 0.1–30 MeV energy range, in both imaging “telescope” and single detector “burst spectroscopy” mode. GRB 990123, one of the most recent bright bursts seen by COMPTEL, was caught in the optical while the gamma-ray emission was ongoing. The burst spectral shape can be characterized by a peak in ν−Fν just below 1 MeV and a power-law tail above(photon index∼−2.4,) and flattening below. There is also spectral evolution by downward movement of the peak and/or softening of the power laws. We present light-curves, time resolved spectra and an image map for …
Milagro: A Tev Observatory For Gamma-Ray Bursts, B L. Dingus, R Atkins, W Benbow, D Berley, M L. Chen, D G. Coyne, R W. Ellsworth, D Evans, A Falcone, L Fleysher, R Fleysher, G Gisler, J A. Goodman, T J. Haines, C M. Hoffman, S Hugenberger, L A. Kelley, I Leonor, Mark L. Mcconnell, J F. Mccullough, J E. Mcenery, R S. Miller, A I. Mincer, M F. Morales, P Nemethy, James M. Ryan, B Shen, A Shoup, C Sinnis, A J. Smith, G W. Sullivan, O T. Tumer, K Wang, M O. Wascko, S Westerhoff, D A. Williams, T Yang, G B. Yodh
Milagro: A Tev Observatory For Gamma-Ray Bursts, B L. Dingus, R Atkins, W Benbow, D Berley, M L. Chen, D G. Coyne, R W. Ellsworth, D Evans, A Falcone, L Fleysher, R Fleysher, G Gisler, J A. Goodman, T J. Haines, C M. Hoffman, S Hugenberger, L A. Kelley, I Leonor, Mark L. Mcconnell, J F. Mccullough, J E. Mcenery, R S. Miller, A I. Mincer, M F. Morales, P Nemethy, James M. Ryan, B Shen, A Shoup, C Sinnis, A J. Smith, G W. Sullivan, O T. Tumer, K Wang, M O. Wascko, S Westerhoff, D A. Williams, T Yang, G B. Yodh
Space Science Center
Observation of prompt TeV γ-rays from GRBs requires a new type of detector to overcome the low duty factor and small field of view of current TeV observatories. Milagro is such a new type of very high energy (> a few 100 GeV) gamma-ray observatory, which has a large field of view of >1 steradian and 24 hours/day operation. Milagrito, a prototype for Milagro, was operated from February 1997 to May 1998. During the summer of 1998, Milagrito was dismantled and Milagro was built. Both detectors use a 80 m×60 m×8 m pond of water in which a 3 m×3 …
Estimation Of Grb Detection By Fiberglast, Surasak Phengchamnan, K Aisaka, Muzaffer Atac, W Robert Binns, J Buckley, M L. Cherry, David B. Cline, Paul F. Dowkontt, John W. Epstein, M H. Finger, Gerald J. Fishman, T G. Guzik, P L. Hink, Martin H. Israel, S C. Kappadath, Gerald Karr, R M. Kippen, John R. Macri, Robert S. Mallozzi, Mark L. Mcconnell, Yuriy Pischalnikov, W Paciesas, Thomas A. Parnell, Geoffrey N. Pendleton, R D. Preece, Georgia A. Richardson, Keith R. Rielage, James M. Ryan, J G. Stacy, O T. Tumer, Donald B. Wallace, Robert B. Wilson
Estimation Of Grb Detection By Fiberglast, Surasak Phengchamnan, K Aisaka, Muzaffer Atac, W Robert Binns, J Buckley, M L. Cherry, David B. Cline, Paul F. Dowkontt, John W. Epstein, M H. Finger, Gerald J. Fishman, T G. Guzik, P L. Hink, Martin H. Israel, S C. Kappadath, Gerald Karr, R M. Kippen, John R. Macri, Robert S. Mallozzi, Mark L. Mcconnell, Yuriy Pischalnikov, W Paciesas, Thomas A. Parnell, Geoffrey N. Pendleton, R D. Preece, Georgia A. Richardson, Keith R. Rielage, James M. Ryan, J G. Stacy, O T. Tumer, Donald B. Wallace, Robert B. Wilson
Space Science Center
FiberGLAST is one of several instrument concepts being developed for possible inclusion as the primary Gamma-ray Large Area Space Telescope (GLAST) instrument. The predicted FiberGLAST effective area is more than 12,000 cm2 for energies between 30 MeV and 300 GeV, with a field of view that is essentially flat from 0°–80°. The detector will achieve a sensitivity more than 10 times that of EGRET. We present results of simulations that illustrate the sensitivity of FiberGLAST for the detection of gamma-ray bursts.
Improved Comptel Maps Of The Milky Way, H Bloemen, K Bennett, W Collmar, R Diehl, W Hermsen, A Iyudin, J Knodlseder, Mark L. Mcconnell, James M. Ryan, V Schonfelder, A W. Strong
Improved Comptel Maps Of The Milky Way, H Bloemen, K Bennett, W Collmar, R Diehl, W Hermsen, A Iyudin, J Knodlseder, Mark L. Mcconnell, James M. Ryan, V Schonfelder, A W. Strong
Space Science Center
In the course of the mission we have gradually developed an analysis method that separates in an iterative manner the celestial emission and the (a priori unknown) instrumental background. It has become our standard analysis tool for point sources. We illustrate here that this method is widely applicable now. It provides mutually consistent sets of model-fitting parameters (spectra) and sky maps, both for continuum and line studies. Because of the wide applicability, it has been possible to make various cross-checks while building up confidence in this procedure.
Comptel Time-Averaged All-Sky Point Source Analysis, W Collmar, V Schonfelder, A W. Strong, H Bloemen, W Hermsen, Mark L. Mcconnell, James M. Ryan, K Bennett
Comptel Time-Averaged All-Sky Point Source Analysis, W Collmar, V Schonfelder, A W. Strong, H Bloemen, W Hermsen, Mark L. Mcconnell, James M. Ryan, K Bennett
Space Science Center
We use all COMPTEL data from the beginning of the CGRO mission (April ’91) up to the end of CGRO Cycle 6 (November ’97) to carry out all-sky point source analyses in the four standard COMPTEL energy bands for different time periods. We apply our standard maximum-likelihood method to generate all-sky significance and flux maps for point sources by subtracting off the diffuse emission components via model fitting. In addition, fluxes of known sources have been determined for individual CGRO Phases/Cycles to generate lightcurves with a time resolution of the order of one year. The goal of the analysis is …
Energetic Proton Spectra In The 11 June 1991 Solar Flare, C A. Young, M B. Arndt, A Connors, Mark L. Mcconnell, G Rank, James M. Ryan, R Suleiman, V Schonfelder
Energetic Proton Spectra In The 11 June 1991 Solar Flare, C A. Young, M B. Arndt, A Connors, Mark L. Mcconnell, G Rank, James M. Ryan, R Suleiman, V Schonfelder
Space Science Center
We have studied a subset of the 11 June 1991 solar flare γ-ray data that we believe arise from soft proton or ion spectra. Using data from the COMPTEL instrument on the Compton Observatory we discuss the gamma-ray intensities at 2.223 MeV, 4–7 MeV, and 8–30 MeV in terms of the parent proton spectrum responsible for the emission.
Results From The Milagrito Experiment, A J. Smith, R Atkins, W Benbow, D Berley, M L. Chen, D G. Coyne, B L. Dingus, D E. Dorfan, R W. Ellsworth, D Evans, A Falcone, L Fleysher, R Fleysher, G Gisler, J A. Goodman, T J. Haines, C M. Hoffman, S Hugenberger, L A. Kelley, I Leonor, Mark L. Mcconnell, J F. Mccullough, J E. Mcenery, R S. Miller, A I. Mincer, M F. Morales, P Nemethy, James M. Ryan, B Shen, A Shoup, G Sinnis, G W. Sullivan, O T. Tumer, K Wang, M O. Wascko, S Westerhoff, D A. Williams, T Yang, G B. Yodh
Results From The Milagrito Experiment, A J. Smith, R Atkins, W Benbow, D Berley, M L. Chen, D G. Coyne, B L. Dingus, D E. Dorfan, R W. Ellsworth, D Evans, A Falcone, L Fleysher, R Fleysher, G Gisler, J A. Goodman, T J. Haines, C M. Hoffman, S Hugenberger, L A. Kelley, I Leonor, Mark L. Mcconnell, J F. Mccullough, J E. Mcenery, R S. Miller, A I. Mincer, M F. Morales, P Nemethy, James M. Ryan, B Shen, A Shoup, G Sinnis, G W. Sullivan, O T. Tumer, K Wang, M O. Wascko, S Westerhoff, D A. Williams, T Yang, G B. Yodh
Space Science Center
The Milagro water Cherenkov detector near Los Alamos, New Mexico is the first air shower detector capable of continuously monitoring the sky at energies between 500 GeV and 20 TeV. Preliminary results of the Milagro experiment are presented. A predecessor of the Milagro detector, Milagrito, was operational from February 1997 to May 1998. Milagrito consisted of 228 8″ photomultiplier tubes (PMTs) arranged in a grid with a 2.8 meter spacing and submerged in 1–2 meters of water. During its operation, Milagrito collected in excess of 9 billion events with a median energy of about 3 TeV. The detector’s sensitivity …
Gamma Ray Measurements Of The 1991 November 15 Solar Flare, M B. Arndt, K Bennett, A Connors, Mark L. Mcconnell, G Rank, James M. Ryan, V Schonfelder, R Suleiman, C A. Young
Gamma Ray Measurements Of The 1991 November 15 Solar Flare, M B. Arndt, K Bennett, A Connors, Mark L. Mcconnell, G Rank, James M. Ryan, V Schonfelder, R Suleiman, C A. Young
Space Science Center
The 1991 November 15 X1.5 flare was a well observed solar event. Comprehensive data from ground-based observatories and spacecraft provide the basis for a contextual interpretation of gamma-ray spectra from the Compton Gamma Ray Observatory (CGRO). In particular, spectral, spatial, and temporal data at several energies are necessary to understand the particle dynamics and the acceleration mechanism(s) within this flare. X-ray images, radio, Ca XIX data and magnetograms provide morphological information on the acceleration region [4,5], while gamma-ray spectral data provide information on the parent ion spectrum. Furthermore, time profiles in hard X-rays and gamma-rays provide valuable information on temporal …
The Development Of A Position-Sensitive Czt Detector With Orthogonal Co-Planar Anode Strips, K Larson, L A. Hamel, V T. Jordanov, John R. Macri, Mark L. Mcconnell, James M. Ryan, O Tousignant, A Vincent
The Development Of A Position-Sensitive Czt Detector With Orthogonal Co-Planar Anode Strips, K Larson, L A. Hamel, V T. Jordanov, John R. Macri, Mark L. Mcconnell, James M. Ryan, O Tousignant, A Vincent
Space Science Center
We report on the simulation, construction, and performance of prototype CdZnTe imaging detectors with orthogonal coplanar anode strips. These detectors employ a novel electrode geometry with non-collecting anode strips in one dimension and collecting anode pixels, interconnected in rows, in the orthogonal direction. These detectors retain the spectroscopic and detection efficiency advantages of single carrier (electron) sensing devices as well as the principal advantage of conventional strip detectors with orthogonal anode and cathode strips, i.e. an N×N array of imaging pixels are with only 2N electronic channels. Charge signals induced on the various electrodes of a prototype detector with 8×8 …
Comptel Upper Limits For The 56co Γ-Rays From Sn1998bu, R Georgii, S Pluschke, R Diehl, W Collmar, G G. Lichti, V Schonfelder, H Bloemen, J Knodlseder, Mark L. Mcconnell, James M. Ryan, K Bennett
Comptel Upper Limits For The 56co Γ-Rays From Sn1998bu, R Georgii, S Pluschke, R Diehl, W Collmar, G G. Lichti, V Schonfelder, H Bloemen, J Knodlseder, Mark L. Mcconnell, James M. Ryan, K Bennett
Space Science Center
The type Ia supernova SN 1998bu in M96 was observed by COMPTEL for a total of 88 days starting 17 days after the detection of the SN. A special mode improving the low-energy sensitivity was invoked. We obtained images in the 847 keV and 1238 keV lines of 56Co using an improved point-spread function for the low-energies. We do not detect SN1998bu. Sensitive upper limits at both energies constrain the standard supernova model for this event.
First Results Of A Study Of Tev Emission From Grbs In Milagrito, J E. Mcenery, R Atkins, W Benbow, D Berley, M L. Chen, D G. Coyne, B L. Dingus, D E. Dorfan, R W. Ellsworth, D Evans, A Falcone, L Fleysher, R Fleysher, G Gisler, J A. Goodman, T J. Haines, C M. Hoffman, S Hugenberger, L A. Kelley, I Leonor, Mark L. Mcconnell, J F. Mccullough, R S. Miller, A I. Mincer, M F. Morales, P Nemethy, James M. Ryan, B Shen, A Shoup, C Sinnis, A J. Smith, G W. Sullivan, O T. Tumer, K Wang, M O. Wascko, S Westerhoff, D A. Williams, T Yang, G B. Yodh
First Results Of A Study Of Tev Emission From Grbs In Milagrito, J E. Mcenery, R Atkins, W Benbow, D Berley, M L. Chen, D G. Coyne, B L. Dingus, D E. Dorfan, R W. Ellsworth, D Evans, A Falcone, L Fleysher, R Fleysher, G Gisler, J A. Goodman, T J. Haines, C M. Hoffman, S Hugenberger, L A. Kelley, I Leonor, Mark L. Mcconnell, J F. Mccullough, R S. Miller, A I. Mincer, M F. Morales, P Nemethy, James M. Ryan, B Shen, A Shoup, C Sinnis, A J. Smith, G W. Sullivan, O T. Tumer, K Wang, M O. Wascko, S Westerhoff, D A. Williams, T Yang, G B. Yodh
Space Science Center
Milagrito, a detector sensitive to γ-rays at TeV energies, monitored the northern sky during the period February 1997 through May 1998. With a large field of view and high duty cycle, this instrument was used to perform a search for TeV counterparts to γ-ray bursts. Within the Milagrito field of view 54 γ-ray bursts at keV energies were observed by the Burst And Transient Satellite Experiment (BATSE) aboard the Compton Gamma-Ray Observatory. This paper describes the results of a preliminary analysis to search for TeV emission correlated with BATSE detected bursts. Milagrito detected an excess of events coincident both spatially …
Summary Of The First Comptel Source Catalogue, V Schonfelder, K Bennett, J J. Blom, H Bloemen, W Collmar, A Connors, R Diehl, W Hermsen, A Iyudin, R M. Kippen, J Knodlseder, L Kuiper, G G. Lichti, Mark L. Mcconnell, D Morris, R Much, U Oberlack, James M. Ryan, G Stacy, H Steinle, A W. Strong, R Suleiman, R Vandijk, M Varendorff, C Winkler, O R. Williams
Summary Of The First Comptel Source Catalogue, V Schonfelder, K Bennett, J J. Blom, H Bloemen, W Collmar, A Connors, R Diehl, W Hermsen, A Iyudin, R M. Kippen, J Knodlseder, L Kuiper, G G. Lichti, Mark L. Mcconnell, D Morris, R Much, U Oberlack, James M. Ryan, G Stacy, H Steinle, A W. Strong, R Suleiman, R Vandijk, M Varendorff, C Winkler, O R. Williams
Space Science Center
No abstract provided.
Milagro: A Tev Gamma-Ray Monitor Of The Northern Hemisphere Sky, B L. Dingus, R Atkins, W Benbow, D Berley, M L. Chen, D G. Coyne, D E. Dorfan, R W. Ellsworth, D Evans, A Falcone, L Fleysher, R Fleysher, G Gisler, J A. Goodman, T J. Haines, C M. Hoffman, S Hugenberger, L A. Kelley, I Leonor, Mark L. Mcconnell, J F. Mccullough, J E. Mcenery, R S. Miller, A I. Mincer, M F. Morales, P Nemethy, James M. Ryan, B Shen, A Shoup, C Sinnis, A J. Smith, G W. Sullivan, O T. Tumer, K Wang, M O. Wascko, S Westerhoff, D A. Williams, T Yang, G B. Yodh
Milagro: A Tev Gamma-Ray Monitor Of The Northern Hemisphere Sky, B L. Dingus, R Atkins, W Benbow, D Berley, M L. Chen, D G. Coyne, D E. Dorfan, R W. Ellsworth, D Evans, A Falcone, L Fleysher, R Fleysher, G Gisler, J A. Goodman, T J. Haines, C M. Hoffman, S Hugenberger, L A. Kelley, I Leonor, Mark L. Mcconnell, J F. Mccullough, J E. Mcenery, R S. Miller, A I. Mincer, M F. Morales, P Nemethy, James M. Ryan, B Shen, A Shoup, C Sinnis, A J. Smith, G W. Sullivan, O T. Tumer, K Wang, M O. Wascko, S Westerhoff, D A. Williams, T Yang, G B. Yodh
Space Science Center
A new type of very high energy (> a few 100 GeV) gamma-ray observatory, Milagro, has been built with a large field of view of >1 steradian and nearly 24 hours/day operation. Milagrito, a prototype for Milagro, was operated from February 1997 to May 1998. During the summer of 1998, Milagrito was dismantled and Milagro was built. Both detectors use a 80 m×60 m×8 mpond of water in which a 3 m×3 m grid of photomultiplier tubes detects the Cherenkov light produced in the water by the relativistic particles in extensive air showers. Milagrito was smaller and had only one …
The Tigre Gamma-Ray Telescope, Terence J. O'Neill, D Battacharya, D Dixon, M Polson, R S. White, Allen Zych, James M. Ryan, Mark L. Mcconnell, John R. Macri, J Samimi, A Akyuz, W M. Mahoney, L Varnell
The Tigre Gamma-Ray Telescope, Terence J. O'Neill, D Battacharya, D Dixon, M Polson, R S. White, Allen Zych, James M. Ryan, Mark L. Mcconnell, John R. Macri, J Samimi, A Akyuz, W M. Mahoney, L Varnell
Space Science Center
TIGRE is an advanced telescope for gamma-ray astronomy with a few arcmin resolution. From 0.3 to 10 MeV it is a Compton telescope. Above 1 MeV, its multi-layers of double sided silicon strip detectors allow for Compton recoil electron tracking and the unique determination for incident photon direction. From 10 to 100 MeV the tracking feature is utilized for gamma-ray pair event reconstruction. Here we present TIGRE energy resolutions, background simulations and the development of the electronics readout system.
Detection Of 6 November 1997 Ground Level Event By Milagrito, A Falcone, R Atkins, W Benbow, D Berley, M L. Chen, D G. Coyne, B L. Dingus, D E. Dorfan, R W. Ellsworth, D Evans, L Fleysher, R Fleysher, G Gisler, J A. Goodman, T J. Haines, C M. Hoffman, S Hugenberger, L A. Kelley, I Leonor, John R. Macri, Mark L. Mcconnell, J F. Mccullough, J E. Mcenery, R S. Miller, A I. Mincer, M F. Morales, P Nemethy, James M. Ryan, B Shen, A Shoup, G Sinnis, A J. Smith, G W. Sullivan, O T. Tumer, K Wang, M O. Wascko, S Westerhoff, D A. Williams, T Yang, G B. Yodh
Detection Of 6 November 1997 Ground Level Event By Milagrito, A Falcone, R Atkins, W Benbow, D Berley, M L. Chen, D G. Coyne, B L. Dingus, D E. Dorfan, R W. Ellsworth, D Evans, L Fleysher, R Fleysher, G Gisler, J A. Goodman, T J. Haines, C M. Hoffman, S Hugenberger, L A. Kelley, I Leonor, John R. Macri, Mark L. Mcconnell, J F. Mccullough, J E. Mcenery, R S. Miller, A I. Mincer, M F. Morales, P Nemethy, James M. Ryan, B Shen, A Shoup, G Sinnis, A J. Smith, G W. Sullivan, O T. Tumer, K Wang, M O. Wascko, S Westerhoff, D A. Williams, T Yang, G B. Yodh
Space Science Center
Solar Energetic Particles (SEPs) with energies exceeding 10 GeV associated with the 6 November 1997 solar flare/CME (coronal mass ejection) have been detected with Milagrito, a prototype of the Milagro Gamma Ray Observatory. While SEP acceleration beyond 1 GeV is well established, few data exist for protons or ions beyond 10 GeV. The Milagro observatory, a ground based water Cherenkov detector designed for observing very high energy gamma ray sources, can also be used to study the Sun. Milagrito, which operated for approximately one year in 1997/98, was sensitive to solar proton and neutron fluxes above ∼4 GeV. In its …
Minute-Of-Arc Resolution Gamma Ray Imaging Experiment—Margie, S C. Kappadath, P P. Altice, M L. Cherry, T G. Guzik, J G. Stacy, John R. Macri, Mark L. Mcconnell, James M. Ryan, D L. Band, J L. Matteson, Terence J. O'Neill, Allen Zych, J Buckley, P L. Hink
Minute-Of-Arc Resolution Gamma Ray Imaging Experiment—Margie, S C. Kappadath, P P. Altice, M L. Cherry, T G. Guzik, J G. Stacy, John R. Macri, Mark L. Mcconnell, James M. Ryan, D L. Band, J L. Matteson, Terence J. O'Neill, Allen Zych, J Buckley, P L. Hink
Space Science Center
MARGIE (Minute-of-Arc Resolution Gamma-ray Imaging Experiment) is a large area(∼104 cm2), wide field-of-view (∼1 sr), hard X-ray/gamma-ray (∼20–600 keV) coded-mask imaging telescope capable of performing a sensitive survey of both steady and transient cosmic sources. MARGIE has been selected for a NASA mission-concept study for an Ultra Long Duration (100 day) Balloon flight. We describe our program to develop the instrument based on new detector technology of either cadmium zinc telluride (CZT) semiconductors or pixellated cesium iodide (CsI) scintillators viewed by fast-timing bi-directional charge-coupled devices (CCDs). The primary scientific objectives are to image faint Gamma-Ray Bursts (GRBs) in near-real-time at …