Large Area Double Scattering Telescope for Balloon-Borne Studies of Neutrons and Gamma Rays

Zych, A. D.; Herzo, D.; Koga, R.; Millard, W. A.; Moon, S.; Ryan, J. M.; Wilson, Robert B.; White, R. S.; Dayton, B.

doi:10.1109/tns.1975.4327713

Cited by 18 publications

(5 citation statements)

References 5 publications

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“…OBSERVATIONS. The gamma ray telescope used for the observations is shown in Figure 1 Zych et al, 1975). A gamma ray is identified by a scatter in the liquid scintillator S1 followed by a second scatter in S2 with no accompanying signal from anticoincidence shields Al and A2.…”

mentioning

confidence: 99%

Gamma-ray spectroscopy in astrophysics

Ramaty

Kline

Weaver

1978

Nature

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This was the first symposium devoted entirely to spectroscopy in gamma ray astronomy. Its purposes were to bring together most of the scientists contributing to all the aspects, experimental and theoretical, of this new field and to discuss and compare ideas, measurements, calcu lations and technical experience in what we confidently expect to be a very important new discipline in high energy astrophysics.This goal was achieved, we feel, in that a very large fraction of all that is known about gamma ray spectroscopy in astrophysics was indeed presented or discussed at the Symposium, yet many of these results are new, presented here for the first time. Further, the discipline is on the brink of moving to the next level of development within the coming year, with a number of satellite experiments and major balloon experiments in gamma ray spectroscopy and in related astrophysical sciences about to be launched. We therefore felt that we should publish the Proceedings as soon as possible, without the delays involved in reformatting the manuscripts and extensive editing. We hope that the information that will thus become available will prove to be useful to all workers in these fields.We have ordered the papers approximately as presented, with experimental and theoretical papers combined in each session. The introductory session is followed by the sessions on solar, stellar, and planetary gamma ray spectroscopy, and on cosmic gamma ray spectroscopy, with the technical discussions and previews of new experiments in the last two sessions.The Symposium was organized by the editors of these proceedings, T. L. Cline and R. Ramaty. We wish to thank the Symposium Session Chairmen, D. D. Clayton, and M. M. Shapiro, and the Workshop Session Chairmen, G. J. Fishman and N. S. Wall, for their assistance. We are grateful to R. C. Reedy for supplying us the manuscript on Planetary Gamma Ray Spectro scopy which was not presented at the Symposium. This paper is taken from the Proceedings of the Ninth Lunar and Planetary Science Conference (Pergamon Press 1978, with permission). We are also indebted to R. W. Bussard and R. P. Weaver for their help in running the conference. We thank F. B. McDonald for his continued support of this Symposium, and R. S. Cooper for his interest and his contribution. We thank Barbara Pratt in particular for her excellent secretarial help with both the organization of the Symposium and the preparation of this document. It is a pleasure for me to be here and welcome you all to the Goddard Space Flight Center. I noticed from the agenda that we have speakers from all the major groups that are interested in high energy astronomy and in particular in gamma ray astronomy virtually in the entire free world. The agenda is particularly interesting to me and I intend to spend as much of my time here over the next day as I can. I would like to make a couple of points. The people here at Goddard know that when they give me an oppor tunity to come and welcome you, the potential is always there for me to say something...

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confidence: 99%

Gamma-ray spectroscopy in astrophysics

Ramaty

Kline

Weaver

1978

Nature

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“…where E p is the proton recoil energy. We can estimate the scattered neutron energy E n using neutron time of flight between two scatters using E n = 1 2 m n v 2 = 1 2 m n d ∆t 2 (5) where m n is the mass of a neutron, v is the speed of the scattered neutron, d is the distance between the first and second neutron elastic scatter, and ∆t is the time between the two scatters. A second neutron scatter must occur, otherwise scattered neutron energy cannot be estimated and cone back-projection is impossible.…”

Section: Theorymentioning

confidence: 99%

“…One of the first known neutron scatter telescopes was proposed in 1968 [2]. The device was used to measure solar neutrons and the resulting albedo neutrons from earth at an altitude of 120,000 feet [3][4][5]. The device consisted of two large planes of mineral oil liquid scintillator, optically separated into four cells per plane, located 1 m apart.…”

Section: Previous Workmentioning

confidence: 99%

Model-based design evaluation of a compact, high-efficiency neutron scatter camera

Weinfurther

Mattingly

Brubaker

et al. 2018

Nuclear Instruments and Methods in Physics Research Section A:

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This paper presents the model-based design and evaluation of an instrument that estimates incident neutron direction using the kinematics of neutron scattering by hydrogen-1 nuclei in an organic scintillator. The instrument design uses a single, nearly contiguous volume of organic scintillator that is internally subdivided only as necessary to create optically isolated pillars, i.e., long, narrow parallelepipeds of organic scintillator. Scintillation light emitted in a given pillar is confined to that pillar by a combination of total internal reflection and a specular reflector applied to the four sides of the pillar transverse to its long axis. The scintillation light is collected at each end of the pillar using a photodetector, e.g., a microchannel plate photomultiplier (MCP-PM) or a silicon photomultiplier (SiPM). In this optically segmented design, the (x, y) position of scintillation light emission (where the x and y coordinates are transverse to the long axis of the pillars) is estimated as the pillar's (x, y) position in the scintillator "block", and the z-position (the position along the pillar's long axis) is estimated from the amplitude and relative timing of the signals produced by the photodetectors at each end of the pillar. The neutron's incident direction and energy is estimated from the (x, y, z)-positions of two sequential neutron-proton scattering interactions in the scintillator block using elastic scatter kinematics. For proton recoils greater than 1 MeV, we show that the (x, y, z)-position of neutron-proton scattering can be estimated with < 1 cm root-mean-squared [RMS] error and the proton recoil energy can be estimated with < 50 keV RMS error by fitting the photodetectors' response time history to models of optical photon transport within the scintillator pillars. Finally, we evaluate several alternative designs of this proposed single-volume scatter camera made of pillars of plastic scintillator (SVSC-PiPS), studying the effect of pillar dimensions, scintillator material (EJ-204, EJ-232Q and stilbene), and photodetector (MCP-PM vs. SiPM) response vs. time. We demonstrate that the most precise estimates of incident neutron direction and energy can be obtained using a combination of scintillator material with high luminosity and a photodetector with a narrow impulse response. Specifically, we conclude that an SVSC-PiPS constructed using EJ-204 (a high luminosity plastic scintillator) and an MCP-PM will produce the most precise estimates of incident neutron direction and energy.

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“…More information can be extracted if we know about the recoil proton as well. Two tanks containing a liquid scintillator are used in a balloon-borne detector system [168,169]. Each tank is (21) ' nnlllmnt.npi-•• nnlllmnhnr • Initial Neutron Fig.…”

Section: The Associated Particle Double Scattering Spectrometermentioning

confidence: 99%

7 Neutron Detectors

1997

Experimental Techniques in Nuclear Physics

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Large Area Double Scattering Telescope for Balloon-Borne Studies of Neutrons and Gamma Rays

Cited by 18 publications

References 5 publications

Gamma-ray spectroscopy in astrophysics

Gamma-ray spectroscopy in astrophysics

Model-based design evaluation of a compact, high-efficiency neutron scatter camera

7 Neutron Detectors

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