Techniques in balloon X-ray astronomy

Abstract The first balloon observation of a cosmic X-ray source, the Crab Nebula, was made in 1965, only three years after the initial discovery of such sources by rocket observations. Since then balloon data has provided much information on the positions, spectra, time variability and pulsed nature...
Ausführliche Beschreibung

Gespeichert in:

Autor*in:	Peterson, L. E. [verfasserIn] Pelling, R. M. Matteson, J. L.

Format:	Artikel
Sprache:	Englisch

Erschienen:	1972

Schlagwörter:	Isotropy Scintillation Counter Proportional Counter Exploratory Work Solid State Detector

Anmerkung:	© D. Reidel Publishing Company 1972

Übergeordnetes Werk:	Enthalten in: Space science reviews - Kluwer Academic Publishers, 1962, 13(1972), 2 vom: Juni, Seite 320-336
Übergeordnetes Werk:	volume:13 ; year:1972 ; number:2 ; month:06 ; pages:320-336

Links:	Volltext

DOI / URN:	10.1007/BF00175321

Katalog-ID:	OLC2033660869

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allfields	10.1007/BF00175321 doi (DE-627)OLC2033660869 (DE-He213)BF00175321-p DE-627 ger DE-627 rakwb eng 600 VZ 16,12 ssgn Peterson, L. E. verfasserin aut Techniques in balloon X-ray astronomy 1972 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1972 Abstract The first balloon observation of a cosmic X-ray source, the Crab Nebula, was made in 1965, only three years after the initial discovery of such sources by rocket observations. Since then balloon data has provided much information on the positions, spectra, time variability and pulsed nature of localized sources, and on the spectrum and isotropy of diffuse galactic and universal components. Measurements are limited to energies above about 20 keV by atmospheric attenuation at 2–3 g cm −2 depth and to below several hundred keV by detector sensitivity. Detectors usually consist of large area NaI or CsI scintillation counters with anticoincidence collimators for rejection of charged particles and scattered X-rays. Proportional counters are occasionally used at lower energies and solid state detectors are used where extreme energy resolution is important. The instruments require a pointing capability on the order of 1.0 to 0.1°, depending on the collimator aperture. Digital data is either recorded on board or telemetered using a PCM technique. Exploratory work in the 0.2–10 MeV γ-ray range is starting now, and balloon observations may be expected to make important contributions in the near future. Isotropy Scintillation Counter Proportional Counter Exploratory Work Solid State Detector Pelling, R. M. aut Matteson, J. L. aut Enthalten in Space science reviews Kluwer Academic Publishers, 1962 13(1972), 2 vom: Juni, Seite 320-336 (DE-627)129086606 (DE-600)4860-4 (DE-576)014420724 0038-6308 nnns volume:13 year:1972 number:2 month:06 pages:320-336 https://doi.org/10.1007/BF00175321 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_150 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2015 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4103 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4310 GBV_ILN_4314 AR 13 1972 2 06 320-336
spelling	10.1007/BF00175321 doi (DE-627)OLC2033660869 (DE-He213)BF00175321-p DE-627 ger DE-627 rakwb eng 600 VZ 16,12 ssgn Peterson, L. E. verfasserin aut Techniques in balloon X-ray astronomy 1972 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1972 Abstract The first balloon observation of a cosmic X-ray source, the Crab Nebula, was made in 1965, only three years after the initial discovery of such sources by rocket observations. Since then balloon data has provided much information on the positions, spectra, time variability and pulsed nature of localized sources, and on the spectrum and isotropy of diffuse galactic and universal components. Measurements are limited to energies above about 20 keV by atmospheric attenuation at 2–3 g cm −2 depth and to below several hundred keV by detector sensitivity. Detectors usually consist of large area NaI or CsI scintillation counters with anticoincidence collimators for rejection of charged particles and scattered X-rays. Proportional counters are occasionally used at lower energies and solid state detectors are used where extreme energy resolution is important. The instruments require a pointing capability on the order of 1.0 to 0.1°, depending on the collimator aperture. Digital data is either recorded on board or telemetered using a PCM technique. Exploratory work in the 0.2–10 MeV γ-ray range is starting now, and balloon observations may be expected to make important contributions in the near future. Isotropy Scintillation Counter Proportional Counter Exploratory Work Solid State Detector Pelling, R. M. aut Matteson, J. L. aut Enthalten in Space science reviews Kluwer Academic Publishers, 1962 13(1972), 2 vom: Juni, Seite 320-336 (DE-627)129086606 (DE-600)4860-4 (DE-576)014420724 0038-6308 nnns volume:13 year:1972 number:2 month:06 pages:320-336 https://doi.org/10.1007/BF00175321 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_150 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2015 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4103 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4310 GBV_ILN_4314 AR 13 1972 2 06 320-336
allfields_unstemmed	10.1007/BF00175321 doi (DE-627)OLC2033660869 (DE-He213)BF00175321-p DE-627 ger DE-627 rakwb eng 600 VZ 16,12 ssgn Peterson, L. E. verfasserin aut Techniques in balloon X-ray astronomy 1972 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1972 Abstract The first balloon observation of a cosmic X-ray source, the Crab Nebula, was made in 1965, only three years after the initial discovery of such sources by rocket observations. Since then balloon data has provided much information on the positions, spectra, time variability and pulsed nature of localized sources, and on the spectrum and isotropy of diffuse galactic and universal components. Measurements are limited to energies above about 20 keV by atmospheric attenuation at 2–3 g cm −2 depth and to below several hundred keV by detector sensitivity. Detectors usually consist of large area NaI or CsI scintillation counters with anticoincidence collimators for rejection of charged particles and scattered X-rays. Proportional counters are occasionally used at lower energies and solid state detectors are used where extreme energy resolution is important. The instruments require a pointing capability on the order of 1.0 to 0.1°, depending on the collimator aperture. Digital data is either recorded on board or telemetered using a PCM technique. Exploratory work in the 0.2–10 MeV γ-ray range is starting now, and balloon observations may be expected to make important contributions in the near future. Isotropy Scintillation Counter Proportional Counter Exploratory Work Solid State Detector Pelling, R. M. aut Matteson, J. L. aut Enthalten in Space science reviews Kluwer Academic Publishers, 1962 13(1972), 2 vom: Juni, Seite 320-336 (DE-627)129086606 (DE-600)4860-4 (DE-576)014420724 0038-6308 nnns volume:13 year:1972 number:2 month:06 pages:320-336 https://doi.org/10.1007/BF00175321 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_150 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2015 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4103 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4310 GBV_ILN_4314 AR 13 1972 2 06 320-336
allfieldsGer	10.1007/BF00175321 doi (DE-627)OLC2033660869 (DE-He213)BF00175321-p DE-627 ger DE-627 rakwb eng 600 VZ 16,12 ssgn Peterson, L. E. verfasserin aut Techniques in balloon X-ray astronomy 1972 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1972 Abstract The first balloon observation of a cosmic X-ray source, the Crab Nebula, was made in 1965, only three years after the initial discovery of such sources by rocket observations. Since then balloon data has provided much information on the positions, spectra, time variability and pulsed nature of localized sources, and on the spectrum and isotropy of diffuse galactic and universal components. Measurements are limited to energies above about 20 keV by atmospheric attenuation at 2–3 g cm −2 depth and to below several hundred keV by detector sensitivity. Detectors usually consist of large area NaI or CsI scintillation counters with anticoincidence collimators for rejection of charged particles and scattered X-rays. Proportional counters are occasionally used at lower energies and solid state detectors are used where extreme energy resolution is important. The instruments require a pointing capability on the order of 1.0 to 0.1°, depending on the collimator aperture. Digital data is either recorded on board or telemetered using a PCM technique. Exploratory work in the 0.2–10 MeV γ-ray range is starting now, and balloon observations may be expected to make important contributions in the near future. Isotropy Scintillation Counter Proportional Counter Exploratory Work Solid State Detector Pelling, R. M. aut Matteson, J. L. aut Enthalten in Space science reviews Kluwer Academic Publishers, 1962 13(1972), 2 vom: Juni, Seite 320-336 (DE-627)129086606 (DE-600)4860-4 (DE-576)014420724 0038-6308 nnns volume:13 year:1972 number:2 month:06 pages:320-336 https://doi.org/10.1007/BF00175321 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_150 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2015 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4103 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4310 GBV_ILN_4314 AR 13 1972 2 06 320-336
allfieldsSound	10.1007/BF00175321 doi (DE-627)OLC2033660869 (DE-He213)BF00175321-p DE-627 ger DE-627 rakwb eng 600 VZ 16,12 ssgn Peterson, L. E. verfasserin aut Techniques in balloon X-ray astronomy 1972 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1972 Abstract The first balloon observation of a cosmic X-ray source, the Crab Nebula, was made in 1965, only three years after the initial discovery of such sources by rocket observations. Since then balloon data has provided much information on the positions, spectra, time variability and pulsed nature of localized sources, and on the spectrum and isotropy of diffuse galactic and universal components. Measurements are limited to energies above about 20 keV by atmospheric attenuation at 2–3 g cm −2 depth and to below several hundred keV by detector sensitivity. Detectors usually consist of large area NaI or CsI scintillation counters with anticoincidence collimators for rejection of charged particles and scattered X-rays. Proportional counters are occasionally used at lower energies and solid state detectors are used where extreme energy resolution is important. The instruments require a pointing capability on the order of 1.0 to 0.1°, depending on the collimator aperture. Digital data is either recorded on board or telemetered using a PCM technique. Exploratory work in the 0.2–10 MeV γ-ray range is starting now, and balloon observations may be expected to make important contributions in the near future. Isotropy Scintillation Counter Proportional Counter Exploratory Work Solid State Detector Pelling, R. M. aut Matteson, J. L. aut Enthalten in Space science reviews Kluwer Academic Publishers, 1962 13(1972), 2 vom: Juni, Seite 320-336 (DE-627)129086606 (DE-600)4860-4 (DE-576)014420724 0038-6308 nnns volume:13 year:1972 number:2 month:06 pages:320-336 https://doi.org/10.1007/BF00175321 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_150 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2015 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4103 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4310 GBV_ILN_4314 AR 13 1972 2 06 320-336
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author	Peterson, L. E.
spellingShingle	Peterson, L. E. ddc 600 ssgn 16,12 misc Isotropy misc Scintillation Counter misc Proportional Counter misc Exploratory Work misc Solid State Detector Techniques in balloon X-ray astronomy
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topic	ddc 600 ssgn 16,12 misc Isotropy misc Scintillation Counter misc Proportional Counter misc Exploratory Work misc Solid State Detector
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title	Techniques in balloon X-ray astronomy
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title_sort	techniques in balloon x-ray astronomy
title_auth	Techniques in balloon X-ray astronomy
abstract	Abstract The first balloon observation of a cosmic X-ray source, the Crab Nebula, was made in 1965, only three years after the initial discovery of such sources by rocket observations. Since then balloon data has provided much information on the positions, spectra, time variability and pulsed nature of localized sources, and on the spectrum and isotropy of diffuse galactic and universal components. Measurements are limited to energies above about 20 keV by atmospheric attenuation at 2–3 g cm −2 depth and to below several hundred keV by detector sensitivity. Detectors usually consist of large area NaI or CsI scintillation counters with anticoincidence collimators for rejection of charged particles and scattered X-rays. Proportional counters are occasionally used at lower energies and solid state detectors are used where extreme energy resolution is important. The instruments require a pointing capability on the order of 1.0 to 0.1°, depending on the collimator aperture. Digital data is either recorded on board or telemetered using a PCM technique. Exploratory work in the 0.2–10 MeV γ-ray range is starting now, and balloon observations may be expected to make important contributions in the near future. © D. Reidel Publishing Company 1972
abstractGer	Abstract The first balloon observation of a cosmic X-ray source, the Crab Nebula, was made in 1965, only three years after the initial discovery of such sources by rocket observations. Since then balloon data has provided much information on the positions, spectra, time variability and pulsed nature of localized sources, and on the spectrum and isotropy of diffuse galactic and universal components. Measurements are limited to energies above about 20 keV by atmospheric attenuation at 2–3 g cm −2 depth and to below several hundred keV by detector sensitivity. Detectors usually consist of large area NaI or CsI scintillation counters with anticoincidence collimators for rejection of charged particles and scattered X-rays. Proportional counters are occasionally used at lower energies and solid state detectors are used where extreme energy resolution is important. The instruments require a pointing capability on the order of 1.0 to 0.1°, depending on the collimator aperture. Digital data is either recorded on board or telemetered using a PCM technique. Exploratory work in the 0.2–10 MeV γ-ray range is starting now, and balloon observations may be expected to make important contributions in the near future. © D. Reidel Publishing Company 1972
abstract_unstemmed	Abstract The first balloon observation of a cosmic X-ray source, the Crab Nebula, was made in 1965, only three years after the initial discovery of such sources by rocket observations. Since then balloon data has provided much information on the positions, spectra, time variability and pulsed nature of localized sources, and on the spectrum and isotropy of diffuse galactic and universal components. Measurements are limited to energies above about 20 keV by atmospheric attenuation at 2–3 g cm −2 depth and to below several hundred keV by detector sensitivity. Detectors usually consist of large area NaI or CsI scintillation counters with anticoincidence collimators for rejection of charged particles and scattered X-rays. Proportional counters are occasionally used at lower energies and solid state detectors are used where extreme energy resolution is important. The instruments require a pointing capability on the order of 1.0 to 0.1°, depending on the collimator aperture. Digital data is either recorded on board or telemetered using a PCM technique. Exploratory work in the 0.2–10 MeV γ-ray range is starting now, and balloon observations may be expected to make important contributions in the near future. © D. Reidel Publishing Company 1972
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title_short	Techniques in balloon X-ray astronomy
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