Energy calibration of the GEMPix in the energy range of 6 keV to 2 MeV

Terrestrial Gamma-ray Flashes (TGFs) are sub milliseconds bursts of high energy photons associated with lightning flashes in thunderstorms. The Atmosphere-Space Interactions Monitor (ASIM), launched in April 2018, is the first space mission specifically designed to detect TGFs. We will mainly focus on data from the High Energy Detector (HED) which is sensitive to photons with energies from 300 keV to > 30 MeV, and include data from the Low Energy Detector (LED) sensitive in 50 keV to 370 keV energy range. Both HED and LED are part of the Modular X- and Gamma-ray Sensor (MXGS) of ASIM. The energy spectrum of TGFs, together with Monte Carlo simulations, can provide information on the production altitude and beaming geometry of TGFs. Constraints have already been set on the production altitude and beaming geometry using other spacecraft and radio measurements. Some of these studies are based on cumulative spectra of a large number of TGFs (e.g. [1]), which smooth out individual variability. The spectral analysis of individual TGFs has been carried out up to now for Fermi TGFs only, showing spectral diversity [2]. Crucial key factors for individual TGF spectral analysis are a large number of counts, an energy range extended to several tens of MeV, a good energy calibration as well as knowledge and control of any instrumental effects affecting the measurements.We strive to put stricter constraints on the production altitude and beaming geometry, by comparing Monte Carlo simulations to energy spectra from single ASIM TGFs. We will present the dataset and method, including the correction for instrumental effects, and preliminary results on individual TGFs.Thanks to ASIM&#8217;s large effective area and low orbital altitude, single TGFs detected by ASIM have much more count statistics than observations from other spacecrafts capable of detecting TGFs. ASIM has detected over 550 TGFs up to date (January 2020), and ~115 have more than 100 counts. This allows for a large sample for individual spectral analysis.References:<ol><li>Dwyer, J. R., and D. M. Smith (2005), A comparison between Monte Carlo simulations of runaway breakdown and terrestrial gamma-ray flash observations, Geophys. Res. Lett., 32, L22804, doi:10.1029/2005GL023848.</li> <li>Mailyan et al. (2016), The spectroscopy of individual terrestrial gamma-ray flashes: Constraining the source properties, J. Geophys. Res. Space Physics, 121, 11,346&#8211;11,363, doi:10.1002/2016JA022702.</li> </ol>

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Absolute x-ray energy calibration over a wide energy range using a diffraction-based iterative method

Review of Scientific Instruments ◽

10.1063/1.4722166 ◽

2012 ◽

Vol 83 (6) ◽

pp. 063901 ◽

Cited By ~ 11

Author(s):

Xinguo Hong ◽

Zhiqiang Chen ◽

Thomas S. Duffy

Keyword(s):

Iterative Method ◽

Energy Range ◽

Energy Calibration ◽

Wide Energy Range ◽

X Ray ◽

Wide Energy

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The TES beamline (8-BM) at NSLS-II: tender-energy spatially resolved X-ray absorption spectroscopy and X-ray fluorescence imaging

Journal of Synchrotron Radiation ◽

10.1107/s1600577519012761 ◽

2019 ◽

Vol 26 (6) ◽

pp. 2064-2074 ◽

Cited By ~ 7

Author(s):

Paul Northrup

Keyword(s):

Energy Range ◽

Fluorescence Imaging ◽

Absorption Spectroscopy ◽

Small Sample ◽

Energy Calibration ◽

Helium Atmosphere ◽

X Ray ◽

Spatially Resolved ◽

X Ray Absorption

The tender-energy X-ray spectroscopy (TES) beamline at the National Synchrotron Light Source II (NSLS-II) is now operational for general users. Its scientific mission includes static and in situ X-ray fluorescence imaging and spatially resolved X-ray absorption spectroscopy for characterization of complex heterogeneous, structured and dynamic natural or engineered materials and systems. TES is optimized for the tender-energy range, offering routine operations from 2.0 to 5.5 keV, with capabilities to reach down to 1.2 or up to 8 keV with configuration change. TES is designed as an extended X-ray absorption fine-structure microprobe (EXAFS microprobe) for applications of micrometre-scale EXAFS spectroscopy to heterogeneous samples. Beam size is user-tunable from ∼2 to 25 µm. Energy may be scanned on-the-fly or in traditional step scanning. Importantly, the position of the microbeam at the sample location does not move significantly during energy scanning or when changing energy across the entire routine energy range. This enables full EXAFS of a particle or domain the same size as the probe beam, and measurement of the same spot at different energies. In addition, there is no measureable drift in energy calibration (repeatability) scan-to-scan and over 24 h. This is critical where simultaneous calibration measurements are generally not feasible, and for speciation mapping where precise and stable control of incident energy is essential. The sample environment is helium atmosphere at room pressure with infrastructure for in situ electrochemistry and catalysis in small sample cells or microreactors. As the first bend-magnet beamline at NSLS-II, noteworthy commissioning aspects are described. Example measurements are presented to illustrate its capabilities.

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LaBr3(Ce) Crystal Spectrometric Detection Unit for Studying the Field of Capture Gamma Radiation with Energies from 4 MeV to 9 MeV

ANRI ◽

10.37414/2075-1338-2020-102-3-50-57 ◽

2020 ◽

Vol 0 (3) ◽

pp. 50-57

Author(s):

Damian Komar ◽

Valery Kozhemyakin ◽

Vladimir Guzov ◽

Yuliya Verhusha ◽

Andrey Antonov ◽

...

Keyword(s):

Gamma Radiation ◽

Energy Range ◽

High Energy ◽

Energy Calibration ◽

Energy Capture ◽

Calibration Facility ◽

Detection Unit

The paper describes some features of the LaBr3(Ce) crystal in comparison with the NaI(Tl) crystal. The instrumental spectra obtained by the spectrometric detection unit with a LaBr3(Ce) crystal in the fields of high-energy capture gamma radiation at neutron calibration facility AT-140 in the energy range from 4 MeV to 9 MeV are presented. It was shown that the energy calibration of LaBr3(Ce) – based spectrometers can be performed in the range from 30 keV to 10 MeV using high-energy capture gamma radiation at AT-140 and the lanthanum intrinsic radioactivity line without resorting to OSGI sources.

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Spectral Analysis of Individual Terrestrial Gamma-ray Flashes Detected by ASIM

10.5194/egusphere-egu21-5015 ◽

2021 ◽

Author(s):

Anders Lindanger ◽

Martino Marisaldi ◽

David Sarria ◽

Nikolai Østgaard ◽

Nikolai Lehtinen ◽

...

Keyword(s):

Monte Carlo ◽

Spectral Analysis ◽

Energy Spectrum ◽

Monte Carlo Simulations ◽

Energy Range ◽

Gamma Ray ◽

High Energy ◽

Space Physics ◽

Energy Calibration ◽

Energy Detector

Terrestrial Gamma-ray Flashes (TGFs) are sub-millisecond bursts of high-energy photons associated with lightning flashes in thunderstorms. The Atmosphere-Space Interactions Monitor (ASIM), launched in April 2018, is the first space mission specifically designed to detect TGFs. We will mainly focus on data from the High Energy Detector (HED) which is sensitive to photons with energies from 300 keV to > 30 MeV, and include data from the Low Energy Detector (LED) sensitive in 50 keV to 370 keV energy range. Both HED and LED are part of the Modular X- and Gamma-ray Sensor (MXGS) of ASIM.The energy spectrum of TGFs, together with Monte Carlo simulations, can provide information on the production altitude and beaming geometry of TGFs. Constraints have already been set on the production altitude and beaming geometry using other spacecraft and radio measurements. Some of these studies are based on cumulative spectra of a large number of TGFs (e.g. [1]), which smooth out individual variability. The spectral analysis of individual TGFs has been carried out up to now for Fermi TGFs only, showing spectral diversity [2]. Crucial key factors for individual TGF spectral analysis are a large number of counts, an energy range extended to several tens of MeV, a good energy calibration as well as knowledge and control of any instrumental effects affecting the measurements.Thanks to ASIM&#8217;s large effective area and low orbital altitude, single TGFs detected by ASIM have much more count statistics than observations from other spacecraft capable of detecting TGFs. By comparing Monte Carlo simulations to the energy spectrum from single ASIM TGFs we will aim to put stricter constraints on the production altitude and beaming geometry of TGFs. We will present the dataset, method, and some results of the spectral analysis of individual TGFs.References:1. Dwyer, J. R., and D. M. Smith (2005), A comparison between Monte Carlo simulations of runaway breakdown and terrestrial gamma-ray flash observations, Geophys. Res. Lett., 32, L22804, doi:10.1029/2005GL023848.2. Mailyan et al. (2016), The spectroscopy of individual terrestrial gamma-ray flashes: Constraining the source properties,&#160;J. Geophys. Res. Space Physics,&#160;121, 11,346&#8211;11,363, doi:10.1002/2016JA022702.

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Solar Flare Energetic Neutral Emission Measurements in the Project Coronas-I

International Astronomical Union Colloquium ◽

10.1017/s0252921100026208 ◽

1994 ◽

Vol 144 ◽

pp. 635-639

Author(s):

J. Baláž ◽

A. V. Dmitriev ◽

M. A. Kovalevskaya ◽

K. Kudela ◽

S. N. Kuznetsov ◽

...

Keyword(s):

Solar Flare ◽

Energy Range ◽

Gamma Rays ◽

Pulse Shape ◽

Gamma Ray ◽

Pulse Shape Discrimination ◽

Shape Discrimination ◽

Solar Neutron ◽

Low Altitude

AbstractThe experiment SONG (SOlar Neutron and Gamma rays) for the low altitude satellite CORONAS-I is described. The instrument is capable to provide gamma-ray line and continuum detection in the energy range 0.1 – 100 MeV as well as detection of neutrons with energies above 30 MeV. As a by-product, the electrons in the range 11 – 108 MeV will be measured too. The pulse shape discrimination technique (PSD) is used.

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