51 research outputs found
IDeF-X ASIC for Cd(Zn)Te spectro-imaging systems
Joint progresses in Cd(Zn)Te detectors, microelectronics and interconnection
technologies open the way for a new generation of instruments for physics and
astrophysics applications in the energy range from 1 to 1000 keV. Even working
between -20 and 20 degrees Celsius, these instruments will offer high spatial
resolution (pixel size ranging from 300 x 300 square micrometers to few square
millimeters), high spectral response and high detection efficiency. To reach
these goals, reliable, highly integrated, low noise and low power consumption
electronics is mandatory. Our group is currently developing a new ASIC detector
front-end named IDeF-X, for modular spectro-imaging system based on the use of
Cd(Zn)Te detectors. We present here the first version of IDeF-X which consists
in a set of ten low noise charge sensitive preamplifiers (CSA). It has been
processed with the standard AMS 0.35 micrometer CMOS technology. The CSA are
designed to be DC coupled to detectors having a low dark current at room
temperature. The various preamps implemented are optimized for detector
capacitances ranging from 0.5 up to 30 pF.Comment: 8 pages, 11 figures, IEEE NSS-MIC conference in Rome 2004, submitted
to IEEE TNS, correction in unit of figure
Development of a modular CdTe detector plane for gamma-ray burst detection below 100 keV
We report on the development of an innovative CdTe detector plane (DPIX)
optimized for the detection and localization of gamma-ray bursts in the X-ray
band (below 100 keV). DPIX is part of an R&D program funded by the French Space
Agency (CNES). DPIX builds upon the heritage of the ISGRI instrument, currently
operating with great success on the ESA INTEGRAL mission. DPIX is an assembly
of 200 elementary modules (XRDPIX) equipped with 32 CdTe Schottky detectors
(4x4 mm2, 1 mm thickness) produced by ACRORAD Co. LTD. in Japan. These
detectors offer good energy response up to 100 keV. Each XRDPIX is readout by
the very low noise front-end electronics chip IDeF-X, currently under
development at CEA/DSM/DAPNIA. In this paper, we describe the design of XRDPIX,
the main features of the IDeF-X chip, and will present preliminary results of
the reading out of one CdTe Schottky detector by the IDeF-X V1.0 chip. A
low-energy threshold around 2.7 keV has been measured. This is to be compared
with the 12-15 keV threshold of the ISGRI-INTEGRAL and BAT-SWIFT instruments,
which both use similar detector material.Comment: 5 pages, 4 figures in color, Advances in Space Research, COSPAR
meeting, Beijing (2006
The silicon micro-strip detector plane for the LOFT/Wide Field Monitor
The main objective of the Wide Field Monitor (WFM) on the LOFT mission is to
provide unambiguous detection of the high-energy sources in a large field of
view, in order to support science operations of the LOFT primary instrument,
the LAD. The monitor will also provide by itself a large number of results on
the timing and spectral behaviour of hundreds of galactic compact objects,
Active Galactic Nuclei and Gamma-Ray Bursts. The WFM is based on the coded
aperture concept where a position sensitive detector records the shadow of a
mask projected by the celestial sources. The proposed WFM detector plane, based
on Double Sided micro-Strip Silicon Detectors (DSSD), will allow proper
2-dimensional recording of the projected shadows. Indeed the positioning of the
photon interaction in the detector with equivalent fine resolution in both
directions insures the best imaging capability compatible with the allocated
budgets for this telescope on LOFT. We will describe here the overall
configuration of this 2D-WFM and the design and characteristics of the DSSD
detector plane including its imaging and spectral performances. We will also
present a number of simulated results discussing the advantages that this
configuration offers to LOFT. A DSSD-based WFM will in particular reduce
significantly the source confusion experienced by the WFM in crowded regions of
the sky like the Galactic Center and will in general increase the observatory
science capability of the mission.Comment: Proceedings of SPIE, Vol. 8443, Paper No. 8443-89, 201
First year of energetic particle measurements in the inner heliosphere with Solar Orbiter's Energetic Particle Detector
Context. Solar Orbiter strives to unveil how the Sun controls and shapes the heliosphere and fills it with energetic particle radiation. To this end, its Energetic Particle Detector (EPD) has now been in operation, providing excellent data, for just over a year.
Aims. EPD measures suprathermal and energetic particles in the energy range from a few keV up to (near-) relativistic energies (few MeV for electrons and about 500 MeV nuc−1 for ions). We present an overview of the initial results from the first year of operations and we provide a first assessment of issues and limitations. In addition, we present areas where EPD excels and provides opportunities for significant scientific progress in understanding how our Sun shapes the heliosphere.
Methods. We used the solar particle events observed by Solar Orbiter on 21 July and between 10 and 11 December 2020 to discuss the capabilities, along with updates and open issues related to EPD on Solar Orbiter. We also give some words of caution and caveats related to the use of EPD-derived data.
Results. During this first year of operations of the Solar Orbiter mission, EPD has recorded several particle events at distances between 0.5 and 1 au from the Sun. We present dynamic and time-averaged energy spectra for ions that were measured with a combination of all four EPD sensors, namely: the SupraThermal Electron and Proton sensor (STEP), the Electron Proton Telescope (EPT), the Suprathermal Ion Spectrograph (SIS), and the High-Energy Telescope (HET) as well as the associated energy spectra for electrons measured with STEP and EPT. We illustrate the capabilities of the EPD suite using the 10 and 11 December 2020 solar particle event. This event showed an enrichment of heavy ions as well as 3He, for which we also present dynamic spectra measured with SIS. The high anisotropy of electrons at the onset of the event and its temporal evolution is also shown using data from these sensors. We discuss the ongoing in-flight calibration and a few open instrumental issues using data from the 21 July and the 10 and 11 December 2020 events and give guidelines and examples for the usage of the EPD data. We explain how spacecraft operations may affect EPD data and we present a list of such time periods in the appendix. A list of the most significant particle enhancements as observed by EPT during this first year is also provided.Ministerio de Economía y CompetitividadAgencia Estatal de Investigació
STROBE-X: a probe-class mission for x-ray spectroscopy and timing on timescales from microseconds to years
We describe the Spectroscopic Time-Resolving Observatory for Broadband Energy X-rays (STROBE-X), a probeclass mission concept that will provide an unprecedented view of the X-ray sky, performing timing and spectroscopy over both a broad energy band (0.2–30 keV) and a wide range of timescales from microseconds to years. STROBE-X comprises two narrow-field instruments and a wide field monitor. The soft or low-energy band (0.2–12 keV) is covered by an array of lightweight optics (3-m focal length) that concentrate incident photons onto small solid-state detectors with CCD-level (85–175 eV) energy resolution, 100 ns time resolution, and low background rates. This technology has been fully developed for NICER and will be scaled up to take advantage of the longer focal length of STROBE-X. The higher-energy band (2–30 keV) is covered by large-area, collimated silicon drift detectors that were developed for the European LOFT mission concept. Each instrument will provide an order of magnitude improvement in effective area over its predecessor (NICER in the soft band and RXTE in the hard band). Finally, STROBE-X offers a sensitive wide-field monitor (WFM), both to act as a trigger for pointed observations of X-ray transients and also to provide high duty-cycle, high time-resolution, and high spectral-resolution monitoring of the variable X-ray sky. The WFM will boast approximately 20 times the sensitivity of the RXTE All-Sky Monitor, enabling multi-wavelength and multi-messenger investigations with a large instantaneous field of view. This mission concept will be presented to the 2020 Decadal Survey for consideration
The enhanced X-ray Timing and Polarimetry mission – eXTP: an update on its scientific cases, mission profile and development status
The enhanced X-ray Timing and Polarimetry mission (eXTP) is a flagship observatory for X-ray timing, spectroscopy and polarimetry developed by an International Consortium. Thanks to its very large collecting area, good spectral resolution and unprecedented polarimetry capabilities, eXTP will explore the properties of matter and the propagation of light in the most extreme conditions found in the Universe. eXTP will, in addition, be a powerful X-ray observatory. The mission will continuously monitor the X-ray sky, and will enable multiwavelength and multi-messenger studies. The mission is currently in phase B, which will be completed in the middle of 2022
First year of energetic particle measurements in the inner heliosphere with Solar Orbiter's Energetic Particle Detector
Context. Solar Orbiter strives to unveil how the Sun controls and shapes the heliosphere and fills it with energetic particle radiation. To this end, its Energetic Particle Detector (EPD) has now been in operation, providing excellent data, for just over a year.Aims. EPD measures suprathermal and energetic particles in the energy range from a few keV up to (near-) relativistic energies (few MeV for electrons and about 500 MeV nuc(-1) for ions). We present an overview of the initial results from the first year of operations and we provide a first assessment of issues and limitations. In addition, we present areas where EPD excels and provides opportunities for significant scientific progress in understanding how our Sun shapes the heliosphere.Methods. We used the solar particle events observed by Solar Orbiter on 21 July and between 10 and 11 December 2020 to discuss the capabilities, along with updates and open issues related to EPD on Solar Orbiter. We also give some words of caution and caveats related to the use of EPD-derived data.Results. During this first year of operations of the Solar Orbiter mission, EPD has recorded several particle events at distances between 0.5 and 1 au from the Sun. We present dynamic and time-averaged energy spectra for ions that were measured with a combination of all four EPD sensors, namely: the SupraThermal Electron and Proton sensor (STEP), the Electron Proton Telescope (EPT), the Suprathermal Ion Spectrograph (SIS), and the High-Energy Telescope (HET) as well as the associated energy spectra for electrons measured with STEP and EPT. We illustrate the capabilities of the EPD suite using the 10 and 11 December 2020 solar particle event. This event showed an enrichment of heavy ions as well as He-3, for which we also present dynamic spectra measured with SIS. The high anisotropy of electrons at the onset of the event and its temporal evolution is also shown using data from these sensors. We discuss the ongoing in-flight calibration and a few open instrumental issues using data from the 21 July and the 10 and 11 December 2020 events and give guidelines and examples for the usage of the EPD data. We explain how spacecraft operations may affect EPD data and we present a list of such time periods in the appendix. A list of the most significant particle enhancements as observed by EPT during this first year is also provided.</p
Response of a CMS HGCAL silicon-pad electromagnetic calorimeter prototype to 20-300 GeV positrons
The Compact Muon Solenoid Collaboration is designing a new high-granularity
endcap calorimeter, HGCAL, to be installed later this decade. As part of this
development work, a prototype system was built, with an electromagnetic section
consisting of 14 double-sided structures, providing 28 sampling layers. Each
sampling layer has an hexagonal module, where a multipad large-area silicon
sensor is glued between an electronics circuit board and a metal baseplate. The
sensor pads of approximately 1 cm are wire-bonded to the circuit board and
are readout by custom integrated circuits. The prototype was extensively tested
with beams at CERN's Super Proton Synchrotron in 2018. Based on the data
collected with beams of positrons, with energies ranging from 20 to 300 GeV,
measurements of the energy resolution and linearity, the position and angular
resolutions, and the shower shapes are presented and compared to a detailed
Geant4 simulation
Performance of the CMS High Granularity Calorimeter prototype to charged pion beams of 20300 GeV/c
The upgrade of the CMS experiment for the high luminosity operation of the
LHC comprises the replacement of the current endcap calorimeter by a high
granularity sampling calorimeter (HGCAL). The electromagnetic section of the
HGCAL is based on silicon sensors interspersed between lead and copper (or
copper tungsten) absorbers. The hadronic section uses layers of stainless steel
as an absorbing medium and silicon sensors as an active medium in the regions
of high radiation exposure, and scintillator tiles directly readout by silicon
photomultipliers in the remaining regions. As part of the development of the
detector and its readout electronic components, a section of a silicon-based
HGCAL prototype detector along with a section of the CALICE AHCAL prototype was
exposed to muons, electrons and charged pions in beam test experiments at the
H2 beamline at the CERN SPS in October 2018. The AHCAL uses the same technology
as foreseen for the HGCAL but with much finer longitudinal segmentation. The
performance of the calorimeters in terms of energy response and resolution,
longitudinal and transverse shower profiles is studied using negatively charged
pions, and is compared to GEANT4 predictions. This is the first report
summarizing results of hadronic showers measured by the HGCAL prototype using
beam test data.Comment: To be submitted to JINS
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