THESEUS is a space mission concept aimed at exploiting Gamma-Ray Bursts for investigating the early Universe and at providing a substantial advancement of multi-messenger and time-domain ...astrophysics. These goals will be achieved through a unique combination of instruments allowing GRB and X-ray transient detection over a broad field of view (more than 1sr) with 0.5–1 arcmin localization, an energy band extending from several MeV down to 0.3 keV and high sensitivity to transient sources in the soft X-ray domain, as well as on-board prompt (few minutes) follow-up with a 0.7 m class IR telescope with both imaging and spectroscopic capabilities. THESEUS will be perfectly suited for addressing the main open issues in cosmology such as, e.g., star formation rate and metallicity evolution of the inter-stellar and intra-galactic medium up to redshift ∼10, signatures of Pop III stars, sources and physics of re-ionization, and the faint end of the galaxy luminosity function. In addition, it will provide unprecedented capability to monitor the X-ray variable sky, thus detecting, localizing, and identifying the electromagnetic counterparts to sources of gravitational radiation, which may be routinely detected in the late ’20s/early ’30s by next generation facilities like aLIGO/ aVirgo, eLISA, KAGRA, and Einstein Telescope. THESEUS will also provide powerful synergies with the next generation of multi-wavelength observatories (e.g., LSST, ELT, SKA, CTA, ATHENA).
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The e-ASTROGAM mission De Angelis, A.; Tatischeff, V.; Tavani, M. ...
Experimental astronomy,
10/2017, Volume:
44, Issue:
1
Journal Article
Peer reviewed
Open access
e-ASTROGAM (‘enhanced ASTROGAM’) is a breakthrough Observatory space mission, with a detector composed by a Silicon tracker, a calorimeter, and an anticoincidence system, dedicated to the study of ...the non-thermal Universe in the photon energy range from 0.3 MeV to 3 GeV – the lower energy limit can be pushed to energies as low as 150 keV, albeit with rapidly degrading angular resolution, for the tracker, and to 30 keV for calorimetric detection. The mission is based on an advanced space-proven detector technology, with unprecedented sensitivity, angular and energy resolution, combined with polarimetric capability. Thanks to its performance in the MeV-GeV domain, substantially improving its predecessors, e-ASTROGAM will open a new window on the non-thermal Universe, making pioneering observations of the most powerful Galactic and extragalactic sources, elucidating the nature of their relativistic outflows and their effects on the surroundings. With a line sensitivity in the MeV energy range one to two orders of magnitude better than previous generation instruments, e-ASTROGAM will determine the origin of key isotopes fundamental for the understanding of supernova explosion and the chemical evolution of our Galaxy. The mission will provide unique data of significant interest to a broad astronomical community, complementary to powerful observatories such as LIGO-Virgo-GEO600-KAGRA, SKA, ALMA, E-ELT, TMT, LSST, JWST, Athena, CTA, IceCube, KM3NeT, and the promise of eLISA.
e-ASTROGAM ('enhanced ASTROGAM') is a breakthrough Observatory space mission, with a detector composed by a Silicon tracker, a calorimeter, and an anticoincidence system, dedicated to the study of ...the non-thermal Universe in the photon energy range from 0.3 MeV to 3 GeV - the lower energy limit can be pushed to energies as low as 150 keV for the tracker, and to 30 keV for calorimetric detection. The mission is based on an advanced space-proven detector technology, with unprecedented sensitivity, angular and energy resolution, combined with polarimetric capability. Thanks to its performance in the MeV-GeV domain, substantially improving its predecessors, e-ASTROGAM will open a new window on the non-thermal Universe, making pioneering observations of the most powerful Galactic and extragalactic sources, elucidating the nature of their relativistic outflows and their effects on the surroundings. With a line sensitivity in the MeV energy range one to two orders of magnitude better than previous generation instruments, e-ASTROGAM will determine the origin of key isotopes fundamental for the understanding of supernova explosion and the chemical evolution of our Galaxy. The mission will provide unique data of significant interest to a broad astronomical community, complementary to powerful observatories such as LIGO-Virgo-GEO600-KAGRA, SKA, ALMA, E-ELT, TMT, LSST, JWST, Athena, CTA, IceCube, KM3NeT, and LISA.
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The spectral response of several crystals grown by the Traveling Heater Method (THM) were investigated. An energy resolution of 0.98% for a Pseudo Frisch-Grid of 4 times 4 times 9 mm 3 and 2.1% FWHM ...for a coplanar-grid of size 11 times 11 times 5 mm 3 were measured using 137 Cs-662 keV. In addition a 4% FWHM at 122 keV has also been measured on 20 times 20 X 5 mm 3 monolithic pixellated devices. The material shows great potential toward producing large-volume detectors with spectral performance that meets the requirement for high-resolution gamma-ray spectroscopy.
CdZnTe drift detector with correction for hole trapping van Pamelen, M.A.J.; Budtz-Jørgensen, C.
Nuclear instruments & methods in physics research. Section A, Accelerators, spectrometers, detectors and associated equipment,
07/1998, Volume:
411, Issue:
1
Journal Article
Peer reviewed
The results are presented of a CdZnTe drift detector for which the energy determination can be corrected for hole trapping. The electronic noise and the hole contribution to the signal are reduced ...and the signals are also corrected for any residual effects of hole trapping. This is achieved by using drift strips and an anode strip on one side of the detector crystal in combination with a single planar electrode on the other side. Below 100
keV, the resolution (in FWHM) was electronic noise limited. Using a planar electrode, the peak of
241Am at 59.6
keV has a width of 14.1
keV. The resolution improved to 3.21
keV when using the anode strip. This is comparable to the electronic noise of 3.11
keV. At 661
keV, no peak could be observed in the spectrum of
137Cs with the planar electrode. However, with the anode strip, a peak with a width of 17.9
keV was observed. The resolution improved further to 6.9
keV after correction for hole trapping. After correction, the peak-to-valley ratio was 40
:
1, with a peak-to-Compton ratio of 4
:
1.
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We present measurements of ion-energy distributions of the ions impinging on the grounded anode of a pulsed argon DC-glow discharge (cathode voltages of –300 to –450 V, and a gas pressure of 0.5 ...mbar) with on and off pulse times of 100–900 μs. During the on pulses of the discharge, as expected, low energy ions (<10 eV) were observed, originating from the potential difference between the plasma (i.e. the plasma potential) and the grounded anode. However, during the initial tens of microseconds of the off pulse, ions were detected with energies of the order of the cathode potential (i.e. several hundred eV). Furthermore, voltage measurements of a floating anode show that the plasma potential has a high positive voltage peak during the onset of the off pulse. The explanation of the observed phenomena must be sought in the sudden change in the boundary conditions of the discharge and the subsequent redistribution of charged particles, leading ultimately to the collapse of the discharge. This has been confirmed by Monte-Carlo simulations of the discharge.
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38.
Radiation damage measurements on CZT drift strip detectors Kuvvetli, I.; Budtz-Jørgensen, C.; Korsbech, U. ...
Nuclear instruments & methods in physics research. Section A, Accelerators, spectrometers, detectors and associated equipment,
10/2003, Volume:
512, Issue:
1
Journal Article
Peer reviewed
At DSRI, in collaboration with the cyclotron facility at Copenhagen University Hospital, we have performed a study of radiation effects exposing a 2.7
mm thick CZT drift strip detector to 30
MeV ...protons. The detector characteristics were evaluated after exposure to a number of fluences in the range from 2×10
8 to 60×10
8
p
+/cm
2. Even for the highest fluences, which had a dramatic effect on the spectroscopic performance, we were able to recover the detectors after an appropriate annealing procedure. The radiation damage was studied as a function of depth inside the detector material. A numerical model that emulates the physical processes of the charge transport in the CZT detector was used to derive the charge trapping parameter,
μτ
e (the product of charge mobility and trapping time) as a function of fluence. The analysis showed that the electron trapping increased proportionately with the proton dose. The radiation contribution to the electron trapping was found to obey the following relation:
(μτ
e
−
1
)
rad
=(2.5±0.2)×10
−7×Φ
(
V/cm)
2
with the proton fluence,
Φ in p
+/cm
2. The trapping depth dependence, however, did not agree well with the damage profile calculated using the standard Monte Carlo simulations, TRIM
1, for the proton-induced radiation effects. The present results suggest that proton-induced nuclear reactions contribute significantly to the radiation damage. Further work will elaborate on these effects.
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