96 research outputs found
Estimate of the impact of background particles on the X-Ray Microcalorimeter Spectrometer on IXO
We present the results of a study on the impact of particles of galactic
(GCR) and solar origin for the X-ray Microcalorimeter Spectrometer (XMS) aboard
an astronomical satellite flying in an orbit at the second Lagrangian point
(L2). The detailed configuration presented in this paper is the one adopted for
the International X-Ray Observatory (IXO) study, however the derived estimates
can be considered a conservative limit for ATHENA, that is the IXO redefined
mission proposed to ESA. This work is aimed at the estimate of the residual
background level expected on the focal plane detector during the mission
lifetime, a crucial information in the development of any instrumental
configuration that optimizes the XMS scientific performances. We used the
Geant4 toolkit, a Monte Carlo based simulator, to investigate the rejection
efficiency of the anticoincidence system and assess the residual background on
the detector.Comment: 18 pages, 9 figure
The LOFT (Large Observatory for X-ray Timing) background simulations
The Large Observatory For X-ray Timing (LOFT) is an innovative medium-class
mission selected for an assessment phase in the framework of the ESA M3 Cosmic
Vision call. LOFT is intended to answer fundamental questions about the
behaviour of matter in the very strong gravitational and magnetic fields around
compact objects. With an effective area of ~10 m^2 LOFT will be able to measure
very fast variability in the X-ray fluxes and spectra. A good knowledge of the
in-orbit background environment is essential to assess the scientific
performance of the mission and to optimize the instrument design. The two main
contributions to the background are cosmic diffuse X-rays and high energy
cosmic rays; also, albedo emission from the Earth is significant. These
contributions to the background for both the Large Area Detector and the Wide
Field Monitor are discussed, on the basis of extensive Geant-4 simulations of a
simplified instrumental mass model.Comment: Proceedings of SPIE, Vol. 8443, Paper No. 8443-209, 201
Measurement of the effect of Non Ionising Energy Losses on the leakage current of Silicon Drift Detector prototypes for the LOFT satellite
The silicon drift detectors are at the basis of the instrumentation aboard
the Large Observatory For x-ray Timing (LOFT) satellite mission, which
underwent a three year assessment phase within the "Cosmic Vision 2015 - 2025"
long-term science plan of the European Space Agency. Silicon detectors are
especially sensitive to the displacement damage, produced by the non ionising
energy losses of charged and neutral particles, leading to an increase of the
device leakage current and thus worsening the spectral resolution.
During the LOFT assessment phase, we irradiated two silicon drift detectors
with a proton beam at the Proton Irradiation Facility in the accelerator of the
Paul Scherrer Institute and we measured the increase in leakage current. In
this paper we report the results of the irradiation and we discuss the impact
of the radiation damage on the LOFT scientific performance.Comment: 21 pages, 7 figures, 2 tables. Accepted for publication by Journal of
Instrumentation (JINST
Hyper-velocity impact test and simulation of a double-wall shield concept for the Wide Field Monitor aboard LOFT
The space mission LOFT (Large Observatory For X-ray Timing) was selected in
2011 by ESA as one of the candidates for the M3 launch opportunity. LOFT is
equipped with two instruments, the Large Area Detector (LAD) and the Wide Field
Monitor (WFM), based on Silicon Drift Detectors (SDDs). In orbit, they would be
exposed to hyper-velocity impacts by environmental dust particles, which might
alter the surface properties of the SDDs. In order to assess the risk posed by
these events, we performed simulations in ESABASE2 and laboratory tests. Tests
on SDD prototypes aimed at verifying to what extent the structural damages
produced by impacts affect the SDD functionality have been performed at the Van
de Graaff dust accelerator at the Max Planck Institute for Nuclear Physics
(MPIK) in Heidelberg. For the WFM, where we expect a rate of risky impacts
notably higher than for the LAD, we designed, simulated and successfully tested
at the plasma accelerator at the Technical University in Munich (TUM) a
double-wall shielding configuration based on thin foils of Kapton and
Polypropylene. In this paper we summarize all the assessment, focussing on the
experimental test campaign at TUM.Comment: Proc. SPIE 9144, Space Telescopes and Instrumentation 2014:
Ultraviolet to Gamma Ray, 91446
Radiation tests of the Silicon Drift Detectors for LOFT
During the three years long assessment phase of the LOFT mission, candidate
to the M3 launch opportunity of the ESA Cosmic Vision programme, we estimated
and measured the radiation damage of the silicon drift detectors (SDDs) of the
satellite instrumentation. In particular, we irradiated the detectors with
protons (of 0.8 and 11 MeV energy) to study the increment of leakage current
and the variation of the charge collection efficiency produced by the
displacement damage, and we "bombarded" the detectors with hypervelocity dust
grains to measure the effect of the debris impacts. In this paper we describe
the measurements and discuss the results in the context of the LOFT mission.Comment: Proc. SPIE 9144, Space Telescopes and Instrumentation 2014:
Ultraviolet to Gamma Ray, 91446
A magnetic electron repeller to improve the ATHENA/WFI background level
The WFI is a DEPFET-based device developed at MPE as one of the two focal plane instruments for the next large ESA's mission for high energy astrophysics ATHENA. The expected level of instrumental background induced by the radiation environment in space is one of the parameters driving the camera design and it is required to be below 5∙10 cts/cm2 /sec/keV to enhance some of the unique observing capabilities of this detector. Background reduction can be obtained in a passive way by optimizing the detector shielding specifications (e.g. materials, thicknesses) and discarding frame regions affected by X-ray-like counts. In principle a higher rejection efficiency could be achieved with an active anticoincidence system surrounding the detector, in practice this cannot be done as it would make very complicated the camera readout and introduce dead-time. In this proceeding we discuss how a passive shielding against soft electrons with efficiency comparable to that of an active anticoincidence and no dead-time issue could be obtained by means of permanent magnets. We present results of a very preliminary feasibility study conducted in the framework of AHEAD and demonstrate theoretically the effectiveness of this solution. Nevertheless, an actual implementation would have as drawbacks an increased mass of the camera due to the presence of magnets and a potentially disturbing residual field in the detector environment
In-orbit background of X-ray microcalorimeters and its effects on observations
Methods.There are no experimental data about the background experienced by
microcalorimeters in the L2 orbit, and thus the particle background levels were
calculated by means of Monte Carlo simulations: we considered the original
design configuration and an improved configuration aimed to reduce the
unrejected background, and tested them in the L2 orbit and in the low Earth
orbit, comparing the results with experimental data reported by other X-ray
instruments.To show the results obtainable with the improved configuration we
simulated the observation of a faint, high-redshift, point source (F[0.5-10
keV]~6.4E-16 erg cm-2 s-1, z=3.7), and of a hot galaxy cluster at R200
(Sb[0.5-2 keV]=8.61E-16 erg cm-2 s-1 arcmin-2,T=6.6 keV). Results.First we
confirm that implementing an active cryogenic anticoincidence reduces the
particle background by an order of magnitude and brings it close to the
required level.The implementation and test of several design solutions can
reduce the particle background level by a further factor of 6 with respect to
the original configuration.The best background level achievable in the L2 orbit
with the implementation of ad-hoc passive shielding for secondary particles is
similar to that measured in the more favorable LEO environment without the
passive shielding, allowing us to exploit the advantages of the L2 orbit.We
define a reference model for the diffuse background and collect all the
available information on its variation with epoch and pointing direction.With
this background level the ATHENA mission with the X-IFU instrument is able to
detect ~4100 new obscured AGNs with F>6.4E-16 erg cm-2 s-1 during three years,
to characterize cluster of galaxies with Sb(0.5-2 keV)>9.4E-16 erg cm-2 s-1
sr-1 on timescales of 50 ks (500 ks) with errors <40% (<12%) on
metallicity,<16% (4.8%) on temperature,2.6% (0.72%) on the gas density, and
several single-element abundances.Comment: the PDF has poor quality, it will be improved in the futur
The Microchannel X-ray Telescope for the Gamma-Ray Burst mission SVOM
We present the Microchannel X-ray Telescope, a new light and compact
focussing telescope that will be flying on the Sino-French SVOM mission
dedicated to Gamma-Ray Burst science. The MXT design is based on the coupling
of square pore micro-channel plates with a low noise pnCCD. MXT will provide an
effective area of about 50 cmsq, and its point spread function is expected to
be better than 3.7 arc min (FWHM) on axis. The estimated sensitivity is
adequate to detect all the afterglows of the SVOM GRBs, and to localize them to
better then 60 arc sec after five minutes of observation.Comment: 12 pages, 8 figures, to be published in SPIE Astronomical Telescopes
+ Instrumentation, Montreal, June 201
The Microchannel X-ray Telescope on Board the SVOM Satellite
We present the Micro-channel X-ray Telescope (MXT), a new narrow-field (about
1{\deg}) telescope that will be flying on the Sino-French SVOM mission
dedicated to Gamma-Ray Burst science, scheduled for launch in 2021. MXT is
based on square micro pore optics (MPOs), coupled with a low noise CCD. The
optics are based on a "Lobster Eye" design, while the CCD is a focal plane
detector similar to the type developed for the seven eROSITA telescopes. MXT is
a compact and light (<35 kg) telescope with a 1 m focal length, and it will
provide an effective area of about 45 cmsq on axis at 1 keV. The MXT PSF is
expected to be better than 4.2 arc min (FWHM) ensuring a localization accuracy
of the afterglows of the SVOM GRBs to better than 1 arc min (90\% c.l. with no
systematics) provided MXT data are collected within 5 minutes after the
trigger. The MXT sensitivity will be adequate to detect the afterglows for
almost all the SVOM GRBs as well as to perform observations of non-GRB
astrophysical objects. These performances are fully adapted to the SVOM science
goals, and prove that small and light telescopes can be used for future small
X-ray missions.Comment: 6 pages, 6 figures, proceedings of the conference "Swift: 10 years of
Discovery", Rome, December 2-5, 2014. To be published by Po
Monte-Carlo Simulations of the Suzaku-XRS Residual Background Spectrum
Cryogenic micro-calorimeters are suitable to detect small amounts of energy deposited by electromagnetic and nuclear interactions, which makes them attractive in a variety of applications on ground and in space. The only X-ray microcalorimeter that operated in orbit to date is the X-Ray Spectrometer on-board of the Japanese Suzaku satellite. We discuss the analysis of the components of its residual background spectrum with the support of Monte-Carlo simulations
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