5 research outputs found
Active and passive shielding design optimization and technical solutions for deep sensitivity hard X-ray focusing telescopes
The 10-100 keV region of the electromagnetic spectrum contains the potential
for a dramatic improvement in our understanding of a number of key problems in
high energy astrophysics. A deep inspection of the universe in this band is on
the other hand still lacking because of the demanding sensitivity (fraction of
microCrab in the 20-40 keV for 1 Ms integration time) and imaging (~15" angular
resolution) requirements. The mission ideas currently being proposed are based
on long focal length, grazing incidence, multi-layer optics, coupled with focal
plane detectors with few hundreds microns spatial resolution capability. The
required large focal lengths, ranging between 8 and 50 m, can be realized by
means of extendable optical benches (as foreseen e.g. for the HEXIT-SAT, NEXT
and NuSTAR missions) or formation flight scenarios (e.g. Simbol-X and XEUS).
While the final telescope design will require a detailed trade-off analysis
between all the relevant parameters (focal length, plate scale value, angular
resolution, field of view, detector size, and sensitivity degradation due to
detector dead area and telescope vignetting), extreme attention must be
dedicated to the background minimization. In this respect, key issues are
represented by the passive baffling system, which in case of large focal
lengths requires particular design assessments, and by the active/passive
shielding geometries and materials. In this work, the result of a study of the
expected background for a hard X-ray telescope is presented, and its
implication on the required sensitivity, together with the possible
implementation design concepts for active and passive shielding in the
framework of future satellite missions, are discussed.Comment: 13 pages, 6 figures. Proceedings of SPIE conference "Optics for EUV,
X-Ray, and Gamma-Ray Astronomy II", San Diego (CA, USA), July 31st - August
4th, 2005, Vol. 5900. Full color figures are available at
http://www.bo.iasf.cnr.it/~malaguti/papers/SPIE2005_1.ps.g
Design of a CZT Gamma-Camera for GRB and Fast Transient Follow-up: a Wide-Field-Monitor for the EDGE Mission
The success of the SWIFT/BAT and INTEGRAL missions has definitely opened a
new window for follow-up and deep study of the transient gamma-ray sky. This
now appears as the access key to important progresses in the area of
cosmological research and deep understanding of the physics of compact objects.
To detect in near real-time explosive events like Gamma-Ray bursts,
thermonuclear flashes from Neutron Stars and other types of X-ray outbursts we
have developed a concept for a wide-field gamma-ray coded mask instrument
working in the range 8-200 keV, having a sensitivity of 0.4 ph cm-2 s-1 in 1s
(15-150 keV) and arcmin location accuracy over a sky region as wide as 3sr.
This scientific requirement can be achieved by means of two large area, high
spatial resolution CZT detection planes made of arrays of relatively large
(~1cm2) crystals, which are in turn read out as matrices of smaller pixels. To
achieve such a wide Field-Of-View the two units can be placed at the sides of a
S/C platform serving a payload with a complex of powerful X-ray instruments, as
designed for the EDGE mission. The two units will be equipped with powerful
signal read out system and data handling electronics, providing accurate
on-board reconstruction of the source positions for fast, autonomous target
acquisition by the X-ray telescopes.Comment: 9 pages, 7 figures, SPIE Conference on UV, X-ray, and Gamma-Ray
Instrumentation for Astronomy, San Diego 26-30 August 200
The Processing and Power Unit of the METIS Coronagraph aboard the Solar Orbiter Space Mission
The Multi Element Telescope for Imaging and Spectroscopy (METIS) is the coronagraph selected for the Solar Orbiter
payload, adopted in October 2011 by ESA for the following Implementation Phase. The instrument design has been
conceived by a team composed by several research institutes with the aim to perform both VIS and EUV narrow-band
imaging and spectroscopy of the solar corona. METIS, owing to its multi-wavelength capability, will address some of
the major open issues in understanding the physical processes in the corona and the solar wind origin and properties,
exploiting the unique opportunities offered by the SO mission profile.
The METIS Processing and Power Unit (MPPU) is the Instrument's power supply and on-board data handling modular
electronics, designed to address all the scientific requirements of the METIS Coronagraph. MPPU manages data and
command flows, the timing and power distribution networks and its architecture reflects several trade-off solutions with
respect to the allocated resources in order to reduce any possible electronics single-point failure. This paper reports on
the selected HW and SW architectures adopted after the Preliminary Design Review (PDR), performed by ESA in early
2012