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Proceedings Paper

The Cryogenic AntiCoincidence detector for ATHENA: the progress towards the final pixel design
Author(s): Claudio Macculi; Luigi Piro; Donatella Cea; Luca Colasanti; Simone Lotti; Lorenzo Natalucci; Flavio Gatti; Daniela Bagliani; Michele Biasotti; Dario Corsini; Giulio Pizzigoni; Guido Torrioli; Marco Barbera; Teresa Mineo; Emanuele Perinati
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Paper Abstract

“The Hot and Energetic Universe” is the scientific theme approved by the ESA SPC for a Large mission to be flown in the next ESA slot (2028th) timeframe. ATHENA is a space mission proposal tailored on this scientific theme. It will be the first X-ray mission able to perform the so-called “Integral field spectroscopy”, by coupling a high-resolution spectrometer, the X-ray Integral Field Unit (X-IFU), to a high performance optics so providing detailed images of its field of view (5’ in diameter) with an angular resolution of 5” and fine energy-spectra (2.5eV@E<7keV). The X-IFU is a kilo-pixel array based on TES (Transition Edge Sensor) microcalorimeters providing high resolution spectroscopy in the 0.2-12 keV range. Some goals is the detection of faint and diffuse sources as Warm Hot Intergalactic Medium (WHIM) or galaxies outskirts. To reach its challenging scientific aims, it is necessary to shield efficiently the X-IFU instrument against background induced by external particles: the goal is 0.005 cts/cm^2/s/keV. This scientific requirement can be met by using an active Cryogenic AntiCoincidence (CryoAC) detector placed very close to X-IFU (~ 1 mm below). This is shown by our GEANT4 simulation of the expected background at L2 orbit. The CryoAC is a TES based detector as the X-IFU sharing with it thermal and mechanical interfaces, so increasing the Technology Readiness Level (TRL) of the payload. It is a 2x2 array of microcalorimeter detectors made by Silicon absorber (each of about 80 mm^2 and 300 μm thick) and sensed by an Ir TES. This choice shows that it is possible to operate such a detector in the so-called athermal regime which gives a response faster than the X-IFU (< 30 μs), and low energy threshold (above few keV). Our consortium has developed and tested several samples, some of these also featured by the presence of Al-fins to efficiently collect the athermal phonons, and increased x-ray absorber area (up to 1 cm^2). Here the results of deep test related to one of the last sample produced (namely AC-S5), and steps to reach the final detector design will be discussed.

Paper Details

Date Published: 24 July 2014
PDF: 14 pages
Proc. SPIE 9144, Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray, 91445S (24 July 2014); doi: 10.1117/12.2054946
Show Author Affiliations
Claudio Macculi, INAF - Istituto di Astrofisica e Planetologia Spaziali (Italy)
Luigi Piro, INAF - Istituto di Astrofisica e Planetologia Spaziali (Italy)
Donatella Cea, INAF - Istituto di Astrofisica e Planetologia Spaziali (Italy)
Luca Colasanti, INAF - Istituto di Astrofisica e Planetologia Spaziali (Italy)
Simone Lotti, INAF - Istituto di Astrofisica e Planetologia Spaziali (Italy)
Lorenzo Natalucci, INAF - Istituto di Astrofisica e Planetologia Spaziali (Italy)
Flavio Gatti, Univ. degli Studi di Genova (Italy)
Daniela Bagliani, Univ. degli Studi di Genova (Italy)
Michele Biasotti, Univ. degli Studi di Genova (Italy)
Dario Corsini, Univ. degli Studi di Genova (Italy)
Giulio Pizzigoni, Univ. degli Studi di Genova (Italy)
Guido Torrioli, Istituto di Fotonica e Nanotecnologie, CNR (Italy)
Marco Barbera, Univ. degli Studi di Palermo (Italy)
Teresa Mineo, INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica di Palermo (Italy)
Emanuele Perinati, Institut für Astronomie und Astrophysik Tübingen, Eberhard Karls Univ. Tübingen (Germany)


Published in SPIE Proceedings Vol. 9144:
Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray
Tadayuki Takahashi; Jan-Willem A. den Herder; Mark Bautz, Editor(s)

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