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Proceedings Paper

The on-board electronics for the near infrared spectrograph and photometer (NISP) of the EUCLID Mission
Author(s): Leonardo Corcione; Sebastiano Ligori; Favio Bortoletto; Carlotta Bonoli; Luca Valenziano; Rafael Toledo-Moreo; Maurizio D'Alessandro; Massimo Trifoglio; Gianluca Morgante; Carlos Colodro-Conde; Rafael Rebolo-López; Jacinto Muñoz; Isidro Villò
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Paper Abstract

The Near Infrared Spectrograph and Photometer (NISP) is one of the instruments on board the EUCLID mission. The focal plane array (FPA) consists of 16 HAWAII-2RG HgCdTe detectors from Teledyne Imaging Scientific (TIS), for NIR imaging in three bands (Y, J, H) and slitless spectroscopy in the range 0.9−2µm. Low total noise measurements (i.e. total noise < 8 electrons) are achieved by operating the detectors in multiple non-destructive readout mode for the implementation of both the Fowler and Up-The-Ramp (UTR) sampling, which also enables the detection and removal of cosmic ray events. The large area of the NISP FPA and the limited satellite telemetry available impose to perform the required data processing on board, during the observations. This requires a well optimized on-board data processing pipeline, and high-performance control electronics, suited to cope with the time constraints of the NISP acquisition sequences. This paper describes the architecture of the NISP on-board electronics, which take charge of several tasks, including the driving of each individual HAWAII-2RG detectors through their SIDECAR ASICs, the data processing, inclusive of compression and storage, and the instrument control tasks. We describe the implementation of the processing power needed for the demanding on-board data reduction. We also describe the basic operational modes that will be managed by the system during the mission, along with data flow and the Telemetry/TeleCommands flow. This paper reports the NISP on-board electronics architecture status at the end of the Phase B1, and it is presented on behalf of the Euclid Consortium.

Paper Details

Date Published: 21 September 2012
PDF: 12 pages
Proc. SPIE 8442, Space Telescopes and Instrumentation 2012: Optical, Infrared, and Millimeter Wave, 844232 (21 September 2012); doi: 10.1117/12.926004
Show Author Affiliations
Leonardo Corcione, INAF - Osservatorio Astrofisico di Torino (Italy)
Sebastiano Ligori, INAF - Osservatorio Astrofisico di Torino (Italy)
Favio Bortoletto, INAF - Osservatorio Astronomico di Padova (Italy)
Carlotta Bonoli, INAF - Osservatorio Astronomico di Padova (Italy)
Luca Valenziano, INAF - IASF Bologna (Italy)
Rafael Toledo-Moreo, Univ. Politécnica de Cartagena (Spain)
Maurizio D'Alessandro, INAF - Osservatorio Astronomico di Padova (Italy)
Massimo Trifoglio, INAF - IASF Bologna (Italy)
Gianluca Morgante, INAF - IASF Bologna (Italy)
Carlos Colodro-Conde, Univ. Politécnica de Cartagena (Spain)
Rafael Rebolo-López, Instituto de Astrofísica de Canarias (Spain)
Jacinto Muñoz, SENER Ingeniería y Sistemas SA (Spain)
Isidro Villò, Univ. Politécnica de Cartagena (Spain)


Published in SPIE Proceedings Vol. 8442:
Space Telescopes and Instrumentation 2012: Optical, Infrared, and Millimeter Wave
Mark C. Clampin; Giovanni G. Fazio; Howard A. MacEwen; Jacobus M. Oschmann Jr., Editor(s)

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