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Euclid's Near-Infrared Spectrometer and Photometer ready for flight -- review of final performance
Authors:
E. Medinaceli,
L. Valenziano,
N. Auricchio,
E. Franceschi,
F. Gianotti,
P. Battaglia,
R. Farinelli,
A. Balestra,
S. Dusini,
C. Sirignano,
E. Borsato,
L. Stanco,
A. Renzi,
A. Troja,
L. Gabarra,
S. Ligori,
V. Capobianco,
L. Corcione,
D. Bonino,
G. Sirri,
L. Patrizii,
M. Tenti,
D. Di Ferdinando,
C. Valieri,
N. Mauri
, et al. (22 additional authors not shown)
Abstract:
ESA's mission Euclid, while undertaking its final integration stage, is fully qualified. Euclid will perform an extragalactic survey ($0<z<2$) by observing in the visible and near-infrared wavelength range. To detect infrared radiation, it is equipped with the Near Infrared Spectrometer and Photometer (NISP) instrument, operating in the 0.9--2 $μ$m range. In this paper, after introducing the surve…
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ESA's mission Euclid, while undertaking its final integration stage, is fully qualified. Euclid will perform an extragalactic survey ($0<z<2$) by observing in the visible and near-infrared wavelength range. To detect infrared radiation, it is equipped with the Near Infrared Spectrometer and Photometer (NISP) instrument, operating in the 0.9--2 $μ$m range. In this paper, after introducing the survey strategy, we focus our attention on the NISP Data Processing Unit's Application Software, highlighting the experimental process to obtain the final parametrization of the on-board processing of data produced by the array of 16 Teledyne HAWAII-2RG (HgCdTe) detectors. We report results from the latest ground test campaigns with the flight configuration hardware - complete optical system (Korsh anastigmat telescope), detectors array (0.56 deg$^2$ field of view), and readout systems (16 Digital Control Units and Sidecar ASICs). The performance of the on-board processing is then presented. We also describe a major issue found during the final test phase. We show how the problem was identified and solved thanks to an intensive coordinated effort of an independent review `Tiger' team, lead by ESA, and a team of NISP experts from the Euclid Consortium. An extended PLM level campaign at ambient temperature in Liège and a dedicated test campaign conducted in Marseille on the NISP EQM model eventually confirmed the resolution of the problem. Finally, we report examples of the outstanding spectrometric (using a Blue and two Red Grisms) and photometric performance of the NISP instrument, as derived from the end-to-end payload module test campaign at FOCAL 5 -- CSL; these results include the photometric Point Spread Function (PSF) determination and the spectroscopic dispersion verification.
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Submitted 6 November, 2023;
originally announced November 2023.
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Euclid Near Infrared Spectrometer and Photometer instrument flight model presentation, performance and ground calibration results summary
Authors:
T. Maciaszek,
A. Ealet,
W. Gillard,
K. Jahnke,
R. Barbier,
E. Prieto,
W. Bon,
A. Bonnefoi,
A. Caillat,
M. Carle,
A. Costille,
F. Ducret,
C. Fabron,
B. Foulon,
J. L. Gimenez,
E. Grassi,
M. Jaquet,
D. Le Mignant,
L. Martin,
T. Pamplona,
P. Sanchez,
J. C. Clémens,
L. Caillat,
M. Niclas,
A. Secroun
, et al. (73 additional authors not shown)
Abstract:
The NISP (Near Infrared Spectrometer and Photometer) is one of the two Euclid instruments. It operates in the near-IR spectral region (950-2020nm) as a photometer and spectrometer. The instrument is composed of: a cold (135 K) optomechanical subsystem consisting of a Silicon carbide structure, an optical assembly, a filter wheel mechanism, a grism wheel mechanism, a calibration unit, and a thermal…
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The NISP (Near Infrared Spectrometer and Photometer) is one of the two Euclid instruments. It operates in the near-IR spectral region (950-2020nm) as a photometer and spectrometer. The instrument is composed of: a cold (135 K) optomechanical subsystem consisting of a Silicon carbide structure, an optical assembly, a filter wheel mechanism, a grism wheel mechanism, a calibration unit, and a thermal control system, a detection system based on a mosaic of 16 H2RG with their front-end readout electronic, and a warm electronic system (290 K) composed of a data processing / detector control unit and of an instrument control unit that interfaces with the spacecraft via a 1553 bus for command and control and via Spacewire links for science data.
This paper presents: the final architecture of the flight model instrument and subsystems, and the performance and the ground calibration measurement done at NISP level and at Euclid Payload Module level at operational cold temperature.
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Submitted 18 October, 2022;
originally announced October 2022.
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Ariel: Enabling planetary science across light-years
Authors:
Giovanna Tinetti,
Paul Eccleston,
Carole Haswell,
Pierre-Olivier Lagage,
Jérémy Leconte,
Theresa Lüftinger,
Giusi Micela,
Michel Min,
Göran Pilbratt,
Ludovic Puig,
Mark Swain,
Leonardo Testi,
Diego Turrini,
Bart Vandenbussche,
Maria Rosa Zapatero Osorio,
Anna Aret,
Jean-Philippe Beaulieu,
Lars Buchhave,
Martin Ferus,
Matt Griffin,
Manuel Guedel,
Paul Hartogh,
Pedro Machado,
Giuseppe Malaguti,
Enric Pallé
, et al. (293 additional authors not shown)
Abstract:
Ariel, the Atmospheric Remote-sensing Infrared Exoplanet Large-survey, was adopted as the fourth medium-class mission in ESA's Cosmic Vision programme to be launched in 2029. During its 4-year mission, Ariel will study what exoplanets are made of, how they formed and how they evolve, by surveying a diverse sample of about 1000 extrasolar planets, simultaneously in visible and infrared wavelengths.…
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Ariel, the Atmospheric Remote-sensing Infrared Exoplanet Large-survey, was adopted as the fourth medium-class mission in ESA's Cosmic Vision programme to be launched in 2029. During its 4-year mission, Ariel will study what exoplanets are made of, how they formed and how they evolve, by surveying a diverse sample of about 1000 extrasolar planets, simultaneously in visible and infrared wavelengths. It is the first mission dedicated to measuring the chemical composition and thermal structures of hundreds of transiting exoplanets, enabling planetary science far beyond the boundaries of the Solar System. The payload consists of an off-axis Cassegrain telescope (primary mirror 1100 mm x 730 mm ellipse) and two separate instruments (FGS and AIRS) covering simultaneously 0.5-7.8 micron spectral range. The satellite is best placed into an L2 orbit to maximise the thermal stability and the field of regard. The payload module is passively cooled via a series of V-Groove radiators; the detectors for the AIRS are the only items that require active cooling via an active Ne JT cooler. The Ariel payload is developed by a consortium of more than 50 institutes from 16 ESA countries, which include the UK, France, Italy, Belgium, Poland, Spain, Austria, Denmark, Ireland, Portugal, Czech Republic, Hungary, the Netherlands, Sweden, Norway, Estonia, and a NASA contribution.
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Submitted 10 April, 2021;
originally announced April 2021.