A detector interferometric calibration experiment for high precision astrometry

Crouzier, Antoine; Malbet, Fabien; Hénault, François; Léger, Alain; Cara, C.; LeDuigou, J. M.; Preis, Olivier; Kern, P.; Delboulbé, A.; Martín, G.; Feautrier, Philippe; Stadler, Eric; Lafrasse, S.; Rochat, S.; Ketchazo, Christian; Donati, Modeste; Doumayrou, E.; Lagage, Pierre-Olivier; Shao, Michael; Goullioud, Renaud; Nemati, Bijan; Zhai, Chengxing; Béhar, Etienne; Potin, S.; Saint-Pe, M.; Dupont, J.

doi:10.1051/0004-6361/201526321

Cited by 21 publications

(13 citation statements)

References 40 publications

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“…The small differential displacement of an Earth-hosting star with respect to the background reference stars due to the orbiting planet can only be measured if the uncertainties on the geometry of the focal plane array (FPA) are calibrated to sub-microarcsecond over many arcminutes (a precision below 10 À5 pixels). An interferometric laser metrology system illuminating the FPA can help to retrieve the position of the PSF centroid (Crouzier et al 2016).…”

Section: Metrology and Calibration Techniquesmentioning

confidence: 99%

Astrophotonics: astronomy and modern optics

Minardi¹,

Harris

Labadie

2021

Astron Astrophys Rev

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Much of the progress in astronomy has been driven by instrumental developments, from the first telescopes to fiber fed spectrographs. In this review, we describe the field of astrophotonics, a combination of photonics and astronomical instrumentation that is gaining importance in the development of current and future instrumentation. We begin with the science cases that have been identified as possibly benefiting from astrophotonic devices. We then discuss devices, methods and developments in the field along with the advantages they provide. We conclude by describing possible future perspectives in the field and their influence on astronomy.

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Section: Metrology and Calibration Techniquesmentioning

confidence: 99%

Astrophotonics: astronomy and modern optics

Minardi¹,

Harris

Labadie

2021

Astron Astrophys Rev

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“…[4][5]. Here are firstly presented tentative product breakdown structures for the NEAT test bench and flight instrument ( § 2.1), before describing in more details the most important sub-system requirements and design ( § 2.2).…”

Section: System Requirements and Designmentioning

confidence: 99%

“…The selected detector array for the NEAT breadboard is the CCD 39-01 from E2V company, in order to take advantage of its high frame rate and quantum well size [5]. When in primary vacuum, the chip can be cooled down to -10°C by a Peltier module in order to reduce noise.…”

Section: Detection Unit (Du)mentioning

confidence: 99%

“…Moreover, in order to achieve the required astrometric precision of 1 microarcsecond, the locations of stellar images formed by the telescope at the detector plane shall be measured within an accuracy equivalent to 5 10 -6 pixels typically. Because such a stringent requirement is beyond the technical state-of-theart by one or several magnitude orders [2][3], IPAG (Institut de Planétologie et d'Astrophysique de Grenoble) and CNES (Centre National d'Etudes Spatiales) have developed together an optical test bench incorporating an interferometric metrology system measuring pixel gains and centroid location errors [4][5]. The latest results from this test bench are presented in another paper in this conference series [6].…”

Section: Introductionmentioning

confidence: 99%

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NEAT breadboard system analysis and performance models

Hénault

Crouzier

Malbet³

et al. 2014

SPIE Proceedings

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NEAT (Nearby Earth Astrometric Telescope) is an astrometric space mission aiming at detecting Earth-like exoplanets located in the habitable zone of nearby solar-type stars. For that purpose, NEAT should be able to measure stellar centroids within an accuracy of 5 10 -6 pixels. In order to fulfil such stringent requirement, NEAT incorporates an interferometric metrology system measuring pixel gains and location errors. To validate this technology and assess the whole performance of the instrument, a dedicated test bench has been built at IPAG, in Grenoble (France). In this paper are summarized the main system engineering considerations allowing to define sub-systems specifications. Then we describe the general architecture of the performance models (including photometric, interferometric, and final astrometric budgets) and confront their predictions with the experimental results obtained on the test bench. It is concluded that most of error items are well understood, although some of them deserve further investigations.

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“…The low impact of stellar activity on the astrometric signal compared to radial velocity is therefore one of the reasons why high-precision astrometric space missions have been proposed to detect low-mass planets around stars in our neighbourhood (Léger et al 2015;Janson et al 2018), such as the Space Interferometry Mission (SIM; e.g. Shao et al 1995;Svensson & Ludwig 2005;Catanzarite et al 2008;Makarov et al 2009), the Nearby Earth Astrometric Telescope (NEAT; Malbet et al 2012;Crouzier et al 2016), or Telescope for A&A 644, A77 (2020) Habitable Exoplanets and Interstellar/Intergalactic Astronomy (THEIA; Theia Collaboration 2017), although they present a huge technological challenge (e.g. Malbet et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Activity time series of old stars from late F to early K

Meunier

Lagrange

2020

A&A

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Context. Stellar activity strongly affects and may prevent the detection of Earth-mass planets in the habitable zone of solar-type stars with radial velocity technics. Astrometry is in principle less sensitive to stellar activity because the situation is more favourable: the stellar astrometric signal is expected to be fainter than the planetary astrometric signal compared to radial velocities. Aims. We quantify the effect of stellar activity on high-precision astrometry when Earth-mass planets are searched for in the habitable zone around old main-sequence solar-type stars. Methods. We used a very large set of magnetic activity synthetic time series to characterise the properties of the stellar astrometric signal. We then studied the detectability of exoplanets based on different approaches: first based on the theoretical level of false positives derived from the synthetic time series, and then with blind tests for old main-sequence F6-K4 stars. Results. The amplitude of the signal can be up to a few times the solar value depending on the assumptions made for activity level, spectral type, and spot contrast. The detection rates for 1 MEarth planets are very good, however, with extremely low false-positive rates in the habitable zone for stars in the F6-K4 range at 10 pc. The standard false-alarm probability using classical bootstrapping on the time series strongly overestimates the false-positive level. This affects the detection rates. Conclusions. We conclude that if technological challenges can be overcome and very high precision is reached, astrometry is much more suitable for detecting Earth-mass planets in the habitable zone around nearby solar-type stars than radial velocity, and detection rates are much higher for this range of planetary masses and periods when astrometric techniques are used than with radial velocity techniques.

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A detector interferometric calibration experiment for high precision astrometry

Cited by 21 publications

References 40 publications

Astrophotonics: astronomy and modern optics

Astrophotonics: astronomy and modern optics

NEAT breadboard system analysis and performance models

Activity time series of old stars from late F to early K

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