Compact high-resolution micro-spectrometer on chip: spectral calibration and first spectrum

Diard, Thomas; Barrière, Florence de la; Ferrec, Yann; Guérineau, Nicolas; Rommeluère, Sylvain; Coarer, E. Le; Martín, G.

doi:10.1117/12.2223692

Cited by 9 publications

(4 citation statements)

References 5 publications

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“…Its primary instrument fits in 6U, and the entire spacecraft is only 12U. The instrument is a Fourier Transform spectrometer based on a Fizeau interferometer using the µSPOC (Micro Spectrometer on a Chip) concept (Diard et al., 2016). In its current version, ATISE has 6 lines of sight distributed along a vertical, each with a field of view of 1° in the vertical direction and 1.5° in the horizontal direction.…”

Section: Sswrf Missions To Address Space Weather Research and Operati...mentioning

confidence: 99%

Small Satellite Mission Concepts for Space Weather Research and as Pathfinders for Operations

et al. 2022

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Solar activity drives rapid variations in the radiation and plasma environment in interplanetary and geospace. These variations occur on timescales of minutes and hours, associated with solar flares and coronal mass ejections (CMEs), to a few days, as complex magnetic features on the Sun, such as active regions and coronal holes, rotate across the solar disk. These phenomena result in orders-of-magnitude increases in the fluxes of high-energy (extreme ultraviolet [EUV], and especially X-ray and gamma ray) photons and energetic, often relativistic particles (electrons, protons, alphas, and heavier ions) streaming through interplanetary space. These enhanced photon and particle fluxes pose direct risks to humans and electronics in space. The increased radiation and associated propagating disturbances in the interplanetary magnetic field (e.g., from CMEs or so-called "co-rotating

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Section: Sswrf Missions To Address Space Weather Research and Operati...mentioning

confidence: 99%

Small Satellite Mission Concepts for Space Weather Research and as Pathfinders for Operations

et al. 2022

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“…the Jacquinot advantage) and, provided the measurement is detector noise limited, its multiplexing nature (Fellgett's advantage). The lSPOC system developed recently by IPAG and ONERA (Diard et al, 2016) is particularly attractive as it combines the above mentioned advantages with those of a very compact design without moving parts.…”

Section: The Lspoc Interferometermentioning

confidence: 99%

AMICal Sat and ATISE: two space missions for auroral monitoring

Barthélemy¹,

Калегаев²,

Vialatte³

et al. 2018

J. Space Weather Space Clim.

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A lack of observable quantities renders it generally difficult to confront models of Space Weather with experimental data and drastically reduces the forecast accuracy. This is especially true for the region of Earth’s atmosphere between altitudes of 90 km and 300 km, which is practically inaccessible, except by means of remote sensing techniques. For this reason auroral emissions are an interesting proxy for the physical processes taking place in this region. This paper describes two future space missions, AMICal Sat and ATISE, that will rely on CubeSats to observe the aurora. These satellites will perform measurements of auroral emissions in order to reconstruct the deposition of particle precipitations in auroral regions. ATISE is a 12U CubeSat with a spectrometer and imager payloads. The spectrometer is built using the micro-Spectrometer-On-a-Chip (μSPOC) technology. It will work in the 370–900 nm wavelength range and allow for short exposure times of around 1 s. The spectrometer will have six lines of sight. The joint imager is a miniaturized wide-field imager based on the Teledyne-E2V ONYX detector in combination with a large aperture objective. Observation will be done at the limb and will enable reconstruction of the vertical profile of the auroral emissions. ATISE is planned to be launched in mid 2021. AMICal Sat is a 2U CubeSat that will embed the imager of ATISE and will observe the aurora both in limb and nadir configurations. This imager will enable measuring vertical profiles of the emission when observing in a limb configuration similar to that of ATISE. It will map a large part of the night side auroral oval with a resolution of the order of a few km. Both the spectrometer and imager will be calibrated with a photometric precision better than 10% using the moon as a wide-field, stable and extended source. Ground-based demonstrators of both instruments have been tested in 2017 in Norway and Svalbard. Even though some issues still need to be solved, the first results are very encouraging for the planned future space missions. Data interpretation will be done using the forward Transsolo code, a 1D kinetic code solving the Boltzmann equation along a local vertical and enabling simulation of the thermospheric and ionospheric emissions using precipitation data as input.

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“…The spectral resolution is limited to a few thousands by the maximum OPD at the final edge of the detector. A high spectral resolution version has more recently been developed, called SWIFTS-LA (SWIFTS Large Aperture) [55] or SPOC-HR [87]. In this configuration the 2 nd dimension of the 2D detector is also used for optical path modulation, and spectro-imaging capability is lost.…”

Section: Spectrometer On Chip (Spoc)mentioning

confidence: 99%

Spectrographs for astrophotonics

Blind,

Coarer,

Kern

et al. 2017

Preprint

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The next generation of Extremely Large Telescopes (ELT), with diameters up to 39 meters, is planned to begin operation in the next decade and promises new challenges in the development of instruments since the instrument size increases in proportion to the telescope diameter D, and the cost as D 2 or faster. The growing field of astrophotonics (the use of photonic technologies in astronomy) could solve this problem by allowing mass production of fully integrated and robust instruments combining various optical functions, with the potential to reduce the size, complexity and cost of instruments. Astrophotonics allows for a broad range of new optical functions, with applications ranging from sky background filtering, high spatial and spectral resolution imaging and spectroscopy. In this paper, we want to provide astronomers with valuable keys to understand how photonics solutions can be implemented (or not) according to the foreseen applications. The paper introduces first key concepts linked to the characteristics of photonics technologies, placed in the framework of astronomy and spectroscopy. We then describe a series of merit criteria that help us determine the potential of a given micro-spectrograph technology for astronomy applications, and then take an inventory of the recent developments in integrated micro-spectrographs with potential for astronomy. We finally compare their performance, to finally draw a map of typical science requirements and pin the identified integrated technologies on it. We finally emphasize the necessary developments that must support micro-spectrograph in the coming years.

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Compact high-resolution micro-spectrometer on chip: spectral calibration and first spectrum

Cited by 9 publications

References 5 publications

Small Satellite Mission Concepts for Space Weather Research and as Pathfinders for Operations

Small Satellite Mission Concepts for Space Weather Research and as Pathfinders for Operations

AMICal Sat and ATISE: two space missions for auroral monitoring

Spectrographs for astrophotonics

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