The RUSALKA device for measuring the carbon dioxide and methane concentration in the atmosphere from on board the International Space Station

Korablev, Oleg; Kalinnikov, Y.; Титов, А. Н.; Rodin, A. V.; Smirnov, Yu. V.; Poluarshinov, M. A.; Kostrova, E. A.; Kalyuzhnyi, A. V.; Trokhimovskiĭ, A. Yu.; Vinogradov, I.; Fedorova, Anna; Иванов, А. В.; Venkstern, A. A.; Barke, V. V.; Roste, O. Z.

doi:10.1364/jot.78.000317

Cited by 20 publications

(8 citation statements)

References 12 publications

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“…Also, the echelle grating efficiency quickly decreases away from the blaze angle (center of the detector) and, combined with a similar effect of the AOTF bandpass curve, induces a significant reduction of signal near the edges of the detector. The closest analogue of NIR is the RUSALKA instrument (Russian acronym for Manual Spectral Analyzer of the Atmosphere Constituents), flown on the International Space Station (ISS) in -2012(Korablev et al 2011. RUSALKA covered the spectral range of 0.7-1.65 µm with a resolving power of λ/ λ ≈ 20,000, and demonstrated its capability to measure terrestrial CO 2 and CH 4 lines in a nadir viewing.…”

Section: Nir Channelmentioning

confidence: 99%

“…It was built by Space Research Institute (IKI) in Moscow (Russia) within a very constrained timeframe (only three years separate the approval of the mission and the delivery of the proto-flight model, PFM). ACS design leverages on previous developments thus providing high technology readiness levels at the onset of the project: two of the three channels were initially conceived and built for the unsuccessful Phobos-Grunt project (Korablev et al , 2013, while one instrument flew onboard the International Space Station from 2009 to 2012 (Korablev et al 2011). Some components/subsystems were contributed by LATMOS (CNRS) in France.…”

Section: Introductionmentioning

confidence: 99%

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The Atmospheric Chemistry Suite (ACS) of Three Spectrometers for the ExoMars 2016 Trace Gas Orbiter

et al. 2017

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The Atmospheric Chemistry Suite (ACS) package is an element of the Russian contribution to the ESA-Roscosmos ExoMars 2016 Trace Gas Orbiter (TGO) mission. ACS consists of three separate infrared spectrometers, sharing common mechanical, electrical, and thermal interfaces. This ensemble of spectrometers has been designed and developed in response to the Trace Gas Orbiter mission objectives that specifically address the requirement of high sensitivity instruments to enable the unambiguous detection of trace gases of potential geophysical or biological interest. For this reason, ACS embarks a set of instruments achieving simultaneously very high accuracy (ppt level), very high resolving power (>10,000) and large spectral coverage (0.7 to 17 µm-the visible to thermal infrared range). The near-infrared (NIR) channel is a versatile spectrometer covering the 0.7-1.6 µm spectral range with a resolving power of ∼20,000. NIR employs the combination of an echelle grating with an AOTF (Acousto-Optical Tunable Filter) as diffraction order selector. This channel will be mainly operated in solar occultation and nadir, and can also perform limb observations. The scientific goals of NIR are the measurements of water vapor, aerosols, and dayside or night side airglows. The mid-infrared (MIR) channel is a cross-dispersion echelle instrument dedicated to solar occultation measurements in the 2.2-4.4 µm range. MIR achieves a resolving power of >50,000. It has been designed to accomplish the most sensitive measurements ever of the trace gases present in the Martian atmosphere. The thermal-infrared channel (TIRVIM) is a 2-inch double pendulum Fourier-transform spectrometer encompassing the spectral range of 1.7-17 µm with apodized resolution varying from 0.2 to 1.3 cm −1 . TIRVIM is primarily dedicated to profiling temperature from the surface up to ∼60 km and to monitor aerosol abundance in nadir. TIRVIM also has a limb and solar occultation capability. The technical concept of the instrument, its accommodation on the spacecraft, the optical designs as well as some of the calibrations, and the expected performances for its three channels are described.

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Section: Nir Channelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The Atmospheric Chemistry Suite (ACS) of Three Spectrometers for the ExoMars 2016 Trace Gas Orbiter

et al. 2017

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“…SOIR, operating since 2006 exclusively in solar occultations allowed to obtain vertical profiles of minor constituents in the Venusian atmosphere, and important isotope ratios. In the following, a pilot experiment RUSALKA (Russian acronym for handheld Spectral AnaLyser for Constituents of Atmosphere, also stands for the mermaid) to demonstrate the possibility to measure the greenhouse gases in the terrestrial atmosphere using a SOIR-type instrument in the spectral range 0.7-1.7 µm was realized on ISS [19]. Different cosmonaut crews operated RUSALKA from 2009 through 2012.…”

Section: The Aotfs In Spacementioning

confidence: 99%

AOTF spectrometers in space missions and their imaging capabilities

Korablev¹,

Trokhimovsky²,

Kalinnikov

2017

International Conference on Space Optics — ICSO 2016

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“…Its design capitalizes on the previous developments of high technology readiness: two instruments built for unsuccessful Phobos-Grunt project [4][5][6] and one instrument flown at the ISS in 2009-2012 [7]. Some components/subsystems are contributed by German Institut für Planetenforschung (DLR) and LATMOS…”

Section: Introductionmentioning

confidence: 99%

High resolution middle infrared spectrometer, a part of atmospheric chemistry suite (ACS) for EXOMARS 2016 trace gas orbiter

Trokhimovskiy

Korablev

Ivanov

et al. 2017

International Conference on Space Optics — ICSO 2014

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The Atmospheric Chemistry Suite (ACS) package is a part of Russian contribution to ExoMars ESARoscosmos mission for studies of the Martian atmosphere and climate. ACS consists of three separate infrared spectrometers, sharing common mechanical, electrical, and thermal interfaces. The mid-infrared (MIR) channel is a cross-dispersion high resolution echelle instrument dedicated to solar occultation measurements and sensitive studies of trace gases. The MIR channel is a spectrometer working in 2.3-4.2 µm spectral range, covering simultaneously up to almost 300 nm per exposure, targeting the resolving power of 50,000. A crossdispersion concept on echelle and ordinary diffraction grating allows acquisition of the wide wavelength domain at once. That provides a strategic advantage for maximizing the number of gaseous species detected simultaneously and good special resolution of measurements during fast occultation sessions. Moving the second grating allows to switch from one group of the diffraction orders to another prior to a series of measurements, or desired positions during one measurement sequence. The concept of the cross-dispersion echelle instrument, which is widely accepted in astronomy, has been already employed in planetary missions with VIRTIS-H instrument presently in flight on Rosetta and Venus Express missions.Targeting very high spectral resolution the MIR channel operates in solar occultation only. A telescope with relative aperture of 1:3 forms the image of the solar disk on the slit. The FOV is determined by the slit and it consists 0.1×2.9 mrad. The spectral resolution of the spectrometer is fully slit-limited, and the resolving power of λ/Δλ ≥ 50000 at 3.3 µm is supported. Two secondary cross-dispersion diffraction gratings (plain, 180 and 361 grooves per mm) are mounted back-to-back on a stepper motor to change observed echelle orders. We have chosen two secondary gratings philosophy to switch between them depending on the long or short wavelength range we are on. Changing the position of the secondary grating in angular steps of 1.8°, from 10 to 30 echelle orders are available for simultaneous record depending on the wavelength. 100 steps are evidently used to switch between gratings prior measurements. The full spectral range is covered on diffraction orders from 142 to 248. For each observation detector area is covered by 10 to 30 stripes, each corresponding to single echelle diffraction order. Given the complexity of the diffraction orders pattern, full detector frames will be transmitted to the ground, with lossless compression. However, the onboard averaging will be possible. Single data frame will be accumulated for 0.5 seconds, stacking of a number of shorter exposures.

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The RUSALKA device for measuring the carbon dioxide and methane concentration in the atmosphere from on board the International Space Station

Cited by 20 publications

References 12 publications

The Atmospheric Chemistry Suite (ACS) of Three Spectrometers for the ExoMars 2016 Trace Gas Orbiter

The Atmospheric Chemistry Suite (ACS) of Three Spectrometers for the ExoMars 2016 Trace Gas Orbiter

AOTF spectrometers in space missions and their imaging capabilities

High resolution middle infrared spectrometer, a part of atmospheric chemistry suite (ACS) for EXOMARS 2016 trace gas orbiter

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