Vavilovskii Zhurnal Genetiki i Selektsii = Vavilov Journal of Genetics and Breeding. 2019;23(5):582-587 (in Russian) Page 587, in Acknowledgements instead of The animals and behavioral testing are ...supported by the budget project (No. 0324-2019-0041). The MRI study is supported by the budget project (No. 0259-2019-0004). All studies are implemented using the equipment of Center for Genetic Resources of Laboratory Animals at ICG SB RAS, supported by the Ministry of Education and Science of Russia (Unique ID# of the project: RFMEFI62117X0015). should read The animals and behavioral testing are supported by the budget project (No. 0324-2019-0041). The MRI study is supported by the budget project (No. 0259-2019-0004). All studies are implemented using the equipment of Center for Genetic Resources of Laboratory Animals at ICG SB RAS, supported by the Ministry of Education and Science of Russia (Unique ID# of the project: RFMEFI62117X0015). The study was conducted within the basic part of the state task of the Ministry of Science and Higher Education of the Russian Federation (No. 17.7255.2017/8.9). The original article can be found under DOI 10.18699/VJ19.528.
The design, principle of operation, and results of tests of a Fourier-transform spectrometer, which is designed for studying the composition of the Martian atmosphere by the transmission technique, ...are described. A standard specimen of the instrument must operate on the landing platform after its delivery to Mars. The spectral range of the manufactured specimen is 0.5–4 μm, the spectral resolution is 0.04 cm
–1
, the aperture is 25 mm, and the mass is 1.1 kg.
The design and principle of operation of a mirror system that was designed for the automatic guidance of a spectrometer field of view with an aperture of 25 mm at the Sun and tracking the Sun with an ...accuracy of up to 1 mrad are described. The spectrometer will be installed on a landing platform on the surface of Mars. A prototype with a mass of 900 g was manufactured and tested.
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.
The design and performance features of an IR Fourier-transform spectrometer for studying the Martial atmosphere in the spectrum range of 600–5500 cm
–1
during the ExoMars-2016 mission are described. ...The obtained spectral resolution is in agreement with the theoretical value (0.2 cm
–1
); the threshold of the instrument sensitivity is approximately 0.1 mW/(m
2
sr cm
–1
).
The Planetary Fourier Spectrometer (PFS) experiment on board the Mars Express mission has two channels covering the 1.2–5.5
μ
m short wavelength channel (SWC) and the 5.5–45
μ
m (LWC). The SWC ...measures part of the thermal emission spectrum and the solar reflected spectrum of Mars between 1700 and 8200
cm
−1 with a spectral resolution of 1.3
cm
−1, in absence of apodisation. We present here the calibration of this channel and its performance. The instrument calibration has been performed on ground, before launch, in space during near earth verification (NEV) measurements, and at Mars. Special attention has been given to the problem of microvibrations on board the spacecraft.
In order to obtain correct results, the source–instrument–detector interaction for the thermal part is studied very accurately. The instrument shows a nonlinear behaviour with source intensity. The SNR increases with amplification, hence high gain factors are usually used. The detector is, in space, cooled by a passive radiator, and works around 210–215
K. The calibration source (an internal lamp) shows variations during a pericentre pass and therefore impose a complex procedure for the SW channel calibration. Mechanical microvibrations strongly affect part of the spectrum. We discuss the validity of the present calibration, and indicate possible future developments. Samples of the calibrated data are given to show the performance of the experiment and its scientific potentialities.
Nanoparticles (NPs) can be transported via the nose-to-brain (N2B) route. Nonetheless, quantitative data on their spatiotemporal dynamics and regulation of the N2B transport are largely lacking. We ...surveyed metal oxide/hydroxide NPs as magnetic resonance imaging (MRI) contrasts for quantitative N2B tracking. NPs containing divalent transition metals were the only ones capable of N2B transmission. Using T
1
-weighted (T
1
W) MRI, we showed that Mn
3
O
4
-NPs were readily engulfed by olfactory receptor neurons (ORNs) without disrupting olfactory sensing, and we mapped their N2B trajectory. Within neurons, the Mn
3
O
4
-NPs were localized to the cytosol, mitochondria, and vesicles, and moved at mixed fast and slow axonal transport velocities intra- and extra-vesicularly through ORNs. The NPs’ axonal transport is dependent on neuronal activity and microtubule integrity. The Mn
3
O
4
-NPs were trans-synaptically transmitted through at least four synapses across the olfactory tract. Trans-synaptic transmission of the NPs was dependent on N-type Ca
2+
channels and NMDA receptors but blocked by GABA
B
receptor activation. A five-parameter Weibull signal increase/decrease model fitted to the T
1
W MRI data allowed for estimating kinetic parameters of Mn
3
O
4
-NP accumulation/elimination. Absolute and relative accumulation rates, but not elimination, correlated negatively with the number of synapses from ORNs, indicating a coupling of the NPs’ N2B transport with spontaneous neuronal activity. Accordingly, olfactory stimuli (2,5-dimethylpyrazine and acetophenone) significantly modulated and rerouted the Mn
3
O
4
-NP N2B transport odor specifically. Finally, the NPs’ trans-synaptic transmission was impaired by aging and the onset of Parkinson’s disease. These data suggest new approaches to diagnostics, functional neuroimaging, and controlling N2B drug delivery.
An AOST Fourier spectrometer of the Phobos-Soil project is intended for studying Mars and Phobos by means of measurements of IR radiation spectra of the Martian surface and atmosphere, the Phobos ...surface, and the spectrum of solar radiation passing through the Martian atmosphere on its limb. The main scientific problems to be solved with the spectrometer on Mars are measurements of methane content, search for minor constituents, and study of diurnal variations in the temperature and atmospheric aerosol. The spectrometer will also study the Martian and Phobos surface both remotely and after landing. The spectral range of the instrument is 2.5–25 μm, the best spectral resolution (without apodization) is 0.6 cm
−1
, and the instantaneous field of view is 2.5°. The recording time of one spectrum is equal to 5 s in solar observations and 50 s in observations of Mars and Phobos. The instrument has self-thermal stabilization and two-axis pointing systems, as well as a built-in radiation source for flight calibration. The spectrometer mass is 4 kg, and power consumption is up to 13 W. Scientific problems, measurement modes, and, briefly, engineering implementation of the experiment are discussed in this work.
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