Near-Infrared Mapping Spectrometer Of The Phobos Space Mission To The Planet Mars

1988 ◽  
Author(s):  
P Puget ◽  
S Cazes ◽  
A Soufflot ◽  
J.P Bibring ◽  
M Combes
Keyword(s):  
Near Infrared ◽  
Space Mission

Twinkle: a low-Earth orbit, visible and infrared observatory for exoplanet and solar system spectroscopy

2020 ◽  
Author(s):  
Billy Edwards ◽  
Marcell Tessenyi ◽  
Giorgio Savini ◽  
Giovanna Tinetti ◽  
Ian Stotesbury ◽  
...  
Keyword(s):  
Solar System ◽  
Near Infrared ◽  
Surface Composition ◽  
Thermal Environment ◽  
Space Mission ◽  
Low Earth Orbit ◽  
Atmospheric Composition ◽  
Solar System Objects ◽  
Scientific Potential ◽  
Asteroids And Comets

<p>The Twinkle Space Mission is a space-based observatory that has been conceived to measure the atmospheric composition of exoplanets, stars and solar system objects. The satellite is based on a high-heritage platform and will carry a 0.45 m telescope with a visible and infrared spectrograph providing simultaneous wavelength coverage from 0.5 - 4.5 μm. The spacecraft will be launched into a Sun-synchronous low-Earth polar orbit and will operate in this highly stable thermal environment for a baseline lifetime of seven years.</p> <p>Twinkle’s rapid pointing and non-sidereal tracking capabilities will enable the observation of a diverse array of Solar System objects, including asteroids and comets. Twinkle aims to provide a visible and near-infrared spectroscopic population study of asteroids and comets to study their surface composition and monitor activity. Its wavelength coverage and position above the atmosphere will make it particularly well-suited for studying hydration features that are obscured by telluric lines from the ground as well as searching for other spectral signatures such as organics, silicates and CO<sub>2</sub>.</p> <p>Twinkle is available for researchers around the globe in two ways:</p> <p>1) joining its collaborative multi-year survey programme, which will observe hundreds of exoplanets and solar system objects; and</p> <p>2) accessing dedicated telescope time on the spacecraft, which they can schedule for any combination of science cases.</p> <p>I will present an overview of Twinkle’s capabilities and discuss the broad range of targets the mission could observe, demonstrating the huge scientific potential of the spacecraft.</p>

scholarly journals Icarus: In-situ monitoring of the surface degradation on a near-Sun asteroid

2021 ◽  
Author(s):  
Mikael Granvik ◽  
Tuomas Lehtinen ◽  
Andrea Bellome ◽  
Joan-Pau Sánchez
Keyword(s):  
Near Infrared ◽  
Low Cost ◽  
Bulk Composition ◽  
European Space Agency ◽  
Space Mission ◽  
In Situ Monitoring ◽  
The Sun ◽  
Spacecraft Design ◽  
Cost Constraints ◽  
Space Agency

<div class="page" title="Page 1"> <div class="layoutArea"> <div class="column"> <p>Icarus is a mission concept designed to record the activity of an asteroid during a close encounter with the Sun. The primary science goal of the mission is to unravel the nontrivial mechanism(s) that destroy asteroids on orbits with small perihelion distances. Understanding the destruction mechanism(s) allows us to constrain the bulk composition and interior structure of asteroids in general. The Icarus mission does not only aim to achieve its science goals but also functions as a technical demonstration of what a low-cost space mission can do. The proposed space segment will include a single spacecraft capable of surviving and operating in the harsh environment near the Sun. The spacecraft design relies on the heritage of missions such as Rosetta, MESSENGER, Parker Solar Probe, BepiColombo, and Solar Orbiter. The spacecraft will rendezvous with an asteroid during its perihelion passage and records the changes taking place on the asteroid’s surface. The primary scientific payload has to be capable of imaging the asteroid’s surface in high resolution using visual and near-infrared channels as well as collecting and analyzing particles that are ejected from the asteroid. The payload bay also allows for additional payloads relating to, for example, solar research. The Icarus spacecraft and the planned payloads have high technology readiness levels and the mission is aimed to fit the programmatic and cost constraints of the F1 mission (Comet Interceptor) by the European Space Agency. Considering the challenging nature of the Icarus trajectory and the fact that the next F-class mission opportunity (F2) is yet to be announced, we conclude that Icarus is feasible as an F-class mission when certain constraints such as a suitable launch configuration are met (e.g., if EnVision is selected as M5). A larger mission class, such as the M class by the European Space Agency, would be feasible in all circumstances.</p> </div> </div> </div>

scholarly journals Comparison of PRISMA Data with Model Simulations, Hyperion Reflectance and Field Spectrometer Measurements on ‘Piano delle Concazze’ (Mt. Etna, Italy)

Sensors ◽  
2020 ◽  
Vol 20 (24) ◽  
pp. 7224
Author(s):  
Vito Romaniello ◽  
Malvina Silvestri ◽  
Maria Fabrizia Buongiorno ◽  
Massimo Musacchio
Keyword(s):  
Near Infrared ◽  
Pearson Correlation ◽  
Test Site ◽  
Short Wave ◽  
Space Mission ◽  
Mean Difference ◽  
Atmospheric Transmission ◽  
Complete Evaluation ◽  
Model Simulations ◽  
Mt Etna

In this work, we compare first acquisitions from the ASI-PRISMA (Agenzia Spaziale Italiana-PRecursore IperSpettrale della Missione Applicativa) space mission with model simulations, past data acquired by the Hyperion sensor and field spectrometer measurements. The test site is ‘Piano delle Concazze’ (Mt. Etna, Italy), suitable for calibration purposes due to its homogeneity characteristics. The area measures at about 0.2 km2 and is composed of very homogeneous trachybasalt rich in plagioclase and olivine. Three PRISMA acquisitions, achieved on 31 July and 8 and 17 August 2019, are analyzed. Firstly, spectral profiles of PRISMA top of atmosphere (TOA) radiance are compared with MODerate resolution atmospheric TRANsmission (MODTRAN) simulations. The Pearson correlation coefficient is equal to 0.998 and 0.994 for VNIR (Visible and Near InfraRed) and SWIR (Short-Wave InfraRed) spectral ranges, respectively. PRISMA radiance overestimates values simulated by MODTRAN for all considered days, showing a mean bias of +5.22 and of +0.91 Wm−2sr−1µm−1 for VNIR and SWIR, respectively. The relative mean difference between reflectance values estimated by PRISMA and Hyperion, on the test area, is around +19%, despite the great difference in time acquisition (up to 19 years); PRISMA slightly overestimates Hyperion reflectance with an absolute mean difference of about +0.0083, within the variability of Hyperion acquisitions of ±0.0250 (corresponding to ±2 standard deviation). Finally, FieldSpec measurements also confirm the great quality of PRISMA reflectance estimations. The absolute mean difference results are around +0.0089 (corresponding to a relative error of about +21%). In the study, we investigate only the lower values of reflectance characterizing the test site. A more complete evaluation of PRISMA performances needs to consider other test sites with different optical characteristics.

scholarly journals Development of a near-infrared high-resolution spectrograph (WINERED) for a survey of bulge stars

2007 ◽  
Vol 3 (S248) ◽  
pp. 510-511
Author(s):  
T. Tsujimoto ◽  
N. Kobayashi ◽  
C. Yasui ◽  
S. Kondo ◽  
A. Minami ◽  
...  
Keyword(s):  
Chemical Composition ◽  
High Resolution ◽  
Radial Velocity ◽  
Optical System ◽  
Near Infrared ◽  
Space Mission ◽  
Proper Motions ◽  
Galactic Bulge ◽  
System A ◽  
Combined Data

AbstractWe are developing a new near-infrared high-resolution (R[max] = 100,000) and high-sensitive spectrograph WINERED, which is specifically customized for short NIR bands at 0.9–1.35 μm. WINERED employs an innovative optical system; a portable design and a warm optics without any cold stops. The planned astrometric space mission JASMINE will provide precise positions, distances, and proper motions of the bulge stars. The missing components, the radial velocity and chemical composition will be measured by WINERED. These combined data brought by JASMINE and WINERED will certainly reveal the nature of the Galactic bulge. We plan to complete this instrument for observations of single objects by the end of 2008 and to attach it to various 4–10m telescopes as a PI-type instrument. We hope to upgrade WINERED with a multi-object feed in the future for efficient survey of the JASMINE bulge stars.

scholarly journals Multispectral Polarization State Analyzer of Scanning Polarimeter ScanPol

2020 ◽  
Vol 2020 ◽  
pp. 1-15
Author(s):  
Ivan Syniavskyi ◽  
Yevgen Oberemok ◽  
Yuriy Ivanov ◽  
Mikhail Sosonkin
Keyword(s):  
Atmospheric Aerosols ◽  
Linear Polarization ◽  
Near Infrared ◽  
Signal To Noise Ratio ◽  
Polarization State ◽  
Spectral Characteristics ◽  
Space Mission ◽  
Polarization Measurement ◽  
Stokes Parameters ◽  
Near Ultraviolet

We present the results of the development of a representational model of the multispectral polarization state analyzer of the ScanPol scanning polarimeter for the space experiment Aerosol-UA. The aim of the Ukrainian space mission Aerosol-UA is to create a database based on continuous satellite measurements of the optical characteristics of aerosol and cloud particles in the Earth’s atmosphere over a long period of time. The ScanPol polarimeter is designed to acquire spatial, temporal, and spectral-polarimetric measurements simultaneously to minimize instrumental “parasitic” effects and effects of “false” polarizations due to scene movement. Simultaneity is provided by separation of the initial spatial field by a pair of conjugated telescopes and a pair of Wollaston prisms. ScanPol provides to measure the first three Stokes parameters I, Q, and U of the radiation reflected by atmospheric aerosols and the Earth’s surface for a six solar reflectance spectral bands in the near ultraviolet (NUV), visible (VIS), and near-infrared (NIR) spectral channels centered in the wavelengths 370 nm, 410 nm, 555 nm, 865 nm, 1378 nm, and 1620 nm. Stokes parameters I, Q, and U are used to determine a degree of linear polarization of radiation that will allow obtaining the phase function and polarization characteristics of aerosol particle scattering, estimate their size, and determine the aerosol type and optical thickness. The polarimeter optical layout is considered, and the spectral characteristics of the transmission of optical channels are given. Obtained signal-to-noise ratio exceeded 500 for wavelengths 370 nm and 410 nm and exceeded 1000 for other wavelengths. The design of the chosen photodetectors is based on surface mount type photodiodes: Si-photodiodes Hamamatsu S10356-01 for the optical range of 370–860 nm and InGaAs-photodiodes Hamamatsu G8941-011620 for wavelengths 1378 nm and 1620 nm. The effect of orientation of Wollaston prisms axes on polarization measurement error is considered. The errors of azimuth mount of Wollaston prisms ≤2 arcmin in ScanPol leads to error of degree of linear polarization ≤0.0012.

scholarly journals Predicting the global far-infrared SED of galaxies via machine learning techniques

2020 ◽  
Vol 634 ◽  
pp. A57 ◽  
Author(s):  
W. Dobbels ◽  
M. Baes ◽  
S. Viaene ◽  
S. Bianchi ◽  
J. I. Davies ◽  
...  
Keyword(s):  
Machine Learning ◽  
Energy Balance ◽  
Near Infrared ◽  
Spectral Energy Distribution ◽  
Far Infrared ◽  
Space Mission ◽  
Machine Learning Techniques ◽  
Spectral Energy ◽  
Learning Framework ◽  
Learning Techniques

Context. Dust plays an important role in shaping a galaxy’s spectral energy distribution (SED). It absorbs ultraviolet (UV) to near-infrared radiation and re-emits this energy in the far-infrared (FIR). The FIR is essential to understand dust in galaxies. However, deep FIR observations require a space mission, none of which are still active today. Aims. We aim to infer the FIR emission across six Herschel bands, along with dust luminosity, mass, and effective temperature, based on the available UV to mid-infrared (MIR) observations. We also want to estimate the uncertainties of these predictions, compare our method to energy balance SED fitting, and determine possible limitations of the model. Methods. We propose a machine learning framework to predict the FIR fluxes from 14 UV–MIR broadband fluxes. We used a low redshift sample by combining DustPedia and H-ATLAS, and extracted Bayesian flux posteriors through SED fitting. We trained shallow neural networks to predict the far-infrared fluxes, uncertainties, and dust properties. We evaluated them on a test set using a root mean square error (RMSE) in log-space. Results. Our results (RMSE = 0.19 dex) significantly outperform UV–MIR energy balance SED fitting (RMSE = 0.38 dex), and are inherently unbiased. We can identify when the predictions are off, for example when the input has large uncertainties on WISE 22 μm, or when the input does not resemble the training set. Conclusions. The galaxies for which we have UV–FIR observations can be used as a blueprint for galaxies that lack FIR data. This results in a “virtual FIR telescope”, which can be applied to large optical-MIR galaxy samples. This helps bridge the gap until the next FIR mission.

Twinkle: a low-Earth orbit, visible and infrared observatory for exoplanet and solar system spectroscopy

2021 ◽  
Author(s):  
Billy Edwards ◽  
Marcell Tessenyi ◽  
Ian Stotesbury ◽  
Richard Archer ◽  
Ben Wilcock ◽  
...  
Keyword(s):  
Solar System ◽  
Near Infrared ◽  
Surface Composition ◽  
Space Mission ◽  
Low Earth Orbit ◽  
Earth Orbit ◽  
Spectral Signatures ◽  
Solar System Objects ◽  
Scientific Potential ◽  
Asteroids And Comets

<div>The Twinkle Space Mission is a space-based observatory that has been conceived to measure the atmospheric composition of exoplanets, stars and solar system objects. Twinkle’s collaborative multi-year global survey programmes will deliver visible and infrared spectroscopy of thousands of objects within and beyond our solar system, enabling participating scientists to produce world-leading research in planetary and exoplanetary science.</div> <div> </div> <p>Twinkle’s rapid pointing and non-sidereal tracking capabilities will enable the observation of a diverse array of Solar System objects, including asteroids and comets. Twinkle aims to provide a visible and near-infrared (0.5-4.5 micron) spectroscopic population study of asteroids and comets to study their surface composition and monitor activity. Its wavelength coverage and position above the atmosphere will make it particularly well-suited for studying hydration features that are obscured by telluric lines from the ground as well as searching for other spectral signatures such as organics, silicates and CO<sub>2</sub>.</p> <p>I will present an overview of Twinkle’s capabilities and discuss the broad range of targets the mission could observe, including the measurements it will take to support <span class="size">JAXA's Martian Moons eXploration (MMX) mission, demonstrating the broad scientific potential of the spacecraft.</span></p>

scholarly journals Exploring exoplanetary systems beyond 1AU with WFIRST

2013 ◽  
Vol 8 (S299) ◽  
pp. 62-63
Author(s):  
Matthew T. Penny ◽  
B. Scott Gaudi
Keyword(s):  
Near Infrared ◽  
Space Mission ◽  
Wide Field ◽  
Large Space ◽  
New Horizons ◽  
Exoplanetary Systems ◽  
Infrared Imager ◽  
Sensitivity Range ◽  
Peak Sensitivity ◽  
Low Mass

AbstractThe Wide Field InfraRed Survey Telescope (WFIRST) was the top ranked large space mission of the New Worlds, New Horizons Decadal Survey, and is currently under active study by NASA. Its primary instrument will be a large-format high-resolution near-infrared imager and slitless spectrometer. A primary goal of WFIRST will be to perform a high-cadence microlensing survey of the Galactic bulge to search for low-mass exoplanets beyond the ice line. We highlight some of the expected results of the WFIRST exoplanet survey. For example, the survey will probe the abundance of Earth-mass planets from less than 1 AU outwards, including free-floating planets. In its peak sensitivity range of ~2–5 AU, WFIRST will be sensitive to planets with masses lower than Mercury, and even down to the mass of Ganymede. Overall, WFIRST is expected to detect several thousand bound planets, in addition to several thousand free-floating planets. WFIRST will complete the exoplanet census begun by Kepler, enabling an unprecedented understanding of planetary systems and their formation.

The boot software of the control unit of the near infrared spectrograph of the Euclid space mission: technical specification

2016 ◽  
Author(s):  
Jaime Gómez-Sáenz-de-Tejada ◽  
Rafael Toledo-Moreo ◽  
Carlos Colodro-Conde ◽  
David Pérez-Lizán ◽  
Jesús Fernández-Conde ◽  
...  
Keyword(s):  
Near Infrared ◽  
Technical Specification ◽  
Control Unit ◽  
Space Mission
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