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10 results for “Spectral Composition”
Spectral reflectance data of Mercury's surface collected by the Mercury Atmospheric and Surface Composition Spectrometer (MASCS) instrument during orbital observations of the NASA MESSENGER mission between 2011 and 2015 resampled to a [55399 × 396] tabular data format.
<p>MASCS is a three sensor point spectrometer with a spectral coverage from 200 nm to 1450 nm.<br> Single spectra are resamples in to steps to a format useful for our ML application : a datacube with ~400 spectral channel covering the whole surface of Mercury.<br> The final dataset has dimension [N×M] where N is the number of grid cells (360 × 180 = 64, 800) and M is the number of spectral features (396).<br> Due to the incomplete coverage and data filtering, some grid cells are empty.<br> After removing these empty cells, the size of the dataset is [55399 × 396].</p> <p>This specific product is stored as a gzip compressed json, where each element is a grid cell.<br> We are in the process to publish a complete pipeline to produce this product from RAW data on https://github.com/epn-ml/MESSENGER-Mercury-Surface-Cassification-Unsupervised_DLR/ .</p> <p>Spectral reflectance data of Mercury’s surface collected by the Mercury Atmospheric and Surface Composition Spectrometer (MASCS) instrument during orbital observations of the NASA MESSENGER mission between 2011 and 2015.<br> MASCS is a three sensor point spectrometer with a spectral coverage from 200 nm to 1450 nm.<br> Single spectra are resamples in to steps to a format useful for our ML application : a datacube with ~400 spectral channel covering the whole surface of Mercury.<br> The final dataset has dimension [N×M] where N is the number of grid cells (360 × 180 = 64, 800) and M is the number of spectral features (396).<br> Due to the incomplete coverage and data filtering, some grid cells are empty.<br> After removing these empty cells, the size of the dataset is [55399 × 396].</p> <p>0. Pre-filtering<br> We used the most recent dataset that had large-scale photometric corrections and thus was almost free from observation geometry effects.<br> However, extreme geometry are still present and are typically associated with high noise and some residual instrumental effects.<br> Based on our empirical tests, we filtered out observations with an emission/incidence angle ≥80∘.<br> We also calculated the median value per wavelength and per cell grid when constructing the global hyperspectral data cube and filtered out observations falling under the 2nd percentile and above 99.9th percentile to clean some residual geometry effects.<br> With this approach we create an effective noise filter while retaining enough observations to be able to analyse the entirety of the surface of the planet.</p> <p>1. Spectral resmpling<br> Unprocessed MASCS spectra could have 512 or 256 channes, depending on binning.<br> We resampled the data in the spectral dimension to a common wavelength range from 260 nm to 1052 nm with a 4 nm resolution (2 nm spectral sampling), resulting in 396 spectral channels.<br> This approach slightly oversamples the original 4.77 nm spectral resolution and removes some points from the original 200-1050 nm range.<br> The resulting data matrix is expressed in tabular form, with each row representing a single grid cell or pixel on the surface.<br> The elements of each row are the spectral reflectance values from the VIS instrument at 396 (resampled) wavelengths.</p> <p>2. Spatial resmpling<br> The whole dataset of ∼ 5 million spectra is resampled to a planet-wide rectangular grid of 1×1deg in the latitudinal band between ± 80.<br> The cell longitudinal size varies between ∼ 40 km at the equator to a minimum of ∼ 10 km at ±80∘.<br> Thus, the area spanned by each grid cell depends on the latitude. However, the same is true for the acquisition process, where higher spatial resolution is reached near the equator and lower resolution at the poles.</p>
Compositional maps of the lunar polar regions derived from the Kaguya Spectral Profiler and the Lunar Orbiter Laser Altimeter data
<p>Compositional maps of the lunar polar regions derived from the Kaguya Spectral Profiler and the Lunar Orbiter Laser Altimeter data as described in Lemelin et al. (2022). </p> <p>This folder includes different GeoTIFF files described and shown in Lemelin et al. (2022). The files are projected in Polar Stereographic Projection, at a spatial resolution of 1000 m/pixel. A version of each of the following file is given for the north and south polar region (50-90 N/S).</p> <p>- Gridded and interpolated Spectral Profiler reflectance mosaics scaled to the LOLA dataset at 1064 nm<br> - Data counts used in the gridded and interpolated Spectral Profiler reflectance mosaics scaled to the LOLA dataset at 1064 nm<br> - Spectral Profiler FeO mosaics <br> - Spectral Profiler OMAT mosaics <br> - Spectral Profiler plagioclase mosaics <br> - Spectral Profiler olivine mosaics <br> - Spectral Profiler low-calcium pyroxene mosaics<br> - Spectral Profiler high-calcium pyroxene mosaics <br> - Nanophase iron mosaics <br> - Correlation coefficient mosaics</p>
Contrasting light demands determine the coordination of plants’ non-structural carbohydrates and economic strategy over the range of solar spectral composition
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Testing trait plasticity over the range of spectral composition of sunlight in forb species differing in shade tolerance
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Spectral composition of light pollution affects melatonin suppression and West Nile virus infection resistance and mortality in the House Sparrow (Passer domesticus).
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Data from: Stressful colors: corticosterone concentrations in a free-living songbird vary with the spectral composition of experimental illumination
Organisms have evolved under natural daily light/dark cycles for millions of years. These cycles have been disturbed as night-time darkness is increasingly replaced by artificial illumination. Investigating the physiological consequences of free-living organisms in artificially lit environments is crucial to determine whether nocturnal lighting disrupts circadian rhythms, changes behaviour, reduces fitness and ultimately affects population numbers. We make use of a unique, large-scale network of replicated field sites which were experimentally illuminated at night using lampposts emanating either red, green, white or no light to test effect on stress hormone concentrations (corticosterone) in a songbird, the great tit (Parus major). Adults nesting in white-light transects had higher corticosterone concentrations than in the other treatments. We also found a significant interaction between distance to the closest lamppost and treatment type: individuals in red light had higher corticosterone levels when they nested closer to the lamppost than individuals nesting farther away, a decline not observed in the green or dark treatment. Individuals with high corticosterone levels had fewer fledglings, irrespective of treatment. These results show that artificial light can induce changes in individual hormonal phenotype. As these effects vary considerably with light spectrum, it opens the possibility to mitigate these effects by selecting street lighting of specific spectra.
Code produced by the study "Advantages of assimilating multi-spectral satellite retrievals of atmospheric composition: A demonstration using MOPITT carbon monoxide products".
<p>This is the code used in the manuscript entitled "Advantages of assimilating multi-spectral satellite retrievals of atmospheric composition: A demonstration using MOPITT carbon monoxide products".</p>
Dataset and code for 'Signal to Noise Ratio and Spectral Sampling Constraints on Olivine Detection and Compositional Determination in the Intermediate Infrared Region'
<p>Feature fitting code and spectra of olivine samples used in paper "<em>Signal to Noise Ratio and Spectral Sampling Constraints on Olivine Detection and Compositional Determination in the Intermediate Infrared Region: Applications in Planetary Sciences</em>"</p>
Data from: Stressful colors: corticosterone concentrations in a free-living songbird vary with the spectral composition of experimental illumination
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Spectral and thermometric properties altering through crystal field strength modification and host material composition in luminescent thermometers based on Fe3+ doped AB2O4 type nanocrystals (A= Mg, Ca; B=Al, Ga)
<p>The growing interest in the use of luminescence thermometry for noncontact temperature reading in very specific conditions imposes the need to develop an approach allowing modification of the luminescence parameters of the thermometer accordingly to the requirements. Therefore, in response to these expectations, this manuscript reports an approach to modulating the spectral position and the luminescence thermal quenching rate of Fe<sup>3+</sup> ions by modifying the crystal field strength and the host material composition of nanocrystalline AB<sub>2</sub>O<sub>4</sub> type nanocrystals (A= Mg, Ca; B=Al, Ga). It was proved that in a group of MgAl<sub>2</sub>O<sub>4</sub>, MgGa<sub>2</sub>O<sub>4</sub>, CaAl<sub>2</sub>O<sub>4</sub>, and CaGa<sub>2</sub>O<sub>4</sub> nanocrystals doped with Fe<sup>3+</sup> ions the emission spectral range, as well as the relative thermal sensitivity (from 0.2%/<sup>o</sup>C for MAO to 2.07%/<sup>o</sup>C for CGO) and the operating temperature range, can be easily modified by the host material composition. For instance, a maximal relative thermal sensitivity of 2.58%/<sup>o</sup>C is obtained for Fe<sup>3+</sup>, Tb<sup>3+</sup> co-doped CaAl<sub>2</sub>O<sub>4 </sub>nanocrystals. The proposed approach is a step toward the intentional designing of the highly sensitive luminescent thermometer.</p>
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Allen Brain Atlas
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International Brain Laboratory public data
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OpenNeuro
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