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16 results for “Light Spectra”
Modeling of the micro-focused Brillouin light scattering spectra
<p><strong>This repository contains data and code presented in paper titled: Modeling of the micro-focused Brillouin light scattering spectra</strong></p> <p> </p> <h2><strong>Data</strong></h2> <p>The structure of this archive is divided by the usage of the data in individual figures in paper titled "Modeling of the micro-focused Brillouin light scattering spectra", which can be found in zip file named <em>ModelingOfTheMicro-focusedBrillouinLightScatteringSpectra-1.0.0_FigsData.zip</em></p> <p>the encoding in .dat files is utf-8<br>All the presented data are in .dat files (no need to open <em>.opju </em>to get access to the data)<br>The <em>.opju</em> is source file of OriginLab software and can be open by freely available tools - <a href="https://www.originlab.com/viewer/" target="_blank" rel="noopener">www.originlab.com/viewer/</a></p> <p>Each folder contains another <em>info.txt</em> where the data are described individually</p> <h2>Software</h2> <p>All the codes used to generate figures in the paper can be found on the Github platform in publicly available repository. The code can be used and modified if the authors and paper are credited. <a title="github.com/CEITECmagnonics/ModelingOfTheMicro-focusedBrillouinLightScatteringSpectra" href="https://github.com/CEITECmagnonics/ModelingOfTheMicro-focusedBrillouinLightScatteringSpectra" target="_blank" rel="noopener">https://github.com/CEITECmagnonics/ModelingOfTheMicro-focusedBrillouinLightScatteringSpectra</a></p> <p>Release v1.0.0 is available in <em>ModelingOfTheMicro-focusedBrillouinLightScatteringSpectra-1.0.0_code.zip</em></p> <p> </p> <p>The software also uses another freely available tool for calculating spin wave dispersion: <a title="github.com/CEITECmagnonics/SpinWaveToolkit" href="https://github.com/CEITECmagnonics/SpinWaveToolkit" target="_blank" rel="noopener">https://github.com/CEITECmagnonics/SpinWaveToolkit</a></p>
Diffuse reflectance spectra of coated plates and corresponding plots transformed Kubelka-Munk function versus the energy of light (eV)
<p>The link contains UV-DRS results of TiO<sub>2</sub>/Fe<sub>2</sub>O<sub>3</sub> layered composites (from commercial nanoparticles) and corresponding bandgap energies</p>
Dataset: Fano meets Stokes: Four-order-of-magnitude enhancement of asymmetric Brillouin light scattering spectra
<p>Dataset accompanying publication:</p> <p>Rafał Białek, Thomas Vasileiadis, Mikołaj Pochylski, Bartłomiej Graczykowski, Fano meets Stokes: Four-order-of-magnitude enhancement of asymmetric Brillouin light scattering spectra, Photoacoustics, Volume 30, 2023, 100478, ISSN 2213-5979, https://doi.org/10.1016/j.pacs.2023.100478.</p>
MCMC samples for X-ray spectra fits summarised in the paper "A strangely light neutron star"
<p>Posterior samples for NS mass and radius described based on fitting of XMM-Newton and Suzaku spectra of the CCO in HESS J1731-347 and described in the paper the paper "A strangely light neutron star" (DOI: <a href="https://doi.org/10.21203/rs.3.rs-1509469/v1">10.21203/rs.3.rs-1509469/v1</a>). Two files uploaded contain posterior samples based based </p> <p>a) on fitting X-ray data alone using single temperature carbon atmosphere model and Gaia parallax priors (xray_only_carbatm.txt)</p> <p>b) on fitting the same X-ray data but including also all additional priors described in the main text and full priors on distance rather than inverted parallax value (full_priors_carbatm.txt). Note that initial version contained wrong file uploaded by error, so the correct file to use in this case is full_priors_carbatm_corr.txt. We urge, however, to use a) as a baseline, i.e. as input for incorporating of other constraints for two reasons: first, the procedure of incorporating other constraints adopted by us and you may be different, and second, this file contains relatively small number of samples as it was mainly meant as illustration putting our results in context of other constraints and to give an idea of impact which our measurement has on EOS selection for a particular family of EOSs, so the result would be different if other set of EOSs is considered. </p> <p>in addition a file with updated weights for EOSs used by Dietrich et al 2021 (2020Sci...370.1450D, available on https://github.com/diettim/NMMA) which take into the account constrains from X-ray spectral fitting presented in our work for the CCO and constrains based on modeling of the 4U 1702-429 bursts reported by Nattila et al 2017 (2017A&A...608A..31N) are included in file chiralEFT_MTOV_NICER_GW170817_AT2017gfo_cco_weights.txt. This file is based on and has the same syntax as file chiralEFT_MTOV_NICER_GW170817_AT2017gfo_weighting.dat provided by Dietrich et al 2021 available on https://github.com/diettim/NMMA along with the corresponding tabulated EOS files.</p> <p> </p>
Photoactivation of the Orange Carotenoid Protein Requires Two Light-Driven Reactions Mediated by a Metastable Monomeric Intermediate – Absorption Spectra and Global Analysis Results, Molecular Dynamics Simulations
<p>Time-resolved absorption and molecular dynamics trajectory datasets associated with: Rose, J. B.; Gascón, J. A.; Sutter, M.; Sheppard, D. I.; Kerfeld, C. A.; Beck, W. F. Photoactivation of the Orange Carotenoid Protein Requires Two Light-Driven Reactions Mediated by a Metastable Monomeric Intermediate. <i>Phys. Chem. Chem. Phys.</i> <strong>2023</strong>, DOI: 10.1039/d3cp04484j.</p>
Mass spectra for single Scrippsiella trochoidea cells: light vs. dark & replete vs. N limiting conditions
<p>Data files for 77 <em>Scrippsiella trochoidea </em>cells measured in single cell MS experiments. Information about the experimental conditions, corresponding file names, the number of cells for which data are recorded in each respective file, and the range of acquisition times for individual cells can be found in the supplemental documentation of the corresponding manuscript titled : "Single Cell Metabolomic Analysis of <em>Scrippsiella trochoidea</em>" in Frontiers in Plant Science. </p> <p>Note: .mzML is a standard MS file format that can be viewed using freeware such as mMass (<a href="http://www.mmass.org/">http://www.mmass.org/</a>) and ProteoWizard (<a href="http://proteowizard.sourceforge.net/index.shtml">http://proteowizard.sourceforge.net/index.shtml</a>).</p> <p> </p> <p> </p> <p> </p>
X-ray Emission of Nearby Low-mass and Sun-like Stars with Directly Imageable Habitable Zones: X-ray Spectra and Light Curves
<p>This repository contains the X-ray light curves extracted from the XMM-Newton and Chandra observations and the best-fit X-ray spectral models (with and without emission lines) from all stars detected at high significance in Binder et al. (2024), ApJS, ..., ...</p> <p>Description of Files:</p> <h3>LightCurves.zip</h3> <p>Summary: Light curve files (327) for all stars detected at high significance; in FITS (BinTableHDU) format with 7-14 extensions. The following types of data are included:</p> <ul> <li>"*_source.lc" : EPIC/PN source light curves of stars detected with more than ~500 net counts in an XMM-Newton observation</li> <li>"*_bkg.lc" : EPIC/PN background light curves of stars detected with more than ~500 net counts in an XMM-Newton observation</li> <li>"*_sub_lc.fits" : Background-subtracted light curves of stars detected with more than ~50 net counts in a Chandra observation</li> </ul> <h3>Spectra.zip</h3> <p>Summary: Spectra (152) for all stars detected at high significance (with >500 net counts in Chandra observations and >2000 net counts in XMM-Newton observations) in ASCII (ECSV format). We provide both the continuum spectra and spectra containing line emission. For stars that exhibit X-ray count rate variability, we provide spectra for specific variability types (see Binder et al. 2024 for details). The following types of data are included:</p> <ul> <li>"*_continuum.dat" : Continuum-only best-fit spectra</li> <li>"*_lines.dat" : Best-fit spectra containing line emission</li> </ul>
Experimental light at night of different spectra alters movement patterns of bats along ecological corridors
<p>Data used for the study. </p> <p>Meaning of codes for "spectra" and "lamppost_side" variables:</p> <p>- C = control</p> <p>- G = green</p> <p>- R = red</p> <p>- W = white</p> <p>- L = left</p> <p>- R = right</p>
Severe and widespread reductions in nighttime activity of nocturnal moths under modern artificial lighting spectra
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Light curves and frequency spectra (ordem alternativa para tese)
<p>(1) Tabela de classificação e (2) curvas de luz com análise de frequências, ordenados de acordo com a classificação primária de variabilidade.</p>
Light curves and frequency spectra
<p>The light curve, wavelet transform, and frequency spectra analysis of each stars in our sample. The upper panel displays the light curves of the star, with it’s EPIC identifier. The middle panel shows the wavelet transform of the light curves. The lower panel presents the frequency spectra of the stars, with the blue line indicating the frequencies obtained using the cleanest method and triangles indicating the frequencies found with the ivs-KULeuven iterative prewhitening routine (Degroote et al. 2009). Each star is identified by its EPIC number.</p>
Dynamic light scattering size distribution, ζ-potential data, and fluorescence spectra
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Data from: Response of bats to light with different spectra: light-shy and agile bat presence is affected by white and green, but not red light
Artificial light at night has shown a remarkable increase over the past decades. Effects are reported for many species groups, and include changes in presence, behaviour, physiology and life-history traits. Among these, bats are strongly affected, and how bat species react to light is likely to vary with light colour. Different spectra may therefore be applied to reduce negative impacts. We used a unique set-up of eight field sites to study the response of bats to three different experimental light spectra in an otherwise dark and undisturbed natural habitat. We measured activity of three bat species groups around transects with light posts emitting white, green and red light with an intensity commonly used to illuminate countryside roads. The results reveal a strong and spectrum-dependent response for the slow-flying Myotis and Plecotus and more agile Pipistrellus species, but not for Nyctalus and Eptesicus species. Plecotus and Myotis species avoided white and green light, but were equally abundant in red light and darkness. The agile, opportunistically feeding Pipistrellus species were significantly more abundant around white and green light, most likely because of accumulation of insects, but equally abundant in red illuminated transects compared to dark control. Forest-dwelling Myotis and Plecotus species and more synanthropic Pipistrellus species are thus least disturbed by red light. Hence, in order to limit the negative impact of light at night on bats, white and green light should be avoided in or close to natural habitat, but red lights may be used if illumination is needed.
Simulations of light curves and spectra for superluminous Type Ic supernovae powered by magnetars
<p>Model spectra from <a href="https://ui.adsabs.harvard.edu/abs/2019A%26A...621A.141D">Dessart 2019, A&A, 621, 141</a>.</p>
Spectra and light curves presented in Double detonations: variations in Type Ia supernovae due to different core and He shell masses – II. Synthetic observables
<p>Dataset containing simulated spectra and light curves presented in the paper "Double detonations: variations in Type Ia supernovae due to different core and He shell masses – II. Synthetic observables" (<a href="https://ui.adsabs.harvard.edu/abs/2022MNRAS.517.5289C/abstract">ADS</a>).</p> <p> </p>
Data from: Response of bats to light with different spectra: light-shy and agile bat presence is affected by white and green, but not red light
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