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235 results for “spectroscopic”
Research data supporting "Raman spectroscopic imaging for quantification of depth-dependent and local heterogeneities in native and engineered cartilage"
<p>Research data supporting the publication: Albro M. et al., 2018, npj Regenerative Medicine, DOI: https://doi.org/10.1038/s41536-018-0042-7.</p>
Data and results for manuscript: "Imaging and functional characterization of crop root systems using spectroscopic electrical impedance measurements"
<p>This package contains measured raw EIT data, electrical imaging results, spectral results from the Debye decomposition, and the Python scripts used to generate the plots in the manuscript titled:<br> <br> Imaging and functional characterization of crop root systems using spectroscopic electrical impedance measurement</p>
Extended Data for Publication "Testing the Spectroscopic Extraction of Suppression of Convective Blueshift"
<p>Efforts to detect low-mass exoplanets using stellar radial velocities (RVs) are currently limited by magnetic photospheric activity. Suppression of convective blueshift is the dominant magnetic contribution to RV variability in low-activity Sun-like stars. Due to convective plasma motions, the magnitude of RV contributions from the suppression of convective blueshift is roughly correlated with the depth of formation of photospheric spectral lines used to compute the RV time series. Meunier et al. (2017), used this relation to demonstrate a method for spectroscopic extraction of the suppression of convective blueshift in order to isolate RV contributions, including planetary RVs, that contribute equally to the timeseries for each spectral line. In this publication, we extract disk-integrated solar RVs from observations over a 2.5 year time span made with the solar telescope integrated with the HARPS-N spectrograph at the Telescopio Nazionale Galileo (La Palma, Canary Islands, Spain). We apply the methods outlined by Meunier et al. (2017) - as part of this analysis, we fit Gaussian line profiles to 765 iron lines measured over 457 exposures.</p> <p>Here, we provide the complete line list (Table 1; Table1_LineList.csv) used in our analysis, and the resulting RVs time series in their entirety (Table 3; Table3_TimeSeries.csv). Wavelengths are given in Angstroms, and RVs in m/s.</p> <p>We also include 4 CSV files with the line fit parameters of each line profile: Each row corresponds to a single exposure time (corresponding to the JDs in Table 3) and each column corresponds to a specific spectral line (with wavelength specified in Table 1).</p> <p>We fit each spectral line to a Gaussian of the form:</p> <p><span class="math-tex">\(f(\lambda) = p_1 - p_2 \exp \left[- {1 \over 2} \left({{\lambda - p_3} \over p_4}\right)^2 \right]\)</span></p> <p>p<sub>1</sub> is the continuum level in arbitrary units (LineProfiles_Continuum.csv)<br> p<sub>2</sub> is the line strength in arbitrary units (LineProfiles_Amplitude.csv)<br> p<sub>3</sub> is the line shift in Angstroms (LineProfiles_Shift.csv)<br> p<sub>4</sub> is the line width in Angstroms (LineProfiles_Width.csv)</p>
Reproduction package for the article "Spectroscopic Monitoring of the Candidate Tidal Disruption Event in F01004–2237"
<p>This is the reproduction package for the Article "Spectroscopic Monitoring of the Candidate Tidal Disruption Event in F01004-2237" by Cannizzaro et al (2021). It contains the reduced optical data and the scripts used for the emission lines fitting.</p>
Data from: Spectroscopic approach to correction and visualisation of bright-field light transmission microscopy biological data
<p>The most realistic information about the transparent sample such as a live cell can be obtained only using bright-field light microscopy. At high-intensity pulsing LED illumination, we captured a primary 12-bit-per-channel (bpc) response from an observed sample using a bright-field wide-field microscope equipped with a high-resolution (4872x3248) image sensor. In order to suppress data distortions originating from the light interactions with undesirable elements in the optical path, poor sensor reproduction (geometrical defects of the camera sensor and some peculiarities of sensor sensitivity), this uncompressed 12-bpc data underwent a kind of correction after simultaneous calibration of all the parts of the experimental arrangement. Moreover, the final intensities of the corrected images are proportional to the photon fluxes detected by a camera sensor. It can be visualized in 8-bpc intensity depth after the Least Information Loss compression [Lect. Notes Bioinform. 9656, 527 (2016)].</p>
Selection function for spectroscopic surveys (main set).
<p>Selection function values for large spectroscopic surveys. Supplementary material for A&A paper Minst&Hekker 2018 (https://ui.adsabs.harvard.edu/#abs/2018arXiv181012296M/abstract). Main set (all stars in each survey)</p>
Spectroscopic ellipsometry mapping of PAAO:DLC:Ag (AJ-8-03-31-DLCAg sample)
<p>Spectroscopic ellipsometry measurement data obtained from the porous anodized aluminum oxide (PAAO) covered with hydrogenated amorphous diamond-like carbon and silver (DLC:Ag) nanocomposite. The sample was made by 2 processes: (1) anodization of aluminum polycrystal in 0.3 mol/L oxalic acid at 40 V for 5 minutes and 4 seconds and then (2) depositing DLC:Ag employing reactive unbalanced magnetron sputtering in direct current mode using silver target (80 sccm argon gas flow, 5.4 sccm C<sub>2</sub>H<sub>2</sub> gas flow, 405 V voltage, 0.09-0.10 A current, 7·10<sup>-3</sup> mbar work pressure, 2 minutes 32 seconds process duration).</p> <p>The measurements were carried out at 20 × 20 locations covering all of the sample surface (approximately 4.8 × 4.8 mm<sup>2</sup>). The coordinates of each of 400 locations are available in "mapping_points.csv" file. All measurement data is also included in a single "AJ-8-03-31-DLCAg Ellipsometry Mapping Measurements.rar" file.</p> <p>Ellipsometer: rotating compensator GES5-E (Semilab).</p> <p>Light source: 75 W xenon short arc lamp with 185-2000 nm wavelength spectrum.</p> <p>Detector: UV-Vis CCD with 0.8 nm resolution.</p> <p>Spectral range: approximately 230-960 nm.</p> <p>Light incidence angles: 55°, 60°, 65°, 70°, 75°.</p> <p>Light beam size: microspot (365 × 470 μm<sup>2</sup> at 75° angle of incidence).</p> <p>The same sample was also measured using the same spectroscopic ellipsometry method before being covered with DLC:Ag. The data can be found here: <a href="https://doi.org/10.5281/zenodo.7056065">https://doi.org/10.5281/zenodo.7056065</a></p>
Spectroscopic ellipsometry mapping of PAAO:DLC:Ag (AJ-7-03-31-DLCAg sample)
<p>Spectroscopic ellipsometry measurement data obtained from the porous anodized aluminum oxide (PAAO) covered with hydrogenated amorphous diamond-like carbon and silver (DLC:Ag) nanocomposite. The sample was made by 2 processes: (1) anodization of aluminum polycrystal in 0.3 mol/L oxalic acid at 40 V for 4 minutes and 35 seconds and then (2) depositing DLC:Ag employing reactive unbalanced magnetron sputtering in direct current mode using silver target (80 sccm argon gas flow, 5.4 sccm C<sub>2</sub>H<sub>2</sub> gas flow, 405 V voltage, 0.09-0.10 A current, 7·10<sup>-3</sup> mbar work pressure, 2 minutes 32 seconds process duration).</p> <p>The measurements were carried out at 20 × 20 locations covering all of the sample surface (approximately 4.8 × 4.8 mm<sup>2</sup>). The coordinates of each of 400 locations are available in "mapping_points.csv" file. All measurement data is also included in a single "AJ-7-03-31-DLCAg Ellipsometry Mapping Measurements.rar" file.</p> <p>Ellipsometer: rotating compensator GES5-E (Semilab).</p> <p>Light source: 75 W xenon short arc lamp with 185-2000 nm wavelength spectrum.</p> <p>Detector: UV-Vis CCD with 0.8 nm resolution.</p> <p>Spectral range: approximately 230-960 nm.</p> <p>Light incidence angles: 55°, 60°, 65°, 70°, 75°.</p> <p>Light beam size: microspot (365 × 470 μm<sup>2</sup> at 75° angle of incidence).</p> <p>The same sample was also measured using the same spectroscopic ellipsometry method before being covered with DLC:Ag. The data can be found here: <a href="https://doi.org/10.5281/zenodo.7053393">https://doi.org/10.5281/zenodo.7053393</a></p>
Cool, Luminous, and Highly Variable Stars in the Magellanic Clouds. II: Spectroscopic Data of Thorne-Zytkow Object and Super-AGB Star Candidates
<p>This dataset contains Magellan MIKE spectroscopy of a population of cool, luminous stars in the Magellanic Clouds, a sample of confirmed Magellanic Cloud red supergiants, and spectrophotometric standard stars. The spectra were analyzed in the paper "Cool, Luminous, and Highly Variable Stars in the Magellanic Clouds. II: Spectroscopic and Environmental Analysis of Thorne-\.Zytkow Object and Super-AGB Star Candidates" by O'Grady et al. (2022). More details are provided in the README. </p>
JWST Advanced Deep Extragalactic Survey: Thumbnail Images of Spectroscopically-Confirmed Galaxies at z>10.
<p>JWST NIRCam FITS image thumbnails for the spectroscopically-confirmed high-redshift galaxy sample in Robertson et al., arXiv:2212.04480. The tar file expands into the following directories:</p> <p>JADES-GS-z10-0/</p> <p>JADES-GS-z11-0/</p> <p>JADES-GS-z12-0/</p> <p>JADES-GS-z13-0/</p> <p>Each directory contains the F090W, F115W, F150W, F200W, F277W, F335M, F356W, F410M, and F444W FITS images of the galaxies. The FITS headers contain information about the observations, the units of the data, and the locations of the objects on the sky.</p>
Speciation and Structures in Pt Surface Sites Stabilized by N-Heterocyclic Carbene Ligands Revealed by DNP Enhanced Indirect-ly Detected 195Pt NMR Spectroscopic Signatures and Fingerprint Analysis
<p>Raw NMR data for the paper published under DOI: 10.1021/jacs.2c08300</p>
Data and software: 'Survey Operations for the Dark Energy Spectroscopic Instrument'
<p>Supplementary material to the DESI publication "Survey Operations for the Dark Energy Spectroscopic Instrument".</p><p>The main "figures.py" script generates the figures in the paper from the included data files. The software relies on the DESI software stack available at github.com/desihub, and conveniently available at NERSC in the default DESI environment.</p><p>Some documentation on the code implementing the survey and for running the survey simulations is available here:</p><ul><li>https://desisurvey.readthedocs.io/en/latest/</li><li>https://surveysim.readthedocs.io/en/latest/</li></ul><p>Contents:</p><ul><li>Configuration files<ul><li>config-main-actual.yaml: a yaml file giving the configuration for the survey simulation software (https://github.com/desihub/surveysim/releases/tag/0.12.5), specifying things like interexposure times and downtime, using the actual long shutdowns we had.</li><li>config-main-nominal.yaml: a yaml file giving the configuration for the survey simulation software, using the nominal long shutdowns we planned for.</li><li>config-main.yaml: same as config-main-nominal.yaml, except with the default name looked for by the survey simulation software.</li><li>rules-main.yaml: configuration rules file controlling how the next tile selector selects files for observation, implementing our depth-first strategy.</li></ul></li><li>Software files<ul><li>figures.py: main routines for generating the plots in this publication. Running `python figures.py` will create all of the figures used in this paper.</li><li>precess.py: set of routines implementing the precession of the Earth's pole used by figures.py for accurate airmass calculations.</li><li>downtime.py: routines used by figures.py for computing statistics about DESI's time usage, in particular the downtime.</li><li>util_efs.py: utility routines, primarily for making plots used by figures.py</li><li>util_efs_c.pyx: cython routines used by util_efs.py</li><li>margincomputations.py: routines for computing survey margin; i.e., how well we did relative to how much time was available.</li></ul></li><li>Data files<ul><li>Survey<ul><li>exposures-daily-main-20220614.ecsv: list of main survey exposures taken through 2022-06-14, following processing by the offline pipeline.</li><li>exposures-20220614.ecsv: list of main survey exposures taken through 2022-06-14, before processing by the offline pipeline. This largely duplicates exposures-daily, but contains much less information and contains more records for rare cases when exposures cannot be processed by the offline pipeline.</li><li>tiles-4112-packing-20210405-decorated-fixed.fits: file giving the geometry of DESI tile centers on the sky, plus associated information, like the extinction and stellar density at those locations.</li><li>tiles-daily.csv</li></ul></li><li>Simulation<ul><li>ephem_2019-01-01_2027-12-31.fits: ephemerides for DESI site for 2019 through 2027, generated by the desisurvey software ephemerides module. https://github.com/desihub/desisurvey</li><li>desi-status-end-nominal.ecsv: tile file giving completion of each DESI tile, for a survey simulation using the nominal configuration file.</li><li>desi-status-end-actual-noslew.ecsv: tile file giving completion of each DESI tile, for a survey simulation using the actual configuration file, without slew optimization</li><li>desi-status-end-actual.ecsv: tile file giving the completion of each DESI tile, for a survey simulation using the actual configuration file.</li><li>exposures_actual-noslew.fits: exposures generated by survey simulation software using the 'actual' configuration, with slew optimization disabled.</li><li>exposures_actual.fits: exposures file generated by survey simulation software using the 'actual' configuration.</li><li>exposures_nominal.fits: exposures file generated by survey simulation software using the 'nominal' configuration.</li><li>stats_actual.fits: statistics file generated by survey simulation software using the 'actual' configuration, containing information about DESI time usage.</li><li>stats_actual-noslew.fits: same as stats_actual.fits, except with slew time optimization disabled.</li><li>stats_nominal.fits: same as stats_actual.fits, except with the nominal survey sim configuration file.</li><li>tiles-daily.csv: tile file with detailed information on all tiles completed by the survey</li><li>tiles-main-20220614.ecsv: tile file with tile completeness information on 20220614</li><li>tiles-main.ecsv: tile file with completeness information on tiles in the survey</li><li>performance_current.csv.gz: performance information detailing state of DESI instrument every second, used for tracking downtime statistics.</li></ul></li></ul></li></ul><p>Dependencies: The included software uses the 'surveysim,' 'desisurvey,' and 'desimodel' packages, available on github through the desihub organization. Otherwise it depends on the usual astronomy software stack: numpy scipy matplotlib astropy. Alternatively, people with access to NERSC can load the default DESI environment and pull in all needed dependencies.</p>
A Spectroscopic Study of Mars-Analog Materials with Amorphous Sulfate and Chloride Phases: Implications for Detecting Amorphous Materials on the Martian Surface
<p>This repository contains the raw and baseline or continuum corrected data associated with the manuscript entitled:</p> <p> A Spectroscopic Study of Mars-Analog Materials with Amorphous Sulfate and Chloride Phases: Implications for Detecting Amorphous Materials on the Martian Surface</p> <p>This work is being submitted to The Planetary Science Journal</p> <p>ABSTRACT</p> <p>The Chemistry and Mineralogy X-ray diffraction (XRD) instrument aboard the Curiosity rover has consistently identified substantial amorphous material at Gale Crater. The amorphous component is compositionally variable, but often includes elevated sulfur and iron, suggesting that amorphous ferric sulfate (AFS) may be present. Understanding the spectral changes of common Martian materials exposed to ferric sulfate brines as they desiccate to AFS is a key step in bridging the gap between simple mixing studies and analyses of complex/realistic reaction assemblages. Visible and near-infrared reflectance (VNIR), mid-infrared attenuated total reflectance (MIR, FTIR-ATR), and Raman spectra, along with XRD data are presented for basaltic glass, hematite, gypsum, nontronite, and magnesite, each at three grain sizes (<25, 25-63, and 63-180 μm), mixed with ferric sulfate alone or also with NaCl, hydrated through deliquescence, and then rapidly desiccated in 11% relative humidity or via vacuum. All desiccated products are partially or completely XRD amorphous; crystalline phases include starting materials and trace precipitates, leaving the bulk of the ferric sulfate in the amorphous fraction. Due to considerable spectral masking, the detectability of AFS is highly dependent on spectroscopic technique and the observed mineral assemblage. This has strong implications for remote and in-situ observations of Martian samples which include an amorphous component. AFS is only identifiable in VNIR spectra for magnesite, nontronite, and gypsum samples; hematite and basaltic glass samples appear similar to pure materials. Sulfate features dominate Raman spectra for nontronite and basaltic glass samples; the analog material dominates Raman spectra of hematite and gypsum samples. MIR spectra reveal all end members most clearly except for basaltic glass samples, where the analog material is almost completely masked. NaCl leads to similar FTIR-ATR and Raman features, regardless of analog material.</p> <p>Associated photographs of samples in this project can be found at:</p> <p>https://www.lionsandlamms.com/</p> <p>This research was supported by NSF award #1819209.</p>
Data for AJ paper: Mass ratio of single-line spectroscopic binaries with visual orbits using Bayesian inference and suitable priors
<p>Data and plots for paper "Mass ratio of single-line spectroscopic binaries with visual orbits using Bayesian inference and suitable priors" accepted for publication in The Astronomical Journal.</p>
Phtometry measurements using spectroscopic ellipsometer of PAAO containing samples in air and water (AoI 45 deg., 60 deg., varying polarizer and analyser angles)
<p>The file contains raw intensity data measured in reflection mode for various material combinations: porous anodized aluminium oxide (PAAO), gold nanoparticles (Au NPs), diamond-like carbon with silver nanoparticles composite (DLC:Ag), quartz, and silicon.</p> <p>List of investigated samples:</p> <table> <thead> <tr> <th scope="col">Sample name</th> <th scope="col">Sample description</th> </tr> </thead> <tbody> <tr> <td>AJ1</td> <td>Aluminium substrate, ~241 nm thickness PAAO (anodized in 0.3 mol/L oxalic acid at 40 V for 3 min 16 s), 60 nm diameter Au NPs (dip-coated at a speed of 1 μm/s)</td> </tr> <tr> <td>AJ2</td> <td>Aluminium substrate, ~259 nm thickness PAAO (anodized in 0.3 mol/L oxalic acid at 40 V for 3 min 37 s), 60 nm diameter Au NPs (dip-coated at a speed of 1 μm/s)</td> </tr> <tr> <td>AJ3</td> <td>Aluminium substrate, ~293 nm thickness PAAO (anodized in 0.3 mol/L oxalic acid at 40 V for 4 min 8 s), 60 nm diameter Au NPs (dip-coated at a speed of 1 μm/s)</td> </tr> <tr> <td>AJ4</td> <td>Aluminium substrate, ~317 nm thickness PAAO (anodized in 0.3 mol/L oxalic acid at 40 V for 4 min 30 s), 60 nm diameter Au NPs (dip-coated at a speed of 1 μm/s)</td> </tr> <tr> <td>AJ5</td> <td>Aluminium substrate, ~345 nm thickness PAAO (anodized in 0.3 mol/L oxalic acid at 40 V for 4 min 57 s), 60 nm diameter Au NPs (dip-coated at a speed of 1 μm/s)</td> </tr> <tr> <td>AJ6</td> <td>Aluminium substrate, ~276 nm thickness PAAO (anodized in 0.3 mol/L oxalic acid at 40 V for 3 min 42 s), ~55 nm thickness, 20 V.% Ag concentration DLC:Ag (magnetron sputtered using silver target, 80 sccm argon gas flow, 5.4 sccm C<sub>2</sub>H<sub>2</sub> gas flow, 405 V voltage, 0.09-0.10 A current, 7·10<sup>-3</sup> mbar work pressure, 2 minutes 32 seconds process duration)</td> </tr> <tr> <td>AJ7</td> <td>Aluminium substrate, ~316 nm thickness PAAO (anodized in 0.3 mol/L oxalic acid at 40 V for 4 min 25 s), ~55 nm thickness, 20 V.% Ag concentration DLC:Ag (magnetron sputtered using silver target, 80 sccm argon gas flow, 5.4 sccm C<sub>2</sub>H<sub>2</sub> gas flow, 405 V voltage, 0.09-0.10 A current, 7·10<sup>-3</sup> mbar work pressure, 2 minutes 32 seconds process duration)</td> </tr> <tr> <td>AJ8</td> <td>Aluminium substrate, ~345 nm thickness PAAO (anodized in 0.3 mol/L oxalic acid at 40 V for 5 min 4 s), ~55 nm thickness, 20 V.% Ag concentration DLC:Ag (magnetron sputtered using silver target, 80 sccm argon gas flow, 5.4 sccm C<sub>2</sub>H<sub>2</sub> gas flow, 405 V voltage, 0.09-0.10 A current, 7·10<sup>-3</sup> mbar work pressure, 2 minutes 32 seconds process duration)</td> </tr> <tr> <td>Q140</td> <td>Quartz substrate, ~55 nm thickness, 20 V.% Ag concentration DLC:Ag (magnetron sputtered using silver target, 80 sccm argon gas flow, 5.4 sccm C<sub>2</sub>H<sub>2</sub> gas flow, 405 V voltage, 0.09-0.10 A current, 7·10<sup>-3</sup> mbar work pressure, 2 minutes 32 seconds process duration)</td> </tr> <tr> <td>Si140</td> <td>Silicon substrate, ~55 nm thickness, 20 V.% Ag concentration DLC:Ag (magnetron sputtered using silver target, 80 sccm argon gas flow, 5.4 sccm C<sub>2</sub>H<sub>2</sub> gas flow, 405 V voltage, 0.09-0.10 A current, 7·10<sup>-3</sup> mbar work pressure, 2 minutes 32 seconds process duration)</td> </tr> </tbody> </table> <p>Ellipsometer: rotating compensator GES5-E (Semilab).</p> <p>Light source: 75 W xenon short arc lamp with 185-2000 nm wavelength spectrum.</p> <p>Detector: UV-Vis CCD with 0.8 nm resolution.</p> <p>Spectral range: approximately 230-960 nm.</p> <p>Mode: photometry.</p> <p>Light incidence angles: 45°, 60°.</p> <p>Polarizer angles: 0°, 90°.</p> <p>Analyzer angles: 0°, 45°, 90°.</p> <p>Light beam size: microspot (365 × 470 μm<sup>2</sup> at 75° angle of incidence).</p> <p>The reference was measured from aluminum mirror provided with the ellipsometer for each variation of measurement set-up.</p> <p>Each sample was first measured in air and then after immersion in water. Focusing was performed before each measurement.</p> <p>.smdx and .mup files are generated by the ellipsometer and can be opened using Semilab software. Their file names contain sample name, polarizer angle (Pol), analyzer angle (Ana), incidence angle (ang), and surrounding medium (air/water). .csv files are exported data related to each sample. .jpg files are for illustrative purposes to show the spectra. .rar file contains all the files in this upload.</p> <p> </p>
Data from: Spectroscopic approach to correction and visualisation of bright-field light transmission microscopy biological data
Open the record for dataset details and reuse information.
All Luminosity Templates Associated with "Classifying Single Stars and Spectroscopic Binaries Using Optical Stellar Templates"
<p>Zip files for the luminosity normalized individual stellar templates, and all combinations of SB2 templates. The templates are in fits format. The first table extension contains the template (wavelength, luminosity, variance, error). These luminosity templates have units of erg /s /angstrom.</p>
Spectroscopic and XRD data from PHS
<p>Visible and Near infrared as well as Mid infrared spectroscopic data from PHS deposit along with their XRD analysis. </p>
Spectroscopic data set for an unusual white dwarf
<p>The tar file includes fits-formatted count (d*) and flux (ca*) spectra of an unusual white dwarf obtained at the MDM observatory. The spectra are wavelength calibrated. Users should exercise caution when quoting absolute flux. Heliocentric velocity corrections are not applied. The count spectra list the wavelength (angstrom) and the total count, and the flux spectra list the wavelength (angstrom) and the flux in units of erg/cm^2/s/angstrom.</p>
Data for figures and tables in: "Validation of the Scientific Program for the Dark Energy Spectroscopic Instrument"
<p>Supplementary material to DESI's publication 'Validation of the Scientific Program for the Dark Energy Spectroscopic Instrument' to comply with the data management plan.</p>
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DANDI Archive for NWB datasets
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International Brain Laboratory public data
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OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.