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235 results for “spectroscopic”
The Spitzer Spectroscopic Data Fusion - Merged Spectroscopic Redshift Catalogs in Spitzer Fields
<p>The Spitzer Spectroscopic Data Fusion merges miscellaneous spectroscopic information available within "popular" extragalactic survey fields.</p> <p>Last Updated on 20 March 2025 - <a href="https://zenodo.org/record/6368347">https://zenodo.org/record/6368347</a> - <a href="https://www.mattiavaccari.net/df/specz">https://www.mattiavaccari.net/df/specz</a></p> <p>Based on the Spitzer Data Fusion Project - <a href="https://doi.org/10.5281/zenodo.7850783">https://doi.org/10.5281/zenodo.7850783</a> - <a href="https://mattiavaccari.net/df">https://mattiavaccari.net/df</a></p> <p>Merged Spec-Z ("specz-merged") catalogs merge miscellaneous spec-z information available within a given field. Different spec-z catalogs available within a given field are merged (using a search radius of 1.0 arcsec), and for sources with multiple spec-z measurements the most reliable one is chosen following the (largely arbitrarily) assumed order of decreasing reliability indicated below for each field. If CAT1,...,CATN spec-z catalogs are available in a given field, Z_1 from CAT1 (i.e. NED) is adopted as "best" redshift (i.e. ZBEST), if available, otherwise Z_2 from CAT_2 is adopted if available, and so on up to Z_N and CAT_N. In using ZBEST it's thus important to bear in mind that this is not necessarily actually the "best" redshift for science purposes, and in particular that the choice of NED as CAT1 is often not ideal. However, Z_1,...,Z_N are included to allow users to define the "best" redshift based on their science needs when multiple redshift estimates are available for a given source. ZFLAG specifies which catalog is providing the ZBEST value according to the CATN number below. ZCLASS is meant to provide further info about the class/quality of the spectroscopic redshift measurement, but for the time being is not populated and is simply a copy of ZFLAG. ZWHERE is an additional binary/bit flag indicating in which of the N catalogs each source was given a spec-z estimate in. ZWHERE will e.g. be 2^0=1 if a redshift if available <em>only</em> from CAT_1, whereas it will be 2^0+2^1=3 if a redshift is available *only* from CAT1 and CAT2,<br>so that a source with a redshift available from all catalogues will have ZWHERE=2^0+...+2^n.</p> <p>See AAAREADME.SPECZ-MERGED within the ZIP archive for further information.</p>
Supplementary material for the paper "DS Andromedae, A Detached Eclipsing Double-Lined Spectroscopic Binary in the Galactic Cluster NGC 752
<p>Supplementary material supporting the paper "DS Andromedae: A Detached Eclipsing Double-Lined Spectroscopic</p> <p>Binary in the Galactic Cluster NGC 752" by E. F. Milone, S. J. Schiller, Th. Mellergaard Amby, and S. Frandsen.</p> <p>It includes:</p> <p>A Read-me file in three formats (docx, rtf, pdf); Unabridged Section 3 with extended modeling details (pdf);</p> <p>Extended spreadsheet version of Table 3 of adjusted parameters (pdf); Extended spreadsheet version of Table 8 of absolute</p> <p>parameters (pdf); and Complete Table 15 of photometric data (txt): and a sample DC input file (for Model 41, used in the</p> <p>DS And modeling) in dat format.</p>
DEIMOS Spectroscopic observations of MS0451-03
<p>The tar file contains extracted spectroscopic observations of galaxies in the field of MS 0451-03 galaxy cluster. The observations were obtained with the DEIMOS instrument on the Keck Observatory. Details of the observations are given in Crawford et al., 2011, ApJ, 741, 98, <a href="https://ui.adsabs.harvard.edu/link_gateway/2011ApJ...741...98C/doi:10.1088/0004-637X/741/2/98">DOI: 10.1088/0004-637X/741/2/98</a>. The catalogs associated with that paper also have further information about these objects.</p> <p>The following files are included:</p> <p>1. w05.m*-crawford.fits: A catalog for each of the masks. This catalog includes the information about the object in each slit as well as the measurement of the redshift. The</p> <p>2. iraf.w05.m*.*.*.fits. These are 1-D extracted files in an iraf compatible format. The names of the files correspond to the mask, slit, and original id in the catalog used for selection. Unfortunately, due to an bug in the original extraction software, the primary target appears usually appears in the file named serendip1 and not the file with the object id.</p>
Catalogue of Bayesian SZNet's spectroscopic redshift predictions
<p>The "dr16q_superset_redshift.csv" file provides a catalogue of spectroscopic redshift predictions for spectra from the <a href="https://www.sdss.org/dr16/algorithms/qso_catalog/">16th data release of the Sloan Digital Sky Survey (SDSS) quasar superset catalogue</a> <a href="https://ui.adsabs.harvard.edu/abs/2020ApJS..250....8L/abstract">(Lyke et al., 2020)</a>. Redshifts are predicted by a Bayesian convolutional neural network named Bayesian SZNet with associated predictive uncertainties in the form of predictive variances. The catalogue is released in the CSV format with the following columns:</p> <ul> <li><em>plate</em>: spectroscopic plate number;</li> <li><em>mjd</em>: modified Julian day of the spectroscopic observation;</li> <li><em>fiberid</em>: fiber identification number;</li> <li><em>z_pred</em>: redshift from Bayesian SZNet;</li> <li><em>variance</em>: predictive variance associated with redshift from Bayesian SZNet;</li> <li><em>z</em>: primary redshift;</li> <li><em>source</em><em>_z</em>: origin of the reported redshift in <em>z;</em></li> <li><em>is_qso_final</em>: flag indicating quasars included in the DR16Q <a href="https://ui.adsabs.harvard.edu/abs/2020ApJS..250....8L/abstract">(Lyke et al., 2020)</a>;</li> <li><em>z_vi</em>: redshift from visual inspection;</li> <li><em>z_pipe</em>: redshift from the SDSS pipeline;</li> <li><em>zwarning</em>: quality flag on the redshift from the SDSS pipeline;</li> <li><em>z_dr12q</em>: redshift from the DR12Q catalogue <a href="http://ui.adsabs.harvard.edu/abs/2017A%26A...597A..79P/abstract">(Pâris et al., 2017)</a>;</li> <li><em>z_dr7q_sch</em>: redshift from the DR7Q catalogue <a href="https://ui.adsabs.harvard.edu/abs/2010AJ....139.2360S/abstract">(Schneider et al., 2010)</a>;</li> <li><em>z_dr6q_hw</em>: redshift from the DR6 catalogue <a href="https://ui.adsabs.harvard.edu/abs/2010MNRAS.405.2302H/abstract">(Hewett and Wild, 2010)</a>;</li> <li><em>z_10k</em>: redshift from the random visual inspection of 10000 spectra in the DR16Q superset;</li> <li><em>z_pca</em>: redshift from the <a href="https://ascl.net/2106.017">redvsblue algorithm</a>;</li> <li><em>z_qn</em>: redshift from QuasarNET <a href="https://arxiv.org/abs/1808.09955">(Busca and Balland, 2018)</a>;</li> <li><em>z_pred_1</em> to <em>z_pred_256</em>: sampled redshifts from Bayesian SZNet;</li> </ul> <p>where columns <em>z</em>, <em>source_z</em>, <em>is_qso_final</em>, <em>z_vi</em>, <em>z_pipe</em>, <em>zwarning</em>, <em>z_dr12q</em>, <em>z_dr7q_sch</em>, <em>z_dr6q_hw</em>, <em>z_10k</em>, <em>z_pca</em>, and <em>z_qn</em> are taken from the 16th data release of the SDSS quasar superset catalogue.</p>
Reproduction package for the paper "Exploring the directly imaged HD 1160 system through spectroscopic characterization and high-cadence variability monitoring"
<p>This is a basic reproduction package for the paper <a href="https://doi.org/10.1093/mnras/stae1315">"Exploring the directly imaged HD 1160 system through spectroscopic characterization and high-cadence variability monitoring" by Sutlieff et al. (2024)</a>. It aims to provide the most important data products to check and reproduce the main results of the paper.</p>
Supplementary Material for "A comparative high-resolution spectroscopic analysis of in situ and accreted globular clusters"
<p>This is a file containing supplementary material for the paper <em>A comparative high-resolution spectroscopic analysis of in situ and accreted globular clusters.</em> For each star in target globular clusters, it lists crucial information on the linelist analyzed. In particular:</p> <ol> <li>Star ID.</li> <li>Chemical element.</li> <li>Wavelength.</li> <li>log <em>gf</em></li> <li>Excitation potential.</li> <li>Measured equivalent width with uncertaintiy.</li> </ol>
Electrochemical and Spectroscopic Data supported by Computational Models for Exploring the Metal- and Ligand-Based Oxidation of Mackinawite Nanoparticles
<p>Supporting information to our study, where under anaerobic conditions, ferrous iron reacts with sulfide producing FeS precipitate, which can then undergo a temperature, redox potential, and pH dependent maturation process resulting in the formation of oxidized mineral phases such as gregite or pyrite. The dataset provide information about the chemical speciation of iron-sulfide by cyclic voltammetry, Raman and X-ray absorption spectroscopic techniques. Nanoparticulate FeS was found to get oxidized to a Fe<sup>3+</sup> containing FeS phase at -0.5 V vs. Ag/AgCl (pH = 7) and in a concomitant oxidation step, polysulfides are proposed to give a material described as Fe<sup>2+</sup><sub>(1−3x)</sub>Fe<sup>3+</sup><sub>(2x)</sub>S<sup>2-</sup><sub>(1-y)</sub>(S<sub>n</sub><sup>2-</sup>)<sub>y</sub>. The thermodynamic differences between ligand- and metal-based oxidation processes from density functional theory can be used to describe one- and two-electron electronic and structural transformations. These findings together point to the existence of a previously unknown, metastable FeS phase located between FeS and greigite (Fe<sup>2+</sup>Fe<sup>3+</sup><sub>2</sub>S<sup>2-</sup><sub>4</sub>) along a metal oxidation path, and Fe<sup>2+</sup>S<sup>2-</sup> and pyrite (Fe<sup>2+</sup>S<sub>2</sub><sup>2-</sup>) along a ligand oxidation path, respectively.</p>
HETDEX Public Source Catalog 1: 220 K Sources including over 50K Lyman Alpha Emitters From an Untargeted Wide-area Spectroscopic Survey
<p>We present the first publicly released catalog of sources obtained from the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX). HETDEX is an integral field spectroscopic survey designed to measure the Hubble expansion parameter and angular diameter distance at 1.88 < z < 3.52 by using the spatial distribution of more than a million Lyα-emitting galaxies over a total target area of 540 deg2. The catalog comes from contiguous fiber spectra coverage of 25 deg2 of sky from January 2017 through June 2020, where object detection is performed through two complementary detection methods: one designed to search for line emission and the other a search for continuum emission. The HETDEX public release catalog is dominated by emission-line galaxies and includes 51,863 Lyα-emitting galaxy (LAE) identifications and 123,891 [O II]-emitting galaxies at z < 0.5. Also included in the catalog are 37,916 stars, 5,274 low-redshift (z < 0.5) galaxies without emission lines, and 4,976 active galactic nuclei. The catalog provides sky coordinates, redshifts, line identifications, classification information, line fluxes, [O II] and Lyα line luminosities where applicable, and spectra for all identified sources processed by the HETDEX detection pipeline. Extensive testing demonstrates that HETDEX redshifts agree to within ∆z < 0.02, 96.1% of the time to those in external spectroscopic catalogs. We measure the photometric counterpart fraction in deep ancillary Hyper Suprime-Cam imaging and find that only 55.5% of the LAE sample has an r-band continuum counterpart down to a limiting magnitude of r ∼ 26.2 mag (AB) indicating that an LAE search of similar sensitivity with photometric pre-selection would miss nearly half of the HETDEX LAE catalog sample.<br> <br> Two catalogs make up HETDEX Source Catalog 1:<br> <br> 1. The Source Observation Table: hetdex_sc1_vX.dat/.fits/.ecsv<br> With SPECTRA arrays included: hetdex_sc1_spec_vX.fits<br> <br> One row per source observation. The table provides basic coordinates/redshift/source information for each observation of a unique astornomical source. The larger file hetdex_sc1_spec_vX.fits contains the same info from the first table plus addition data units of spectral array data.<br> <br> 2. The Detection Information Table: hetdex_sc1_detinfo_vX.fits<br> One row per line or continuum detection. Bright sources can be comprised of multiple line or continuum emission. This catalog provides specific detection information such as line parameter info (S/N, line flux, line width)<br> <br> 3. Jupyter Notebook with access example: HETDEX_source_catalog_1.ipynb/.pdf/.html</p> <p>We request that the following acknowledgement be included in any paper using data or software from HETDEX public data releases:</p> <blockquote> <p>HETDEX is led by the University of Texas at Austin McDonald Observatory and Department of Astronomy with participation from the Ludwig-Maximilians-Universität München, Max-Planck-Institut für Extraterrestrische Physik (MPE), Leibniz-Institut für Astrophysik Potsdam (AIP), Texas A&M University, Pennsylvania State University, Institut für Astrophysik Göttingen, The University of Oxford, Max-Planck-Institut für Astrophysik (MPA), The University of Tokyo and Missouri University of Science and Technology.</p> <p>Observations for HETDEX were obtained with the Hobby-Eberly Telescope (HET), which is a joint project of the University of Texas at Austin, the Pennsylvania State University, Ludwig-Maximilians-Universität München, and Georg-August-Universität Göttingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. The Visible Integral-field Replicable Unit Spectrograph (VIRUS) was used for HETDEX observations. VIRUS is a joint project of the University of Texas at Austin, Leibniz-Institut für Astrophysik Potsdam (AIP), Texas A&M University, Max-Planck-Institut fürExtraterrestrische Physik (MPE), Ludwig-Maximilians-Universität München, Pennsylvania State University, Institut für Astrophysik Göttingen, University of Oxford, and the Max-Planck-Institut fur Astrophysik (MPA).</p> <p>Funding for HETDEX has been provided by the partner institutions, the National Science Foundation, the State of Texas, the US Air Force, and by generous support from private individuals and foundations.</p> </blockquote> <p> </p>
Dataset for A Novel Spectroscopic Approach for Vaseline Quality Discrimination
<p>This dataset contains spectroscopic measurement data and Orange project files used in the INDIN 2023 paper "A Novel Spectroscopic Approach for Vaseline Quality Discrimination".<br> <br> The paper only discusses the analysis using 2 principal components.</p>
Gemini/TEXES Spectroscopic Observations of Jupiter (March 12-14 2017)
<p>This dataset contains Gemini/TEXES spectroscopic maps of Jupiter, acquired between March 12-14 2017 in support of NASA's Juno mission. The data and its reduction/analysis is fully described in <em>Fletcher et al. (2020), Jupiter's Equatorial Plumes and Hot Spots: Spectral Mapping from Gemini/TEXES and Juno/MWR, Journal of Geophysical Research - Planets.</em></p> <p>As described in that paper, TEXES scan maps were acquired in seven groups (three on March 12, three on March 13, and one on March 14), with each group containing scan maps at 9 spectral settings (539, 587, 745, 819, 900, 960, 1165, 1248 and 2145 cm-1). Each setting spans approximately 10-20 cm-1, with variable spectral resolution as described in the article. </p> <p>Each scan map has been geometrically registered (i.e., latitudes, longitudes, and emission angles have been assigned), wavelength calibrated, and destriped. Radiometric calibration is in its raw form, based on TEXES observations of the telluric sky emission and a blank card in the instrument. However, we found it necessary to scale these spectra to match observations from Cassini/CIRS, using the following scale factors for all spectra:</p> <ul> <li>fac538= 0.9</li> <li>fac587= 0.687705</li> <li>fac744= 0.872656</li> <li>fac819= 0.600016</li> <li>fac901= 0.544984</li> <li>fac960= 0.427803</li> <li>fac1161=0.636066</li> <li>fac1248=1.0</li> <li>fac2145=1.0</li> </ul> <p>The format of the individual files (IDL "save" files) is as follows:</p> <ul> <li>EMMIMG FLOAT = Array[721, 361] - emission angles for each point in the map</li> <li>HDR STRING = Array[126] - header containing information about each observation</li> <li>IMAGE_REDUCT FLOAT = Array[149, 183] - summed image of Jupiter from all points in a spectral scan.</li> <li>IMG FLOAT = Array[374, 721, 361] - cylindrically mapped Jupiter data at 374 wavenumber positions.</li> <li>OLAT FLOAT = Array[361] - planetographic latitudes</li> <li>OLON FLOAT = Array[721] - System III West longitudes.</li> <li>SKY FLOAT = Array[374] - sky emission on the wavenumber grid.</li> <li>SUBLAT FLOAT - sub-observer latitude</li> <li>SUBLON FLOAT - sub-observer longitude</li> <li>TRUESKY FLOAT = Array[374] - sky emission on the wavenumber grid.</li> <li>WAVENUMBER DOUBLE = Array[374] - wavenumber array</li> </ul>
A small dataset for analyzing spectroscopic parameters from low-cost electronic structure methods
<p>This dataset comprises two files: `lee_bayesian_dataset.csv` and `raw_outputs.tar.xz`. The former corresponds to an aggregated table of data used for subsequent analysis, and the latter are raw output files from Gaussian '09. This dataset corresponds to 6916 calculations of 76 representative molecules with high-resolution gas-phase rotational constants.</p> <p> </p> <p>This version corresponds to the data used for our publication:</p> <p>Bayesian Analysis of Theoretical Rotational Constants from Low-Cost Electronic Structure Methods</p> <p>https://pubs.acs.org/doi/10.1021/acs.jpca.9b09982</p>
Raman spectroscopic data derived from Calluna vulgaris charcoals, experimentally generated across a range of natural wildfire temperatures
<p>This data has been derived from deconvolved Raman spectra, utilising two first order bands - D (Disordered) and G (Graphitic). Spectra were collected from experimentally pyrolysed charcoals, made from Calluna vulgaris (Ling Heather) separated into three main components; stem, root and flower. For each component at 250, 400, 600 and 800 degrees centigrade respectively, 5 charcoal samples (A, B, C, D, E) were analysed. Following deconvolution, median values for each spectra were produced. These correspond to parameters derived from the Raman data, including D- and G-band width (FWHM), intensity (ID/IG or 'R1') and area (AD/AG) ratios, band separation (G-D or 'RBS'), and band width ratios (D-FWHM/G-FWHM). All parameters have been compiled for each component material, and displayed graphically within this dataset.</p>
Data for article: Time-Resolved Spectroscopic Investigation of Charge Trapping in Carbon Nitrides Photocatalysts for Hydrogen Generation
<p>This is the data presented in the article titled 'Time-Resolved Spectroscopic Investigation of Charge Trapping in Carbon Nitrides Photocatalysts for Hydrogen Generation', published in the Journal of the American Chemical Society. DOI:10.1021/jacs.7b01547</p> <p>http://pubs.acs.org/doi/abs/10.1021/jacs.7b01547</p> <p> </p>
PdZn/ZrO2+SAPO-34 bifunctional catalyst for CO2 conversion: Further insights by spectroscopic characterization
<p>Supplementary material: atomic concentrations calculated from XPS, XPS spectra</p>
Processing, Spectroscopic and Laboratory Testing Data from a Medical Grade Hot-Melt Extrusion Process
<p>This dataset contains a collection of raw processing data, spectroscopic data, and laboratory test results of medical-grade polymer extrusion experiments. The data was collected in several experiments conducted in a hot-melt extrusion process. The process involved extruding PLA through a slit die and drawing the extruded strands onto spools to obtain the desired dimensional and mechanical properties. The strands were later knitted to form the final medical implant. Throughout the experiments, the extrusion process and equipment were upgraded and refined. Various operational scenarios were simulated under different nozzle configurations. The experiments start using a single-screw extruder and later progress to a double-screw extruder. Medical Grade PURASORB PLA (PLDLA 96/4) material was used when the hardware upgrades were complete. This dataset contains many variations in experimental conditions. However, enough overlap exists to derive working datasets from this compiled raw data.</p> <p> </p> <p>Two working datasets have been derived from this compiled raw data. Using a double-screw extruder, both working Datasets investigate polymer degradation in the hot-melt extrusion process. Both derived datasets are included in this collection.</p> <p> </p> <p>Two Jupyter notebooks are included in this data collection. The first notebook gives an example of how an initial dataset can be derived from the raw data using data science techniques. The second notebook gives an example of how a final dataset can be created from the initial dataset.</p>
Asteroseismology of the young open cluster NGC 2516 I: Photometric and spectroscopic observations
<p>A column-to-column explaination is here:</p> <p>gaia_dr3_source_id: Gaia DR3 source ID</p> <p>TIC: TIC number</p> <p>gaia_RA: RA by Gaia</p> <p>gaia_DEC: DEC by Gaia</p> <p>gaia_G_apparent_mag: Gaia G band magnitude</p> <p>gaia_G_apparent_mag_err: Gaia G band magnitude uncertainty</p> <p>gaia_G_absolute_mag: Gaia G band absolute magnitude, without the correction of extinction</p> <p>gaia_G_absolute_mag_err: uncertainty of gaia_G_absolute_mag</p> <p>log_Luminosity: log of luminosity, calculated by Gaia effective temperature, with the bolometric correction and extinction correction. Use with caution.</p> <p>log_Luminosity_err: uncertainty of log_Luminosity</p> <p>Gaia_Teff: effective temperature provided by Gaia. Use with caution.</p> <p>Gaia_Teff_err: uncertainty of Gaia_Teff. Use with caution. A uncertainty value of '100' means the temperature is absent by Gaia, so we use the temperature from the TIC input catalog.</p> <p>BP-RP: Gaia colour index.</p> <p>BP-RP_err: uncertainty of BP-RP</p> <p>Teff_by_spectra: effective temperature by FEROS spectra, better than Gaia_Teff, only available for nine stars. "9999" means no data available.</p> <p>Teff_by_spectra_err: uncertainty of Teff_by_spectra. "9999" means no data available.</p> <p>log_L_by_Teff_spectra: log of luminosity calculated by Teff_by_spectra, with the bolometric correction and extinction correction, better than log_Luminosity.</p> <p>log_L_by_Teff_spectra_err: uncertainty of log_L_by_Teff_spectra</p> <p>spectra_logg: log g by FEROS spectra, only available for nine stars. "9999" means no data available.</p> <p>spectra_logg_err: uncertainty of spectra_logg</p> <p>spectra_vsini: projected equatorial velocity by FEROS spectra, only available for nine stars. "9999" means no data available.</p> <p>spectra_vsini_err: uncertainty of spectra_vsini</p> <p>spectra_matellicity: matellicity by FEROS spectra, only available for nine stars. "9999" means no data available.</p> <p>spectra_matellicity_err: uncertainty of spectra_matellicity</p> <p>spectra_radial_velocity: radial velocity by FEROS spectra, only available for nine stars. "9999" means no data available.</p> <p>spectra_radial_velocity_err: uncertainty of spectra_radial_velocity</p> <p>spectra_microturbulent: microturbulent velocity by FEROS spectra, only available for nine stars. "9999" means no data available.</p> <p>spectra_microturbulent_err: uncertainty of spectra_microturbulent</p> <p>spectra_SNR: signal-to-noise ratio of the FEROS spectra</p> <p>Pi0: asymptotic spacing of g modes, measured by g modes, only available for 11 stars. '9999' means no data available.</p> <p>Pi0_err: uncertainty of Pi0</p> <p>core_rotation_g_mode: near-core rotation rate in unit of days^{-1}, measured by g modes, only available for 11 stars. '9999' means no data available.</p> <p>surface_modulation_period: surface rotation period measured by surface modulations. '9999' means no data available.</p> <p>surface_modulation_period_err: uncertainty of surface_modulation_period</p> <p> </p>
Overcoming the Probing-Depth Dilemma in Spectroscopic Analyses of Batteries with Muon-Induced X-ray Emission (MIXE)
<p>Datasets used in the publication "Overcoming the Probing-Depth Dilemma in Spectroscopic Analyses of Batteries with Muon-Induced X-ray Emission (MIXE)".</p> <p>fig_2: MIXE spectra of (a) an empty laminated Al pouch, (b) a Li metal foil in a laminated Al pouch, (c) a NMC622 electrode in a laminated Al pouch</p> <p>fig_3: MIXE spectrum of a NMC811 electrode in a laminated Al pouch, measured at 23.8 MeV/c</p> <p>fig_4b: Muon stopping profile simulated using PHITS for the cell geometry depicted in Figure 4a of the main manuscript</p> <p>fig_4c: Depth-resolved MIXE spectra of a NMC811||graphite Li-ion battery. Raw data at the 11 momenta measured, and table with the integrated peak areas for selected (K-L) lines.</p> <p><strong><em>Update in version 2: raw datasets now have one energy column for each momentum. The datasets are of different lengths for each momentum and there was and error in copying the data in version 1. </em></strong></p> <p> </p> <p>fig_4c: Table with calculated elemental ratios of the different transition metals (Ni, Mn and Co), at the momenta corresponding to implantation in the NMC811 electrode</p> <p>fig_s2: MIXE spectrum of a NMC622 electrode in a laminated Al pouch, measured at 23.0 MeV/c</p> <p>fig_s3: MIXE spectrum of a NMC111 electrode in a laminated Al pouch, measured at 22.8 MeV/c</p> <p>fig_s4_s5_simulations: Raw data of the muon implantation simulations for the NMC811/graphite cell </p> <p><strong><em>Update in version 2: added fig_s4_s5_simulations file</em></strong></p> <p> </p> <p>fig_s6: Labelled MIXE spectra (all peaks identified) of a NMC811 electrode in a laminated Al pouch, measured at 24.0, 26.0 and 28.0 MeV/c</p>
Spectroscopic ellipsometry mapping of PAAO (AJ-1-04-20 sample)
<p>Spectroscopic ellipsometry measurement data obtained from the porous anodized aluminum oxide (PAAO). The sample was made by anodization of aluminum monocrystal in 0.3 mol/L oxalic acid at 40 V for 3 minutes and 16 seconds.</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-1-04-20 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: 50°, 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 after being covered with gold nanoparticles. The data can be found here: https://doi.org/10.5281/zenodo.7059281</p>
Spectroscopic ellipsometry mapping of PAAO (AJ-3-04-20 sample)
<p>Spectroscopic ellipsometry measurement data obtained from the porous anodized aluminum oxide (PAAO). The sample was made by anodization of aluminum monocrystal in 0.3 mol/L oxalic acid at 40 V for 4 minutes and 8 seconds.</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-3-04-20 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: 50°, 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 after being covered with gold nanoparticles. The data can be found here: https://doi.org/10.5281/zenodo.7115166</p>
Spectroscopic ellipsometry mapping of PAAO (AJ-2-04-20 sample)
<p>Spectroscopic ellipsometry measurement data obtained from the porous anodized aluminum oxide (PAAO). The sample was made by anodization of aluminum monocrystal in 0.3 mol/L oxalic acid at 40 V for 3 minutes and 37 seconds.</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-2-04-20 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: 50°, 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 after being covered with gold nanoparticles. The data can be found here: https://doi.org/10.5281/zenodo.7059828</p>
ScienceDex guides
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These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
Allen Brain Atlas
Allen Brain Atlas is an Allen Institute collection of brain map atlases, datasets, APIs, and analysis tools covering mouse, human, and non-human primate brain resources.
Annotated Behaviour and Observability Dataset (ABODe)
ABODe is a University of Edinburgh DataShare dataset for behavior classification in group-housed mice using home-cage video, identities, bounding boxes, ground-plate positions, and annotator labels.
DANDI Archive for NWB datasets
DANDI is a BRAIN Initiative archive for publishing and sharing neurophysiology data, including electrophysiology, optophysiology, and behavioral data packaged as NWB and related standards.
International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
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.