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235 results for “spectroscopic”
Solid-state $^{13}$C-NMR spectroscopic determination of sidechain mobilities in zirconium-based metal-organic frameworks
<p>This Dataset contains the raw data contained in the figures of our journal article in <i>Magnetic Resonance</i>: <a href="https://doi.org/10.5194/mr-2023-13">https://doi.org/10.5194/mr-2023-13</a>.</p>
Dataset for publication: "Spectroscopic properties and photoluminescence of the Li2B4O7:Mn,Sm glass"
<p>Dataset for the article: B.V. Padlyak, I.I. Kindrat, V.T. Adamiv, A. Drzewiecki, I. Stefaniuk, Spectroscopic properties and photoluminescence of the Li2B4O7:Mn,Sm glass, Materials Research Bulletin 175 (2024) 112788, <a title="Persistent link using digital object identifier" href="https://doi.org/10.1016/j.materresbull.2024.112788" target="_blank" rel="noreferrer noopener">https://doi.org/10.1016/j.materresbull.2024.112788</a></p> <p> </p>
Stellar chromospheric activity database of solar-like stars based on the Ca II H and K lines of LAMOST Low-Resolution Spectroscopic Survey: the bolometric and photospheric calibration
<p>This database contains the stellar chromospheric activity parameters of solar-like stars based on the Ca II H and K lines from the spectra of the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) Low-Resolution Spectroscopic Survey (LRS). We extract 1,122,495 LRS spectra of solar-like stars from the LAMOST Data Release 8 v2.0 and provide the chromospheric activity parameters $S_{\rm tri}$, $S_{\rm MWO}$, $R_{\rm HK}$ and $R'_{\rm HK}$, as well as their uncertainties in the database. $R_{\rm HK}$ and $R'_{\rm HK}$ are derived from the method in the classic literature (denoted with classic) and the method based on the PHOENIX model (denoted with PHOENIX). These stellar chromospheric activity indexes and their uncertainties, along with the relevant spectroscopic parameters from the LAMOST catalogs, are saved in a CSV-format file (name: CaIIHK_Activity_Indexes_LAMOST_DR8_LRS.csv).</p> <p> </p> <p>Columns in the catalog of the database:</p> <p>obsid - Unique observation identifier of LAMOST LRS spectrum</p> <p>obsdate-Spectral observation date</p> <p>fitsname - FITS file name of LAMOST LRS spectrum</p> <p>snrg - Signal-to-noise ratio in the $g$ band ($\mathrm{S/N}_g$) of LAMOST LRS spectrum</p> <p>snrr - Signal-to-noise ratio in the $r$ band ($\mathrm{S/N}_r$) of LAMOST LRS spectrum</p> <p>teff - Effective temperature ($T_\mathrm{eff}$) derived from the LASP (unit: K)</p> <p>teff_err - Uncertainty of $T_\mathrm{eff}$ derived from the LASP (unit: K)</p> <p>logg - Surface gravity ($\log\,g$) derived from the LASP (unit: dex)</p> <p>logg_err - Uncertainty of $\log\,g$ derived from the LASP (unit: dex)</p> <p>feh - Metallicity ([Fe/H]) derived from the LASP (unit: dex)</p> <p>feh_err - Uncertainty of [Fe/H] derived from the LASP (unit: dex)</p> <p>rv - Radial velocity ($V_r$) derived from the LASP (unit: km/s)</p> <p>rv_err - Uncertainty of $V_r$ derived from the LASP (unit: km/s)</p> <p>ra_obs - Right ascension (RA) of fiber pointing (unit: degree)</p> <p>dec_obs - Declination (DEC) of fiber pointing (unit: degree) </p> <p>gaia_source_id - Source identifier in Gaia DR3 catalog</p> <p>gaia_g_mean_mag - $G$ magnitude in Gaia DR3 catalog</p> <p>S_tri* - $S_{\rm tri}$ index of LAMOST LRS </p> <p>S_tri_err* - Uncertainty of $S_{\rm tri}$ </p> <p>S_MWO* - $S_{\rm MWO}$ </p> <p>S_MWO_err* - Uncertainty of $S_{\rm MWO}$ </p> <p>log_R_HK_classic* - $\log\,R_{\rm HK,classic}$ </p> <p>log_R_HK_classic_err* - Uncertainty of $\log\,R_{\rm HK,classic}$ </p> <p>log_R_p_HK_classic* - $\log\,R'_{\rm HK,classic}$ </p> <p>log_R_p_HK_classic_err* - Uncertainty of $\log\,R'_{\rm HK,classic}$ </p> <p>log_R_HK_PHOENIX* - $\log\,R_{\rm HK,PHOENIX}$ </p> <p>log_R_HK_PHOENIX_err* - Uncertainty of $\log\,R_{\rm HK,PHOENIX}$ </p> <p>log_R_p_HK_PHOENIX* - $\log\,R'_{\rm HK,PHOENIX}$ </p> <p>log_R_p_HK_PHOENIX_err* - Uncertainty of $\log\,R'_{\rm HK,PHOENIX}$ </p> <p>(Note: The columns denoted by an asterisk represent the parameters provided by this database, and the remaining columns are collected from the data release of LAMOST DR8 V2.0. If the values are not available, they will be filled with '-9999' in this database.)</p>
Photophysical and Spectroscopic dataset for Ag-In-Zn-S alloyed nanocrystals as photocatalysts of controlled light-mediated radical polymerization
<p>(1) Energy-dispersive spectra of alloyed Ag<sub>1.0</sub>In<sub>1.5</sub>Zn<sub>0.3</sub>S<sub>3.3</sub> (R) and Ag<sub>1.0</sub>In<sub>10.3</sub>Zn<sub>12.4</sub>S<sub>11.8</sub> (G) nanocrystals.</p> <p>(2) HR-TEM images of alloyed Ag<sub>1.0</sub>In<sub>1.5</sub>Zn<sub>0.3</sub>S<sub>3.3</sub> (R) and Ag<sub>1.0</sub>In<sub>10.3</sub>Zn<sub>12.4</sub>S<sub>11.8</sub> (G) nanocrystals.</p> <p>(3) X-ray powder diffractograms of alloyed Ag<sub>1.0</sub>In<sub>1.5</sub>Zn<sub>0.3</sub>S<sub>3.3</sub> (R) and Ag<sub>1.0</sub>In<sub>10.3</sub>Zn<sub>12.4</sub>S<sub>11.8</sub> (G) nanocrystals.</p> <p>(4) UV-vis-NIR spectra of toluene dispersion of Ag<sub>1.0</sub>In<sub>1.5</sub>Zn<sub>0.3</sub>S<sub>3.3</sub> (R) Ag<sub>1.0</sub>In<sub>10.3</sub>Zn<sub>12.4</sub>S<sub>11.8</sub> (G) nanocrystals.</p> <p>(5) Photoluminescence excitation and emission spectra of toluene dispersion of Ag<sub>1.0</sub>In<sub>1.5</sub>Zn<sub>0.3</sub>S<sub>3.3</sub> (R) and Ag<sub>1.0</sub>In<sub>10.3</sub>Zn<sub>12.4</sub>S<sub>11.8</sub> (G) nanocrystals.</p> <p>(6) <sup>1</sup>H and <sup>13</sup>C NMR spectra (in benzene-<em>d<sub>6</sub></em>) of the reaction mixture used for the photocatalytic bulk and solution polymerization of methyl methacrylate (MMA) with <a name="_Hlk161909311"></a>Ag<sub>1.0</sub>In<sub>1.5</sub>Zn<sub>0.3</sub>S<sub>3.3</sub> (R) and Ag<sub>1.0</sub>In<sub>10.3</sub>Zn<sub>12.4</sub>S<sub>11.8</sub> (G) nanocrystals as a photocatalyst.</p> <p>(7) SEC profiles of PMMA prepared in bulk and solution polymerization.</p> <p>(8) MALDI-TOF spectra in the low and high molecular weight ranges of PMMA synthesized in the presence of Ag<sub>1.0</sub>In<sub>1.5</sub>Zn<sub>0.3</sub>S<sub>3.3</sub> (R) and Ag<sub>1.0</sub>In<sub>10.3</sub>Zn<sub>12.4</sub>S<sub>11.8</sub> (G) nanocrystals as photocatalysts.</p> <p>(9) EPR spectra of adducts generated for Ag<sub>1.0</sub>In<sub>1.5</sub>Zn<sub>0.3</sub>S<sub>3.3</sub> (R) and Ag<sub>1.0</sub>In<sub>10.3</sub>Zn<sub>12.4</sub>S<sub>11.8</sub> (G) nanocrystals + 5,5-dimethyl-1-pyrroline-<em>N</em>-oxide (DMPO) under illumination by a green LED (l = 523 nm).</p> <p>This work was supported by the National Science Centre of Poland, Grant No. 2022/45/B/ST5/02120</p>
Dataset of hydrogen Balmer line indexes for stellar chromospheric activity of solar-like stars based on the LAMOST spectroscopic surveys
<p><span>This dataset consists of three catalogs of the data of the hydrogen Balmer line indexes of solar-like stars for stellar chromospheric activity based on the LAMOST Low-Resolution Spectroscopic Survey (LRS) and Medium-Resolution Spectroscopic Survey (MRS): (1) LRS spectral catalog, (2) MRS spectral catalog, and (3) stellar source catalog. These catalogs are stored as three CSV-format data files. The columns contained in the catalogs are described below. The observational and spectroscopic parameters of the spectral samples in the dataset are from LAMOST DR9 v2.0. Unavailable values in the dataset are marked as −9999.0.</span></p> <p><span> </span></p> <p><span>(1) LRS spectral catalog (Balmer_line_indexes_LRS_spectral_catalog_LAMOST_DR9.csv)</span></p> <p><span>obsid - unique LAMOST observation identifier of LRS</span></p> <p><span>obsdate - date of LRS observation (UTC)</span></p> <p><span>uid - unique LAMOST source identifier</span></p> <p><span>ra - right ascension of stellar source in LRS catalog (unit: degree)</span></p> <p><span>dec - declination of stellar source in LRS catalog (unit: degree)</span></p> <p><span>sn_g - LRS g-band signal-to-noise ratio</span></p> <p><span>sn_r - LRS r-band signal-to-noise ratio</span></p> <p><span>teff - stellar effective temperature determined from LRS data (unit: K)</span></p> <p><span>teff_err - uncertainty of teff (unit: K)</span></p> <p><span>logg - stellar surface gravity determined from LRS data (unit: dex)</span></p> <p><span>logg_err - uncertainty of logg (unit: dex)</span></p> <p><span>feh - stellar metallicity determined from LRS data (unit: dex)</span></p> <p><span>feh_err - uncertainty of feh (unit: dex)</span></p> <p><span>rv - radial velocity determined from LRS data (unit: km/s)</span></p> <p><span>rv_err - uncertainty of rv (unit: km/s)</span></p> <p><span>L_halpha - Hα activity index of LRS data</span></p> <p><span>L_halpha_err - uncertainty of L_halpha</span></p> <p><span>L_hbeta - Hβ activity index of LRS data</span></p> <p><span>L_hbeta_err - uncertainty of L_hbeta</span></p> <p><span>L_hgamma - Hγ activity index of LRS data</span></p> <p><span>L_hgamma_err - uncertainty of L_hgamma</span></p> <p><span>L_hdelta - Hδ activity index of LRS data</span></p> <p><span>L_hdelta_err - uncertainty of L_hdelta</span></p> <p><span> </span></p> <p><span>(2) MRS spectral catalog (Balmer_line_indexes_MRS_spectral_catalog_LAMOST_DR9.csv)</span></p> <p><span>obsid - unique LAMOST observation identifier of MRS</span></p> <p><span>obsdate - date of MRS observation (UTC)</span></p> <p><span>uid - unique LAMOST source identifier</span></p> <p><span>ra - right ascension of stellar source in MRS catalog (unit: degree)</span></p> <p><span>dec - declination of stellar source in MRS catalog (unit: degree)</span></p> <p><span>sn_B - MRS blue-band signal-to-noise ratio</span></p> <p><span>sn_R - MRS red-band signal-to-noise ratio</span></p> <p><span>teff - stellar effective temperature determined from MRS data (unit: K)</span></p> <p><span>teff_err - uncertainty of teff (unit: K)</span></p> <p><span>logg - stellar surface gravity determined from MRS data (unit: dex)</span></p> <p><span>logg_err - uncertainty of logg (unit: dex)</span></p> <p><span>feh - stellar metallicity determined from MRS data (unit: dex)</span></p> <p><span>feh_err - uncertainty of feh (unit: dex)</span></p> <p><span>rv_r0 - radial velocity determined from the red band data of MRS (unit: km/s)</span></p> <p><span>rv_r0_err - uncertainty of rv_r0 (unit: km/s)</span></p> <p><span>M_halpha – Hα activity index of MRS data</span></p> <p><span>M_halpha_err - uncertainty of M_halpha</span></p> <p><span> </span></p> <p><span>(3) stellar source catalog (Balmer_line_indexes_stellar_source_catalog_LAMOST_DR9.csv)</span></p> <p><span>uid - unique LAMOST source identifier</span></p> <p><span>ra - right ascension of stellar source from LRS catalog (unit: degree)</span></p> <p><span>dec - declination of stellar source from LRS catalog (unit: degree)</span></p> <p><span>teff - stellar effective temperature from LRS catalog (unit: K)</span></p> <p><span>teff_err - uncertainty of teff (unit: K)</span></p> <p><span>logg - stellar surface gravity from LRS catalog (unit: dex)</span></p> <p><span>logg_err - uncertainty of logg (unit: dex)</span></p> <p><span>feh - stellar metallicity from LRS catalog (unit: dex)</span></p> <p><span>feh_err - uncertainty of feh (unit: dex)</span></p> <p><span>L_halpha - Hα activity index of LRS data</span></p> <p><span>L_halpha_err - uncertainty of L_halpha</span></p> <p><span>L_hbeta - Hβ activity index of LRS data</span></p> <p><span>L_hbeta_err - uncertainty of L_hbeta</span></p> <p><span>L_hgamma - Hγ activity index of LRS data</span></p> <p><span>L_hgamma_err - uncertainty of L_hgamma</span></p> <p><span>L_hdelta - Hδ activity index of LRS data</span></p> <p><span>L_hdelta_err - uncertainty of L_hdelta</span></p> <p><span>M_halpha - Hα activity index of MRS data</span></p> <p><span>M_halpha_err - uncertainty of M_halpha</span></p> <p><span>l_halpha - Hα absolute flux index of LRS data (unit: 1/</span><span>Å</span><span>)</span></p> <p><span>l_halpha_err - uncertainty of l_halpha (unit: 1/</span><span>Å</span><span>)</span></p> <p><span>l_hbeta - Hβ absolute flux index of LRS data (unit: 1/</span><span>Å</span><span>)</span></p> <p><span>l_hbeta_err - uncertainty of l_hbeta (unit: 1/</span><span>Å</span><span>)</span></p> <p><span>l_hgamma - Hγ absolute flux index of LRS data (unit: 1/</span><span>Å</span><span>)</span></p> <p><span>l_hgamma_err - uncertainty of l_hgamma (unit: 1/</span><span>Å</span><span>)</span></p> <p><span>l_hdelta - Hδ absolute flux index of LRS data (unit: 1/</span><span>Å</span><span>)</span></p> <p><span>l_hdelta_err - uncertainty of l_hdelta (unit: 1/</span><span>Å</span><span>)</span></p> <p><span>m_halpha</span><span> - Hα absolute flux index of MRS data (unit: 1/</span><span>Å</span><span>)</span></p> <p><span>m_halpha_err - uncertainty of m_halpha (unit: 1/</span><span>Å</span><span>)</span></p> <p><span> </span></p> <p><span> </span></p>
Raman spectroscopic mapping and atomic force microscopy statistical analyses for the determination of WS2 flake thickness
<p><span>This database contains the statistical analyses carried out in order to evaluate the thickness of the WS</span><sub><span>2</span></sub><span> nanoflakes. In order to have a reliable comparison we determine the methodology of comparing Raman spectroscopic mapping and atomic force microscopy (AFM). </span></p> <p><span>In case of Raman spectroscopy, the thickness is evaluated by employing the separation of the two vibrational mode, namely E</span><sub><span>2g</span></sub><span> and A</span><sub><span>1g</span></sub><span>. This method is well-established and the number of layers has been previously tabulated in different articles. </span></p> <p><span>Each spectrum of the Raman analysis, is performed with a 100X objective in a confocal microscope, with a 473 nm laser excitation, a laser power of 0.5 mW and an acquisition time of 1 s.</span></p> <p><span>The AFM analysis are carried out in tapping mode with a 512-pixel x 512-pixel resolution and and a scan rate of 1Hz per line.</span></p>
UV-Vis spectroscopic investigation of WS2 flakes, AuNP@WS2 and porphyrin-functionalized AuNP@WS2
<p>This dataset contains UV-Vis spectroscopic analysis of WS2 nanoflakes decorated with Au NP and THPP (<span>5,10,15,20-tetrakis(4-hydroxyphenyl)porphyrin</span>).</p>
HETDEX-LOFAR Spectroscopic Redshift Catalog
<p>We combine the power of blind integral field spectroscopy from the Hobby-Eberly Telescope (HET) Dark Energy Experiment (HETDEX) with sources detected by the Low Frequency Array (LOFAR) to construct the HETDEX-LOFAR Spectroscopic Redshift Catalog. Starting from the first data release of the LOFAR Two-metre Sky Survey (LoTSS), including a value-added catalog with photometric redshifts, we extracted 28,705 HETDEX spectra. Using an automatic classifying algorithm, we assigned each object a star, galaxy, or quasar label along with a velocity/redshift, with supplemental classifications coming from the continuum and emission line catalogs of the internal, fourth data release from HETDEX (HDR4). We measured 9,087 new redshifts; in combination with the value-added catalog, our final spectroscopic redshift sample is 9,710 sources. This new catalog contains the highest substantial fraction of LOFAR galaxies with spectroscopic redshift information; it improves archival spectroscopic redshifts, and facilitates research to determine the [O II] emission properties of radio galaxies from 0.0 < z < 0.5, and the Lyα emission characteristics of both radio galaxies and quasars from 1.9 < z < 3.5. Additionally, by combining the unique properties of LOFAR and HETDEX, we are able to measure star formation rates (SFR) and stellar masses. Using the Visible Integral-field Replicable Unit Spectrograph (VIRUS), we measure the emission lines of [O III], [Ne III], and [O II] and evaluate line-ratio diagnostics to determine whether the emission from these galaxies is dominated by AGN or star formation.</p> <p> </p> <p>The catalog is comprised of one FITS file with two extensions:</p> <ul> <li>No. 0 (1036, 28705): The first extension contains the spectrum, of length 1036, for each object. The corresponding wavelength values range from 3470 - 5540 angstroms.</li> <li>No. 1 (28705 rows x 13 columns): The second extension contains the derived values found for each source. The table below describes each column: <table> <tbody> <tr> <td><strong>COLUMN NAME</strong></td> <td><strong>DESCRIPTION</strong></td> <td><strong>DATA TYPE</strong></td> </tr> <tr> <td>objID</td> <td>LoTSS Object ID</td> <td>string</td> </tr> <tr> <td>source_name</td> <td>Source Name</td> <td>string</td> </tr> <tr> <td>RA</td> <td>PanSTARRS1 Right Ascension (J2000)</td> <td>float</td> </tr> <tr> <td>Dec</td> <td>PanSTARRS1 Declination (J2000)</td> <td>float</td> </tr> <tr> <td>z_diagnose</td> <td>Best fit redshift from Diagnose</td> <td>float</td> </tr> <tr> <td>z_hdr4</td> <td>Best fit redshift from ELiXer</td> <td>float</td> </tr> <tr> <td>z_archive</td> <td>Spectroscopic redshift from value-added LoTSS catalog</td> <td>float</td> </tr> <tr> <td>z_best</td> <td>HETDEX-LOFAR redshift</td> <td>float</td> </tr> <tr> <td>z_best_src</td> <td>1 = Diagnose, 2 = HDR4, 3 = Archive</td> <td>integer</td> </tr> <tr> <td>classification</td> <td>STAR, AGN, LOWZGAL, HIGHZGAL, or ARCHIVE</td> <td>string</td> </tr> <tr> <td>log_mass</td> <td>MCSED derived stellar mass</td> <td>float</td> </tr> <tr> <td>log_SFR</td> <td>MCSED derived star formation rate</td> <td>float</td> </tr> <tr> <td>log_L150</td> <td>MCSED derived 150 MHz luminosity</td> <td>float</td> </tr> </tbody> </table> </li> </ul> <p> </p> <p>We request that the following acknowledgement be included in any paper using HETDEX-LOFAR data:</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>We request that the following papers are cited when using any HETDEX-LOFAR data:</p> <p>Debski, M. H., Zeimann, G. R., Hill, G. J., et al. 2024, arXiv e-prints, arXiv:2411.08974, doi: 10.48550/arXiv.2411.08974</p>
Unraveling Molecular Structure: A Multimodal Spectroscopic Dataset for Chemistry
<p>This repository contains the data associated with: "Unraveling Molecular Structure: A Multimodal Spectroscopic Dataset for Chemistry" (see here: <a href="https://rxn4chemistry.github.io/multimodal-spectroscopic-dataset/">https://rxn4chemistry.github.io/multimodal-spectroscopic-dataset/</a>)</p>
Dataset for "Spectroscopic investigation of faeces with surface-enhanced Raman scattering: a case study with coeliac patients on gluten-free diet"
<p>This dataset contains all the spectra and OTU table data used in the paper "Spectroscopic investigation of faeces with surface-enhanced Raman scattering: a case study with coeliac patients on gluten-free diet", plus the R code to import the TXT (ASCII) files into a dataset, preprocess data, analzye data and generate the figures shown in the paper.</p> <p>Spectral data are available in 2 different format:</p> <p>- the original TXT files (as generated from the Raman instrument, 1 file = 1 spectrum)</p> <p>- as RData file (an hyperSpec object including metadata), directly to be opened in R</p> <p>The OTU table is available either as a single XLSX file or as a RData file to be opened in R.</p> <p>The R code used to generate the figures is available as a single file "Rcode.R".</p>
Spectroscopic and Electric Properties of the TaO$^+$ Molecule Ion for the Search of New Physics: A Platform for Identification and State Control: Dataset
<p>This dataset collects the unprocessed (= outputs from calculations) results discussed in the paper titled "Spectroscopic and Electric Properties of the TaO<sup>+</sup> Molecule Ion for the Search of New Physics: A Platform for Identification and State Control", by Ayaki Sunaga and Timo Fleig.</p>
Stellar chromospheric activity spectral database of solar-type stars based on the LAMOST Low-Resolution Spectroscopic Survey(disused)
<p>A stellar chromospheric activity spectral database of solar-type stars is constructed based on the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) Low-Resolution Spectroscopic Survey (LRS). The database contains 1,330,654 high-quality LRS spectra of solar-type stars with <em>T</em><sub>eff</sub> ranging from 4800 K to 6800 K. We measure the mean fluxes at line cores of the Ca II H&K lines using a 1 Å rectangular bandpass as well as a 1.09 Å full width at half maximum (FWHM) triangular bandpass, and the mean fluxes of two 20 Å pseudo-continuum bands on the two sides of the lines. Three chromospheric activity indexes, <em>S</em><sub>rec</sub> using the rectangular bandpass, and <em>S</em><sub>tri</sub> and <em>S</em><sub>MWL</sub> using the triangular bandpass, are evaluated based on the measured fluxes. The uncertainties of all the obtained parameters are estimated. We also produce spectrum diagrams of Ca II H&K lines for all the spectra in the database. This database with more than one million high-quality LAMOST LRS spectra and basal chromospheric activity parameters can be further used for investigating activity characteristics of solar-type stars and solar-stellar connection.</p> <p> </p> <p>The entity of the database is composed of (1) a catalog of spectral sample and activity parameters, and (2) a library of spectrum diagrams.</p> <p>(1) Catalog of Spectral Sample and Activity Parameters<br> CaIIHK_Sindex_LAMOST_DR7_LRS.csv</p> <p>(2) Library of Spectrum Diagrams<br> spectrum_diagrams_000-049.zip (46 subfolders)<br> spectrum_diagrams_050-099.zip (40 subfolders)<br> spectrum_diagrams_100-149.zip (47 subfolders)<br> spectrum_diagrams_150-199.zip (49 subfolders)<br> spectrum_diagrams_200-249.zip (47 subfolders)<br> spectrum_diagrams_250-299.zip (45 subfolders)<br> spectrum_diagrams_300-349.zip (41 subfolders)<br> spectrum_diagrams_350-399.zip (39 subfolders)<br> spectrum_diagrams_400-449.zip (45 subfolders)<br> spectrum_diagrams_450-499.zip (35 subfolders)<br> spectrum_diagrams_500-549.zip (27 subfolders)<br> spectrum_diagrams_550-599.zip (38 subfolders)<br> spectrum_diagrams_600-649.zip (32 subfolders)<br> spectrum_diagrams_650-699.zip (26 subfolders)<br> spectrum_diagrams_700-749.zip (28 subfolders)</p> <p> </p>
Stellar chromospheric activity spectral database of solar-type stars based on the LAMOST Low-Resolution Spectroscopic Survey (disused)
<p>A stellar chromospheric activity spectral database of solar-type stars is constructed based on the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) Low-Resolution Spectroscopic Survey (LRS). The database contains 1,330,654 high-quality LRS spectra of solar-type stars with effective temperature ranging from 4800 K to 6800 K. We measure the mean fluxes at line cores of the Ca II H&K lines using a 1 Å rectangular bandpass as well as a 1.09 Å full width at half maximum (FWHM) triangular bandpass, and the mean fluxes of two 20 Å pseudo-continuum bands on the two sides of the lines. Three chromospheric activity indexes, <em>S</em><sub>rec</sub> based on the 1 Å rectangular bandpass, and <em>S</em><sub>tri</sub> and <em>S</em><sub>MWL</sub> based on the 1.09 Å FWHM triangular bandpass, are evaluated from the measured fluxes. The uncertainties of all the obtained parameters are estimated. We also produce spectrum diagrams of Ca II H&K lines for all the spectra in the database. This database with more than one million high-quality LAMOST LRS spectra and basal chromospheric activity parameters can be further used for investigating activity characteristics of solar-type stars and solar-stellar connection.</p> <p> </p> <p>The entity of the database is composed of (1) a catalog of spectral sample and activity parameters, and (2) a library of spectrum diagrams.</p> <p>(1) Catalog of Spectral Sample and Activity Parameters<br> CaIIHK_Sindex_LAMOST_DR7_LRS.csv</p> <p>(2) Library of Spectrum Diagrams<br> spectrum_diagrams_000-049.zip (46 subfolders)<br> spectrum_diagrams_050-099.zip (40 subfolders)<br> spectrum_diagrams_100-149.zip (47 subfolders)<br> spectrum_diagrams_150-199.zip (49 subfolders)<br> spectrum_diagrams_200-249.zip (47 subfolders)<br> spectrum_diagrams_250-299.zip (45 subfolders)<br> spectrum_diagrams_300-349.zip (41 subfolders)<br> spectrum_diagrams_350-399.zip (39 subfolders)<br> spectrum_diagrams_400-449.zip (45 subfolders)<br> spectrum_diagrams_450-499.zip (35 subfolders)<br> spectrum_diagrams_500-549.zip (27 subfolders)<br> spectrum_diagrams_550-599.zip (38 subfolders)<br> spectrum_diagrams_600-649.zip (32 subfolders)<br> spectrum_diagrams_650-699.zip (26 subfolders)<br> spectrum_diagrams_700-749.zip (28 subfolders)</p>
Supplementary tables for the article "A novel approach for discovering correlations between elemental and molecular composition using laser-based spectroscopic techniques"
<p>Table S1. Collection conditions of zooplankton samples. Data in the salinity and temperature columns, separated by a slash sign, are the characteristics of surface and bottom water.</p> <p>Table S2. The results of elemental analysis of zooplankton by ICP-AES and ICP-MS (as provided by IO RAS).</p> <p>Table S3. List of emission signals used to construct spider diagrams.</p> <p>Table S4. List of spectral ranges eliminated from LIBS data to improve the performance of chemometric algorithms.</p> <p>Raw LIBS and Raman spectra of zooplankton.</p> <p> </p>
Stellar chromospheric activity spectral database of solar-type stars based on the LAMOST Low-Resolution Spectroscopic Survey(disused)
<p>A stellar chromospheric activity spectral database of solar-type stars is constructed based on the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) Low-Resolution Spectroscopic Survey (LRS). The database contains 1,330,654 high-quality LRS spectra of solar-type stars with effective temperature ranging from 4800 K to 6800 K. We measure the mean fluxes at line cores of the Ca II H&K lines using a 1 Å rectangular bandpass as well as a 1.09 Å full width at half maximum (FWHM) triangular bandpass, and the mean fluxes of two 20 Å pseudo-continuum bands on the two sides of the lines. Three chromospheric activity indexes, <em>S</em><sub>rec</sub> based on the 1 Å rectangular bandpass, and <em>S</em><sub>tri</sub> and <em>S</em><sub>MWL</sub> based on the 1.09 Å FWHM triangular bandpass, are evaluated from the measured fluxes. The uncertainties of all the obtained parameters are estimated. We also produce spectrum diagrams of Ca II H&K lines for all the spectra in the database. This database with more than one million high-quality LAMOST LRS spectra and basal chromospheric activity parameters can be further used for investigating activity characteristics of solar-type stars and solar-stellar connection.</p> <p> </p> <p>The entity of the database is composed of (1) a catalog of spectral sample and activity parameters, and (2) a library of spectrum diagrams.</p> <p>(1) Catalog of Spectral Sample and Activity Parameters<br> CaIIHK_Sindex_LAMOST_DR7_LRS.csv</p> <p>(2) Library of Spectrum Diagrams<br> spectrum_diagrams_000-049.zip (46 subfolders)<br> spectrum_diagrams_050-099.zip (40 subfolders)<br> spectrum_diagrams_100-149.zip (47 subfolders)<br> spectrum_diagrams_150-199.zip (49 subfolders)<br> spectrum_diagrams_200-249.zip (47 subfolders)<br> spectrum_diagrams_250-299.zip (45 subfolders)<br> spectrum_diagrams_300-349.zip (41 subfolders)<br> spectrum_diagrams_350-399.zip (39 subfolders)<br> spectrum_diagrams_400-449.zip (45 subfolders)<br> spectrum_diagrams_450-499.zip (35 subfolders)<br> spectrum_diagrams_500-549.zip (27 subfolders)<br> spectrum_diagrams_550-599.zip (38 subfolders)<br> spectrum_diagrams_600-649.zip (32 subfolders)<br> spectrum_diagrams_650-699.zip (26 subfolders)<br> spectrum_diagrams_700-749.zip (28 subfolders)</p>
Reproduction package for Spectroscopically resolved partial phase curve of the rapid heating and cooling of the highly-eccentric Hot Jupiter HAT-P-2b with WFC3
<p>This is a basic reproduction package for the paper "<span>Spectroscopically resolved partial phase curve of the rapid heating and cooling of the highly-eccentric Hot Jupiter </span><span>HAT-P-2b with WFC3</span>"</p> <p>by [Jacobs, B.; Désert, J. -M.; Lewis, N. et al. (2024)]</p> <p>Abstract:</p> <p><span>The extreme environments of transiting close-in exoplanets in highly-eccentric orbits serve as ideal labo</span><span>ratories for testing exo-atmospheric physics. Spectroscopically resolved phase curves not only allow for the </span><span>characterization of their thermal response to irradiation changes but also unveil phase-dependent atmospheric </span><span>chemistry and dynamics.</span></p> <p><span>We observed a partial phase curve of the highly-eccentric close-in giant planet HAT-P-2b (</span><span>e</span> <span>=</span> <span>0</span><span>.</span><span>51023)</span><br><span>with the Wide Field Camera 3 (WFC3) aboard the</span> <span>Hubble Space Telescope</span><span>.</span> <span>Using these data, we update </span><span>the planet’s orbital parameters and radius, and we retrieve high-frequency pulsations consistent with those re</span><span>ported in Spitzer data. We find that the peak in planetary flux occurs at 6</span><span>.</span><span>7</span> <span>±</span> <span>0</span><span>.</span><span>6 hr after periastron, with a </span><span>heating timescale of 9</span><span>.</span><span>0</span><span>+</span><span>3</span><span>.</span><span>5</span><br><span>−</span><span>2</span><span>.</span><span>1</span> <span>hr, and a cooling timescale of 3</span><span>.</span><span>6</span><span>+</span><span>0</span><span>.</span><span>7</span><span>−</span><span>0</span><span>.</span><span>6</span> <span>hr. We compare the light-curve to a suite of</span><br><span>1-dimensional and 3-dimensional forward models, varying the planet’s chemical composition. The strong con</span><span>trast in flux increase and decrease timescales before and after periapse indicates an opacity term that emerges </span><span>during the planet’s heating phase. We suggest that more emerging H</span><span>−</span> <span>than expected from chemical equilibrium </span><span>models could be the reason for the mismatch between models and the data.</span></p> <p><span>We used a common-mode based method that does not assume a functional form to extract phase-resolved </span><span>spectra. The analysis of these spectra is challenging because of the unknown accuracy of the spectral slope and </span><span>absolute flux levels. The phase-resolved spectra are largely featureless, possibly indicating an inhomogeneous </span><span>dayside.</span> <span>However, we identified an anomalously high flux in the spectroscopic bin that coincides with the </span><span>hydrogen Paschen</span> <span>β</span> <span>line and that is potentially connected to the planet’s orbit.</span> <span>We exclude an instrumental </span><span>origin and we discuss several alternative, astrophysical origins.</span></p>
Measured Ti L2,3-edge NEXAFS Spectroscopic Signatures
<p>Measured Ti L2,3-edge NEXAFS of a molecular library as well as mono- and dinuclear peroxo complexes, measured at the X-Treme beamline at the Swiss Light Source (SLS, PSI, Villigen, Switzerland).</p>
Spectroscopic and Interferometric Sum-Frequency Imaging of Strongly Coupled Phonon Polaritons in SiC Metasurfaces - Experimental and Simulation Data
<p>Data repository supporting the manuscript 'Spectroscopic and Interferometric Sum-Frequency Imaging of Strongly Coupled Phonon Polaritons in SiC Metasurfaces'.</p>
Archetype-Based Redshift Estimation for the Dark Energy Spectroscopic Instrument Survey
<p>Supplementary material to DESI's publication "Archetype-Based Redshift Estimation for the Dark Energy Spectroscopic Instrument Survey" by Anand et al. 2024 to comply with the data management plan. The material includes all the data shown in the figures of the results of the paper.</p>
CRIRES+ reduced spectroscopic observations of WASP-189
<h1>Reduced CRIRES+ spectroscopy observations of WASP-189 from 2022-07-01</h1> <p>This records contains the reduced data as used in the publication of Lesjak et al. 2024 "<em>Retrieving wind properties from the ultra-hot dayside of WASP-189 b with CRIRES+</em>" in press with Astronomy & Astrophysics.</p> <p>The raw data from the CRIRES+ instrument were reduced using the instrument pipeline and the reduction steps are described in the article.</p> <h2>Acknowledgements</h2> <p>If you make use of this data in your research, please cite the Lesjak et al. 2024 article and this record with its DOI (10.5281/zenodo.12663686) and its reference, the bibtex reference is:</p> <pre><code>@dataset{lavail_2024_12663686, author = {Lavail, Alexis}, title = {{CRIRES+ reduced spectroscopic observations of WASP-189}}, month = jul, year = 2024, publisher = {Zenodo}, version = {1.0}, doi = {10.5281/zenodo.12663686}, url = {https://doi.org/10.5281/zenodo.12663686} }</code></pre> <p> Note also that ESO requests an acknowledgement, which in this case would be: "<em>Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 109.23HN.002</em>".</p> <p>This data is released under a Creative Commons Attribution 4.0 International license.</p> <h2>Format of the data</h2> <p>The data are contained in a pickle file. Instructions on how to read pickle files can be found on the python wiki at <a href="https://wiki.python.org/moin/UsingPickle">https://wiki.python.org/moin/UsingPickle</a>:</p> <pre><code>import pickle data = pickle.load(open('wasp189_220630.pickle', 'rb'))</code></pre> <p>The data consists of a dictionary, the keys can be explored with the following command:</p> <pre><code>print(data.keys())</code></pre> <p>The keys are the following:</p> <ul> <li>script_version</li> <li>nodpos</li> <li>rawfilename</li> <li>nodpair</li> <li><strong>wave</strong></li> <li>wave_model</li> <li><strong>spec</strong></li> <li><strong>err</strong></li> <li>snr</li> <li>airmass</li> <li>bjd_tdb</li> <li>berv</li> <li>orders</li> <li>rawheaders</li> <li>slitfunctionFWHM-det1</li> <li>slitfunctionFWHM-det2</li> <li>slitfunctionFWHM-det3</li> </ul> <p>The keys in boldface (<strong>wave</strong>, <strong>spec</strong>, <strong>err</strong>) contain the reduced data, respectively the wavelength (expressed in vacuum in nanometres), the extracted spectrum (in ADU), and the error spectrum (in ADU). The other keys contain metadata and supplementary information as explained below. Each key contains a numPy array. The shape of the arrays can be expressed using three sizes:</p> <ol> <li>n_obs: the number of observations in the dataset</li> <li>n_pix = 2008: the number of pixels in each segment</li> <li>n_orders : the numbers of segment (each spectral order is split over three detectors creating three segments)</li> </ol> <p>The size of each array can be investigated with e.g</p> <pre><code>for key in data.keys(): try: print(key,':', data[key].shape) except: print(key) </code></pre> <p>which results in </p> <pre><code>script_version nodpos : (152,) rawfilename : (152,) nodpair : (152,) wave : (19, 152, 2008) wave_model : (19, 152, 2008) spec : (19, 152, 2008) err : (19, 152, 2008) snr : (19, 152) airmass : (152,) bjd_tdb : (152,) berv : (152,) orders : (19,) rawheaders : (152, 2484, 3) slitfunctionFWHM-det1 : (152, 8, 3) slitfunctionFWHM-det2 : (152, 7, 3) slitfunctionFWHM-det3 : (152, 7, 3) </code></pre> <h2>What's in the data?</h2> <ul> <li>script_version: version number of the python script used to produce the data</li> <li>nodpos: string, ('A' or 'B') the nodding position of the observation</li> <li>rawfilename: string, the filename of the raw science file from the ESO archive </li> <li>nodpair: string, ('pairNN') where NN is the number of nodding pair used in the data reduction: science files are reduced in pair with one nodding 'A' spectrum and one 'B'</li> <li><strong>wave</strong>: array containing the pipeline-derived wavelength solution for the spectrum in nanometers in vacuum<strong><br></strong></li> <li>wave_model: refined and more precise wavelength solution using molecfit fitting the telluric spectrum as explained in Sect. 2.1 of the paper</li> <li><strong>spec:</strong> reduced spectrum in ADU from the CRIRES+ pipeline. The spectra have been divided by the blaze spectrum (extracted spectrum from the flat-field lamp) to rectify the shape of the continuum and simplify spectrum, normalization<strong><br></strong></li> <li><strong>err</strong>: the error spectrum in ADU corresponding to the <strong>spec</strong> (signal to noise ration can be computed using spec/err)<strong><br></strong></li> <li>snr: median signal to noise ratio for each segment/observation</li> <li>airmass: airmass for each observation taken from the raw file header (mean of airmass at start and end of each exposure)</li> <li>bjd_tdb: bjd_tdb (barycentric julian date expressed in temps dynamique barycentrique) time at the middle of the exposure computed with barycorrpy (https://github.com/shbhuk/barycorrpy)</li> <li>berv: berv correction at middle of exposure computed with barycorrpy</li> <li>orders: string (D-OO) identifying the segment where D is the detector number (1-3) and OO is the order number (02-08)</li> <li>rawheaders: the fits header from the raw science files</li> <li>slitfunctionFWHM-det1: contains information on the FWHM of the slit function taken from the reduced file headers for the orders of detector 1</li> <li>slitfunctionFWHM-det2: same for detector 2</li> <li>slitfunctionFWHM-det3: same for detector 3</li> </ul>
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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)
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DANDI Archive for NWB datasets
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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.