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1,029 results for “Absorption”
CL emission and absorption spectra of MoS2 pyramids
<p>Cathodoluminescence spectra of MoS2 pyramid on sapphire substrate. Extensive experimental data used for the publication: <a href="https://doi.org/10.1039/D1NR06041D">https://doi.org/10.1039/D1NR06041D</a> "Excitonic absorption and defect related emission in three-dimensional MoS2 pyramids"</p> <p>In the file the maps with the different areas highlighted. To each area corresponds an average spectrum.</p>
Substituent-dependent absorption and fluorescence properties of perylene bisimide radical anions and dianions
<p>Original spectroscopic data to report: </p> <p>R. Renner <em>et. al. Mater. Horiz</em>., <strong>2022</strong>, <em>9</em>, 350–359; DOI: 10.1039/d1mh01019k</p> <p><strong>Abstract</strong>: Perylene-3,4:9,10-bis(dicarboximides) (PBIs) rank among the most important functional dyes and organic semiconductors, but only recently have their radical anions and dianions attracted interest for a variety of applications. Here, we systematically elucidate the functional properties (redox, absorption, and emission) of five PBI anions and dianions bearing different bay-substituents attached to the chromophore core. Cyclic voltammetry measurements reveal the influence of the substituents ranging from electron-withdrawing cyano to electron-donating phenoxy groups on the oxidation and reduction potentials that relate to the HOMO and LUMO levels ranging from −7.07 eV to −6.05 eV and −5.01 eV to −4.05 eV, respectively. Spectroelectrochemical studies reveal a significant number of intense absorption bands in the NIR-spectral range (750–1400 nm) for the radical anions, whereas the dianionic species are characterized by similar spectra to those for the neutral dyes, however being bathochromically shifted and with increased molar extinction coefficients of approximately 100 000 M<sup>−1</sup> cm<sup>−1</sup>. The increase of the transition dipole moment is up to 56% and accompanied by an almost cyanine-like red-shifted (by 300 nm) absorption spectrum for the most electron-poor tetracyanotetrachloro PBI. Whilst the outstanding fluorescence properties of the neutral PBIs are lost for the radical anions, an appreciable near-infrared (NIR) fluorescence with a quantum yield of up to 18% is revealed for the dianions by utilizing a custom-built flow-cell spectroelectrochemistry setup. Time-dependent density functional theory calculations help to assign the absorption bands to the respective electronic transitions.</p>
Scattering and absorption coefficients calculated from size distributions and absorption photometer data at Dome C, Antarctica
<p>The file contains the scattering and absorption coefficients presented in</p> <p>Virkkula et al.: Aerosol optical properties calculated from size distributions, filter samples and absorption photometer data at Dome C, Antarctica and their relationships between seasonal cycles of sources, ACP-2021-562.</p> <p> </p>
Ultrafast Infrared Transient Absorption Spectroscopy of Gas-Phase Ni(CO)4 Photodissociation at 261 nm
<p>This is the data repository for the following publication:</p> <p>Neil C. Cole-Filipiak, Jan Tross, Paul Schrader, Laura M. McCaslin, and Krupa Ramasesha, "Ultrafast infrared transient absorption spectroscopy of gas-phase Ni(CO)4 photodissociation at 261 nm," J. Chem. Phys. 156, 144306 (2022), https://doi.org/10.1063/5.0080844.</p> <p><strong>Abstract:</strong></p> <p>We employ ultrafast mid-infrared transient absorption spectroscopy to probe the rapid loss of carbonyl ligands from gas-phase nickel tetracarbonyl following ultraviolet photoexcitation at 261 nm. Here, nickel tetracarbonyl undergoes prompt dissociation to produce nickel tricarbonyl in a singlet excited state; this electronically excited tricarbonyl loses another CO group over tens of picoseconds. Our results also suggest the presence of a parallel, concerted dissociation mechanism to produce nickel dicarbonyl in a triplet excited state, which likely dissociates to nickel monocarbonyl. Mechanisms for the formation of these photoproducts in multiple electronic excited states are theoretically predicted with one-dimensional cuts through the potential energy surfaces and computation of spin–orbit coupling constants using equation of motion coupled cluster methods (EOM-CC) and coupled cluster theory with single and double excitations (CCSD). Bond dissociation energies are calculated with CCSD, and anharmonic frequencies of ground and excited state species are computed using density functional theory (DFT) and time-dependent density functional theory (TD-DFT).</p> <p> </p> <p><strong>Experimental Data:</strong></p> <p>All data are saved as a .csv file. The first column contains frequencies (in cm<sup>-1</sup>) while the first row indexes each time delay (in ps). High-resolution transient spectra at select time delays are similarly structured. Each transient .csv file is labeled according to molecule, pump wavelength, file contents, pump laser power, pressure, and a date (<em>e.g.</em> NT261_trans_1mW_1.5torr_17Feb2021.csv).</p> <p> </p> <p><strong>Computational Data:</strong></p> <p>This data repository consists of 7 directories, which contain the data used in the main paper. Computational data published in the supplementary material may be requested from the corresponding authors.</p> <p>Anharmonic frequencies and DFT energies can be obtained in the directory "VPT2", where the files are labelled nicoX_*_anharm.out, where X=3,2,1 (the compound) and * corresponds to the electronic state for which the calculation was performed.</p> <p>EOM-CC calculations of the spin-orbit coupling constants at the geometries reported are found within the "SOCC" directory using the naming convention nicoX_[]_so_*.out, where X=3,2, []=an indication of the geometry, and * corresponds to the electronic state for which the calculation was performed.</p> <p>Calculations of the minimum energy crossing points (MECPs) can be found in the directory "MECP" using the naming convention nicoX_min*.out, where X=4,3,2,1, and * corresponds to the two electronic states for which the MECP is calculated (e.g. s0s1).</p> <p>The following 4 directories contain all the EOM-CC output files needed to reproduce the curves from Figure 2: 4to3, 3to2, 4to2, and 2to1, corresponding to panels a, b, c, and d, respectively. The naming conventions for the files within these directories are X_yz.out, where X=the name of the directory, y=the value of the reaction coordiante, and z=s (singlet) or t (triplet).</p>
The dataset by "Spectrally Consistent Scattering, Absorption, and Polarization Properties of Atmospheric Ice Crystals at Wavelengths from 0.2 to 100 μm"
<p>This is the ice crystal single-scattering property dataset introduced in the paper "Yang, Ping, et al. "Spectrally consistent scattering, absorption, and polarization properties of atmospheric ice crystals at wavelengths from 0.2 to 100 μ m." <em>Journal of the Atmospheric Sciences</em> 70.1 (2013): 330-347.".</p>
Longitudinal Variation of H2O Ice Absorption on Miranda
<p>Near-infrared reflectance spectra of the Uranian satellite Miranda.</p> <p><strong>Title: </strong>Longitudinal Variation of H2O Ice Absorption on Miranda<br> <strong>Authors: </strong>Riley DeColibus, Nancy Chanover, Richard Cartwright</p> <p><strong>Description of contents:</strong><br> This .tar package is a collection of reduced near-IR (~0.9 to 2.5 um) disk-integrated reflectance spectra of the Uranian moon Miranda.<br> The package includes:</p> <ul> <li>23 spectra acquired with the TripleSpec spectrograph on the ARC 3.5m telescope at Apache Point Observatory.</li> <li>4 spectra acquired with the GNIRS spectrograph on the 8.1m Gemini North telescope on Maunakea.</li> <li>10 spectra acquired with the SpeX spectrograph on the 3m IRTF telescope on Maunakea.</li> <li>5 "grand average" spectra constructed by robustly averaging all TripleSpec data frames acquired covering certain longitude ranges on Miranda. The SpeX and GNIRS data are not included in these grand averages.</li> <li>1 "grand average" TripleSpec spectrum of Uranus, averaged using observations on five nights in fall 2020.</li> </ul> <p>The filenames are in the following format:</p> <p>Mir_[mean sub-observer longitude]_[UT date]_[instrument].txt</p> <p>The files themselves are plain-text, fixed-width ASCII tables.<br> The first several lines of the file header are commented with "#" characters.<br> An example header and explanation is discussed below in the "Additional comments" section.<br> One uncommented line with column titles precedes the data itself.</p> <p>The 'wl' column is wavelength in micrometers (um).<br> The 'flux' column is an arbitrary flux ratio, normalized to unity at 1.72 um.<br> The 'err' column is the 1-sigma errors on the 'flux' column.</p> <p>The process of data acquisition, reduction, and analysis for the TripleSpec and GNIRS spectra are described in the text of the main paper.<br> The SpeX spectra consist of 7 spectra published by previous authors (Gourgeot et al. 2014, Cartwright et al. 2018), and<br> 3 spectra acquired in 2017 that were not previously published, but were reduced via the same procedures as in Cartwright et al. 2018.</p> <p>These data have been corrected for telluric (atmospheric) absorption and divided by the spectrum of an early G dwarf standard star.<br> We did not attempt to correct differing spectral slopes between different standard stars and the Sun.<br> While we only included one 'grand average' Uranus spectrum as an example, we obtained a spectrum of Uranus on every night that we observed Miranda.<br> Users interested in the individual spectra of Uranus from each date should contact the corresponding author.</p> <p><strong>System requirements:</strong><br> No special programs should be required to read these spectra.<br> They were converted to ASCII tables with the Astropy table reading/writing functionality and should be inherently compatible with it.<br> Note that some spectra do include some invalid values represented with 'nan', and these values should be ignored.</p> <p><strong>Additional comments:</strong></p> <p>The commented lines in the file headers include useful metadata regarding observational details for each spectrum.<br> The main text includes more details on how these quantities were determined.</p> <p><strong>Example header and explanation:</strong><br> # PI = DeColibus [PI of the observing proposal]<br> # INSTRUMENT = TripleSpec [Instrument/instrument mode, if applicable]<br> # UT_DATE = UT201206 [Date of observation in UTYYMMDD format]<br> # BODY = Miranda [Observed astronomical body]<br> # MEAN_LAT = 47.66 [Mean sub-observer latitude]<br> # MEAN_LONG = 274.6 [Mean sub-observer longitude (IAU east-positive)]<br> # START_LONG = 241.5 [Sub-obs longitude of first exposure]<br> # END_LONG = 304.7 [Sub-obs longitude of last exposure]<br> # LONG_RANGE = 63.2 [Degrees of longitude spanned by spectrum]<br> # MEAN_PHASE = 1.72 [Mean phase angle (alpha)]<br> # TOT_EXPTIME = 12960 [Total exposure time (seconds)]<br> # N_FRAMES = 72 [Number of frames contributing to spectrum]<br> # STANDARD = HD 16275 [Star(s) used as telluric standards, typically early G dwarfs]<br> # WAVELENGTH UNITS = micrometers (um)<br> # FLUX UNITS = arbitrary (normalized to unity at 1.72 um)<br> # ERROR UNITS = 1-sigma errors on the above<br> wl flux err <br> 0.910701 -1.165e+00 9.00e+00 <br> 0.910824 -9.227e-01 7.27e+00 <br> 0.910946 -3.486e+00 8.03e+00 <br> ... ... ...</p> <p>The spectra are presented at native resolution and instrumental sampling.<br> The TripleSpec spectrograph has a detector gap between 1.85-1.88 um, and there is no data in this region.</p> <p>As discussed in the main text, the TripleSpec spectra suffer from a "bump" in apparent flux between about 0.95-1.15 micron.<br> This 'bump' is not a real feature in Miranda's spectrum, but results from spurious spectral slopes in different spectral orders.<br> In regions of the spectrum where the wavelength coverage of these spectral orders overlap,<br> merging the spectral orders together results in inflection points that create the resulting 'bump'.</p> <p>Due to its proximity to Uranus, the raw spectra of Miranda are strongly contaminated by scattered light.<br> This contamination (see figure 15 in main text) is strongest between 0.90-0.965 um, 1.02-1.12 um, 1.24-1.32 um, and 1.48-1.63 um.<br> A correction procedure was applied to the TripleSpec spectra to remove this Uranus contamination, described in Appendix A of the paper.</p> <p>However, there may be low-level, residual spectral features resulting from inadequate correction, which may appear as either 'bumps' or 'dips'.<br> We warn the user to be cautious during analysis, as we cannot guarantee that either the spectral slopes<br> or any apparent spectral features at wavelengths shorter than 1.4um are reliable.<br> To a lesser extent, this may also be true of apparent spectral variations <1.4um in the GNIRS and SpeX spectra.</p> <p><strong>For the raw data files, files from intermediate processing steps, more Uranus spectra, or other questions,<br> please contact the corresponding author:</strong><br> Riley DeColibus</p> <p>(contact information omitted, but is included in readme file in download)</p>
Dataset for "Imaging of Small-Scale Heterogeneity and Absorption Using Adjoint Envelope Tomography: Results from Laboratory Experiments"
<p>The codes for Monte-Carlo simulation, scripts used to calculate the misfit kernels, and the processed data of the laboratory experiment.</p>
Figure 3: Absorption spectra of TiO2/CdS composites samples with a di®erent mass proportion-PREPARATION AND CHARACTERIZATION OF TIO2/CDS LAYERS AS POTENTIAL PHOTOELECTROCATALYTIC MATERIALS
<p>Optical properties of TiO2/CdS semi-<br> conductor composites have been investigated using optical absorption and pho-<br> toluminescence spectroscopy. UV-VIS absorption spectra of the as-prepared<br> photocatalysts were taken on a JASCO V-550 spectrometer. The °uorescence<br> spectra were obtained using an ABL&Jasco V 6500 spectro°uorimeter with<br> xenon lamp. The optical studies of the TiO2/CdS composites were performed<br> using the absorption spectra observed in the wavelength range 200-900 nm.<br> Fig. 3 shows the UV-Vis spectra of TiO2/CdS samples.</p>
Fig. 1 in Samara water absorption and floatation in sheoaks, Casuarina and Allocasuarina (Casuarinaceae)
Fig. 1 - Dry samara of Casuarina cristata (A) and dry and wet samara of Allocasuarina verticillata (B, C). The wet samara (C) was photographed after being placed on a droplet of water ~2 min. A wet samara of C. cristata was not included as there was no distinct visual change associated with wetting. / Samara secca di Casuarina cristata (A) e samara secca e bagnata di Allocasuarina verticillata (B, C). La samara bagnata (C) è stata fotografata dopo essere stata posta su una goccia d'acqua per ~2 min. Una samara bagnata di C. cristata non è stata inclusa perché non mostrava un distinto cambiamento visivo associato all'idratazione.
Fig. 3 in Samara water absorption and floatation in sheoaks, Casuarina and Allocasuarina (Casuarinaceae)
Fig. 3 - Proportion of samaras of five accessions each of Casuarina (A) and Allocasuarina (B) as a function of time (general linear model binomial fit, plotted with a logistic function) with floating half-life (sigmoid midpoint). Accessions: A, Casuarina cristata (Ccr), C. cunninghamiana (Ccu), C. glauca (Cgl1 and Cgl2, accessions 1 and 2) and C. obesa (Cob), and B, Allocasuarina acutivalvis (Aac), A. huegeliana (Ahu), A. muelleriana (Amu) and A. verticillata (Ave1 and Ave2, accessions 1 and 2). Casuarina samaras were assessed in five replicate groups of five, whereas Allocasuarina samaras were assessed individually in five replicates because initial tests indicated wet samaras aggregated and sunk together. Error bars are standard errors of the estimates of the sigmoid midpoints (n = 5). / Proporzione di samare di cinque campioni ciascuna di Casuarina (A) e Allocasuarina (B) in funzione del tempo (adattamento binomiale del modello lineare generalizzato, rappresentato con una funzione logistica) con emivita fluttuante (punto medio della sigmoide). Campioni: A, Casuarina cristata (Ccr), C. cunninghamiana (Ccu), C. glauca (Cgl1 e Cgl2, campioni 1 e 2) e C. obesa (Cob), e B, Allocasuarina acutivalvis (Aac), A. huegeliana (Ahu), A. muelleriana (Amu) e A. verticillata (Ave1 e Ave2, accessioni 1 e 2). Le samare di Casuarina sono state valutate in cinque gruppi di cinque repliche, mentre le samare di Allocasuarina sono state valutate individualmente in cinque repliche perché i test iniziali indicavano che le samare bagnate si aggregavano e affondavano insieme. Le barre di errore rappresentano l'errore standard delle stime dei punti medi della sigmoide (n = 5).
Fig. 2 in Samara water absorption and floatation in sheoaks, Casuarina and Allocasuarina (Casuarinaceae)
Fig. 2 - Absorption of water, increasing weight (A) and proportion of water (C), by samaras of five accessions of Casuarina over 48 h: Casuarina cristata (Ccr), C. cunninghamiana (Ccu), C. glauca (Cgl1 and Cgl2) and C. obesa (Cob). Regression lines are for a least squares fit of the model, SamaraWt ~ Time0.5 + 1, and in all cases were significant at p <0.001. Final wet weight (B) and proportion of water (D) of samaras of five accessions of Allocasuarina after being permitted to absorb water for 2 min and then air dried for 24 h through 10 wetting cycles: Allocasuarina acutivalvis (Aac), A. huegeliana (Ahu), A. muelleriana (Amu), and A. verticillata (Ave1 and Ave2). Regression lines are for a nonlinear least squares fit of the model, SamaraWt ~ SSasymp(Cycle, Asym, R0, lrc), where SSasymp is a self-start model to evaluate the asymptotic regression and its gradient in the R package "lme4" (Bates et al., 2015). In all cases, asymptotes (Asym) were significant at p <0.001. / Assorbimento di acqua, aumento di peso (A) e proporzione di acqua (C) in samare di cinque campioni di Casuarina in 48 h: Casuarina cristata (Ccr), C. cunninghamiana (Ccu), C. glauca (Cgl1 e Cgl2) e C. obesa (Cob). Le linee di regressione sono per un'approssimazione ai minimi quadrati del modello non lineare, SamaraWt ~ Time0.5 + 1, e in tutti i casi erano significativi a p <0,001. Peso umido finale (B) e proporzione di acqua (D) di samara di cinque campioni di Allocasuarina dopo avere assorbito acqua per 2 min e poi essere asciugati all'aria per 24 h attraverso 10 cicli di idratazione: Allocasuarina acutivalvis (Aac), A. huegeliana (Ahu), A. muelleriana (Amu) e A. verticillata (Ave1 e Ave2). Linee di regressione sono per un un'approssimazione ai minimi quadrati del modello non lineare, SamaraWt ~ SSasymp(Cycle, Asym, R0, lrc), dove SSasymp è un modello di auto-avvio per valutare la regressione asintotica e il suo gradiente nel pacchetto R "lme4" (Bates et al., 2015). In tutti i casi gli asintoti (Asym) erano significativi a p <0,001.
Toward liquid cell quantum sensing: Ytterbium complexes with ultra-narrow absorption
<p>The energetic disorder induced by fluctuating liquid environments acts in opposition to the precise control required for coherence-based sensing. Overcoming fluctuations requires a protected quantum subspace that only weakly interacts with the local environment. We reported a ytterbium complex that exhibited an ultra-narrow absorption linewidth in solution at room temperature with a full-width at half-maximum of 0.625 meV. Using spectral hole-burning, we measured an even narrower linewidth of 410 peV at 77 K. Narrow linewidths allowed low-field magnetic circular dichroism at room temperature, used to sense Earth-scale magnetic fields. These results demonstrated that ligand protection in lanthanide complexes could significantly diminish electronic state fluctuations. We termed this system an 'atom-like molecular sensor' (ALMS) and proposed approaches to improve its performance.</p>
Numerical dataset for the article "Single-photon absorption by single photosynthetic light-harvesting complexes"
<p>The numerical data for all figures presented in the article "Single-photon absorption by single photosynthetic light-harvesting complexes" published in the Journal of Physics B: Atomic, Molecular and Optical Physics (2018). Data include calculation runtimes and hardware specification, and are provided in csv. format.</p>
Model results for `Surface pond energy absorption across four Himalayan glaciers accounts for 1/8 of total catchment ice loss'
<p>Model setup (setup.mat) and outputs (allkeyres.mat, postproc.mat) for 5000 runs of Monte Carlo supraglacial pond energy-balance modelling in the Langtang catchment of Nepal. The full set of results are included for the median model run (run_..._n1645.zip).</p> <p>Also included are flux gate results for calculation of emergence velocity (fgates...zip).</p>
The optical absorption in semiconductor to semimetal PtSe2 arises from direct transitions - Supporting data
<p>Data supporting the findings of the work:</p> <p>M. Tharrault, S. Ayari, M. Arfaoui, E. Desgué, R. Le Goff, P. Morfin, J. Palomo, M. Rosticher, S. Jaziri, B. Plaçais, P. Legagneux, F. Carosella, C. Voisin, R. Ferreira and E. Baudin, <strong>The optical absorption in semiconductor to semimetal PtSe2 arises from direct transitions</strong><em>, <a href="https://doi.org/10.48550/arXiv.2311.01847">arXiv:2311.01847 [cond-mat.mtrl-sci]</a></em>.</p> <p> </p> <p>The sample names in this study match those used in the <strong>Raman spectroscopy focused study</strong> <a href="https://doi.org/10.1088/2053-1583/ad1e79">https://doi.org/10.1088/2053-1583/ad1e79</a>. Data from that study can be accessed at <a href="https://doi.org/10.5281/zenodo.8256907">https://doi.org/10.5281/zenodo.8256907</a>.</p> <p>See the Supplemental Material for extra details.</p> <p> </p> <p>Files available:</p> <p><strong>Optical absorption spectroscopy.zip:</strong> reflectance, transmittance, real and imaginary 2D optical conductivity for exfoliated and MBE samples.</p> <p><strong>Differential reflectance with temperature.zip:</strong> differential reflectance Delta R / R pour 4 exfoliated thin samples and temperatures from 290K to 440K.</p> <p><strong>Layers label attribution.txt:</strong> number of layers for each sample.</p> <p><strong>Selected samples fig1.txt: </strong>list of samples displayed in the figure 1 of the publication.</p> <p><strong>Band diagrams.zip:</strong> Band diagrams for GGA-computed 1-12L and AB stacked bilayers as well as GW and HSE06 computed 1L and the k-points path used for the diagrams.</p> <p><strong>Optical conductivity DFT.zip:</strong> real 2D optical conductivity and jDOS computed using GGA-IPA for 1-12L and AB stacked bilayers.</p> <p><strong>Optical absorption 1L different models.csv:</strong> GGA-IPA, GW-IPA, GW-BSE and HSE06-IPA real 2D optical conductivities for the monolayer.</p> <p><strong>1L optical absorption with temperature DFT.csv</strong>: 2D real optical conductivity of 1L PtSe2 computed with EPW/ZG Quantum Espresso package for T = 0 K to 450 K.</p> <p><strong>1L electronic spectral function with temperature.zip:</strong> electronic spectral function for 1L PtSe2 for T = 0, 300 and 450 K.</p> <p><strong>Atomic orbitals decomposition.zip:</strong> band diagrams and the corresponding orbital components, as displayed in Supplemental Material.</p> <p><strong>Electronic bandgap correction.txt:</strong> GGA computed bandgaps and corrected by the energy shift.</p>
Supplementary data for "Collision-induced absorptions by pure CO2 in the infrared: New measurements in the 1150–4500 cm−1 spectral range and empirical modeling for applications" published in Icarus. https://doi.org/10.1016/j.icarus.2024.116265
<p>Supplementary data for the paper entitled ""Collision-induced absorptions by pure CO2 in the infrared: New measurements in the 1150–4500 cm−1 spectral range and empirical modeling for applications" published in <em>Icarus</em>. https://doi.org/10.1016/j.icarus.2024.116265</p> <p>These data files contain the coefficients needed to compute the shape of a pure CO2 CIA band at a given temperature (see Eq. (3)) of the paper https://doi.org/10.1016/j.icarus.2024.116265</p> <p>"CIA_shape_coeff.dat" involves a CIA band shape without dimer signatures </p> <p>"CIA_dimer_shape_coeff.dat" involves a CIA band shape with dimer signatures </p> <p>"CIA_Fermi_doublet_shape_coeff.dat" involves the Fermi doublet band shape</p> <p>First column is wavenumber in cm-1, the rest of the columns contain the coefficients.</p>
Acid fractionation during carbonate digestion with phosphoric acid – Assessment of two different techniques applied for clumped and stable isotope analysis using a Tuneable Infrared Laser Differential Absorption Spectrometer (TILDAS) [dataset]
<p>Date files : </p> <table> <tbody> <tr> <td> <p>Data 1 (Relationship between Mixing ratio difference of sample and WRG and D638 value).xlsx;Data 2 (Role of bulk isotope composition (δ628 & δ636) on Δ638).xlsx;Data 3 (CDES scale conversion).xlsx;Data 4 (VPDB scale conversion for d628 and d636).xlsx;Data 5 (Reference material values).xlsx;Data 6 (Break seal method acid fractionation factor of calcite).xlsx;Data 7 (IAB method acid fractionation factor of calcite).xlsx</p> </td> </tr> </tbody> </table>
Source-specific light absorption by carbonaceous components in the complex aerosol matrix from yearly filter-based measurements
<p>Data presented in the main figures of the peer-reviewed journal article "Source-specific light absorption by carbonaceous components in the complex aerosol matrix from yearly filter-based measurements" by Moschos et al. (2021) in <em>Atmospheric Chemistry and Physics</em> (https://doi.org/10.5194/acp-2020-1293).</p>
Reproduction package for the article "Accretion disc cooling and narrow absorption lines in the tidal disruption event AT 2019dsg"
<p>This is the reproduction package for the MNRAS Article "Accretion disc cooling and narrow absorption lines in the tidal disruption event AT 2019dsg" by Cannizzaro et al (2021). It contains the reduced optical data, the scripts used for the emission lines fitting and the code used to perform the host galaxy subtraction.</p>
Insights from Transient Absorption Spectroscopy into Electron Dynamics Along the Ga-Gradient in Cu(In,Ga)Se2 Solar Cells: Data
<p>Excel file with data to all figures published in our article found at https://doi.org/10.1002/aenm.202003446 (Advanced Energy Materials), Synopsis user manual, Matlab code to analyse and fit data</p> <p> </p>
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Allen Brain Atlas
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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.
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OpenNeuro
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