Find research datasets worth reusing
Search datasets from major research repositories and use ShareScore to quickly assess how well each record supports discovery, access, and reuse.
48
datasets available to search
ShareScore release 0.9.0
Dataset results
48 results for “ELF”
ELF dielectric functions for various materials.
<p><strong>Data for the energy loss function (ELF) of selected materials compiled from various publications.</strong></p> <p>The imaginary part of the inverse of the dielectric function, <em>Im</em>{−1/ε(<em>k</em>,hω)}, denoted the energy loss function (ELF), is the leading function that describes the material response to account for energy losses of swift electrons in matter. For this reason, it is a practical advantage to express the dielectric function in the form of a parametrized ELF, instead of the dielectric function itself, as input for the calculation of inelastic scattering cross sections. Here the ELF is expressed as a sum of Drude-Lindhard type oscillators (see e.g. Yubero F, Sanz JM, Ramskov B, Tougaard S. Model for quantitative analysis of reflection-electron-energy-loss spectra: Angular dependence. Phys Rev B. 1996;53:9719-9727)</p> <p><strong>The ELF data describe the dielectric properties of materials.</strong><br> It may be applied to calculate energy loss processes of fast electrons moving in a material as well as in geometries met in REELS, XPS and AES where the effect of the surface and a static core hole are included (see e.g. QUEELS-software that can be downloaded at: doi: 10.5281/zenodo.6022426)</p> <p><strong>The data structure is:</strong><br> For each material, a reference to the data for each material is given<br> After a line with @ , the ELF data follows in lines with the following meaning</p> <p>1. Excitation parameters ac, bc to model core excitations (see Penn, J. Elec. Spectr., 9(1976)29).<br> When ac = 0.001 and bc = -2: no data was available. </p> <p>2. Energy gap (eV)</p> <p>3. Refractive Index</p> <p>in the next lines, are the parameters for the oscillators: one line for each oscillator</p> <p>4. energy position (eV), intensity (eV^2), width (eV), alpha<br> 5.<br> 6.<br> .<br> .</p> <p>Examples of data files that can be directly read by QUEELS for Au and Si are seen in the files ELF_Au.txt and ELF_Si.txt respectively.</p>
The Sonora Substellar Atmosphere Models. IV. Elf Owl: Atmospheric Mixing and Chemical Disequilibrium with Varying Metallicity and C/O Ratios (T- type Models)
<ul> <li><strong>Overview of V2: "The Sonora Substellar Atmosphere Models. V: A Correction to the Disequilibrium Abundance of CO2 for Sonora Elf Owl"</strong></li> </ul> <p> Version 2 of the Sonora Elf Owl Models updates the CO2 and PH3 abundances and spectra. As described in the Wogan et al. (2024) research note (URL OF NOTE GOES HERE), Version 1 of the models did not apply the CO2 quench approximation properly resulting in predicted CO2 abundances that were too small by several orders of magintude in some cases. Version 2 fixes this mistake, updating CO2 abundances and the emission spectra to reflect the new CO2 abundances. Version 2 also removes all spectra contributions of PH3 because Version 1 consistently contained too much PH3 absorption when compared to JWST data (Veiler et al. 2024, <a href="http://doi.org/10.3847/1538-4357/ad6759" target="_blank" rel="noopener noreferrer">http://doi.org/10.3847/1538-4357/ad6759</a>).</p> <p> </p> <ul> <li><strong>Overview of V1</strong></li> </ul> <p> The Sonora Elf Owl Models is a successor to the <a href="../records/5063476#:~:text=This%20particular%20set%20of%20model,g%20are%200.25%20or%200.5.">Sonora Bobcat</a> and <a href="../records/4450269">Sonora Cholla</a> models. The Sonora Elf Owl model grid includes cloud-free radiative-convective equilibrium model atmospheres with vertical mixing induced disequilibrium chemistry with sub-solar to super-solar atmospheric metallicities and Carbon-to-Oxygen ratio. The atmospheric models have been computed using the open-source radiative-convective equilibrium model <a href="https://natashabatalha.github.io/picaso/">PICASO</a>. The parameters included within this grid are effective temperature (<strong><em>Teff</em></strong>), gravity (<strong><em>log(g)</em></strong>), vertical eddy diffusion coefficient (<strong><em>log(Kzz)</em></strong>), atmospheric metallicity (<strong><em>[M/H]</em></strong>), and Carbon-to-Oxygen ratio (<strong><em>C/O</em></strong>).</p> <p>The ranges and increments of these parameters are described in the published paper.<br><br></p> <ul> <li><strong>Three grids available on three links</strong></li> </ul> <p><strong> The model grid has been presented using three Zenodo repositories. This repository has all the models between 575 to 1200 K (applicable for T- type objects). The models for Teff between 275 to 550 K (applicable for Y- type objects) are available in the Zenodo DOI :- <a href="../records/10381250">https://zenodo.org/records/10381250</a>. The models for Teff between 1300 to 2400 K (applicable for L- type objects) are available in the Zenodo DOI :- <a href="../records/10385987">https://zenodo.org/records/10385987</a>.</strong></p> <p> </p> <ul> <li><strong> File types and how to use them</strong></li> </ul> <p> The models have been presented in the Xarray format so that all the atmospheric properties including the T(P) profile, atmospheric chemistry, and thermal emission spectra can be accessed within the same files. A python based Jupyter notebook named "Reading and plotting Elf Owl Models.ipynb" has been also supplied which demonstrates how to open and use these files.</p> <ul> <li> <strong>Spectra</strong></li> </ul> <p> The emission spectra for each atmospheric model has been computed between 0.6 to 15 microns. The reported flux is in the units of erg/s/cm<sup>2</sup>/cm. Note that these fluxes need to be multiplied with R<sup>2</sup>/D<sup>2</sup> before comparing them with the typically observed flux of brown dwarfs/exoplanets. R is the radius of the object, and D is the distance here.</p> <div> </div> <div> <ul> <li><strong>Note on CH4</strong></li> </ul> </div> <p> As stated in <a href="https://ui.adsabs.harvard.edu/abs/2023ApJ...942...71M/abstract">Mukherjee et al. 2023 </a>our CH4 opacity is derived using the <a href="https://iopscience.iop.org/article/10.3847/1538-4365/ab7a1a">Hargreaves et al. 2020</a> HITEMP line list and computed using the HAPI code (<a href="https://www.sciencedirect.com/science/article/abs/pii/S0022407315302466">Kochanov et al. 2016</a>). HAPI automatically pre-weights the isotopologues according to earth abundances that are listed on the HITRAN website (<a href="https://hitran.org/lbl/2?6=on" target="_blank" rel="noopener noreferrer">see here for CH4</a>). Therefore, users should note that there will be minor features of CH3D included in the models. Given the general absence of deuterated molecules in brown dwarfs (Teff>~300) we will include a second posting of models which includes the Elf Owl grid with <strong>only</strong> the major CH4 isotopologue (12C-H4).</p> <div> <ul> <li><strong>Note on PH3</strong></li> </ul> </div> <p> PH3 abundance is treated separately from the general disequilibrium scheme. This is because of the current non-detection of PH3 in many brown dwarf atmospheres (see citations in paper). The current PH3 treatment uses the chemical equilibrium treatment described in Visscher et al. However, after publishing this grid and using the model for analysis of high precision JWST data, we noticed that even the simple chemical equilibrium treatment which reduces the abundance, introduces a noticeable PH3 feature. Therefore in our v2 of this model grid we will further diminish the abundance.</p>
The Sonora Substellar Atmosphere Models. IV. Elf Owl: Atmospheric Mixing and Chemical Disequilibrium with Varying Metallicity and C/O Ratios (L- type Models)
<ul> <li><strong>Overview of V2: "The Sonora Substellar Atmosphere Models. V: A Correction to the Disequilibrium Abundance of CO2 for Sonora Elf Owl"</strong></li> </ul> <p> Version 2 of the Sonora Elf Owl Models updates the CO2 and PH3 abundances and spectra. As described in the Wogan et al. (2024) research note (URL OF NOTE GOES HERE), Version 1 of the models did not apply the CO2 quench approximation properly resulting in predicted CO2 abundances that were too small by several orders of magintude in some cases. Version 2 fixes this mistake, updating CO2 abundances and the emission spectra to reflect the new CO2 abundances. Version 2 also removes all spectra contributions of PH3 because Version 1 consistently contained too much PH3 absorption when compared to JWST data (Veiler et al. 2024, <a href="http://doi.org/10.3847/1538-4357/ad6759" target="_blank" rel="noopener noreferrer">http://doi.org/10.3847/1538-4357/ad6759</a>).</p> <p> </p> <ul> <li><strong>Overview of V1</strong></li> </ul> <p> The Sonora Elf Owl Models is a successor to the <a href="../records/5063476#:~:text=This%20particular%20set%20of%20model,g%20are%200.25%20or%200.5.">Sonora Bobcat</a> and <a href="../records/4450269">Sonora Cholla</a> models. The Sonora Elf Owl model grid includes cloud-free radiative-convective equilibrium model atmospheres with vertical mixing induced disequilibrium chemistry with sub-solar to super-solar atmospheric metallicities and Carbon-to-Oxygen ratio. The atmospheric models have been computed using the open-source radiative-convective equilibrium model <a href="https://natashabatalha.github.io/picaso/">PICASO</a>. The parameters included within this grid are effective temperature (<strong><em>Teff</em></strong>), gravity (<strong><em>log(g)</em></strong>), vertical eddy diffusion coefficient (<strong><em>log(Kzz)</em></strong>), atmospheric metallicity (<strong><em>[M/H]</em></strong>), and Carbon-to-Oxygen ratio (<strong><em>C/O</em></strong>).</p> <p>The ranges and increments of these parameters are described in the published paper.<br><br></p> <ul> <li><strong>Three grids available on three links</strong></li> </ul> <p><strong> The model grid has been presented using three Zenodo repositories. This repository has all the models between 1300 to 2400 K (applicable for L- type objects). The models for Teff between 275 to 550 K (applicable for Y- type objects) are available in the Zenodo DOI :- <a href="../records/10381250">https://zenodo.org/records/10381250</a>. The models for Teff between 575 to 1200 K (applicable for T- type objects) are available in the Zenodo DOI :- <a href="../records/10385821">https://zenodo.org/records/10385821</a>.</strong></p> <p> </p> <ul> <li><strong> File types and how to use them</strong></li> </ul> <p> The models have been presented in the Xarray format so that all the atmospheric properties including the T(P) profile, atmospheric chemistry, and thermal emission spectra can be accessed within the same files. A python based Jupyter notebook named "Reading and plotting Elf Owl Models.ipynb" has been also supplied which demonstrates how to open and use these files.</p> <ul> <li> <strong>Spectra</strong></li> </ul> <p> The emission spectra for each atmospheric model has been computed between 0.6 to 15 microns. The reported flux is in the units of erg/s/cm<sup>2</sup>/cm. Note that these fluxes need to be multiplied with R<sup>2</sup>/D<sup>2</sup> before comparing them with the typically observed flux of brown dwarfs/exoplanets. R is the radius of the object, and D is the distance here.</p> <div> </div> <div> <ul> <li><strong>Note on CH4</strong></li> </ul> </div> <p> As stated in <a href="https://ui.adsabs.harvard.edu/abs/2023ApJ...942...71M/abstract">Mukherjee et al. 2023 </a>our CH4 opacity is derived using the <a href="https://iopscience.iop.org/article/10.3847/1538-4365/ab7a1a">Hargreaves et al. 2020 </a>HITEMP line list and computed using the HAPI code (<a href="https://www.sciencedirect.com/science/article/abs/pii/S0022407315302466">Kochanov et al. 2016</a>). HAPI automatically pre-weights the isotopologues according to earth abundances that are listed on the HITRAN website (<a href="https://hitran.org/lbl/2?6=on" target="_blank" rel="noopener noreferrer">see here for CH4</a>). Therefore, users should note that there will be minor features of CH3D included in the models. Given the general absence of deuterated molecules in brown dwarfs (Teff>~300) we will include a second posting of models which includes the Elf Owl grid with <strong>only</strong> the major CH4 isotopologue (12C-H4).</p> <div> <ul> <li><strong>Note on PH3</strong></li> </ul> </div> <p> In v1, PH3 abundance was treated separately from the general disequilibrium scheme. This is because of the current non-detection of PH3 in many brown dwarf atmospheres (see citations in paper). The current PH3 treatment uses the chemical equilibrium treatment described in Visscher et al. However, after publishing this grid and using the model for analysis of high precision JWST data, we noticed that even the simple chemical equilibrium treatment which reduces the abundance, introduces a noticeable PH3 feature. In v2 we completely remove the contribution of PH3. </p>
Transkripte von elf Video-Ansprachen der Schweizer Regierung vor Volksabstimmungen. Transcripts of Eleven TV Addresses Given by the Swiss Government before Popular Votes
<p>Der Datensatz enthält Transkripte (doc, html, pdf, txt) von elf TV-Ansprachen der Schweizer Regierung vor Volksabstimmungen. Die Ansprachen wurden nach GAT 2 transkribiert. / The dataset contains transcripts (doc, html, pdf, txt) of eleven TV addresses given by the Swiss government before popular votes. The addresses were transcribed according to GAT 2.</p> <p> </p> <p><strong>Quellenangabe der Transkripte / Reference to the Transcripts</strong></p> <p>Schröter, Juliane, Keller, Stefan, 2018. Transkripte von elf Video-Ansprachen der Schweizer Regierung vor Volksabstimmungen. Transcripts of Eleven TV Addresses Given by the Swiss Government before Popular Votes. doi: 10.5281/zenodo.1324476.</p> <p><em>Falls Sie sich nur auf eines oder einige der elf Transkripte beziehen, passen Sie die Quellenangabe bitte entsprechend an. / If you are only referring to one or some of the eleven transcripts, please adopt the reference accordingly. </em></p> <p><em>Disclaimer: Die Mitglieder des Bundesrates haben mündliche Ansprachen gehalten. </em><em>Für den Wortlaut der Transkripte sind sie nicht verantwortlich. / The members of the Federal Council have delivered oral addresses. They are not responsible for the wording of the transcripts.</em></p> <p> </p> <p><strong>Quellenangaben der Videos / References to the Videos</strong></p> <p>Bundesrat, 2017a. [TV-Ansprache zum] Bundesgesetz „Unternehmenssteuerreform III“. Produziert von SRG SSR. <a href="https://www.admin.ch/gov/de/start/dokumentation/abstimmungen/20170212/bundesgesetz-ueber-steuerliche-massnahmen-zur-staerkung-der-wett.html">https://www.admin.ch/gov/de/start/dokumentation/abstimmungen/20170212/bundesgesetz-ueber-steuerliche-massnahmen-zur-staerkung-der-wett.html</a> (Abfrage: 23.05.2018).<br> <br> Bundesrat, 2017b. [TV-Ansprache zum] Energiegesetz. Produziert von SRG SSR. <a href="https://www.admin.ch/gov/de/start/dokumentation/abstimmungen/20170521/Energiegesetz.html">https://www.admin.ch/gov/de/start/dokumentation/abstimmungen/20170521/Energiegesetz.html</a> (Abfrage: 23.05.2018).<br> <br> Bundesrat, 2016. [TV-Ansprache zur] Initiative „Für Ehe und Familie gegen die Heiratsstrafe“. Produziert von SRG SSR. <a href="https://www.srf.ch/play/tv/abstimmungen-teilw--in-gebaerdensprache/video/vorlage-heiratsstrafe-sendung-mit-gebaerdensprache?id=8e482ca4-52e3-4777-b956-529ce64f96d1">https://www.srf.ch/play/tv/abstimmungen-teilw--in-gebaerdensprache/video/vorlage-heiratsstrafe-sendung-mit-gebaerdensprache?id=8e482ca4-52e3-4777-b956-529ce64f96d1</a> (Abfrage: 23.05.2018).<br> <br> Bundesrat, 2015a. [TV-Ansprache zur] Änderung des Bundesgesetzes über Radio und Fernsehen. Produziert von SRG SSR. <a href="https://www.srf.ch/play/tv/abstimmungen/video/br-ansprache-zum-rtvg?id=dd58817b-235b-472a-96a2-a67c721e6775&station=69e8ac16-4327-4af4-b873-fd5cd6e895a7">https://www.srf.ch/play/tv/abstimmungen/video/br-ansprache-zum-rtvg?id=dd58817b-235b-472a-96a2-a67c721e6775&station=69e8ac16-4327-4af4-b873-fd5cd6e895a7</a> (Abfrage: 23.05.2018).<br> <br> Bundesrat, 2015b. [TV-Ansprache zur] Präimplantationsdiagnostik. Produziert von SRG SSR. <a href="https://www.srf.ch/play/tv/ansprachen-bundesrat-in-gebaerdensprache/video/br-ueli-maurer-zum-fortpflanzungsmedizingesetz-fmedg-geb-?id=cbbecc0d-c210-41a9-8190-4d282926c3a8&station=69e8ac16-4327-4af4-b873-fd5cd6e895a7">https://www.srf.ch/play/tv/ansprachen-bundesrat-in-gebaerdensprache/video/br-ueli-maurer-zum-fortpflanzungsmedizingesetz-fmedg-geb-?id=cbbecc0d-c210-41a9-8190-4d282926c3a8&station=69e8ac16-4327-4af4-b873-fd5cd6e895a7</a> (Abfrage: 23.05.2018).<br> <br> Bundesrat, 2014a. [TV-Ansprache zur] Beschaffung des Kampfflugzeuges Gripen. Produziert von SRG SSR. <a href="https://www.srf.ch/play/tv/abstimmungen/video/bundesrat-ueli-maurer-zur-beschaffung-des-kampfflugzeuges-gripen?id=febd8e03-d4c3-42e7-b163-37e9e0d0176c&station=69e8ac16-4327-4af4-b873-fd5cd6e895a7">https://www.srf.ch/play/tv/abstimmungen/video/bundesrat-ueli-maurer-zur-beschaffung-des-kampfflugzeuges-gripen?id=febd8e03-d4c3-42e7-b163-37e9e0d0176c&station=69e8ac16-4327-4af4-b873-fd5cd6e895a7</a> (Abfrage: 23.05.2018).<br> <br> Bundesrat, 2014b. [TV-Ansprache zur] Initiative „Für den Schutz fairer Löhne“. Produziert von SRG SSR. <a href="https://www.srf.ch/play/tv/abstimmungen-teilw--in-gebaerdensprache/video/ansprache-von-bundesrat-johann-schneider-ammann-vom-20-04-2014?id=3ea16bd4-401d-4d68-9d06-b07b83582405">https://www.srf.ch/play/tv/abstimmungen-teilw--in-gebaerdensprache/video/ansprache-von-bundesrat-johann-schneider-ammann-vom-20-04-2014?id=3ea16bd4-401d-4d68-9d06-b07b83582405</a> (Abfrage: 23.05.2018).<br> <br> Bundesrat, 2014c. [TV-Ansprache zur] Initiative „Gegen Masseneinwanderung“. Produziert von SRG SSR. <a href="https://www.youtube.com/watch?v=A91gPrFXFCs">https://www.youtube.com/watch?v=A91gPrFXFCs</a> (Abfrage: 23.05.2018).<br> <br> Bundesrat, 2014d. [TV-Ansprache zur] Initiative „Pädophile sollen nicht mehr mit Kindern arbeiten dürfen“. Produziert von SRG SSR. <a href="https://www.bk.admin.ch/bk/de/home/dokumentation/volksabstimmungen/volksabstimmung-20140518.html">https://www.bk.admin.ch/bk/de/home/dokumentation/volksabstimmungen/volksabstimmung-20140518.html</a> (Abfrage: 18.04.2018).<br> <br> Bundesrat, 2013. [TV-Ansprache zum] Bundesbeschluss über die Familienpolitik. Produziert von SRG SSR. Video bereitgestellt von SRG SSR.<br> <br> Bundesrat, 2010. [TV-Ansprache] Zur Ausschaffungsinitiative und zum Gegenentwurf des Bundesrates. Produziert von SRG SSR. Video bereitgestellt von SRG SSR.</p> <p> </p> <p><strong>Quellenangabe des Transkriptionssystems / Reference to the Conventions of Transcription</strong></p> <p>Selting, Margret, Auer, Peter, Barth-Weingarten, Dagmar et al., 2009. Gesprächsanalytisches Transkriptionssystem 2 (GAT 2). Gesprächsforschung 10, 353-402.</p>
Abb. 1-6 in Elf neue Clytini und Anaglyptini aus Malaysien und Indonesien (Coleoptera, Cerambycidae, Cerambycinae)
Abb. 1-6: (1) Rhaphuma shelfordi nov.sp. (HT, dorsal); (2) Demonax jirouxi nov.sp. (HT, dorsal); (3) Demonax alboapicalis nov.sp. (HT, dorsal); (4) Demonax stenideus nov.sp. (HT, dorsal); (5) Demonax brevefasciatus nov.sp. (HT, dorsal); (6) Demonax truncatus nov.sp. (HT, dorsal).
The ELF WERA stations measurements used in the paper "TGF 181010 study using extremely low frequency electromagnetic waves" by V. Marchenko, J. Mlynarczyk, M. Ostrowski, A. Kulak, O. Senchenko, J. Kubisz, A. Michalec, J. Salvador, N. Diaz
<p>The data analyzed in the paper are provided as text files containing measurements of two stations of the WERA project:</p> <p>File "TGF181010_Hylaty_201810101300.txt" - from the Hylaty station in Poland, </p> <p>File "TGF181010_Patagonia_201810101300.txt" - from the Patagonia station in Argentina.</p> <p>In each file the first column provides time, as measured in seconds since October 10, 2018, 13:00 UT. The second and third columns provide signals from NS and EW magnetic antennas. The duration of each data set is 5 min. The time accuracy for the Hylaty station is below 1 ms and for the Patagonia station up to several ms.</p>
Table S1. The influence of extremely low frequency magnetic field (ELF-MF) on different aspects of the organism function
<p><strong>Table S1.</strong> <strong>The influence of extremely low frequency magnetic field (ELF-MF) on different aspects of the organism function</strong> (papers are listed according to year of publication).</p> <p>In order to prepare the table the bibliography research in PubMed was performed using the following keywords in varied combinations:: “electromagnetic field”, “stress”, “corticosterone“, “noradrenaline”, “HPA axis”, “oxidative stress”, “cellular damage”, “BDNF”, “HSP70”, “neurotransmitters”, “cytokines”, “plasticity”, “viability”, “recovery”; “behavior”. We also used Boolean operator “and” to receive the most relevant search results. All articles written in English were manually screened, and the appropriate were identified. The articles published from 2010 to 2020 were taken into consideration. The papers concerning the effects of extremely low frequency magnetic field on a wide spectrum of molecular, neuronal, hormonal and behavioural stress responses were considered and only information related to ELF-MF effects are included in the Table.</p>
elf_bow
fantasy bow elfs bow made by me turn cycles in blender to see the best resolution Source: Objaverse 1.0 / Sketchfab
The Sonora Substellar Atmosphere Models. IV. Elf Owl: Atmospheric Mixing and Chemical Disequilibrium with Varying Metallicity and C/O Ratios (Y- type Models)
<ul> <li><strong>Overview of V2: "The Sonora Substellar Atmosphere Models. V: A Correction to the Disequilibrium Abundance of CO2 for Sonora Elf Owl"</strong></li> </ul> <p> Version 2 of the Sonora Elf Owl Models updates the CO2 and PH3 abundances and spectra. As described in the Wogan et al. (2024) research note (URL OF NOTE GOES HERE), Version 1 of the models did not apply the CO2 quench approximation properly resulting in predicted CO2 abundances that were too small by several orders of magintude in some cases. Version 2 fixes this mistake, updating CO2 abundances and the emission spectra to reflect the new CO2 abundances. Version 2 also removes all spectra contributions of PH3 because Version 1 consistently contained too much PH3 absorption when compared to JWST data (Veiler et al. 2024, <a href="http://doi.org/10.3847/1538-4357/ad6759" target="_blank" rel="noopener noreferrer">http://doi.org/10.3847/1538-4357/ad6759</a>).</p> <ul> <li><strong>Overview of V1</strong></li> </ul> <p> The Sonora Elf Owl Models is a successor to the <a href="../records/5063476#:~:text=This%20particular%20set%20of%20model,g%20are%200.25%20or%200.5.">Sonora Bobcat</a> and <a href="../records/4450269">Sonora Cholla</a> models. The Sonora Elf Owl model grid includes cloud-free radiative-convective equilibrium model atmospheres with vertical mixing induced disequilibrium chemistry with sub-solar to super-solar atmospheric metallicities and Carbon-to-Oxygen ratio. The atmospheric models have been computed using the open-source radiative-convective equilibrium model <a href="https://natashabatalha.github.io/picaso/">PICASO</a>. The parameters included within this grid are effective temperature (<strong><em>Teff</em></strong>), gravity (<strong><em>log(g)</em></strong>), vertical eddy diffusion coefficient (<strong><em>log(Kzz)</em></strong>), atmospheric metallicity (<strong><em>[M/H]</em></strong>), and Carbon-to-Oxygen ratio (<strong><em>C/O</em></strong>).</p> <p>The ranges and increments of these parameters are described in the published paper.<br><br></p> <ul> <li><strong>Three grids available on three links</strong></li> </ul> <p><strong> The model grid has been presented using three Zenodo repositories. This repository has all the models between Teff of 275 to 550 K (applicable to Y-type objects). The models for Teff between 575 to 1200 K (applicable for T- type objects) are available in the Zenodo DOI :- <a href="../records/10385821">https://zenodo.org/records/10385821</a>. The models for Teff between 1300 to 2400 K (applicable for L- type objects) are available in the Zenodo DOI :- <a href="../records/10385987">https://zenodo.org/records/10385987</a>.</strong></p> <p> </p> <ul> <li><strong> File types and how to use them</strong></li> </ul> <p> The models have been presented in the Xarray format so that all the atmospheric properties including the T(P) profile, atmospheric chemistry, and thermal emission spectra can be accessed within the same files. A python based Jupyter notebook named "Reading and plotting Elf Owl Models.ipynb" has been also supplied which demonstrates how to open and use these files.</p> <ul> <li> <strong>Spectra</strong></li> </ul> <p> The emission spectra for each atmospheric model has been computed between 0.6 to 15 microns. The reported flux is in the units of erg/s/cm<sup>2</sup>/cm. Note that these fluxes need to be multiplied with R<sup>2</sup>/D<sup>2</sup> before comparing them with the typically observed flux of brown dwarfs/exoplanets. R is the radius of the object, and D is the distance here.</p> <div> </div> <div> <ul> <li><strong>Note on CH4</strong></li> </ul> </div> <p> As stated in <a href="https://ui.adsabs.harvard.edu/abs/2023ApJ...942...71M/abstract">Mukherjee et al. 2023 </a>our CH4 opacity is derived using the <a href="https://iopscience.iop.org/article/10.3847/1538-4365/ab7a1a">Hargreaves et al. 2020</a> HITEMP line list and computed using the HAPI code (<a href="https://www.sciencedirect.com/science/article/abs/pii/S0022407315302466">Kochanov et al. 2016</a>). HAPI automatically pre-weights the isotopologues according to earth abundances that are listed on the HITRAN website (<a href="https://hitran.org/lbl/2?6=on" target="_blank" rel="noopener noreferrer">see here for CH4</a>). Therefore, users should note that there will be minor features of CH3D included in the models. Given the general absence of deuterated molecules in brown dwarfs (Teff>~300) we will include a second posting of models which includes the Elf Owl grid with <strong>only</strong> the major CH4 isotopologue (12C-H4).</p> <div> <ul> <li><strong>Note on PH3</strong></li> </ul> </div> <p> PH3 abundance is treated separately from the general disequilibrium scheme. This is because of the current non-detection of PH3 in many brown dwarf atmospheres (see citations in paper). The current PH3 treatment uses the chemical equilibrium treatment described in Visscher et al. However, after publishing this grid and using the model for analysis of high precision JWST data, we noticed that even the simple chemical equilibrium treatment which reduces the abundance, introduces a noticeable PH3 feature. Therefore in our v2 of this model grid we will further diminish the abundance.</p>
The conductivity profile of Earth-ionosphere cavity used in the paper "Finite-difference time-domain analysis of ELF radio wave propagation in the spherical Earth-ionosphere waveguide and its validation based on analytical solutions" by Volodymyr Marchenko, Andrzej Kulak, Janusz Mlynarczyk
<p>The file "Marchenko_FDTD_Paper_Conductivity_Profile.dat" contains the conductivity profile of Earth-ionosphere cavity. The first column provides the altitude (in km) and the second column provides the conductivity (in S/m).</p>
Four-year measurements from Sierra Nevada ELF station. Years 2013, 2017
<p>This folder contains subfolders for the years 2013 (from March, inclusive) and 2017 (January and February) with time domain raw data from the Sierra Nevada ELF station. Each year contains folders for each month, named with the four digits corresponding to year and month, e.g., 1412 stands for the raw data during December 2014. Within each month folder, the data and information files for each sensor and each hour are available. Data are stored in files containing measurements corresponding to a time period of approximately one hour. The filenames begin with a common part, “smplGRTU1_sensor_”, followed by a specific part to denote the sensor used (0 for the NS orientation and 1 for the EW orientation), the date and the initial time of the measurement recorded. For example, smplGRTU1_sensor_0_1412010430, stands for data measured by the NS-oriented magnetometer, in the year 2014, month 12, day 01, hour 04, and starting minute, 30. The information file has the same name but ends with _info.txt. Since the initial time is not fixed, the filenames in each folder are not completely determined. For this reason, each month folder includes two files, 'ficheros0' and 'ficheros1', that contain the set of filenames for that month. Therefore, for each normally measured we have 24 data files and also 24 information files for each sensor. Each hour data file occupies 1.8 MB, so each month has roughly a data volume of 2.6 GB.</p>
Four-year measurements from Sierra Nevada ELF station. Year 2016
<p>This folder contains subfolders for the year 2016 with time domain raw data from the Sierra Nevada ELF station. Each year contains folders for each month, named with the four digits corresponding to year and month, e.g., 1612 stands for the raw data during December 2016. Within each month folder, the data and information files for each sensor and each hour are available. Data are stored in files containing measurements corresponding to a time period of approximately one hour. The filenames begin with a common part, “smplGRTU1_sensor_”, followed by a specific part to denote the sensor used (0 for the NS orientation and 1 for the EW orientation), the date and the initial time of the measurement recorded. For example, smplGRTU1_sensor_0_1412010430, stands for data measured by the NS-oriented magnetometer, in the year 2014, month 12, day 01, hour 04, and starting minute, 30. The information file has the same name but ends with _info.txt. Since the initial time is not fixed, the filenames in each folder are not completely determined. For this reason, each month folder includes two files, 'ficheros0' and 'ficheros1', that contain the set of filenames for that month. Therefore, for each normally measured we have 24 data files and also 24 information files for each sensor. Each hour data file occupies 1.8 MB, so each month has roughly a data volume of 2.6 GB.</p>
Four-year measurements from Sierra Nevada ELF station. Year 2015
<p>This folder contains subfolders for the year 2015 with time domain raw data from the Sierra Nevada ELF station. Each year contains folders for each month, named with the four digits corresponding to year and month, e.g., 1512 stands for the raw data during December 2015. Within each month folder, the data and information files for each sensor and each hour are available. Data are stored in files containing measurements corresponding to a time period of approximately one hour. The filenames begin with a common part, “smplGRTU1_sensor_”, followed by a specific part to denote the sensor used (0 for the NS orientation and 1 for the EW orientation), the date and the initial time of the measurement recorded. For example, smplGRTU1_sensor_0_1412010430, stands for data measured by the NS-oriented magnetometer, in the year 2014, month 12, day 01, hour 04, and starting minute, 30. The information file has the same name but ends with _info.txt. Since the initial time is not fixed, the filenames in each folder are not completely determined. For this reason, each month folder includes two files, 'ficheros0' and 'ficheros1', that contain the set of filenames for that month. Therefore, for each normally measured we have 24 data files and also 24 information files for each sensor. Each hour data file occupies 1.8 MB, so each month has roughly a data volume of 2.6 GB.</p>
Four-year measurements from Sierra Nevada ELF station. Year 2014
<p>This folder contains subfolders for the year 2014 with time domain raw data from the Sierra Nevada ELF station. Each year contains folders for each month, named with the four digits corresponding to year and month, e.g., 1412 stands for the raw data during December 2014. Within each month folder, the data and information files for each sensor and each hour are available. Data are stored in files containing measurements corresponding to a time period of approximately one hour. The filenames begin with a common part, “smplGRTU1_sensor_”, followed by a specific part to denote the sensor used (0 for the NS orientation and 1 for the EW orientation), the date and the initial time of the measurement recorded. For example, smplGRTU1_sensor_0_1412010430, stands for data measured by the NS-oriented magnetometer, in the year 2014, month 12, day 01, hour 04, and starting minute, 30. The information file has the same name but ends with _info.txt. Since the initial time is not fixed, the filenames in each folder are not completely determined. For this reason, each month folder includes two files, 'ficheros0' and 'ficheros1', that contain the set of filenames for that month. Therefore, for each normally measured we have 24 data files and also 24 information files for each sensor. Each hour data file occupies 1.8 MB, so each month has roughly a data volume of 2.6 GB.</p> <p> </p>
Supplementary material 1 from: Pansarin ER, Menezes ELF (2023) A new remarkable Vanilla Mill. (Orchidaceae) species endemic to the Espinhaço Range, Brazil: its phylogenetic position and evolutionary relationships among Neotropical congeners. PhytoKeys 227: 151-165. https://doi.org/10.3897/phytokeys.227.101963
Species of Vanilla included in the molecular study, their locations, vouchers and GenBank accession numbers
Study to Assess the Intrapulmonary Pharmacokinetics of SPR859 by Comparing the Plasma, Epithelial Lining Fluid (ELF), and Alveolar Macrophages (AM) Concentrations Following the Oral Administration of
ClinicalTrials.gov study NCT04710407. IPD Sharing: NO. Countries: 1. Publications: 1.
Effect of Location of Feeding on Glycemic Control in Critically Ill Patients (ELF)
ClinicalTrials.gov study NCT03566992. IPD Sharing: UNDECIDED. Countries: 1. Publications: 4.
Efficacy of Extremely Low Magnetic Field (ELF) in Fibromyalgic Patients
ClinicalTrials.gov study NCT03503760. IPD Sharing: Not stated. Countries: 0. Publications: 8.
Gene expression analysis in the zebrafish fractured scale exposed to ELF-EMFs
GEO Series GSE247669. Danio rerio. 9 samples. Type: Expression profiling by high throughput sequencing.
Transcriptome profiling by RNA-sequencing of the AML cell lines UCSD-AML1 and ELF-153.
GEO Series GSE140347. Homo sapiens. 24 samples. Type: Expression profiling by high throughput sequencing.
ScienceDex guides
Understand access before you commit
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.