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335 results for “Theoretical”
Haloferax volcanii theoretical proteome exported from HaloLex
<p>The theoretical proteome is derived from the annotated Haloferax volcanii DS2 genome (Hartmann et al, 2010).</p> <p>This proteome represents a Gold Standard Protein based annotation (Pfeiffer and Oesterhelt, 2015).</p> <p>Proteome data from Haloferax volcanii were comprehensively analyzed in a community-based effort (Schulze et al, 2020)</p> <p>Various proteome studies are based on versions of this theoretical proteome. Different versions, which are cited in proteome papers, are made available in this series of Zenodo uploads.</p>
Natrialba magadii theoretical proteome exported from HaloLex
<p>The theoretical proteome is derived from the annotated Natrialba magadii ATCC 43099 genome (Siddaramappa et al, 2012).</p> <p>This proteome represents a Gold Standard Protein based annotation (Pfeiffer and Oesterhelt, 2015).</p> <p>This proteome was exported from HaloLex (Pfeiffer et al, 2008)</p> <p>A proteome study is based on this version of the theoretical proteome (Cerletti et al, 2018).</p>
Detailed abundances based on different nuclear physics for theoretical r-process scenarios
<p>This data set contains detailed abundances (at a time t=10^6 years after the event) for individual trajectories for seven different simulations of potential r-process sites, and based on nine different combinations of nuclear mass models and fission fragment distribution models. The data have been used and are discussed in Cote, Eichler, Yagüe, et al. (https://ui.adsabs.harvard.edu/abs/2020arXiv200604833C/abstract) to determine the isotopic ratios of I129/Cm247 and compare them to meteoritic data.</p> <p>Furthermore, a code is included which samples a subset of trajectories reproducing the measured meteoritic I129/Cm247 abundance ratio of 438 +- 92. See the README file and the publication (https://ui.adsabs.harvard.edu/abs/2020arXiv200604833C/abstract) for more details.</p>
Damage Monitoring of Structural Resins Loaded with Carbon Fillers: Experimental and Theoretical Study
<p>Dynamic Mechanical Analysis, Electro-Mechanical Measurement, Simulation model, Dynamic Light Scattering, FTIR spectroscopy</p> <p>Thermogravimetric analysis, Differential Scanning Calorimetry, Electro-Temperature Measurement, </p> <p>Thermal Image Camera , Water sorption measurement, Transmission Electron Microscopy, Stress Strain</p>
Confusion matrices for theoretical young stellar object models
<p>This is a data table supplementing the following publication: </p> <p><em><strong>A framework for modeling the evolution of young stellar objects </strong></em>(Richardson et al. 2025, accepted to ApJ).</p> <p>It contains a set of confusion matrices comparing the evolutionary stages and classes of radiative transfer YSO models selected by proximity to protostellar evolutionary tracks. Models are included in a matrix based on their correspondence to particular modeled accretion histories, zero-age stellar masses, ages, mass accretion efficiencies, and levels of detectability (defined using flux in the ALMA Band 6 wavelength range). Details on the construction and use of the table are contained in the accompanying README file, and more information about the matrices is contained in Section 4.2 of the companion paper.</p> <p>The YSO models populating these matrices are from Richardson et al. (2024); information on them is contained in the <a href="https://ui.adsabs.harvard.edu/abs/2024ApJ...961..188R/abstract" target="_blank" rel="noopener">companion work</a> and <a href="https://zenodo.org/records/10522816" target="_blank" rel="noopener">data release</a>.</p>
(dataset) Interactions of irradiation defects with nitrogen in α-Fe: an integrated experimental and theoretical study
<p>This dataset contains data , simulations and plot scripts in support of the manuscript "<em>Interactions of irradiation defects with nitrogen in <span class="math-tex">\(\alpha\)</span>-Fe: an integrated experimental and theoretical study</em>"</p>
Graph Theoretical Measures of Fast Ripple Networks Support the Epileptic Network Hypothesis
<p>MongoDB JSON files of the (high-frequency oscillation) HFO and electrode databases used for this study and others.</p>
theoretical and experimental study of the deposition of dielectric stacks on twin-hole silica fibers for implementation of compact all-fiber resonators
<p>This dataset includes the Matlab code to engineer theoretically a Bragg stack made of different dielectric layers. By changing the number of alternating stacks, their thickness and the refractive index of each layer it is possible to obtain the transmission curve of the Bragg stack versus the wavelength of the light in a certain range of values. The dataset includes also the experimental measurements of the resonances related to one of the fabricated compact resonators (based on the twin-hole fiber not poled) and obtained sweeping the wavelength of the input light injected through one of the two Bragg stacks and collecting the power at the exit of the other Bragg stack. </p>
Phloem anatomy constraints root system architecture development: theoretical clues from in silico experiments [software and dataset]
<p>Simulation software and results for "<strong>Phloem anatomy constraints root system architecture development: theoretical clues from in silico experiments</strong>"</p>
The SPOTS Models: A Grid of Theoretical Stellar Evolution Tracks and Isochrones For Testing The Effects of Starspots on Structure and Colors
<p><strong>The SPOTS Models: A Grid of Theoretical Stellar Evolution Tracks and Isochrones For Testing The Effects of Starspots on Structure and Colors</strong></p> <p>This repository contains the Stellar Parameters of Tracks with Starspots (SPOTS) grid of theoretical stellar evolutionary tracks and isochrones, presented in Somers, Pinsonneault, and Cao (2020, in prep). Our models were calculated with the Yale Rotating Evolution Code (e.g. van Saders & Pinsonneault, 2013, ApJ 776, 67), including updated which incorporate a treatment of surface starspots (Somers & Pinsonneault, 2015, ApJ 807, 174S). Modelling details can be found in these references. The purpose of this evolutionary suite is to provide the community with state-of-the-art predictions for the influence of starspots and magnetic activity on the structure of stars.</p> <p>The grid includes both isochrones and tracks. They can be downloaded individually from this repository, or in bulk by downloading the .zip files.</p> <p><strong>Isochrones (.isoc):</strong></p> <p>Each isochrone file contains a series of isochrones (stellar properties for a range of masses at fixed age) for ages between 1 Myrs and 4 Gyrs. Each file contains these isochrones for a different surface starspot covering fraction, given by the name of the file -- f000.isoc = 0% covering fraction, f017.isoc = 17% covering fraction, etc. Each isochrone contains several columns with different information, including,</p> <ol> <li>Fundamental properties: mass, age, luminosity, radius, logg, Teff, convective overturn timescale (TauCZ), lithium abundance relative to initial (Li/Li0).</li> <li>Starspot properties: Covering fraction (Fspot), ratio of spot temperature to ambient temperature (Xspot), the temperatures of hot and cool regions (T_hot, T_cool).</li> <li>Two-temperature colors, including Johnson BV, Cousins RI, 2MASS JHK, WISE W1, and Gaia G, BP, RP.</li> </ol> <p>Colors that fell outside of the calibrated range are listed as -99.0.</p> <p><strong>Tracks (.track):</strong></p> <p>We also include individual tracks for every combination of Fspot and Mass considered in the paper. Each .track file lists the mass and starspot covering fraction in the filename -- i.e. m055_f034.track is the model of mass 0.55Msun and with a 34% surface covering fraction. In addition to all the properties included in the isochrones, the track files also include:</p> <ol> <li>The total moment of interia of the model (total_I) and the moment of interia of the surface convection zone (CZ_I)</li> <li>The central and surface hydrogen abundances (X_cen, X_surf) and the surface metallicity (Z/X_surf)</li> <li>The deuterium abundance relative to initial (H2/H2_0)</li> </ol>
Experiments for "Automata Theoretic Approach to Verification of MPLS Networks under Link Failures"
<p><strong>Prerequisites:</strong></p> <ol> <li>A 2020 linux distribution on an x86_64 platform</li> <li>python3 installation with os, sys, json and statistics packages installed for computation of timing statistics</li> <li>pdflatex for visualization of reachability matrices</li> </ol> <p><strong>Contents:</strong></p> <ul> <li>The <em>bin</em> folder contains the pre-compiled binaries for our tool and the backend verifier for pushdown-systems, <em>moped.</em></li> <li>The <em>sources</em> folder contains a snapshot of source-code used for producing the tool binary, namely <ul> <li>AalWiNes, also found at https://github.com/DEIS-Tools/AalWiNes in release v0.92.J (337f1e4c44f8bce2060897b88e706f7ceca38319)</li> <li>PDAAAL, used for pushdown-system manipulation, also found at https://github.com/DEIS-Tools/PDAAAL in release v0.2.2.J (ed1e7fbb4cacd6ffb240a514cfe8472f83d91f60)</li> </ul> </li> <li>The <em>nested</em> folder contains scripts and models for reproducing the results of Table IV</li> <li>The <em>nn-net</em> folder contains scripts and models for constructing reachability-matrices (Table V to Table XII) and operator specific queries</li> <li>Within the <em>nn-net</em> folder, you also find a mapping from alphabetical naming of NORDUnet routers in the paper to numericals <em>(nn-net/index-alpha-map.txt)</em></li> </ul> <p><strong>P-Rex vs HSA (Table IV)</strong></p> <p>We here re-use the HSA-timings computed in <a href="https://doi.org/10.1145/3281411.3281432">https://doi.org/10.1145/3281411.3281432</a></p> <p>The timings for our tool can be obtained by the following commands</p> <pre><code class="language-bash">cd nested ./compute_nested.sh | grep "#"</code></pre> <p>which should compute a sequence of lines in the terminal equal to</p> <pre><code class="language-bash">### Running N0 with aalwines ### Memory: 27064 Kb Time 0.02 seconds ### Running N1 with aalwines ### Memory: 37404 Kb Time 0.03 seconds ### Running N2 with aalwines ### Memory: 47704 Kb Time 0.03 seconds ### Running N3 with aalwines ### Memory: 57784 Kb Time 0.04 seconds ### Running N4 with aalwines ### Memory: 68368 Kb Time 0.04 seconds ### Running N5 with aalwines ### Memory: 78468 Kb Time 0.05 seconds ### Running N6 with aalwines ### Memory: 88980 Kb Time 0.06 seconds </code></pre> <p><strong>Operator Queries</strong></p> <p>The experiments on the queries of the operators can be computed via the commands</p> <pre><code class="language-bash">cd nn-net ./compute_operator.sh </code></pre> <p>which should complete less than 10 minutes.</p> <p>The traces and timings are outputted directly to the terminal.</p> <p><strong>Reachability Matrices (Table V to Table XII)</strong></p> <p>This package folder comes pre-populated with the raw computation results. Notice that the <em>compute_grid.sh</em> command will invalidate these results.</p> <p>To compute the full set of reachability tables, you can use the following commands</p> <pre><code class="language-bash">cd nn-net ./make_queries.sh ./compute_grid.sh</code></pre> <p>Notice, however, that this computation in total takes more than two days to complete on a single core.</p> <p>To reduce the size of the experiment, clear the contents of the <em>query</em> sub-folder an modify the <em>make_queries.sh</em> file by commenting out unwanted queries and parameter-combinations.</p> <p>To obtain a matrix, the command</p> <pre><code class="language-bash">./make_grid.sh aalwines IP IP 0 > ip_ip.tex pdflatex ip_ip.tex</code></pre> <p>which generated the IP IP matrix with 0 failures.<br> For the second argument, the following values are supported <em>IP, MPLS</em> while the third argument can also attain the value of <em>ANY</em>. The fourth argument gives the number of link failures.</p> <p>Timing information for the reachability-matrices can be obtained by</p> <pre><code class="language-bash">python3 ./timing_stats.py aalwines 3 IP_IP_UNDER_0</code></pre> <p>where the third argument determines the reduction-type used, and the fourth argument gives the specific query and engine mode used. In the given example we attain the statistics for reduction-mode 3 for the IP-IP matrix using under-approximation on zero link-failures.</p> <p>The <em>pre-reduction</em> and <em>post-reduction</em> elements of the output give the size of the constructed pushdown system before (and after) reduction respectively.</p>
r-process abundances in neutron-rich merger ejecta given different theoretical nuclear physics inputs
<p>This data release contains nucleosynthesis predictions for the r-process abundances presented in Côté, Eichler, Yagüe, Vassh et al. (2021) for compact object merger ejecta based on the publicly available simulation trajectories of Rosswog et al. (2013). All ejecta for the merger scenarios considered here are very neutron-rich (Ye ~ 0.016-0.11). Calculations were performed with the PRISM code (Mumpower et al. 2018) which accounts for nuclear reheating (here with a reheating efficiency of 50%). Results are reported for several different theoretical nuclear physics inputs but all calculations make use of the GEF fission yield prescription (see Vassh et al. 2019). All abundances are given at 1 Myr (10^6 years) post-merger. Please see the README file for more details and references.</p> <p>When using these nucleosynthesis yields, please cite this Zenodo data release (Vassh et al. 2021), and refer to Vassh et al. (2019) and Côté, Eichler, Yagüe, Vassh et al. (2021) for further details on the nuclear data applied as well as Rosswog et al. (2013), Piran et al. (2013), and Korobkin et al. (2012) for further details on the merger ejecta trajectories.</p>
An observed population of intermediate-mass helium stars that have been stripped in binaries - theoretical, computational and observational data
<p>This Zenodo repository contains the observational and computational data presented in the manuscript "An observed population of intermediate-mass helium stars stripped in binaries" by Drout, Götberg, Ludwig, Groh, de Mink, O'Grady and Smith.</p><p>We organize the data as follows:</p><ul><li>The stacked spectra presented in Figures S16-S21 are located in stacked_spectra.tar.gz, which contains a text file for each star. The text files have three columns that correspond to wavelength in Angstrom, normalized counts, and errors, respectively.<br> </li><li>The spectral model grid computed based on binary evolutionary model output and presented in detail in the Supplementary information section S1.2.1, is labeled with names starting S121. The file S121_evol_based_006_absolute_magnitudes.txt contains the absolute AB magnitudes for the models in UV and optical filters. The .tar.gz S121_evol_based_006_spectra.tar.gz contains files with the full spectral energy distribution and normalized spectra of each model. The .tar.gz S121_evol_based_006_complete_models.tar.gz contains the full CMFGEN models.<br> </li><li>For the stellar atmosphere model grid presented in Supplementary material section S1.2.2, we refer to the Zenodo repository 10.5281/zenodo.7976200, which is made available in association with the second paper in our series. We note that we used a subset of that grid in the article associated with this Zenodo repository. We refer to section S1.2.2 for more details.<br> </li><li>The spectral models demonstrating the mass loss rate variations in Supplementary information section S1.2.3 are presented here with names starting with S123. There is one file containing the absolute magnitudes (S123_mdot_variation_absolute_magnitudes.txt), the S123_mdot_variation_spectra.tar.gz contains the spectral energy distributions and normalized spectra for each of the models, and the S123_mdot_variation_complete_models.tar.gz contains the full CMFGEN models.<br> </li><li>The spectral model grid computed based on main-sequence evolutionary model output and presented in detail in the Supplementary information section S1.3.1, is labeled with names starting S131. The file S131_MS_evol_based_006_absolute_magnitudes.tar.gz contains three files with the absolute AB magnitudes for the models in the UV and optical filters, each file corresponding to either 20%, 60%, or 90% through the main-sequence evolution and labeled f20, f60, and f90, respectively. S131_MS_evol_based_006_spectra.tar.gz contains three folders labeled f20, f60 and f90, which each contains the SEDs (in Flambda and ABmag) and normalized spectra for the corresponding models. The files S131_MS_evol_based_006_complete_models_fX0.tar.gz contain the complete CMFGEN models.<br> </li><li>The custom index files we use for astrometry.net in section S3.1.1 are located in the zip file called S311_astrometry_index_files.zip. This information was used to recalculate the astrometry on the Swift UVOT images of the Magellanic Clouds.<br> </li><li>To make Figure 2B, we calculated the equivalent widths for a set of models assuming a signal-to-noise ratio of 35. This procedure is described in Section S3.7.2. In Figure2B_Model_EWs.zip, we provide three files that each contain these modeled equivalent widths for (1) stripped star models, (2) OB star models, and (3) composite models. <br> </li><li>To make Figure S7 (see also Sections S1.2.3 and S2.2), which is similar to Figure 2B, but presents the effects of varying the wind mass loss of stripped stars, we used a similar set of modeled equivalent widths as when we produced Figure 2B. These modeled equivalent widths are provided in FigureS7_Model_EWs.zip. <br> </li><li>To make Figure 3, we calculated equivalent widths for the model grid described in Section S1.2.2 and the TLUSTY OB star grids (see Section S1.3.2) assuming a signal-to-noise ratio of 100. These model equivalent widths are provided in the file called Figure3_Model_EWs.zip. </li></ul>
Questions for Galops 1-7 horse riding theoretical exams and their textual answers with enumerations
<p><strong>Description in English :</strong></p><p>(Description en Français plus bas)</p><p><strong>Questions for Galops 1-7 horse riding theoretical exams and their textual answers with enumerations</strong></p><p>This French dataset was created to develop a system of automatic correction of textual answers with enumeration for horse riding theoretical exams, as part of Marine Potier's Master's thesis, a student in NLP (Natural Language Processing) at the Université de Franche-Comté.</p><p>This dataset contains 122 questions with their respective possible answers.</p><p>These questions and their answers were manually extracted from the official books published by the French Equestrian Federation.</p><p>We used ChatGPT (v.3.5) in order to get variations of the extracted answers, and every new answer was manually verified to make sure it was correct as well.</p><p>This dataset is available in CSV format and structured according to the following fields :</p><p>- <strong>question_id</strong> : The question ID, representing the level (1 to 7) followed by the question number.</p><p>- <strong>type_question</strong> : Either "sans_ordre" or "avec_ordre". Some answers need to be written in a precise order to be considered correct.</p><p>- <strong>question</strong> : The actual question, which was extracted from the official books.</p><p>- <strong>reponse_correcte</strong> : The correct answer, which was extracted from the official books.</p><p>- <strong>variation_1 to variation_5</strong> : The variations of the correct answer which was reformulated with ChatGPT. All were manually verified afterwards.</p><p> </p><p><strong>Description en Français :</strong></p><p><strong>Questions des examens théoriques Galops 1 à 7 d'équitation et leurs réponses textuelles contenant des énumérations</strong></p><p>Ce dataset en langue française a été créé pour développer un système de correction automatique de réponses textuelles contenant une énumération pour les examens théorique d'équitation (les Galops 1 à 7). Ce projet s'inscrit dans le cadre de mémoire de recherche de Marine Potier, étudiante en Master en Traitement Automatique des Langues à l'Université de Franche-Comté.</p><p>Ce dataset est constitué de 122 questions avec leurs réponses correctes respectives.</p><p>Ces questions et leurs réponses ont été extraites manuellement des guides fédéraux officiels publiés par la Fédération Française d'Équitation.</p><p>Nous avons utilisé ChatGPT (v.3.5) afin de recueillir des variations des réponses extraites. Chaque nouvelle réponse a été vérifiée manuellement pour s'assurer de leur exactitude.</p><p>Ce dataset est disponible en format CSV, et structuré comme expliqué ci-dessous :</p><p>- <strong>question_id</strong> : L'identifiant de la question, représentant le niveau (1 à 7) suivi du numéro de question.</p><p>- <strong>type_question</strong> : Soit "sans_ordre" ou "avec_ordre". Certaines questions nécessitent d'avoir leurs réponses rédigées suivant un ordre précis pour être considérées comme correctes.</p><p>- <strong>question</strong> : La question, extraite des guides fédéraux.</p><p>- <strong>reponse_correcte</strong> : La réponse correcte, extraite des guides fédéraux.</p><p>- <strong>variation_1 à variation_5</strong> : Les variations de la réponse correcte qui a été reformulée à l'aide de ChatGPT. Toutes ont été vérifiées manuellement par la suite.</p>
The data for new theoretical Fe II templates for bright quasars
<p>The compressed <strong>'.tar.gz' </strong>files contain new theoretical Fe II templates that can be used for fitting UV to near-IR (1000-10000 Angstrom) spectra of quasars. The templates were developed using the latest Fe II atomic database of <a href="http://doi.org/10.1093/mnras/sty3198">Smyth et al. (2019)</a> within the CLOUDY C23.0 photoionization code with the following set of parameters.</p> <ul> <li>H-ionizing photons flux: <strong>17 ≤ log ΦH (cm−2 s−1) ≤ 22</strong>, and</li> <li>Gas density: <strong>9≤ log nH (cm−3) ≤ 14, </strong></li> <li>Step size: <strong>0.25 </strong>on log scale.</li> <li>A fixed Hydrogen column density: <strong>10^24 cm−2 </strong></li> <li>Abundance: <strong>solar </strong></li> <li>SED shapes:</li> </ul> <p>(1) Standard "<strong>agn.sed</strong>", a continuum similar to <a href="https://ui.adsabs.harvard.edu/abs/1987ApJ...323..456M/abstract/">Mathews & Ferland (1987)</a></p> <p>(2) Intermediate SED of (<a href="https://ui.adsabs.harvard.edu/abs/2012MNRAS.425..907J/abstract/">Jin et al., 2012</a>) </p> <ul> <li>The Fe II template is available for the microturbulence values 0, 20, 50 and 100 km/s.</li> </ul> <p><strong>(Note: The Fe II templates are also available in the GitHub link: </strong><strong>https://github.com/Ashwani-88/Fe2_template)</strong></p> <p>Each <strong>tar.gz</strong> file consists of Fe II templates for different SED shapes. <br><br>For each SED shape;</p> <p>The new Fe II templates are available in the directory "Templates_including_only_total_Fe2". </p> <p>Additionally, we provide templates for the outward and inward Fe II emissions in the directory "Templates_including_outward_Fe2"</p> <p>The directory for Fe II templates for a microturbulence velocity is named as</p> <p>turb_v<em><strong>n</strong></em></p> <p>where<em> <strong>n</strong></em> is the microturbulence velocity in km/s. <br><br>The files within each directory are named as follows:</p> <p><br>phi<em><strong>a</strong></em>_nH<em><strong>b</strong></em>_m<em><strong>c</strong></em>.dat</p> <p>where <strong><em> a</em></strong> = log value of the H-ionizing photon flux in cm−2 s−1,<br><em><strong>b</strong></em> = log value of the Hydrogen gas density in cm−3, and<br><em><strong>c</strong></em> = the value of microturbulence in km/s.</p> <h2><strong>Each template file in ``Templates_including_only_total_Fe2'' has two columns </strong> </h2> <p> <br>First column: wavelength in Angstrom with 2 Angstrom binning <br>Second column: Fe II line intensity (in erg cm-2 s-1 A-1)</p> <h2>Templates in ``Templates_including_outward_Fe2'' has four columns.</h2> <p><br>First column: wavelength in Angstrom with 1000 logarithmic bins, each ~ 584 km/s wide, between 1000 and 7000 Angstrom. <br>Second column: Total Fe II line intensity (in erg cm-2 s-1 A-1) <br>Third column: Inward Fe II line intensity (in erg cm-2 s-1 A-1) <br>Fourth column: Outward Fe II line intensity (in erg cm-2 s-1 A-1) </p> <p>The Fe II line intensity includes a covering factor of 30 % and is scaled for our test object RM 102. </p> <p> </p>
New calibrated models for the TRGB luminosity and a thorough analysis of theoretical uncertainties
<p>The files contain the grid models for TRGB stars based on <strong>Saltas & Tognelli, 2022, MNRAS, in press (arXiv: 2203.02499)</strong>. See the paper for details on the physics, and the attached readme file for a description of the structure of the attached files. If you use these data in your research please cite the above article. <br> </p>
Raw Data to "Theoretical Study on the Photoacidity of Hydroxypyrene Derivatives in DMSO Using ADC(2) and CC2"
<p>This data is a supplement to the publication entitled "Theoretical Study on the Photoacidity of Hydroxypyrene Derivatives in DMSO Using ADC(2) and CC2" in the The Journal of Physical Chemistry A (DOI: 10.1021/acs.jpca.2c04436). It contains the structures (as '.xyz' files) and HF/DFT energies from the quantum chemical (QC) calculations using TURBOMOLE (version 7.4).</p> <p>Additional information on the file structure is given in the README file.</p>
Theoretical simulations data for "Experimental observation of repulsively bound magnons"
<p>The files contain the data obtained from the theoretical simulations depicted in the figures of the article "Experimental observation of repulsively bound magnons" Nature (2024).</p> <p>The format of the data and to which figure it corresponds is described in the file "read_me_metadata.txt".</p>
A theoretical framework for learning through structural plasticity
<p>This dataset contains the data and scripts used for the preprint:</p> <div> <div><span>Tiddia, G., Sergi, L., & Golosio, B.</span> <span>(</span><span>2023</span><span>)</span><span>.</span> <span>A theoretical framework for learning through structural plasticity</span><span>.</span> <span><em>ArXiv</em></span><span>. DOI:</span> <a href="https://doi.org/10.48550/arXiv.2307.11735" rel="nofollow">https://doi.org/10.48550/arXiv.2307.11735</a></div> </div> <p>The dataset contains a README file with all the instructions for compiling and running the model. </p> <p> </p>
Figure 1 in A new theoretical approach for the study of monophyly of the Brachyura (Crustacea: Decapoda) and its impact on the Anomura
Figure 1. Synapomorphy "d" supports the inclusion of the Podotremata (P) in the Brachyura, while the use of less generalized synapomorphies (a, b) in the definition will result in the exclusion of the Podotremata from the Brachyura. Synapomorphies: a, female sexual opening on thoracic sternite 6; b, presence of sella turcica; c, paired spermatheca; d, intertagmal phragma fused with thoracic interosternite 8/7 (pers. obs.). Other abbreviations: H, Heterotremata; Th, Thoracotremata. Figure 2. Assumption 1: both the Brachyura (H + Th + P) and Podotremata (P) are monophyletic. Under assumption 1 it makes no sense to search for the "lower limit" of the Brachyura. Synapomorphies and abbreviations as in Fig. 1. Figure 3. Assumption 2: Brachyura (H + Th + P) monophyletic; Podotremata (P) not monophyletic. Under assumption 2 it becomes meaningful to search for the sister taxa of the Heterotremata + Thoracotremata clade. Synapomorphies and abbreviations as in Fig. 1. Figure 4. Assumption 3: Brachyura (H + Th + P) not monophyletic; Podotremata (P) monophyletic. Under assumption 3 searching for the "lower limit" of the Brachyura among the Podotremata makes no sense. Synapomorphies and abbreviations as in Fig. 1. Figure 5. Assumption 4: both Brachyura (H + Th + P) and Podotremata (P) not monophyletic. According to corollary 1 searching for the sister taxa of the Heterotremata + Thoracotremata clade and searching for the most basal branch of the brachyuran clade becomes truly relevant. Note that one set of the Podotremata is positioned as paraphyletic complex closely related to the Heterotremata + Thoracotremata clade (H-Th). Synapomorphies and abbreviations as in Fig. 1. Figure 6. Assumption 4; corollary 2. Searching for the most basal branch of the brachyuran clade ("the lower limit") among the Podotremata is completely meaningless. Note that none of the Podotremata (P) is closely related to the Heterotremata + Thoracotremata clade; all form a paraphyletic complex more closely related to some other group of decapods. Synapomorphies and abbreviations as in Fig. 1.
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.