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5,462 results for “binary”
Gravitationally Bound Wide Pairs Hosting Unresolved Astrometric Binaries in Gaia DR3
<p>We present a catalog of 14,791 gravitationally bound wide pairs where one of the components is an unresolved binary with an astrometric orbital or acceleration solution in Gaia DR3. The catalog is separated into two tables corresponding to orbital solutions and acceleration solutions, respectively. </p>
UltraHD CityCLIM example binary output files for one timestep
<p>These files are example numerical output from the UltraHD Large Eddy simulation model in binary format. The UltraHD Large Eddy simulation model was operational from beginning of June 2023 till October 2024 for three different city regions (Luxemburg, Karlsruhe and Valencia). These example outputs consist of arrays with 500x500 float32 values for the following parameters: 2m temperature (t2m), 2m dewpoint (dewpoint), skin temperature (tsk), windspeeds (u10m, v10m), vertical velocity (w), orografic height (hgt), liquid water path (lwp), surface pressure (psfc). Some of these files are used within the CityCLIM cloud environment for numerical analysis within the identification services. The data is from the run from the 19th of July 2024 for forecast minute 2220.</p> <p> </p>
Inlists for "Rethinking Thorne-Żytkow Object Formation: The Fate of X-ray Binary LMC X-4 and Implications for Ultra-long Gamma-ray Bursts"
<div> <div> <div> <p>We use the MESA Isochrones and Stellar Tracks (MIST) package (Dotter 2016; Choi et al. 2016) with MESA v7503 (Paxton et al. 2011, 2013, 2015) and mesasdk x86_64-linux-20141212 revision 245. </p> </div> </div> </div>
Optimal (v, 4, 1) binary cyclically permutable constant weight codes ((v,4,1) optical orthogonal codes (OOC)) and cyclic S(2, 4, v) designs
<p><strong>Optimal (v, 4, 1) binary cyclically permutable constant weight codes ((v,4,1) optical orthogonal codes (OOC)) and cyclic S(2, 4, v) designs.</strong></p> <p><strong>All (v,4,1) OOC</strong> for 26≤v≤76 and v=85: All_oc_26-85_4_1.zip</p> <p><strong>All cyclic 2-(v,4,1) designs</strong> for v=40, 52, 64, 76, 88: d_4_1.zip.</p> <p><strong>Some (v,4,1) OOC: </strong></p> <p>The codes are constructed by backtrack search considering all possibilities for the first two codewords (n=0 and n=1), but only the first 3 possibilities for the n-th codeword (n > 1) are considered for 77≤v≤98: E3oc_77-98_4_1.zip.</p> <p>The codes are constructed by backtrack search considering all possibilities for the first two codewords (n=0 and n=1), but only the first 2 possibilities for the n-th codeword (n > 1) are considered for 99≤v≤136: E2oc_99-136_4_1.zip</p> <p><strong>Some cyclic 2-(v,4,1) designs. </strong>The designs are constructed by backtrack search considering all possibilities for the first two or three baseblocks, but only the first 2 possibilities for the n-th baseblock (n > 1 for strictly cyclic designs, n>2 for designs with one short orbit) are considered for 100≤v≤160: E2d_4_1.zip</p>
2024q1 Binary black hole initial data: equal-mass, nonspinning, quasicircular
<p>Binary black hole initial data with equal masses and no spins on a circular orbit. Generated with the SpECTRE code (https://spectre-code.org), version <span>2024.09.16.</span></p>
AT 2021hdr: a candidate tidal disruption of a gas cloud by a binary super massive black hole system
<p>In this dataset we provide tables for the Zwicky Transient Facility (ZTF) and Swift observations presented in the paper "AT 2021hdr: a candidate tidal disruption of a gas cloud by a binary super massive black hole system", accepted for publication in the Astronomy and Astrophysics Journal (Hernández-García et al. 2024). </p> <p> </p> <p>Files description:</p> <p>-ztf_table:_zenodo.csv: Log of the ZTF forced photometry observations. Include the dates in MJD, filter, apparent magnitudes, and difference fluxes.</p> <p>- swift_table_zenodo.csv: Log of the Swift observations, including the observation ID, date (in MJD), exposure time, count-rate in the 0.5-10 keV energy band, and UV fluxes in the UVW2 and UVM2 filters. </p>
2024/07/29 VAMPIRES Binaries
<p>Each target is saved to a zip folder with the following:</p> <ul> <li><name>.toml is the configuration file used for the VAMPIRES data processing pipeline, which includes all reduction options</li> <li>'aligned' contains data cubes with aligned frames</li> <li>'coadded' contains the coadded final images</li> </ul> <p>In addition, the ephemerides for two astrometric calibrators (HD214850 and HD224930) are calculated in `ephemeris.jl` and saved to the `ephemeris.csv` file.</p> <p> </p> <p>All data were reduced using the VAMPIRES data processing pipeline (https://github.com/scexao-org/vampires_dpp). </p>
The variable evolution of accretor stars in binary systems due to accretion of increasingly helium-rich material
<p>Dataset for paper "The variable evolution of accretor stars in binary systems due to accretion of increasingly helium-rich material".</p> <p>You will need the <a href="https://github.com/Krytic/Kaitiaki">Kaitiaki code</a>.</p>
STonKGs Correct Binary Model
<p>The fine-tuned model trained on the binary formulation of correctness curations.</p>
Yields from paper: ALUMINIUM-26 FROM MASSIVE BINARY STARS II. ROTATING SINGLE STARS UP TO CORE-COLLAPSE AND THEIR IMPACT ON THE EARLY SOLAR SYSTEM
<p>Title: Aluminium-26 From Massive Binary Stars II: ROTATING SINGLE STARS UP TO CORE-COLLAPSE AND THEIR IMPACT ON THE EARLY SOLAR SYSTEM<br> Authors: Brinkman H.E., den Hartogh J. W., Doherty C.L., Pignatari M., Lugaro M.<br> ================================================================================<br> Description of contents: A .tar.gz package containing three files with the complete set<br> of yields from the models presented in this paper. YieldsNR.txt contains the yields for the<br> non-rotating models and Yields150.txt and Yields300.txt the yields for the models<br> rotating at an initial velocity of 150 and 300 km/s, respectively.</p> <p>================================================================================</p>
The Mystery of Magnetic Binaries: Questions, Concerns and Possibilities
<p>Astronomy has become, albeit by necessity, very specialized. Within the stellar variability community, people specialize by variability type, or by observational type, and thus collaborations form to allow for complex studies. One particular area, which is largely unavoidable in such complex studies is binarity, considering the sheer fraction of stars in binaries. Interestingly, magnetism is one area where this seemingly isn't true. So few binaries possess a magnetic component that many people ignore them. In this talk we will review these magnetic binaries and their importance. We will probe some of the unanswered questions, and we will also discuss how useful binarity can be to understanding magnetic interaction.</p>
State-of-the-art evolution models for single, binary and magnetic massive stars
<p>The Universe is threaded by magnetic fields on all scales, from planetary systems to galaxy clusters. In massive stars, they play a pivotal and multifaceted role. They are thought to be crucial in transporting angular momentum throughout the stellar interior and maintaining the overall angular-momentum budget. They may also contribute to chemical mixing, can interact with convective fluid motions and may give rise to distinct seismic signatures. For example, the spin rates of white dwarfs, neutron stars and black holes are strongly determined by the coupling of a star’s core to its envelope. In this talk, I will discuss recent progress in our understanding of how magnetic fields affect single and binary stars, and what are possible origins of the different types of magnetic fields in massive stars. In particular, I will highlight connections to observations and how these can be used to further our understanding of how magnetic fields influence the evolution and final fates of stars.</p>
A massive binary system with a single magnetic star
<p>HD148937 is one of the three Galactic O-type sources belonging to the rare class of Of?p objects. These stars are characterised by recurrent spectral variations, the origin of which is found to be their strong magnetic fields. Originally thought to be a single star, long baseline near-IR interferometry with PIONIER has revealed HD148937 to be a binary system. In this presentation I will discuss our investigations into the source using a combination of multi-epoch GRAVITY and PIONIER data. These data reveal that the two components are of similar brightness but one star shows the BrG line in emission and the other in absorption, confirming that only one of the two stars is magnetic. Combining our data with existing spectroscopic measurements, a preliminary 3D orbit of the system can be obtained and subsequently absolute masses. We use these new constraints to discuss the evolutionary status of this unique object in the context of the origin of the magnetic star.</p>
Different to the core: the pre-supernova structures of massive single and binary-stripped stars
<p>This is a basic reproduction package for the paper "Different to the core: the pre-supernova structures of massive single and binary-stripped stars".</p> <p>This package contains inlists for MESA and processed output.</p>
The Complicated Case of δ Scuti Pulsations and Rotation in KIC 6951642; a long-orbit Single-lined Spectroscopic Binary Star
<p>Abstract: More than four years of HERMES observations have confirmed KIC 6951642 is a very long orbit (≈1770 d) single-lined spectroscopic binary (F0-type) with a fast-rotating companion (vsin i = 123±3 Km/s). The Fourier spectrum of its four-year photometric observations includes plenty of significant frequencies (594) in low- and high-frequency regions. The high-frequency modes appear with various time-delay patterns. We detected several rotationally split 𝛿 Scuti pulsations centered at 13.96 per day (and average frequency spacing of Δ𝑓= 0.723±0.006 per day) for KIC 6951642. The detailed study of all significant low frequencies, extended from 0.72 to 3.60 per day, revealed that the two most dominant frequencies (with the same amplitude and larger than of p-modes) are a combina3on the lowest-frequency modes (𝑓<sub>3</sub> = 𝑓< 0.17 per day), i.e. 𝑓<sub>orhrm</sub> + 𝑚𝑓<sub>orhrm </sub>(𝑚 = 12,14). We suggest the lowest-frequency modes are very large harmonics (orders of 10) of orbital frequency (≈0.0006 per day). We verified the other most dominant low-frequencies as harmonics of rotation frequency 0.721 per day and its combinations. Finally, we reject the probability of hybrid pulsations in the fast-rotating companion of KIC 6951642. We introduce it as a 𝛿 Scuti pulsator with a candidate rotation frequency of 0.721 per day.</p>
Reproduction package for the paper 'Discovery of a probable very fast extragalactic nova in a symbiotic binary'
<p>This is a basic reproduction package (RP) for the paper "Discovery of a probable very fast extragalactic nova in a symbiotic binary". It aims to provide the most important data products to check and reproduce the main results of the paper, listing all software used and data archives containing the public data used.</p> <p>Authors: David Modiano, Rudy Wijnands</p> <p>Arxiv DOI: 2210.06057</p> <p>Paper DOI: 10.1051/0004-6361/202244679</p> <p>Accepted for publication in Astronomy and Astrophysics (date of acceptance: 11/10/2022)</p>
Data Release: Spin it as you like: the (lack of a) measurement of the spin tilt distribution with LIGO-Virgo-KAGRA binary black holes
<p>This is the data release associated with <strong>Vitale et al <a href="https://arxiv.org/abs/2209.06978">2209.06978</a></strong></p> <p><strong>Samples.zip: </strong>Contains all of the hyper posterior samples for the runs listed in Tables G.1.</p> <p>The files are in json format. Bilby offers a dedicated routine to read them in</p> <p> </p> <blockquote> <p>import bilby<br> data= bilby.core.result.read_in_result(path_to_json)</p> </blockquote> <p> </p> <p>See the <a href="https://lscsoft.docs.ligo.org/bilby/">Bilby documentation </a>for what is contained in the result object. </p> <p>For each run, we report the posterior hyper samples for the mass model, reshift model, spin magnitude model, spin tilt model and merger rate [Gpc^-3 yr^-1]</p> <p>Here the name used to store and a short description of each parameter (Follow the references in the Method section of the paper for a description of each sub-model):</p> <ol> <li>Primary mass model (Power Law + Peak for all runs) <ol> <li>power_law_slope_m1, slope of the primary mass power law component</li> <li>minmass_m1, minimum BH mass</li> <li>maxmass_m1, maximum BH mass</li> <li>low_end_smoothing_m1, smoothing at the low-mass end</li> <li>peak_branchingratio_m1, branching ratio between Gaussian peak and power law (1= 100% peak)</li> <li>peak_mean_m1, mean of the Gaussian peak</li> <li>peak_sigma_m1, sigma of the Gaussian peak </li> </ol> </li> <li>Mass ratio model (power law for all runs) <ol> <li>power_law_slope_mass_ratio, slope of the mass ratio </li> </ol> </li> <li>Redshift (power law for all runs) <ol> <li>power_law_slope_redshift, slope of the redshift</li> </ol> </li> <li>Spin magnitude (IID beta distributions for all runs) <ol> <li>alpha_chi, first argument of beta distribution</li> <li>beta_chi, second argument of beta distribution</li> </ol> </li> <li>Cosine of tilt angle <ol> <li>Gaussian models <ol> <li>mu_0_costilt, for Gaussian models w/o correlation, the mean of the left (or only) Gaussian</li> <li>sigma_0_costilt, for Gaussian models w/o correlation, the sigma of the left (or only) Gaussian</li> <li>mu_1_costilt, for Gaussian models w/o correlation, the mean of the right Gaussian</li> <li>sigma_1_costilt, for Gaussian models w/o correlation, the sigma of the right Gaussian</li> <li>mu_a_costilt, for Gaussian model with correlation, the constant part of the Gaussian mean</li> <li>mu_b_costilt, for Gaussian model with correlation, the coefficient of the linearly evolving part of the Gaussian mean</li> <li>sigma_a_costilt, for Gaussian model with correlation, the constant part of the Gaussian sigma</li> <li>sigma_b_costilt, for Gaussian model with correlation, the coefficient of the linearly evolving part of the Gaussian sigma</li> </ol> </li> <li>Beta models <ol> <li>alpha_a_costilt, for all Beta models, the constant part of the first parameter of the Beta distribution</li> <li>alpha_b_costilt, for all Beta models, the coefficient of the linearly evolving part of the first parameter of the Beta distribution</li> <li>beta_a_costilt, for all Beta models, the constant part of the second parameter of the Beta distribution</li> <li>beta_b_costilt, for all Beta models, the coefficient of the linearly evolving part of the second parameter of the Beta distribution</li> </ol> </li> <li>Tukey models: <ol> <li>tukey_x0, the center of the Tukey as defined in appendix E of the paper</li> <li>tukey_k, Tk as defined in appendix E of the paper</li> <li>tukey_r, Tk as defined in appendix E of the paper</li> </ol> </li> <li>Branching ratios: <ol> <li>spin_mixture_0, for 2-component models, this is the branching ratio of the non-isotropic component</li> <li>spin_mixture_1, for Isotropic + Gaussian + Tukey and Isotropic + Gaussian + Beta this is the branching ratio of the <strong>Gaussian</strong> component; for Isotropic + 2 Gaussian this is the branching ratio of the <strong>Gaussian on the right.</strong></li> </ol> </li> </ol> </li> <li>Merger rate <ol> <li>rates, merger rate per unit Gpc cubed per unit year</li> </ol> </li> </ol> <p>Note that some of the parameters for the tilt models might not be used, but still stored (and fixed to - usually - zero). This can be checked by verifying what priors were used for each parameter. For example the <em>Isotropic</em> run was obtained from the <em>Isotropic + Gaussian </em>model by setting the branching ratio of the Gaussian component to zero (at which point the values of mu and sigma costitl are irrelevant) </p> <blockquote> <p>> data['prior']<br> [...]<br> <strong> 'spin_mixture_0': DeltaFunction(peak=0, name=None, latex_label=None, unit=None),</strong><br> </p> </blockquote> <p> </p> <p><strong>Figures.zip:</strong> Contains PDFs for all figures in the paper, plus individual figures for p(costau) and dR/dcostau for each model.</p> <p>Drop me (Salvatore Vitale) an email if anything doesn't work, is missing, or if you spot issues. Thanks! </p> <p> </p>
Datasets of binary and quaternary alloys with Curie temperature and magnetization for the eRSM
<pre>binary_alloys: A material dataset containing 100 transition-rare earth metal binary alloys, comprising nickel (Ni), manganese (Mn), cobalt (Co), or iron (Fe), and the corresponding Curie temperatures ($T_{C}$). This dataset was collected from the Atomwork database of the National Institute of Materials Science \cite{paulingfile,atomwork}. Each binary alloy in $\mathcal{D}_{binary}$ is represented using seven descriptors: (1,2) the atomic number of transition metal ($Z_T$) and rare-earth ($Z_R$) constituents; (3) projection of the spin magnetic moment onto the total angular moment of the $4f$ elections ($J_{4f}\left(1-g_{j}\right)$); (4, 5) covalent radius ($r_{covT}$) and first ionization (${IP}_T$) of the transition metal; (6, 7) concentration of the transition metal ($C_T$) and rare-earth metal ($C_R$). </pre> <pre>quaternary_alloys: A material dataset contains 990 equiatomic quaternary high-entropy alloys, which comprise $14$ transition metals {Ag, Cd, Co, Cr, Cu, Fe, Mn, Mo, Ni, Pd, Rh, Ru, Tc, Zn}, and the corresponding calculated magnetizations and Curie temperatures in the BCC phase. The dataset was collected from an original dataset of 147,630 equiatomic quaternary high-entropy alloys calculated using Korringa-Kohn-Rostoker coherent approximation method . Each alloy in the dataset is represented using 135 compositional descriptors, including the means, standard deviations, and covariance of the atomic representations of their constituent elements and four categorical features indicating the elements comprising the quaternary alloy. </pre>
Data for publication "Surface tension models for binary aqueous solutions: A review and intercomparison"
<p>This repository contains the data of the publication:</p> <p>Title: "Surface tension models for binary aqueous solutions: A review and intercomparison"<br> Authors: Judith Kleinheins, Nadia Shardt, Manuella el Haber, Corinne Ferronato, Barbara Nozière, Thomas Peter, and Claudia Marcolli<br> Date: 2023</p> <p>Abstract: The liquid–air surface tension of aqueous solutions is a fundamental quantity in multi-phase thermodynamics and fluid dynamics and thus relevant in many scientific and engineering fields. Various models have been proposed for its quantitative description. This Perspective gives an overview of the most popular models and their ability to reproduce experimental data. In addition, we propose a new model based on the logistic function which reproduces sigmoidal curve shapes (Sigmoid model) to<br> empirically fit experimental surface tension data. All models were tested on ten binary aqueous solutions of electrolytes and organic molecules. The surface tension of weakly surface active substances is well reproduced by all models. In contrast, only a few models successfully modelled the surface tension of aqueous solutions with strongly surface-active substances. For substances with a solubility limit, usually no experimental data is available for the surface tension of supersaturated solutions and the pure liquid solute. We discuss ways in which these can be estimated and emphasize the need for further research. The newly developed Sigmoid model best reproduces the surface tension of all tested solutions and can be recommended as a model for a broad range of substances and over the entire concentration range.</p>
Tidally perturbed g-mode pulsations in a sample of close eclipsing binaries
<p>Description:<br> Reduced Kepler and TESS light curves of KIC 3228863, KIC 3341457, KIC 4947528, KIC 9108579, and<br> KIC 12785282, as well as various data products obtained at different steps of the analysis presented in Van Reeth<br> et al. (2023): the residual pulsation light curves (after subtracting the harmonic model for the binarity), the<br> optimised prewhitened (Kepler) frequency lists, measured g-mode patterns, and detected tidal g-mode<br> perturbations (both measured directly from orbital-phase-binned data and reconstructed using detected<br> orbital-frequency-spaced multiplets).</p> <p>Abstract:<br> Context. Thanks to the high-precision photometry from space missions such as Kepler and TESS, tidal<br> perturbations and tilting of pulsations have been detected in more than a dozen binary systems. However, only<br> two of these were gravity-mode (g-mode) pulsators.<br> Aims. We aim to detect tidally perturbed g modes in additional binary systems and characterise them<br> observationally.<br> Methods. We perform a custom data reduction of the available Kepler and TESS photometry of a well-studied,<br> published sample of 35 binary systems with gamma Doradus (gamma Dor) pulsators. For each target, we model<br> the binary signal using a sum of 100 sine waves, with frequencies at orbital harmonics, and measure significant<br> pulsation frequencies in an iterative prewhitening analysis of the residual light curve. Pulsations are<br> labelled as tidally perturbed g modes if they are part of both period-spacing patterns and multiplets spaced by<br> integer multiples of the orbital frequency. After visual inspection and confirmation, the properties of these<br> targets and g modes are characterised.<br> Results. We detect tidally perturbed g-mode pulsations for five short-period binaries that are circularised and<br> (almost) synchronously rotating: KIC 3228863, KIC 3341457, KIC 4947528, KIC 9108579, and KIC 12785282.<br> Tidally perturbed g modes that occur within the same star and have the same mode identification (k,m), are found<br> to have near-identical relative amplitude and phase modulations, which are within their respective 1-sigma<br> uncertainties also identical for the Kepler and TESS photometric passbands. By contrast, pulsations with<br> different mode identification (k,m) are found to exhibit different modulations. Moreover, the observed<br> amplitude and phase modulations are correlated, indicating that the binary tides primarily distort the g-mode<br> amplitudes on the stellar surface. The phase modulations are then primarily a geometric effect of the<br> integration of the stellar flux over the visible stellar surface. All selected binaries also exhibit signal<br> that resembles rotational modulation in the Fourier domain. In the case of KIC 3228863, this is caused by the<br> presence of the known tertiary component, and for the other systems we hypothesise that it is caused by<br> temperature variations on the stellar surface. Alternatively, the signal can be overstable convective modes in<br> the stellar core or belong to the non-pulsating companion.<br> Conclusions. While g-mode pulsation periods are known to be a direct probe of the deep interior stellar<br> structure, the binary tides which cause the pulsation modulations are dominant in the outer stellar layers.<br> Hence, in future tidally perturbed g modes may allow us to do core-to-surface asteroseismic modelling of<br> tidally distorted stars.</p>
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Allen Brain Atlas
Allen Brain Atlas is an Allen Institute collection of brain map atlases, datasets, APIs, and analysis tools covering mouse, human, and non-human primate brain resources.
Annotated Behaviour and Observability Dataset (ABODe)
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.