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Data from: Understanding the limits of binary diffusion for enhanced clay barrier design
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Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis
<p>We release dynamical ejecta data from binary neutron star merger simulations. The outflows are extracted at a fixed coordinate sphere with radius 300 G/c^2 Msun (= 443 km). Only material unbound according to the geodesic criterion is considered to be part of the dynamical ejecta. See [1] for more details.</p> <p>Included data:</p> <ul> <li>`Table2.txt`: Table 2 of the paper in machine readable format</li> <li>`tabulated_nucsyn.h5`: nucleosynthesis yields from pre-computed parametrized trajectories. The first three indices of each dataset are Ye, entropy, and expansion timescale tau. For example `Y_final[iYe, ientr, itau, iiso]` gives the final abundance of isotope `iiso` with `A[iiso]` and `Z[iiso]` for a trajectory with initial Ye = `Ye[iYe]`, initial entropy `s[ientr]`, and expansion timescale `tau[itau]`.</li> <li>`tabulated_rho.h5`: gives the density at T = 6 GK corresponding to the Ye, entropy, and expansion timescale used in `tabulated_nucsyn.h5`.</li> <li>`[model].tar`: ejecta data for individual simulations. The naming convention is the same as in the paper.</li> </ul> <p>For each model we provide:</p> <ul> <li>`outflow.txt`: angle integrated outflow rate and cumulated ejecta mass. Data are given in units with Msun = G = c = 1 (eg, the conversion factor for time to seconds is 4.9258e-6).</li> <li>`hist_entropy.dat`: histogram of the ejecta as a function of the entropy (in kb)</li> <li>`hist_vinf.dat`: histogram of the ejecta as a function of the asymptotic velocity (in units of c)</li> <li>`hist_ye.dat`: histogram of the ejecta as a function of the electron fraction Ye.</li> <li>`profile.txt`: time integrated ejecta profiles as a function of the polar angle.</li> <li>`hist_vinf_theta.h5`: histograms of the ejecta as a function of the asymptotic velocity and the polar angle.</li> <li>`hist_ye_theta.h5`: histograms of the ejecta as a function of the asymptotic velocity and the polar angle.</li> <li>`hist_ye_entropy_tau.h5`: histograms of the ejecta as a function of Ye, entropy, and expansion timescale tau.</li> </ul> <p>Additionally we distribute:</p> <ul> <li>Initial data generated with LORENE and associated EOS tables.</li> <li>EOS tables used for the evolution</li> <li>Parameter file used for each simulation</li> </ul> <p>For the multidimensional histograms the indices are ordered as specified in the file name, ie the file `hist_ye_theta.h5` tabulates the ejecta mass as a function of Ye (first index) and polar angle theta (second index).</p> <p><br> [1] D. Radice, A. Perego, K. Hotokezaka, S. A. Fromm, S. Bernuzzi, and L. F. Roberts, <em>Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis</em>, <a href="https://dx.doi.org/10.3847/1538-4357/aaf054">ApJ 869:130 (2018)</a>, <a href="https://arxiv.org/abs/1809.11161">arXiv:1809.11161</a></p>
Dynamics of phase separation of sheared inertialess binary mixtures
<p>Videos (gif files) of the simulated dynamics of phase separation report the maps of mass fraction of species <em>A</em> (<em>f</em>) at different time intervals within the simulated domain. File names are as follows:</p> <p>Sec3.<strong>s</strong>_gamma<strong>G</strong>_Nalpha<strong>N</strong>_MC<strong>n</strong>_tstep<strong>T</strong>-phi</p> <p>where:</p> <p><strong>s</strong> identifies the section number as in the main text (i.e., Sec3.1, Sec3.2, Sec3.3, Sec3.4)</p> <p><strong>G</strong> identifies the value of the dimensionless shear rate (e.g., 0, 10<sup>-2</sup>, etc.)</p> <p><strong>N</strong> identifies the value of the fluidity parameter <em>N</em><em><sub>a</sub></em> (e.g., 10<sup>-2</sup>, 10<sup>2</sup>, etc.)</p> <p><strong>n</strong> identifies the different realizations of the initial random noise (i.e., MC1, MC2)</p> <p><strong>T</strong> identifies the time step in dimensionless time (i.e., tstep20, tstep200)</p>
Fast and Regularized Reconstruction of Building Facades from Street-View Images using Binary Integer Programming
<p>Video demonstrations of the paper "Fast and Regularized Reconstruction of Building Facades from Street-View Images using Binary Integer Programming".</p>
Cosmic Rates of Black Hole Mergers and Pair-Instability Supernovae from Chemically Homogeneous Binary Evolution
<p>Data products and files to reproduce the results from du Buisson et al. (2020).</p> <p><strong>MESA Calculations</strong></p> <p>This work included the calculation of large grids of binary models with the MESA code version 11701. The template used for these calculations is included (template.tar.xz), to model any specific system the files inlist_extra and inlist_extra_sj must be updated with the necessary initial parameters.</p> <p>The resulting data from all simulations is also included in the files named Z*.tar.xz, where the "*" should be replaced for the specific value of log10(Z) for that set of simulations. Data is included in folders with a naming format of logM1_massratio_periodindays, so for instance the folder named 2.100_1.000_2.800 contains a simulation performed for a primary of mass 10^(2.1) Msun, a mass ratio of unity, and an initial orbital period of 2.8 days (note that all simulations are done for a mass ratio of unity). Each folder is a full MESA work directory, including the necessary input files and source code to rerun the simulation. The data files included in each folder are:</p> <ol> <li>LOGS1/history.data.s: A MESA history file containing information of the primary every 5 steps of the simulation. This file has been processed from the original MESA output to reduce its size.</li> <li>binary_history.data.s: Similar to the previous one but containing information of the binary system itself</li> <li>last_profile_1.data.s: MESA profile file containing the interior structure of the star at the end of the simulation. These files are only stored for systems that deplete central carbon, or become pair unstable. This file has also been post-processed to reduce its size, mostly by removing redundant columns and reducing the reported precision.</li> <li>out.txt.s: The last 100 lines of the terminal output from the simulation, useful to quickly glance the outcome.</li> </ol> <p><strong>Summary data tables for the MESA simulations</strong></p> <p>Data tables summarizing the outcome of all simulations are included in the file data_tables.tar.xz. Each of the files contained in that archive have the results from one metallicity, with the name indicating the value of log10(Z). Each row in the files represents one simulation, and the data provided in the different columns is:</p> <ol> <li>"log10(M_1i)(Msun)", "qratio(M_2i/M_1i)", "P_i(days)", "metallicity": The initial parameters of the simulation.</li> <li>"result": A string indicating the outcome of the system (see the header of the data files for a list of outcomes). In particular when the outcome is "double_BH", "PISN", "PPISN", the following columns indicate information at the terminal point of the simulation. For all other outcomes, most of the following columns are empty.</li> <li>had_contact: Specifies whether the system undergoes a contact phase (see header in the data files for allowed values).</li> <li>"M_1f(Msun)", "M_2f(Msun)", "P_f(days)": Final orbital parameters.</li> <li>"merge_time(Gyr)": Time to merge from the system assuming the system forms a binary black hole with masses and period given by the M_1f, M_2f and P_f values.</li> <li>"Kerr_param_1", "Kerr_param_2": Black hole spin assuming all angular momentum and mass is conserved at collapse.</li> <li>For the values listed in 4,5 and 6, we also provide values with an added "wpi" description, these indicate the expected results when including pair and pulsational pair instability supernovae, as described in the paper.</li> <li>"he_core_mass_1": Mass coordinate in Msun of the uppermost layer of the star with a mass fraction of hydrogen < 0.01. Any other arbitrary cut can be computed using the profile data.</li> <li>"c_core_mass_1": Mass coordinate in Msun of the uppermost layer of the star with a mass fraction of helium < 0.01.</li> <li>"total_mass_h1_1", "total_mass_he4_1": Total mass of hydrogen and helium at the end of the simulation</li> <li>The remaining columns contain the same information as points 8,9,10 for the secondary. Since all our simulations have q=1 they're actually redundant.</li> </ol> <p><strong>Montecarlo Simulations</strong></p> <p>Using the results of the MESA calculations, Montecarlo simulations were performed that sample the relevant distribution functions and the cosmic star formation history. The code used to perform these calculations is included in the archive montecarlo_code.tar.xz, and it includes a readme.txt file with instructions on how to use it. The outcome of these Montecarlo simulations is included in the files:</p> <ol> <li>fiducial.tar.xz</li> <li>sfr_c1.tar.xz</li> <li>sfr_c2.tar.xz</li> <li>sfr_c3.tar.xz</li> <li>sfr_c4.tar.xz</li> </ol> <p>The first file contains the information on our standard choice of SFR history, including simulations with no kicks, and with and without PPISN. The other four files correspond to each of the cases of SFR variations that we considered in the paper. Each of these archives contain three files:</p> <ol> <li>direct.txt: Information for systems that form BHs through direct collapse</li> <li>PISN.txt: Sampled systems which undergo PISN.</li> <li>PPISN.txt: Systems that fall in the range where we expect PPISN to occur. Information is provided assuming both direct collapse and PPISN mass loss, so the effect of PPISNe can be distinguished.</li> <li>volume.txt: Comoving value for the simulation. All the formed BHs and PISN listed can be assumed to be a complete sample of a box of this size through cosmic time (formed by the CHE channel of course, we don't include our evolutionary channels here).</li> </ol> <p>The data contained for these systems is</p> <ol> <li>"M1i[Msun]", "Pi[days]", "Z", "z_b": Initial primary mass (same as secondary), orbital period in days, metallicity and birth redshift. We assume the time between birth and formation of the binary black hole or PISN event is negligible.</li> <li>"M1f[Msun]", "Pf[days]": For the case of BH formation, these indicate the mass of the black hole formed by the primary (which is equal to the secondary) and the orbital period at BBH formation. For the case of systems undergoing PISN, they represent instead the properties at the onset of the PISN.</li> <li>"spin": Spin of each BH. We assume the spin is aligned with the orbit. Not included for PISN systems.</li> <li>"z_m": Redshift at which the BBH would merge from GW emission. Not included for PISN systems.</li> <li>"t_d[Gyr]": The delay time between BBH formation and merger due to GW emission. Not included for PISN systems.</li> <li>"p_*": Detection probability for the source assuming a random orientation of the source in the sky with respect to the detector. This includes "O1", "O2" and "O3" for LIGO's first observing runs, as well as "F" for LIGO's design sensitivity. "ET" is used for the detection probability for the Einstein telescope. Not included for PISN systems. Also, for the different studies of SFR variations we only considered LIGO at full design sensitivity and ET.</li> <li>All quantities denoted with "_pp" indicate variations to the previous values in the case we consider pulsational pair instability supernovae, as described in the paper.</li> </ol> <p>The Montecarlo simulations with kicks are not included, but can be recomputed using the source code provided.</p>
Binary 2D morphologies of polymer phase separation
<p>This dataset was generated through the simulation of a time evolving Cahn -Hilliard equation, describing phase separation in binary polymer blends. Several realizations of the equation were done through different values of volume fractions and binary interaction parameters. Morphologies were outputted at constant time intervals. Fill factor information for each instance has been provided as well.</p> <p> </p>
Massive donors in interacting binaries: impact of metallicity
<p>Input files needed to reproduce the simulations as well as output MESA history files (i.e. stellar tracks) to paper "Massive donors in interacting binaries: impact of metallicity". MESA version r11554.</p> <p>Output history files are provided for the models with the chosen reference set of input physical assumptions. History files from other models discussed in the paper can be provided upon request. </p> <p> </p>
Reproduction package for the paper "A strongly changing accretion morphology during the outburst decay of the neutron star X-ray binary 4U 1608-52"
<p>This is a basic reproduction package for the paper "A strongly changing accretion morphology during the outburst decay of the neutron star X-ray binary 4U 1608-52" by J. van den Eijnden et al. (2020). It provides reduced data sets, simulation scripts, X-ray spectral fits, and plotting scripts to allow the reproduction of the work performed in this paper. It also lists software used and data archives containing the public observational data. </p> <p>An open access version of the paper can be found at <a href="https://arxiv.org/abs/2002.04003">https://arxiv.org/abs/2002.04003</a>.</p>
Binary data files from a Sequoia Scientific, Inc Laser In Situ Scattering and Transmissometry sensor integrated into a Teledyne Webb Slocum Glider
<p>This dataset includes raw binary files from a Laser In Situ Scattering and Transmissometry (LISST) sensor integrated into a Teledyne Webb Slocum Glider. The glider deployment data can be found here: <a href="https://marine.rutgers.edu/cool/data/gliders/deployments/deployment.php?deployment=ru28-20170915T1416">(Rutgers Glider RU28</a>). The Sequoia Scientific, Inc. developed LISST particle sizing instrument was modified to fit within a Slocum glider science bay. Binary files can be processed with standard Sequoia Scientific, Inc processing software available here <a href="https://www.sequoiasci.com/product/lisst-200x/">https://www.sequoiasci.com/product/lisst-200x/</a>. Each binary file corresponds to a Slocum glider dive segment and is time synced with the glider RU28 data files. the LISST-Glider instrument was deployed on 09/15/2017 and recovered after 18 days on 10/03/2017.</p>
The evolution of massive binary stars
<p>Input files and data to reproduce the figures of the review paper "The Evolution of Massive Binary Stars".</p><p>Simulations shown in the paper were computed using the Modules for Experiments in Stellar Astrophysics code (MESA), with version r23.05.1 and compiled with the MESA SDK version x86_64-linux-22.6.1.</p><p>Figures were produced using the julia programming language version 1.9.2 together with Makie.jl. A Project.toml and Manifest.toml file are provided to reproduce the environment used to produce the figures.</p>
Hunting Down White Dwarf--Main Sequence Binaries Using Multi-Wavelength Observations
<p>Identification of white dwarfs (WD) with main-sequence (MS) companions and characterization of their properties can put important constraints on our understanding of binary stellar evolution and guide the theoretical predictions for a wide range of interesting transient events relevant for, e.g., Rubin Observatory (LSST), ZTF, and LISA. In this study, we combine ultraviolet (UV) and optical color-magnitude diagrams (CMDs) to identify unresolved WD--MS binaries. In particular, we combine high-precision astrometric and photometric data in the optical from \gaia\ -DR3 and UV data from GALEX GR6/7 to identify 93 WD--MS candidates within 100 pc. Of these, 80 are newly identified. Using the Virtual Observatory SED Analyzer (VOSA) we fit the spectral energy distributions (SEDs) of all our candidates and derive stellar parameters, such as effective temperature, bolometric luminosity, and radius for both companions. We find that our identification method helps identify hotter and smaller WD companions (majority with ≥ 10,000 K and ≤ 0.02 R_Sun) relative to the WDs identified by past surveys. We infer that these WDs are relatively more massive (median ~0.76 M_Sun). We find that most of the MS companions in our binaries are of the K and M spectral types. </p>
An upper limit on the spins of merging binary black holes formed through binary evolution
<p>Input files to reproduce simulations of the paper "An upper limit on the spins of merging binary black holes formed through binary evolution". Mesa version used was r23.05.01 with the MESA SDK x86_64-linux-22.6.1 for stripped star models and MESA version 11701 with MESA SDK x86_64-linux-20190503 for binary models (to reproduce old results). Files for MESA simulations are contained in the folder 'mesa_models', containing the following:</p><ul><li>bin_models: Binary evolution models for a chemically homogeneous binary evolved with different models for angular momentum transport.<ul><li>original: Original simulation from du Buisson et al. 2020 using the TS dynamo</li><li>TSF_Fuller_Lu2021: Same simulation but using the model for the TS dynamo of Fuller & Lu 2021</li><li>solid_body: Simulation done with solid body rotation</li></ul></li><li>Z10Msun: stripped star models with metallicity Zsun/10. Each folder inside contains one model labeled by log10(M/Msun)</li><li>Z50Msun: stripped star models with metallicity Zsun/50. Each folder inside contains one model labeled by log10(M/Msun)</li><li>Z250Msun: stripped star models with metallicity Zsun/250. Each folder inside contains one model labeled by log10(M/Msun)</li></ul><p>In addition, scripts to reproduce figures are included. These were done with julia version 1.9.2 and the Makie plotting package. A Manifest.toml and Project.toml are included to reproduce the environment used to produce the figures and analyze results. The included files are:</p><ul><li>waveform.jl: Recalculates detection probabilities of du Buisson et al. 2020 including the effect of spin.</li><li>simplified_model.jl: Produces figures related to the semi-analytical model presented in the paper. Used for figures 1-4 of the paper</li><li>merger_rates.jl: Produces merger rate predictions. Used for figures 5-10 of the paper.</li></ul><p>Extra folders included are:</p><ul><li>ComputerModernFont: Fonts used for plotting</li><li>duBuisson_data: Original data from du Buisson et al. 2020. This includes both the outcomes of their mesa grids and their population synthesis calculations (see https://zenodo.org/records/3667546 for details).</li><li>sensitivity_curves: Sensitivity curves for GW detectors used to recompute detection probabilities<br><br> </li></ul>
First photometric study and Light curve analysis of the four short period eclipsing binaries: $ZTFJ000030.44 +391106.9$, $ZTFJ000817.08+402532.1$, $ZTFJ002158.44+252934.04$ and $ZTFJ003357.62+415747.8$
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Transneptunian Binary Orbit Fits
<p>A set of Keplerian and non-Keplerian fits to the orbits of 45 individual TNO binaries. We provide full MCMC chains of our fits, as well as all diagnostics and outputs. We have verified that all Keplerian fits are converged. Non-Keplerian fits are not converged in almost all cases, but were run for a set amount of steps to try and identify targets for longer, converged analyses. A full paper about these fits and a discussion of their implications will soon be submitted to the Planetary Science Journal (PSJ).</p> <p>We provide these fits to allow anyone to fully examine the outputs of our fitting process. They can also be used a starting point for future analyses as the MCMC chains contain a full posterior distribution of the orbital properties of each TNO binary. A readme is contained within the dataset describing the outputs and the use of the MCMC chains. For any further assistance, please contact us.</p> <p>A "frozen" version of MultiMoon compatible with the dataset is also included.</p>
Data supplement for "Drops of volatile binary mixtures on brush-covered substrates"
<p>This dataset contains supplementary data for the following publication:</p> <p>Diekmann, J. & Thiele, U.<br>Drops of volatile binary mixtures on brush-covered substrates<br>EPJ-ST: Vol. 233, p. 1615-1624, 2024<br>doi: 10.1140/epjs/s11734-024-01169-4</p> <p> </p> <p>We provide the data and sources necessary to generate figure 2.</p>
Data release: "The metallicity dependence and evolutionary times of merging binary black holes: Combined constraints from individual gravitational-wave detections and the stochastic background"
<p>This data release contains the data to reproduce the results of "<strong>The metallicity dependence and evolutionary times of merging binary black holes: Combined constraints from individual gravitational-wave detections and the stochastic background</strong>" (<a href="https://arxiv.org/abs/2310.17625">arXiv:2310.17625</a>, published version <a href="https://iopscience.iop.org/article/10.3847/1538-4357/ad3d5c">here</a>).</p> <p>The code that was used to generate this data can be found on <a href="https://github.com/kevinturbang/bbh_gwb_time_delay_inference">this GitHub repository</a>. Jupyter notebooks to reproduce the figures of the paper are also included, and can be found <a href="https://github.com/kevinturbang/bbh_gwb_time_delay_inference/tree/main/figures">here</a>.</p>
PixelPop: Nonparametric analysis of correlations in the binary black hole population with LIGO–Virgo–KAGRA data
<p>Data release accompanying the PixelPop papers, analyzing gravitational wave populations.</p> <p>The first dataset (in gwtc3_result_files) is the posterior samples for the runs presented in analysis of LIGO--Virgo--KAGRA data, following the third gravitational wave catalog, see https://arxiv.org/abs/2406.16844. We include a python notebook (example_plot.ipynb) showing how to create the plots presented in this paper.</p> <p>In v2, we also include samples from the predictive distributions. Due to the large uncertainties, marginalizing over the hyperposterior may be a poor representation of the inferred distribution, and so instead we provide samples from the <em>median</em> predictive distribution. That is, samples from the distribution shown in the central panels of the figures. </p> <p>The second dataset (in o4inj_result_files) is the posterior samples accompanying the runs presented in the technical background paper, see https://arxiv.org/abs/2406.16813. </p>
Binary Classification Datasets
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Light curves from Gaia for single stars reported as unresolved binary candidates
<p>Light curves corresponding to the <em>Gaia</em> passbands <em>RP</em> (red), <em>G</em> (green), and <em>BP</em> (blue) for single stars reported as unresolved binary candidates. Isolated outliers (represented by crosses) are photometric errors, not consistent with flares, automatically rejected by variability processing. </p>
Table A.5: Eclipsing binaries
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