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5,090 results for “Black Hole”
Precessing binary-black-hole numerical relativity catalogue (complete data release)
<p>This page contains the minimal data release associated with the catalogue presented in <a href="https://dcc.ligo.org/DocDB/0186/P2300054/001/catalogue.pdf">A catalogue of precessing black-hole-binary numerical-relativity simulations</a>. This catalogue contains 80 single-spin precessing black-hole-binary configurations. </p> <p>The content of the data release is described <a href="https://data.cardiffgravity.org/bam-catalogue/">here</a>, along with instructions on how to parse the data.</p>
Abell 1201: Detection of an Ultramassive Black Hole in a Strong Gravitational Lens
<p>A preprint of the paper "Abell 1201: Detection of an Ultramassive Black Hole in a Strong Gravitational Lens".</p> <p>This repository also contains lens analysis scripts, plotting routines and dynesty chains of the paper.</p>
General-Relativistic Hydrodynamics Simulation of a Neutron Star — Sub-Solar-Mass Black Hole Merger - 3D Ejecta Data
<p>This dataset contains the 3D output for NSbh_R2 run at refinement level l=1 and simulation time t=7950 (t=39.16 ms).</p> <p>Data: Swami Vivekanandji Chaurasia (Stockholm University), Data release packaging: Ivan Markin (University of Potsdam);</p> <p>Simulations for the project have been performed on the national supercomputer HPE Apollo Hawk at the High Performance Computing (HPC) Center Stuttgart (HLRS) under the grant number GWanalysis/44189, on the GCS Supercomputer SuperMUC NG at the Leibniz Supercomputing Centre (LRZ) [project pn29ba], and on the HPC systems Lise/Emmy of the North German Supercomputing Alliance (HLRN) [project bbp00049] for the final production runs. The particular simulation has been run on HLRN.</p>
Example input files for Wolf-Rayet star models in paper "Tidal Spin-up of Black Hole Progenitor Stars"
<p>The files here show example input files for the models in the paper "Tidal Spin-up of Black Hole Progenitor Stars" by Ma & Fuller (2023).</p> <p>File "inlist_MS" and "inlist_WR" show MESA inlists to set up a Wolf-Rayet star model of 10 solar-masses (model 3 in Ma & Fuller 2023, Table 1).<br> We used MESA version r12778 for our calculation.<br> Specifically, "inlist_MS" starts a stellar model at zero-age main-sequence (ZAMS), and evolves it to the end of core hydrogen depletion.<br> After resuming the model from a photo file, "inlist_WR" turns on artificial mass-loss ("relax_mass" and "new_mass") to remove its hydrogen envelope, and then evolves the model throughout the helium burning Wolf-Rayet phase, until the end of core helium depletion.<br> During this phase, pulsation data are also created by MESA ("write_pulse_data_with_profile = .true.").</p> <p><br> File "gyre.in" is an example GYRE input file to solve for oscillation modes in the established Wolf-Rayet star models.<br> We used GYRE version 6.0.1 for our calculation.</p>
GPR surrogate model dataset for remnant black hole properties using perturbation theory and NR
<p>This is the data-set used in <strong><code>BHPTNR_Remnant</code></strong> which is an easy-to-use python package to efficiently predict the remnant mass, remnant spin, peak luminosity and the final kick imparted on the remnant black hole directly from the gravitational radiation using GPR fits. These fits have been built on the remnant data calculated from numerical relativity informed black hole perturbation theory based waveforms.</p>
Example calculation of E1[h1] contribution to the source for second-order metric perturbations of a Schwarzschild black hole
<p>This repository contains data for the h1 an dr0/h1 perturbations that can be used to compute a piece of the source for the second-order metric perturbation. The Mathematica notebook 'SecondOrderE1h1.nb' shows how to combine the data to compute E1[h1].</p> <p>The h1 data was computed using the h1Lorenz code that is available in the Black Hole Perturbation Toolkit (https://github.com/BlackHolePerturbationToolkit/h1Lorenz). The dr0/dh1 data was computed by Leanne Durkan following the method detailed in "Slow evolution of the metric perturbation due to a quasicircular inspiral into a Schwarzschild black hole" by Leanne Durkan and Niels Warburton, arXiv:2206.08179</p> <p>Authors: Leanne Durkan, Niels Warburton</p>
Modified Gravity and the Black Hole Mass Gap
<p><strong>Reproduction package for the paper "Modified Gravity and the Black Hole Mass Gap".</strong></p> <p> </p> <p><strong>The package contains inlist and run_star_extra.f files for MESA that can be used to generate grids of ZAMS models for custom values of the gravitational constant. Also included are inlist and run_star_extra.f files for the PPISN test suite demonstrating how to change the value of G and how to load the ZAMS files during the post-pulse relaxation process. </strong></p>
Dataset from: Fallback Supernova Assembly of Heavy Binary Neutron Stars and Light Black Hole-Neutron Star Pairs and the Common Stellar Ancestry of GW190425 and GW200115
<p>The results of the simulations shown in "Fallback Supernova Assembly of Heavy Binary Neutron Stars and Light Black Hole-Neutron Star Pairs and the Common Stellar Ancestry of GW190425 and GW200115" (<a href="https://arxiv.org/abs/2106.12381">arXiv:2106.12381</a>).</p> <p>Contents:</p> <ol> <li>Run_Details_COMPAS</li> <li>COMPAS_Output_*.hdf5</li> <li>MESA.zip</li> <li>GADGET.zip</li> </ol> <p>If you use any of these data please kindly include a citation to:<br> Alejandro Vigna-Gómez <em>et al</em> 2021 <em>ApJL</em> <strong>920</strong> L17 <a href="https://iopscience.iop.org/article/10.3847/2041-8213/ac2903">doi:10.3847/2041-8213/ac2903</a></p> <p>If you use the MESA profile or history files please also cite:</p> <p>Aguilera-Dena, D.R., et al., in prep.</p> <p>Additionally, we point the reader towards the following GitHub repositories:<br> 1) <a href="https://github.com/aldobatta/fallback-supernova">aldobatta/fallback-supernova</a><br> 2) <a href="https://github.com/avigna/heavy-BinaryNeutronStars">avigna/heavy-BinaryNeutronStars</a></p>
IMPETUS: New Cloudy's radiative tables for accretion onto a galaxy black hole. Calculations II. Table 2.
<p>This is a .ZIP file, which contains the results of Calculations II. The main directory contains sub-directories with ascii files. Each column is properly described in the article.</p>
IMPETUS: New Cloudy's radiative tables for accretion onto a galaxy black hole. Calculations I. Table 2.
<p>This is a .ZIP file, which contains the results of Calculations I. The main directory contains sub-directories with ascii files. Each column is properly described in the article.</p>
IMPETUS: New Cloudy's radiative tables for accretion onto a galaxy black hole. Calculations I-VI. Table 2.
<p>These are gzipped/tar files, which contain the results of Calculations I-VI. The main directories contain sub-directories with ascii files. Each column is properly described in the article. The equilibrium temperature for any configuration can be calculated and plot with the new script at https://doi.org/10.5281/zenodo.4381019.</p>
Dataset for Popov, Strokov, and Surdyaev 2021: Black hole shadows against an optically thick, geometrically thin disk
<p>The datasets contain images of an optically thick, geometrically thin accretion disk distorted by the presence of a Kerr black hole (i.e., black hole shadows). The images are in a compressed text format (.gz) as well as in a graphic format. The training dataset comprises 2,301 images for various values of the disk's outer radius, the spin and sense of rotation of the black hole, and for different viewing angles (w.r.t. the equatorial plane where the disk resides). The test set contains 89 images with parameters which were randomly sampled from the same ranges as in the training set. For details, see the works associated with this record.</p>
Cosmic Cousins: Identification of a Subpopulation of Binary Black Holes Consistent with Isolated Binary Evolution
<p>The accompanying data release for the analyses presented in "Cosmic Cousins: Identification of a Subpopulation of Binary Black Holes Consistent with Isolated Binary Evolution". See the github paper repository at https://github.com/jaxengodfrey/CosmicCousins and the arXiv release of the paper at: https://arxiv.org/abs/2304.01288</p>
Mimicking Mergers: Mistaking Black Hole Captures as Mergers
<p>This record is the data and code release to accompany the paper "Mimicking Mergers: Mistaking Black Hole Captures as Mergers", Guo et al. 2022.</p>
Data for: Bounds on the mass of superradiantly unstable scalar fields around Kerr black holes
<p>Datasets associated with the article <strong>Bounds on the mass of superradiantly unstable scalar fields around Kerr black holes</strong>, arXiv:2405.01003 [gr-qc]. The file datasets.zip contains four subfolders. Each subfolder includes a readme file that provides a description of the datasets. A brief description of each subfolder is given below:</p> <p>1) Folder "notebooks" contains minimal Mathematica notebooks that compute scalar clouds and superradiant instabilites of a Kerr black hole</p> <p>2) Folder "clouds" contains data for the mass of the scalar cloud as a function of the spin of the black hole</p> <p>3) Folder "max_instability" contains data for the peak of superradiant instabilities as a function of the spin of the black hole</p> <p>4) Folder "parameters" contains parameters for an analytical function that fits the numerical values of the mass of the scalar clouds of a Kerr black hole </p>
Mass-redshift dependency of Supermassive Black Hole Binaries for the Gravitational Wave Background
<p>These show the posterior distributions as supplementary material for arXiv:2305.18293 and doi:10.1093/mnras/stae1219</p> <p>The corner plots for the complete 20 parameters with amplitudes hc = 0.5e-15, 1e-15, 2e-15, 3e-15, and 4e-15 for both circular and eccentric population of SMBHBs are presented in the 'free_parameters' folder.</p> <p>The corner plots for the 16 parameters with amplitudes hc = 0.5e-15, 2e-15, and 4e-15 for both circular and eccentric population of SMBHBs using the fitted BH-bulge mass parameters from the simulations can be found in the 'simulation_parameters' folder.</p> <p>The posterior distributions are shown as black contours, while the prior distributions are denoted by light green lines. The top right inlay figure shows the median and central 2sigma range of the recovered characteristic spectrum, where the 5 points denote the frequency bins of 1/(25years), 2/(25years), 3/(25years), 4/(25years) and 5/(25years), which are used as the input data for the Bayesian analysis. To guide the eye the analytic sensitivity curve from the IPTA DR2 is also plotted.</p>
Do black holes remember what they are made of?
<p>This README document describes the contents of the BNS_Simulations.JSON data file used in the research paper titled "Do black holes remember what they are made of?" This JSON file contains all the data pertaining to various binary neutron star (BNS) simulations that were conducted as part of this project.</p> <p>File Content Descriptions:<br>##########################</p> <p>"EOS": This field represents the Equation of State used in the corresponding BNS simulation. There are a total of 15 different EOS used in this project that describes how matter behaves under different physical conditions during the simulation.</p> <p>"sim_name": This is the name of the corresponding BNS simulation run.</p> <p>"Resolution": This indicates the resolution quality of the simulation. It is either "LR" for Low Resolution or "SR" for Standard Resolution.</p> <p>"Grav Mass_1": This is the gravitational mass of the first neutron star in the corresponding BNS pair for the simulation and it is the lighter mass in case of unequal masses. The mass is measured in solar masses.</p> <p>"Grav Mass_2": Similar to "Grav Mass_1", this field denotes the gravitational mass of the second neutron star in the BNS pair and it is the heavier mass in the unequal masses. It is also measured in solar masses.</p> <p>"Lambda_1": This is the tidal parameter of the first neutron star for the corresponding BNS system.</p> <p>"Lambda_2": The tidal parameter for the second neutron star of the same BNS system.</p> <p>"A_22": This field represents the fit amplitude of the (l=2, m=2) mode strain at the point of its minimal mismatch.</p> <p>"A_21": This field contains the fit amplitude of the (l=2, m=1) mode strain, at at the point of minimal mismatch for the (l=2, m=2) mode.</p> <p>Please use this README as reference document to ensure correct interpretation of the data fields when analyzing the data set of the .JSON file and to maintain consistency in data usage across different parts of the research project.</p>
Multi-Generational Black Hole Population Analysis with an Astrophysically Informed Mass Function
<p>We analyze the population statistics of black holes in the LIGO/Virgo/KAGRA GWTC-3 catalog using a parametric mass function derived from simulations of massive stars experiencing pulsational pair-instability supernovae (PPISN). Our formalism enables us to separate the black hole mass function into sub-populations corresponding to mergers between objects formed via different astrophysical pathways, allowing us to infer the properties of black holes formed from stellar collapse and black holes formed via prior mergers separately. Applying this formalism, we find that this model fits the data better than the powerlaw+peak model with Bayes factor 9.7±0.1. We measure the location of the lower edge of the upper black hole mass gap to be 84.05<sub>-12.88</sub><sup>+17.19</sup> M<sub>☉</sub>, providing evidence that the 35M<sub>☉</sub> Gaussian peak detected in the data using other models is not associated with the PPISN pile-up predicted to precede this gap. Incorporating spin, we find that the normalized spins of stellar remnant black holes are close to zero while those of higher generation black holes tend to larger values. All of these results are in accordance with the predictions of stellar structure theory and black hole merger scenarios. Finally, we combine our mass function with the spectral siren method for measuring the Hubble constant to find H₀=36.19<sub>-10.91</sub><sup>+17.50</sup> km/s/Mpc and discuss potential explanations of this low value. Our results demonstrate how astrophysically-informed mass functions can facilitate the interpretation of gravitational wave catalog data to provide information about black hole formation and cosmology. Future data releases will improve the precision of our measurements.</p>
Binary black-hole simulation SXS:BBH:0180
Simulation of a black-hole binary system evolved by the <a href="https://www.black-holes.org/code/SpEC.html">SpEC code</a>.
Binary black-hole simulation SXS:BBH:0187
Simulation of a black-hole binary system evolved by the <a href="https://www.black-holes.org/code/SpEC.html">SpEC code</a>.
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.