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5,090 results for “Black Hole”
Visualization of a black hole scattering and capture orbit
<div> <div>Numerical simulation of two black holes that scatter and then merge, emitting</div> <div>gravitational waves. Simulation with the SpEC code and wave extraction with the</div> <div>SpECTRE code by Oliver Long.</div> </div>
It's written in the massive stars: The role of stellar physics in the formation of black holes
<p>This repository contains additional data for the paper "It's written in the massive stars: The role of stellar physics in the formation of black holes" by E. Laplace, F.R.N. Schneider, and Ph. Podsiadlowski (2024).</p> <p> </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>
Data and scripts for: "Exceptional point and hysteresis in perturbations of Kerr black holes" and "Massive scalar perturbations in Kerr Black Holes: near extremal analysis"
<p>Datasets associated with the article <strong>Exceptional point and hysteresis in perturbations of Kerr black holes </strong>- arXiv:2407.20850 [gr-qc] and <strong>Massive scalar perturbations in Kerr Black Holes: near extremal analysis</strong> - 2408.13964 [gr-qc]. The file Isomonodromy.zip contains three subfolders and the file CFM.zip contains two subfolders. Each subfolder includes a readme file that provides a description of the folder contents. A brief description of each subfolder is given below:</p> <p><strong>1) Isomonodromy.zip</strong></p> <p>1.1) Folder "Data" contains data obtained through the isomonodromic method. Data consists of radial eigenvalues (quasinormal frequencies) and angular eigenvalues as a function of the mass of the scalar field and the spin of the Kerr black hole. </p> <p>1.2) Folder "Notebook - Mathematica" contains a Mathematica notebook to compute the angular eigenvalue expansion and the asymptotic expression for the frequency in the extremal limit. </p> <p>1.3) Folder "Script - Julia" constains a script that implements the isomonodromic method to compute quasinormal modes of massive scalar perturbations in Kerr black holes.</p> <p>Note: This script has been tested with Julia 1.10.7 LTS and ArbNumerics 1.5.3. It is currently NOT compatible with Julia 1.11.X, likely due to changes in memory allocation breaking compatibility with libArb.</p> <p><strong>2) CFM.zip</strong></p> <p>1.1) Folder "Data" contains data obtained through the continued fraction method. Data consists of radial eigenvalues (quasinormal frequencies) and angular eigenvalues as a function of the mass of the scalar field and the spin of the Kerr black hole. </p> <p>1.2) Folder "Notebook - Mathematica" implements the continued fraction method to compute quasinormal modes of massive scalar perturbations in Kerr black holes.</p>
Gravitational Wave Memory Imprints on the CMB from Populations of Massive Black Hole Mergers
<p>Visualisation videos of the effect of gravitational wave (GW) memory onto photons from the cosmic microwave background (CMB).</p>
Data for: `Limits on planetary-mass primordial black holes from the OGLE high-cadence survey of the Magellanic Clouds'
<p>This repository contains data presented in the paper "Limits on planetary-mass primordial black holes from the OGLE high-cadence survey of the Magellanic Clouds".</p>
Posterior samples for "Frequency-Domain Analysis of Black-Hole Ringdowns"
<p>Posterior files associated with <em>Frequency-Domain Analysis of Black-Hole Ringdowns</em> (<a href="http://arxiv.org/abs/2108.09344">arxiv:2108.09344</a>, <a href="https://journals.aps.org/prd/abstract/10.1103/PhysRevD.104.123034">Phys. Rev. D <strong>104</strong>, 123034</a>).</p> <p>Folder naming:</p> <ul> <li>{event name} <ul> <li>SNR{injection signal-to-noise ratio} <ul> <li>frequency_domain <ul> <li>{number of wavelets included in the model}W{QNM content described by lmn indices} <ul> <li>{ringdown start time in ms}_{ringdown start time prior width in ms}</li> </ul> </li> </ul> </li> <li>time_domain <ul> <li>{QNM content described by lmn indices} <ul> <li>{ringdown start time in ms}_{ringdown start time prior width in ms}</li> </ul> </li> </ul> </li> </ul> </li> </ul> </li> </ul> <p> </p> <p>For example, the file </p> <p>GW190521/SNR15/frequency_domain/1W220/12-7_01/posterior_samples.dat</p> <p>contains the results of a frequency-domain analysis of the GW190521-like injection (at signal-to-noise ratio 15) using <span class="math-tex">\(W=1\)</span> wavelet with just the fundamental <span class="math-tex">\(\ell = m = 2\)</span>, <span class="math-tex">\(n=0\)</span> QNM. It has a Gaussian prior on the ringdown start time centered 12.7 ms after the time of peak strain, with a width of 1 ms.</p> <p>The special-case two-interferometer analysis with Virgo excluded has "_HL" appended to its folder name.</p> <p>Each directory contains a 'posterior_samples.dat' file (see the 'plot_example.ipynb' for more information on reading the posterior files) and a 'sampler_output.json' which contains the log-evidence and the estimated error on the log-evidence.</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>
General-Relativistic Hydrodynamics Simulation of a Neutron Star — Sub-Solar-Mass Black Hole Merger - 3D Density Visualization
<p>Matter density distribution of our simulation of a neutron star -- sub-solar mass black hole merger; cf. color bar to obtain a density estimate. The gray region represents the apparent horizon of the black hole.</p> <p>Visualization: Ivan Markin (University of Potsdam); Data: Swami Vivekanandji Chaurasia (Stockholm University)</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 shown here has been run on HLRN.</p>
General-Relativistic Hydrodynamics Simulation of a Neutron Star — Sub-Solar-Mass Black Hole Merger - Kilonova Luminosity Evolution Visualization
<p>Evolution of luminosity maps as seen by observers from the pole with Θ = 0° and from the four angles Φ = 0°, Φ = 90°, Φ = 180° and Φ = 270° in the equatorial plane with Θ = 90°. The maps show the luminosity from each region of the ejecta integrated along the line of sight and are calculated in (6000 − 8000) Å band at 1 day after the merger.</p> <p>Visualization: Ivan Markin (University of Potsdam), Mattia Bulla (University of Ferrara); Data: Anna Neuweiler (University of Potsdam), Swami Vivekanandji Chaurasia (Stockholm University)</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 shown here has been run on HLRN.</p>
Supplementary animations for "Scalar dark matter vortex stabilization with black holes"
<p>Supplementary animations for <a href="https://doi.org/10.48550/arXiv.2301.13220">Scalar dark matter vortex stabilization with black holes</a>, <a href="https://arxiv.org/abs/2301.13220">arxiv:2301.13220, </a><a href="https://doi.org/10.1088/1475-7516/2023/07/004">https://doi.org/10.1088/1475-7516/2023/07/004</a></p>
Data Release: "A parameter-free tour of the binary black hole population"
<p>This dataset contains the results presented in "<strong>A parameter-free tour of the binary black hole population</strong>" (<a href="http://arxiv.org/abs/2302.07289">arXiv:2302.07289</a>).</p> <p>The code used to generate this data can be found in the repository <a href="https://github.com/tcallister/autoregressive-bbh-inference/">https://github.com/tcallister/autoregressive-bbh-inference/</a>. This repository includes <a href="https://github.com/tcallister/autoregressive-bbh-inference/tree/main/data">jupyter notebooks</a> that can be used to open, explore, and plot the files contained in this data set. Additional information about reproducing and/or using this dataset can be found in <a href="https://tcallister.github.io/autoregressive-bbh-inference/">our associated documentation</a>.</p> <p>Further notes:</p> <ul> <li>The files <em>sampleDict_FAR_1_in_1_yr.pickle</em> and <em>injectionDict_FAR_1_in_1.pickle</em>, used as inputs to our analyses, are created via code in the repository <a href="https://github.com/tcallister/get-lvk-data">https://github.com/tcallister/get-lvk-data</a> (see also <a href="https://zenodo.org/record/6505409">https://zenodo.org/record/6505409</a>).</li> <li>The files <em>posteriors_gaussian_spin_samples_FAR_1_in_1.json</em> and <em>o1o2o3_mass_c_iid_mag_iid_tilt_powerlaw_redshift_result.json</em>, used for figure generation, were published by the LIGO Scientific Collaboration, Virgo Collaboration, and KAGRA Collaboration in support of the paper "<a href="https://arxiv.org/abs/2111.03634">The population of merging compact binaries inferred using gravitational waves through GWTC-3</a>" (see <a href="https://zenodo.org/record/5655785">https://zenodo.org/record/5655785</a>).</li> </ul> <p><em>New in this version: </em>This version (Version 3) contains the the newest results generated in the first round of journal referee review and reflected in v2 of the arXiv listing. Includes re-run of all analyses with updated priors, and new results from the injection study discussed in Appendix C.</p>
Dataset: "GW190521: tracing imprints of spin-precession on the most massive black hole binary"
<p>This dataset contains the results presented in "<em>GW190521: tracing imprints of spin-precession on the most massive black hole binary</em>": <a href="https://arxiv.org/abs/2310.01544">https://arxiv.org/abs/2310.01544</a>.</p> <p>The accompanying repository used to take this data and generate the figures in the paper can be found at <a href="https://github.com/simonajmiller/gw190521-timedomain-release/">https://github.com/simonajmiller/gw190521-timedomain-release/</a>.</p>
Supplementary data for paper "Extreme mass-ratio inspiral and waveforms for a spinning body into a Kerr black hole via osculating geodesics and near-identity transformations"
<p>Radiation-reaction fluxes and NIT interpolant data for paper "Extreme mass-ratio inspiral and waveforms for a spinning body into a Kerr black hole via osculating geodesics and near-identity transformations"</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>
Properties of OB star−black hole systems derived from detailedbinary evolution models
<p>Input files to reproduce the MESA simulations used in <a href="https://arxiv.org/abs/1912.09826">Langer et al. (2020)</a></p> <p>MESA version 8845</p> <p>For instructions, refer to the README.md file included.</p>
Is the red and bule colour in the picture are noise?If not then in this photo threre are picture of Black hole
<p>I randomly capturing the sky picture on north side of the sky to take the picture of saptarishimandal. I get this surprising picture like CMB. If ,this is not noise then there sre the picture of black hole ,the objects in the picture whose centre are deep black and sorrounded by bright light.</p> <p> </p>
The impact of stellar rotation on the black hole mass-gap from pair-instability supernovae
<p>Necessary files to reproduce the simulations of the paper "The impact of stellar rotation on the black hole mass-gap from pair-instability supernovae", as well as simulation output.</p> <p>These simulations were performed using MESA version 13311, with a small bugfix that can be applied with the provided <a href="https://zenodo.org/api/files/b21500e4-6cb5-4e3e-b8c5-83d769b24161/hydro_riemann.f90?versionId=36bcfc7a-4535-4494-ba2b-c7ea69b9b362">hydro_riemann.f90</a> file.</p> <p>A description of the included files is as follows:</p> <ul> <li><a href="https://zenodo.org/api/files/b21500e4-6cb5-4e3e-b8c5-83d769b24161/final_profiles.tar.gz?versionId=b85755ce-cd64-4e6b-ac14-d9e5364ee86b">final_profiles.tar.gz</a>: Individual profiles for all models at iron-core collapse (or last profile for PISN models). Files are separated into three folders, 'non_rot', 'rot_ST', 'rot_no_ST' corresponding to non-rotating models, rotating models with ST and rotating models without ST. Names of individual files contain the initial mass and the initial ratio between surface omega and its critical value. So for example, a file named "50.00_0.90_profile.data" represents an initial mass of 50 Msun and an initial rotation rate of 0.9 times critical. This work only contains non-rotating models and models at 0.9 critical though.</li> <li><a href="https://zenodo.org/api/files/b21500e4-6cb5-4e3e-b8c5-83d769b24161/histories.tar.gz?versionId=d3876d5e-c95e-4945-8715-9da428837afa">histories.tar.gz</a>: MESA history files containing various stellar properties describable by a single number at each timestep of the simulation (for instance, mass, effective temperature, etc...). Files follow the same naming scheme as those in final_profiles.tar.gz. For each simulation there is an additional file with a name ending in "pulse_indexes" that contains various lines with two integers per line. These specify for PPISN models the simulation step (or model_number in MESA-speak) at which a pulsation begins, and the step at which it ends.</li> <li><a href="https://zenodo.org/api/files/b21500e4-6cb5-4e3e-b8c5-83d769b24161/tables.tar.gz?versionId=69974ece-20e5-4509-a1a4-7dad7a92f4b6">tables.tar.gz</a>: Machine readable tables summarizing our simulations, these correspond to the data shown in the tables in the paper. The names of the tables "non_rot.txt", "rot_ST.txt" and "rot_no_ST.txt" correspond to non-rotating models, rotating models with ST and rotation models without ST respectively. The meaning of each column is: <ul> <li>M_i[Msun]: Initial mass of the helium star</li> <li>(om/omc)_i: Ratio between omega and its critical value at the star of core helium burning.</li> <li>M_Hedep[Msun]: Mass of the star at core helium depletion</li> <li>M_CO[Msun]: Carbon oxygen core mass at core helium depletion. Defined as the innermost mass coordinate at which Y<0.01.</li> <li>M_preSN[Msun]: Mass at the onset of PPISN/PISN. For models that do not undergo pair-instability, it corresponds to the mass at iron-core collapse.</li> <li>M_He,preSN[Msun]: Total mass in helium of the star at the onset of PPISN/PISN, or at iron-core collapse for non pair-unstable models. This does not represent the mass of the helium-rich envelope, but the total baryonic mass in helium of the star.</li> <li>M_ejecta[Msun]: Mass ejected by pulsations.</li> <li>M_final[Msun]: Final mass of the star at iron-core collapse.</li> <li>number_of_pulses: Number of pulsations.</li> <li>time_to_coll[yrs]: Time between the first pulse and iron-core collapse.</li> <li>max_KE[foe]: Maximum kinetic energy achieved by any pulse, measured in 10^51 erg/s=1 foe.</li> <li>a_i: Dimensionless spin of the star (a=jc/Gm) at the beginning of core helium burning.</li> <li>a_he_dep: Dimensionless spin at core helium depletion</li> <li>a_preSN: Dimensionless spin at the onset of PPISN/PISN.</li> <li>a_f: Final dimensionless spin from our simulations at iron-core collapse.</li> <li>BH_mass[Msun]: Final BH mass predicted from the properties of our model at iron-core collapse following Batta & Ramirez-Ruiz (2019).</li> <li>BH_spin: Final BH spin predicted from the properties of our model at iron-core collapse following Batta & Ramirez-Ruiz (2019).</li> </ul> </li> <li><a href="https://zenodo.org/api/files/b21500e4-6cb5-4e3e-b8c5-83d769b24161/pulses.tar.gz?versionId=5afe548e-3f3f-429a-98f6-b3cb14c77cc6">pulses.tar.gz</a>: Information on individual pulses for each PPISN simulation in our grid. Files are contained in three separate folders "non_rot", "rot_ST" and "rot_no_ST" for models that are non-rotating, rotating with ST and rotating without ST respectively. Naming of individual files is the same as those in final_profiles.tar.gz. Information contained in these tables is: <ul> <li>pulse_num: Integer identifying the pulse.</li> <li>ejecta[Msun]: Total mass ejected by the pulse.</li> <li>time_to_coll[yrs]: Time between the onset of this pulse and iron-core collapse.</li> <li>KE[foe]: Maximum kinetic energy reached during the pulse.</li> </ul> </li> <li><a href="https://zenodo.org/api/files/b21500e4-6cb5-4e3e-b8c5-83d769b24161/template_ST.tar.gz?versionId=ac1563c9-5b0c-422a-8739-2fbc82ff5788">template_ST.tar.gz</a>: Template used for simulations. This template is setup for the simulations that include the ST dynamo and have an initial rotation rate of 90% critical. To modify the rotation rate and the initial mass, modify new_omega_div_omega_crit and initial_mass in the inlist_extra file. To turn of ST, set am_nu_ST_factor=0 in inlist_ppisn. Only one model required additional tuning to comple, the 60 Msun rotating model with ST. For this one, the model was restarted at step 98000 with the value of the option x_ctrl(18) switched from 0.025d0 to 0.25d0. This particular simulation did not reach the automated terminating condition and was stopped manually, but at the end it does have a collapsing iron-core with an infall velocity ~5000 km/s.</li> <li><a href="https://zenodo.org/api/files/b21500e4-6cb5-4e3e-b8c5-83d769b24161/notebook.tar.gz?versionId=d59d2404-1517-4c0a-910e-4adbc14511f8">notebook.tar.gz</a>: jupyter notebook used to process the data from our simulations and produce tables and figures (except for the information on the spin of the primary BH of GW170729).</li> <li><a href="https://zenodo.org/api/files/b21500e4-6cb5-4e3e-b8c5-83d769b24161/GW170729_spin.tar.gz?versionId=47f46740-3c0d-4355-b2a2-9d7a454f388b">GW170729_spin.tar.gz</a>: jupyter notebook used to compute the spin posterior of GW170729 using the data from the first catalogue of gravitational wave transients.</li> </ul>
Data for the paper 'WISDOM Project - VI. Exploring the relation between supermassive black hole mass and galaxy rotation with molecular gas '
<p>This upload includes the data underlying the MNRAS paper Smith et al. (2020) entitled 'WISDOM Project - VI. Exploring the relation between supermassive black hole mass and galaxy rotation with molecular gas' (arXiv:2010.08565). The full author list is available from the paper, and we request that this paper is cited if this data is used in future publications.</p> <p>The upload includes machine-readable versions (csv) of Tables 3, 4, A1 and A2 of the paper. The upload also includes the calibrated spectra from the two observing programmes (191-18 at the IRAM 30m telescope and 2018-04a at the OSO 20m telescope), and the homogenised spectra used in the project. Full descriptions are given in the paper. </p> <p>Table 3: CubeData.csv; The table contains the determined line widths, inclinations, and SMBH masses used for the resolved sample of this project. The references from which the cubes were obtained, are listed in Table 3 of the paper.</p> <p>UnresolvedData.csv: Table 4; The table contains the determined line widths, inclinations, and SMBH masses used for the unresolved sample of this project. The references from which the spectra were obtained, are listed in Table 4 of the paper.</p> <p>IRAMData.csv: Table A1; The table contains a list of galaxies observed using the IRAM 30m telescope as part of project 191-18. For each galaxy the rms noise is listed, and for detected galaxies the spectrally-integrated line intensity measured over the specified velocity range given. The inferred molecular gas mass is also listed. </p> <p>OSO20mData.csv: Table A2; The table contains a list of galaxies observed using the OSO 20m telescope as part of project 2018-04a. For each galaxy the rms noise is listed, and for detected galaxies the spectrally-integrated line intensity measured over the specified velocity range given. The inferred molecular gas mass is also listed. </p> <p>IRAM30m_191-18.tar: Calibrated spectra from programme 191-18.</p> <p>OSO2018-04a.tar: Calibrated spectra from programme 2018-04a.</p> <p>ResolvedSample.tar: Homogenised spectra for the spatially-resolved sample. Note that some spectra were sourced from other works, the original references are given in the fits headers.</p> <p>UnresolvedSample.tar: Homogenised spectra for the spatially-unresolved sample. Note that some spectra were sourced from other works, the original references are given in the fits headers.</p>
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