Find research datasets worth reusing

opencc-by-4.0Mar 2020View details →

Reproduction package for the paper "The effects of surface fossil magnetic fields on massive star evolution - II. Implementation of magnetic braking in MESA and implications for the evolution of surface rotation in OB stars "

This is a reproduction package for the paper "The effects of surface fossil magnetic fields on massive star evolution - II. Implementation of magnetic braking in MESA and implications for the evolution of surface rotation in OB stars" by Keszthelyi et al. (2020), https://doi.org/10.1093/mnras/staa237

opencc-by-4.0Jan 2024View details →

A Study of Primordial Very Massive Star Evolution II: Stellar Rotation and Gamma-Ray Burst Progenitors

Wind ejecta tables of rotating very massive stars from the paper: <a href="https://iopscience.iop.org/article/10.3847/1538-4357/ad1185">A Study of Primordial Very Massive Star Evolution II: Stellar Rotation and Gamma-Ray Burst Progenitors</a>

opencc-by-4.0Nov 2021View details →

BHBH simulations from: Impact of Massive Binary Star and Cosmic Evolution on Gravitational Wave Observations II: Double Compact Object Mergers

The data for all BHBH simulations shown in "Impact of Massive Binary Star and Cosmic Evolution on Gravitational Wave Observations II: Double Compact Object Mergers".  Broekgaarden et al. (2021, submitted, preprint: <a href="https://arxiv.org/abs/2112.05763">https://arxiv.org/abs/2112.05763</a>)   Contents:  <ul> <li>18 zip files that each contain an hdf5 file with the raw data for one of the simulations from Table 1 in the paper. The only exception is the fiducial.zip file and the unstableCaseBB.zip file, which contain both the fiducial (model A) and 'optimistic CE' (model K) data file and the "unstable case BB" (model E)  and "unstable case BB + optimistic CE" (model F) files. These zip files are:  <ul> <li>fiducial.zip,  the Fiducial model (A) and Optimistic CE model (K)</li> <li>massTransferEfficiencyFixed_0_25.zip, the \(\beta\) = 0.25 model (B) </li> <li>massTransferEfficiencyFixed_0_5.zip, the \(\beta\) = 0.5 model (C) </li> <li>massTransferEfficiencyFixed_0_75.zip, the \(\beta\) = 0.75 model (D)</li> <li>unstableCaseBB.zip, the unstable case BB mass transfer model (E) and unstable case BB & optimistic CE model (F) </li> <li>alpha0_1 zip, the \(\alpha = 0.1\) model (G) </li> <li>alpha0_5.zip, the \(\alpha = 0.5\) model (H) </li> <li>alpha2_0.zip, the \(\alpha = 2.0\) model (I) </li> <li>alpha10_0.zip, the \(\alpha = 10.0\) model (J) </li> <li>rapid.zip, the rapid SN model (L) </li> <li>maxNSmass2_0.zip, the max \(m_{\rm{NS}} = 2\, \rm{M}_{\odot}\) model (M) </li> <li>maxNSmass3_0.zip, the max \(m_{\rm{NS}} = 3\, \rm{M}_{\odot}\) model (N)</li> <li>noPISN.zip, the no PISN model (O) </li> <li>ccSNkick_100km_s.zip, the \(\sigma_{\rm{cc}}\)= 100 km/s model (P) </li> <li>ccSNkick_30km_s.zip, the \(\sigma_{\rm{cc}}\)= 30 km/s model (Q)</li> <li> noBHkick.zip, the no BH SN kick model (R)</li> <li>wolf_rayet_multiplier_0_1.zip, the model with Wolf-Rayet wind factor \(f_{\rm{WR}} = 0.1\) (S)</li> <li>wolf_rayet_multiplier_5.zip, the model with Wolf-Rayet wind factor \(f_{\rm{WR}} = 5\) (T)  </li> </ul> </li> <li>2 more zip files containing csv files with the summarized rates to create Figures 1, 2 and 3, which do not require downloading the entire dataset, but instead use these csv files with the summarized rates:  <ul> <li>csvFilesForFigure1_DCOpaper.zip # contains the files to recreate figure 1 with the merger rates per metallicity for BH-BH, BH-NS and NS-NS: <ul> <li>formationRatesTotalAndPerChannel_BHBH_.csv</li> <li>formationRatesTotalAndPerChannel_BHNS_.csv</li> <li>formationRatesTotalAndPerChannel_NSNS_.csv</li> </ul> </li> <li>csvFilesForFigure2_and_3_DCOpaper.zip # contains the files to recreate figure 2 with the merger rates for intrinsic and GW detection weighted, containing the csv files with names:  <ul> <li>rates_MSSFR_Models_BHBH_AllDCOsimulation.csv</li> <li>rates_MSSFR_Models_NSNS_AllDCOsimulation.csv</li> <li>rates_MSSFR_Models_BHNS_AllDCOsimulation.csv</li> </ul> </li> </ul> </li> </ul>   Details of how to use the data (a readme),  as well as scripts to reproduce all results, plots, and figures from the paper are given in the accompanying Github repository <a href="https://github.com/FloorBroekgaarden/Double-Compact-Object-Mergers">https://github.com/FloorBroekgaarden/Double-Compact-Object-Mergers</a>  If you use this data, please cite  Broekgaarden et al. (2021): see <a href="https://ui.adsabs.harvard.edu/abs/2021arXiv211205763B/abstract">https://ui.adsabs.harvard.edu/abs/2021arXiv211205763B/abstract</a>

opencc-by-4.0Feb 2022View details →

Dataset for Bate (2022): Dust coagulation during the early stages of star formation: molecular cloud collapse and first hydrostatic core evolution

This data set contains 12 smoothed particle hydrodynamics (SPH) dump files that were used to produce some of the figures in the journal paper: Bate, Matthew. R., 2022, Monthly Notices of the Royal Astronomical Society, accepted 13 May 2022 Each of the SPH dump files is from a different calculation of the early stages of star formation: the gravitational collapse of a molecular cloud core, including dust coagulation.  Each SPH dump file gives the state of the SPH calculation when the maximum temperature reached 1500 K, except for the beta=0.05 cases which give the state when the maximum hydrogen number density reaches 10^{14} cm^{-3}.  The calculations were each performed using 3 million SPH particles and differed by their initial rotation rate, which was parameterised by beta=0, 0.0025, 0.005, 0.01, 0.02, and 0.05 (the magnitude of the ratio of the rotational and gravitational potential energies).  Dump files from calculations that include and exclude envelope turbulence are provided (both are used for Figure B1).  The dump files associated with each calculation are: beta=0:      B1M0123 (does not include envelope turbulence) beta=0.0025: B1M2123 (does not include envelope turbulence) beta=0.005:  B1M5123 (does not include envelope turbulence) beta=0.01:   B1M1128 (does not include envelope turbulence) beta=0.02:   B1M2126 (does not include envelope turbulence) beta=0.05:   B1M5109_b05_NoEnvTurb (does not include envelope turbulence) beta=0.0:    B1M0123_b0_EnvTurb beta=0.0025: B1M2177_b0025_EnvTurb beta=0.005:  B1M5209_b005_EnvTurb beta=0.01:   B1M1219_b01_EnvTurb beta=0.02:   B1M2221_b02_EnvTurb beta=0.05:   B1M5321_b05_EnvTurb The SPH dump files are Fortran binary files written in big endian format and generated by the sphNG code (Benz 1990; Bate 1995; Bate & Keto 2015). They can be read, visualised, and manipulated using the free, publicly available SPLASH visualisation code (which reads sphNG dump files), written by Daniel J. Price, that can be downloaded from:  http://users.monash.edu.au/~dprice/splash/  The SPLASH configuration files used to produce Figs. 10,11,12,and B1 in Bate (2022) are included with this dataset in a gzipped tar file.

opencc-by-4.0Jun 2022View details →

Protostars and Planets VII -- Figures and Table for "The Origin and Evolution of Multiple Star Systems"

Figures 1-9 and Table 1 for "The Origin and Evolution of Multiple Star Systems" chapter to appear in Protostars and Planet VII.

opencc-by-4.0Sep 2022View details →

Reproduction package for the paper "The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities"

This is a reproduction package for the paper "The effects of surface fossil magnetic fields on massive star evolution - IV. Grids of models at Solar, LMC, and SMC metallicities" by <a href="https://doi.org/10.1093/mnras/stac2598">Keszthelyi et al. (2022).</a>

Asymmetric dark matter may alter the evolution of very low-mass stars and brown dwarfs

MESA inlists and data files for "<a href="https://ui.adsabs.harvard.edu/?#abs/2011PhRvD..84j1302Z">Asymmetric dark matter may alter the evolution of very low-mass stars and brown dwarfs</a>"

opencc-by-4.0Apr 2019View details →

Neutrinos from Beta Processes in a Presupernova: Probing the Isotopic Evolution of a Massive Star

We present datasets for neutrino luminosity, differential in neutrino energy, of 15 \(M_{\odot}\)and 30 \(M_{\odot}\) presupernova stars at various times during the stellar evolution.  We include here the total luminosity from both pair production and beta processes.  The beta process neutrino luminosities are also split into contributions from individual isotopes.  For more information, please see the attached README.txt file.

opencc-by-4.0Aug 2021View details →

NSNS simulations from: Impact of Massive Binary Star and Cosmic Evolution on Gravitational Wave Observations II: Double Compact Object Mergers

The data for all NSNS simulations shown in "Impact of Massive Binary Star and Cosmic Evolution on Gravitational Wave Observations II: Double Compact Object Mergers".  Broekgaarden et al. (2021, submitted, preprint: <a href="https://arxiv.org/abs/2112.05763">https://arxiv.org/abs/2112.05763</a>)   Contents:  <ul> <li>18 zip files that each contain an hdf5 file with the raw data for one of the simulations from Table 1 in the paper. The only exception is the fiducial.zip file and the unstableCaseBB.zip file, which contain both the fiducial (model A) and 'optimistic CE' (model K) data file and the "unstable case BB" (model E)  and "unstable case BB + optimistic CE" (model F) files. These zip files are:  <ul> <li>fiducial.zip,  the Fiducial model (A) and Optimistic CE model (K)</li> <li>massTransferEfficiencyFixed_0_25.zip, the \(\beta\) = 0.25 model (B) </li> <li>massTransferEfficiencyFixed_0_5.zip, the \(\beta\) = 0.5 model (C) </li> <li>massTransferEfficiencyFixed_0_75.zip, the \(\beta\) = 0.75 model (D)</li> <li>unstableCaseBB.zip, the unstable case BB mass transfer model (E) and unstable case BB & optimistic CE model (F) </li> <li>alpha0_1 zip, the \(\alpha = 0.1\) model (G) </li> <li>alpha0_5.zip, the \(\alpha = 0.5\) model (H) </li> <li>alpha2_0.zip, the \(\alpha = 2.0\) model (I) </li> <li>alpha10_0.zip, the \(\alpha = 10.0\) model (J) </li> <li>rapid.zip, the rapid SN model (L) </li> <li>maxNSmass2_0.zip, the max \(m_{\rm{NS}} = 2\, \rm{M}_{\odot}\) model (M) </li> <li>maxNSmass3_0.zip, the max \(m_{\rm{NS}} = 3\, \rm{M}_{\odot}\) model (N)</li> <li>noPISN.zip, the no PISN model (O) </li> <li>ccSNkick_100km_s.zip, the \(\sigma_{\rm{cc}}\)= 100 km/s model (P) </li> <li>ccSNkick_30km_s.zip, the \(\sigma_{\rm{cc}}\)= 30 km/s model (Q)</li> <li> noBHkick.zip, the no BH SN kick model (R)</li> <li>wolf_rayet_multiplier_0_1.zip, the model with Wolf-Rayet wind factor \(f_{\rm{WR}} = 0.1\) (S)</li> <li>wolf_rayet_multiplier_5.zip, the model with Wolf-Rayet wind factor \(f_{\rm{WR}} = 5\) (T)  </li> </ul> </li> <li>2 more zip files containing csv files with the summarized rates to create Figures 1, 2 and 3, which do not require downloading the entire dataset, but instead use these csv files with the summarized rates:  <ul> <li>csvFilesForFigure1_DCOpaper.zip # contains the files to recreate figure 1 with the merger rates per metallicity for BH-BH, BH-NS and NS-NS: <ul> <li>formationRatesTotalAndPerChannel_BHBH_.csv</li> <li>formationRatesTotalAndPerChannel_BHNS_.csv</li> <li>formationRatesTotalAndPerChannel_NSNS_.csv</li> </ul> </li> <li>csvFilesForFigure2_and_3_DCOpaper.zip # contains the files to recreate figure 2 with the merger rates for intrinsic and GW detection weighted, containing the csv files with names:  <ul> <li>rates_MSSFR_Models_BHBH_AllDCOsimulation.csv</li> <li>rates_MSSFR_Models_NSNS_AllDCOsimulation.csv</li> <li>rates_MSSFR_Models_BHNS_AllDCOsimulation.csv</li> </ul> </li> </ul> </li> </ul>   Details of how to use the data (a readme),  as well as scripts to reproduce all results, plots, and figures from the paper are given in the accompanying Github repository <a href="https://github.com/FloorBroekgaarden/Double-Compact-Object-Mergers">https://github.com/FloorBroekgaarden/Double-Compact-Object-Mergers</a>  If you use this data, please cite  Broekgaarden et al. (2021): see <a href="https://ui.adsabs.harvard.edu/abs/2021arXiv211205763B/abstract">https://ui.adsabs.harvard.edu/abs/2021arXiv211205763B/abstract</a>

opencc-by-4.0Aug 2021View details →

BHNS simulations from: Impact of Massive Binary Star and Cosmic Evolution on Gravitational Wave Observations II: Double Compact Object Mergers

The data for all BHNS simulations shown in "Impact of Massive Binary Star and Cosmic Evolution on Gravitational Wave Observations II: Double Compact Object Mergers".  Broekgaarden et al. (2021, submitted, preprint: <a href="https://arxiv.org/abs/2112.05763">https://arxiv.org/abs/2112.05763</a>)   Contents:  <ul> <li>18 zip files that each contain an hdf5 file with the raw data for one of the simulations from Table 1 in the paper. The only exception is the fiducial.zip file and the unstableCaseBB.zip file, which contain both the fiducial (model A) and 'optimistic CE' (model K) data file and the "unstable case BB" (model E)  and "unstable case BB + optimistic CE" (model F) files. These zip files are:  <ul> <li>fiducial.zip,  the Fiducial model (A) and Optimistic CE model (K)</li> <li>massTransferEfficiencyFixed_0_25.zip, the \(\beta\) = 0.25 model (B) </li> <li>massTransferEfficiencyFixed_0_5.zip, the \(\beta\) = 0.5 model (C) </li> <li>massTransferEfficiencyFixed_0_75.zip, the \(\beta\) = 0.75 model (D)</li> <li>unstableCaseBB.zip, the unstable case BB mass transfer model (E) and unstable case BB & optimistic CE model (F) </li> <li>alpha0_1 zip, the \(\alpha = 0.1\) model (G) </li> <li>alpha0_5.zip, the \(\alpha = 0.5\) model (H) </li> <li>alpha2_0.zip, the \(\alpha = 2.0\) model (I) </li> <li>alpha10_0.zip, the \(\alpha = 10.0\) model (J) </li> <li>rapid.zip, the rapid SN model (L) </li> <li>maxNSmass2_0.zip, the max \(m_{\rm{NS}} = 2\, \rm{M}_{\odot}\) model (M) </li> <li>maxNSmass3_0.zip, the max \(m_{\rm{NS}} = 3\, \rm{M}_{\odot}\) model (N)</li> <li>noPISN.zip, the no PISN model (O) </li> <li>ccSNkick_100km_s.zip, the \(\sigma_{\rm{cc}}\)= 100 km/s model (P) </li> <li>ccSNkick_30km_s.zip, the \(\sigma_{\rm{cc}}\)= 30 km/s model (Q)</li> <li> noBHkick.zip, the no BH SN kick model (R)</li> <li>wolf_rayet_multiplier_0_1.zip, the model with Wolf-Rayet wind factor \(f_{\rm{WR}} = 0.1\) (S)</li> <li>wolf_rayet_multiplier_5.zip, the model with Wolf-Rayet wind factor \(f_{\rm{WR}} = 5\) (T)  </li> </ul> </li> <li>2 more zip files containing csv files with the summarized rates to create Figures 1, 2 and 3, which do not require downloading the entire dataset, but instead use these csv files with the summarized rates:  <ul> <li>csvFilesForFigure1_DCOpaper.zip # contains the files to recreate figure 1 with the merger rates per metallicity for BH-BH, BH-NS and NS-NS: <ul> <li>formationRatesTotalAndPerChannel_BHBH_.csv</li> <li>formationRatesTotalAndPerChannel_BHNS_.csv</li> <li>formationRatesTotalAndPerChannel_NSNS_.csv</li> </ul> </li> <li>csvFilesForFigure2_and_3_DCOpaper.zip # contains the files to recreate figure 2 with the merger rates for intrinsic and GW detection weighted, containing the csv files with names:  <ul> <li>rates_MSSFR_Models_BHBH_AllDCOsimulation.csv</li> <li>rates_MSSFR_Models_NSNS_AllDCOsimulation.csv</li> <li>rates_MSSFR_Models_BHNS_AllDCOsimulation.csv</li> </ul> </li> </ul> </li> </ul>   Details of how to use the data (a readme),  as well as scripts to reproduce all results, plots, and figures from the paper are given in the accompanying Github repository <a href="https://github.com/FloorBroekgaarden/Double-Compact-Object-Mergers">https://github.com/FloorBroekgaarden/Double-Compact-Object-Mergers</a>  If you use this data, please cite  Broekgaarden et al. (2021): see <a href="https://ui.adsabs.harvard.edu/abs/2021arXiv211205763B/abstract">https://ui.adsabs.harvard.edu/abs/2021arXiv211205763B/abstract</a>

opencc-by-4.0Apr 2022View details →

Data from "Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): A Panchromatic View of DO Tau's Complex Kilo-au Environment'

Reduced data from Huang et al., 2022, "Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): A Panchromatic View of DO Tau's Complex Kilo-astronomical-unit Environment,' ApJ, 930, 171 (arXiv:2204.01758).  See Table 1 of the article for the corresponding observing program codes and attributions for archival data (if applicable).  Images: DOTau_12CO_automask.image.pbcor.fits: 12CO J=2-1 image cube DOTau_12CO_automask.mom1.fits: 12CO J=2-1 moment 1 map DOTau_12CO_automask.pbcor.2sigcut.mom0.fits: 12CO J=2-1 moment 0 map DOTau_13CO_automask.image.pbcor.fits: 13CO J=2-1 image cube DOTau_13CO_automask.mom1.fits: 13CO J=2-1 moment 1 map DOTau_13CO_automask.pbcor.2sigcut.mom0.fits: 13CO J=2-1 moment 0 map DOTau_C18O_automask.image.pbcor.fits: C18O J=2-1 image cube DOTau_C18O_automask.pbcor.2sigcut.mom0.fits: C18O J=2-1 moment 0 map DOTau_C18O_automask.pbcor.mom1.fits: C18O J=2-1 moment 1 map DOTau_cADI_average.fits: SPHERE H-band cADI image (pixel scale: 0.01225 arcseconds) DOTau_CS_automask.image.pbcor.fits: DO Tau CS J=5-4 image cube DOTau_CS_automask.mom1.fits: DO Tau CS J=5-4 moment 1 map DOTau_CS_automask.pbcor.2sigcut.mom0.fits: DO Tau CS J=5-4 moment 0 map DOTau_DoLP.fits: DO Tau degree of linear polarization map (pixel scale: .0245 arcseconds) DOTau_IDF-RDI.fits: SPHERE total intensity image produced with IDF-RDI (pixel scale: 0.01225 arcseconds) DO-TAU_NICMOS_F110W_MRDILib-18_KL-2_Pixel.fits: HST NICMOS F110W image (pixel scale: 0.075 arcseconds) DO-TAU_NICMOS_F160W_MRDILib-100_KL-1_Pixel.fits: HST NICMOS F160W image (pixel scale: 0.075 arcseconds) DOTau_Qphi_average.fits: SPHERE H-band Qphi image (pixel scale: 0.01225 arcseconds) DO_Tau_STIS_KlipWithin160pixel_counts_s_pixel.fits: HST STIS image (pixel scale: 0.0507 arcseconds) Measurement sets: DOTau_12CO.ms.contsub.tar: Self-calibrated, continuum-subtracted 12CO J=2-1 visibilities DOTau_13CO.ms.contsub.tar: Self-calibrated, continuum-subtracted 13CO J=2-1 visibilities DOTau_C18O.ms.contsub.tar: Self-calibrated, continuum-subtracted C18O J=2-1 visibilities DOTau_CS.ms.contsub.tar: Self-calibrated, continuum-subtracted CS J=5-4 visibilities Scripts: DOTau_1.1mmreduction.py: CASA self-cal and imaging script for CS data  DOTau_1.3mmreduction.py: CASA self-cal and imaging script for CO data

Evolution models of helium white dwarf-main-sequence star merger remnants: the mass distribution of single low-mass white dwarfs

Inlists and data for "<a href="https://ui.adsabs.harvard.edu/#abs/2018MNRAS.474..427Z/abstract">Evolution models of helium white dwarf-main-sequence star merger remnants: the mass distribution of single low-mass white dwarfs</a>"

Dust formation and mass loss around intermediate-mass AGB stars with initial metallicity Zini ≤ 10-4 in the early Universe - I. Effect of surface opacity on stellar evolution and the dust-driven wind

MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2017MNRAS.466.1709T">Dust formation and mass loss around intermediate-mass AGB stars with initial metallicity Zini ≤ 10-4 in the early Universe - I. Effect of surface opacity on stellar evolution and the dust-driven wind</a>

Novel modelling of ultracompact X-ray binary evolution - stable mass transfer from white dwarfs to neutron stars

MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/#abs/2017MNRAS.470L...6S/abstract">Novel modelling of ultracompact X-ray binary evolution - stable mass transfer from white dwarfs to neutron stars</a>

Modeling the early evolution of massive OB stars with an experimental wind routine. The first bi-stability jump and the angular momentum loss problem

MESA run_star_extras associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2017A&A...598A...4K">Keszthelyi et al. (2017)</a>. MESA version 7624. Publication DOI: <a href="https://doi.org/10.1051/0004-6361/201629468">10.1051/0004-6361/201629468</a>

Code dependencies of pre-supernova evolution and nucleosynthesis in massive stars: evolution to the end of core helium burning

MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2015MNRAS.447.3115J">Jones et al. (2015)</a>. MESA version 3709. Publication DOI: <a href="https://doi.org/10.1093/mnras/stu2657">10.1093/mnras/stu2657</a> Files are also available in a gihub repository <a href="https://github.com/swjones/mesa-Teile/tree/master/Jones.etal.2015.MNRAS.447.4.3115">here</a>