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82 results for “Cosmology”
Dark matter flow dataset from cosmological N-body simulation
<p>Dark matter (DM), if exists, is believed to be cold, collisionless, dissipationless, non-baryonic, barely interacting with baryonic matter except through gravity, and sufficiently smooth on large scales with a fluid-like behavior. The flow of dark matter can be best described by a self-gravitating collisionless fluid dynamics (SG-CFD). The statistics of dark matter density, velocity, acceleration, energy, momentum, and their redshift evolution play essential roles for structure formation and evolution. These information can be systematically extracted from cosmological N-body simulations by either i) a structural (halo-based) or ii) a statistical (correlation-based) approach. In this correlation-based statistical dataset, i) all particle pairs with any given separation r in a N-body system are identified; ii) statistical measures are calculated over all particle pairs with the same separation r (pairwise average); iii) the redshift (z) and scale (r) dependence of all statistical measures (correlation/moment/structure/dispersion/spectrum functions for density, velocity and potential etc.) are presented. </p> <p>Applications of cascade and statistical theory for dark matter and bulge-SMBH evolution:</p> <ol> <li>Dark matter particle mass ,size, and properties from energy cascade in dark matter flow: 1) <a href="http://doi.org/10.48550/arXiv.2202.07240">arxiv</a> 2) <a href="https://zenodo.org/record/6640353">zenodo slides</a></li> <li>Origin of MOND acceleration & deep-MOND from acceleration fluctuation & energy cascade: 1) <a href="http://doi.org/10.48550/arXiv.2203.05606">arxiv</a> 2) <a href="https://zenodo.org/record/6640386">zenodo slides</a></li> <li>The baryonic-to-halo mass relation from mass and energy cascade in dark matter flow: 1) <a href="http://doi.org/10.48550/arXiv.2203.06899">arxiv</a> 2) <a href="https://zenodo.org/record/6640355">zenodo slides</a></li> <li>Universal scaling laws and density slope for dark matter haloes: 1) <a href="http://doi.org/10.48550/arXiv.2209.03313">arxiv</a> 2) <a href="https://zenodo.org/record/7059193">zenodo slides</a> 3) <a href="http://doi.org/10.1038/s41598-023-31083-z">paper</a></li> <li>Dark matter halo mass functions and density profiles from mass/energy cascade: 1) <a href="http://doi.org/10.48550/arXiv.2210.01200">arxiv</a> 2) <a href="https://zenodo.org/record/7146473">zenodo slides</a> 3) <a href="https://doi.org/10.1038/s41598-023-42958-6">paper</a></li> <li>Energy cascade for distribution and evolution of supermassive black holes (SMBHs): 2) <a href="http://doi.org/10.5281/zenodo.7490502">zenodo slides</a></li> </ol> <p>Condensed slides for all applications "<a href="http://doi.org/10.5281/zenodo.7508310">Cascade Theory for Turbulence, Dark Matter, and bulge-SMBH evolution </a>"</p> <p>The two relevant datasets and accompanying presentation can be found at: </p> <ol> <li><a href="https://doi.org/10.5281/zenodo.6541230">Dark matter flow dataset Part I: Halo-based statistics from cosmological N-body simulation</a> </li> <li><a href="https://doi.org/10.5281/zenodo.6569898">Dark matter flow dataset Part II: Correlation-based statistics from cosmological N-body simulation</a>.</li> <li><a href="https://doi.org/10.5281/zenodo.6569901">A comparative study of Dark matter flow & hydrodynamic turbulence and its applications</a></li> </ol> <p>The same dataset also available on Github at: <a href="https://github.com/ZhijieXu2022/dark_matter_flow_dataset/">Github: dark_matter_flow_dataset</a> and zenodo at: <a href="http://doi.org/10.5281/zenodo.6586212">Dark matter flow dataset from cosmological N-body simulation</a>.</p> <p>Cascade and statistical theory developed by these datasets:</p> <ol> <li>Inverse mass cascade in dark matter flow and effects on halo mass functions: 1) <a href="http://doi.org/10.48550/arXiv.2109.09985">arxiv</a> 2) <a href="https://zenodo.org/record/6639536">zenodo slides</a> </li> <li>Inverse mass cascade and effects on halo deformation, energy, size, and density profiles: 1) <a href="http://doi.org/10.48550/arXiv.2109.12244">arxiv</a> 2) <a href="https://zenodo.org/record/6640337">zenodo slides</a></li> <li>Inverse energy cascade in dark matter flow and effects of halo shape: 1) <a href="http://doi.org/10.48550/arXiv.2110.13885">arxiv</a> 2) <a href="https://zenodo.org/record/6640331">zenodo slides</a></li> <li>The mean flow, velocity dispersion, energy transfer and evolution of dark matter halos: 1) <a href="http://doi.org/10.48550/arXiv.2201.12665">arxiv</a> 2) <a href="https://zenodo.org/record/6640380">zenodo slides</a></li> <li>Two-body collapse model and generalized stable clustering hypothesis for pairwise velocity 1) <a href="http://doi.org/10.48550/arXiv.2110.05784">arxiv</a> 2) <a href="https://zenodo.org/record/6640306">zenodo slides</a></li> <li>Energy, momentum, spin parameter in dark matter flow and integral constants of motion: 1) <a href="http://doi.org/10.48550/arXiv.2202.04054">arxiv</a> 2) <a href="https://zenodo.org/record/6640322">zenodo slides</a></li> <li>Maximum entropy distributions of dark matter in ΛCDM cosmology: 1) <a href="http://doi.org/10.48550/arXiv.2110.03126">arxiv</a> 2) <a href="https://zenodo.org/record/6640373">zenodo slides</a> 3) <a href="http://doi.org/10.1051/0004-6361/202346429">paper</a></li> <li>Halo mass functions from maximum entropy distributions in dark matter flow: 1) <a href="http://doi.org/10.48550/arXiv.2110.09676">arxiv</a> 2) <a href="https://zenodo.org/record/6640325">zenodo slides</a></li> <li>On the statistical theory of self-gravitating collisionless dark matter flow: 1) <a href="http://doi.org/10.48550/arXiv.2202.00910">arxiv</a> 2) <a href="https://zenodo.org/record/6640705">zenodo slides</a> 3) <a href="http://doi.org/10.1063/5.0151129">paper</a></li> <li>High order kinematic and dynamic relations for velocity correlations in dark matter flow: 1) <a href="http://doi.org/10.48550/arXiv.2202.02991">arxiv</a> 2) <a href="https://zenodo.org/record/6640684">zenodo slides</a></li> <li>Evolution of density and velocity distributions and two-thirds law for pairwise velocity: 1) <a href="http://doi.org/10.48550/arXiv.2202.06515">arxiv</a> 2) <a href="https://zenodo.org/record/6640676">zenodo slides</a></li> </ol>
FIG. 8. — A in Prey into kin: the cosmological role of the pig in the Kelabit Highlands, Sarawak
FIG. 8. — A young couple, Balang Ngeluun and Sinah Balang Ngeluun, posing with their two children and older members of the community with the domestic pig Sus scrofa Linnaeus, 1758 (berak) about to be slaughtered for their namechanging irau in Bario, April 1987. Photo credit: Kaz Janowski.
FIG. 7 in Prey into kin: the cosmological role of the pig in the Kelabit Highlands, Sarawak
FIG. 7. — Balang Pelaba, Baye Ripug, Pun Nibu and another unidentified man participating in a competition to eat fat from a domestic pig (berak) at the namechanging irau held for Balan, the first child of Paran To'oh and Sinah Paran To'oh, in Pa' Dalih in April 1987. Photo credit: Kaz Janowski.
FIG. 3 in Prey into kin: the cosmological role of the pig in the Kelabit Highlands, Sarawak
FIG. 3. — The Kelabit culture hero Tuked Rini shimmering with lalud (cosmic power). Painting by Stephen Baya, 2009.
FIG. 2 in Prey into kin: the cosmological role of the pig in the Kelabit Highlands, Sarawak
FIG. 2. — Huge acorns in the forests of the Kelabit Highlands, the favourite food of the wild pig species Sus scrofa Linnaeus, 1758 and Sus barbatus Müller, 1838. Photo credit: Kaz Janowski, 1988.
FIG. 6 in Prey into kin: the cosmological role of the pig in the Kelabit Highlands, Sarawak
FIG. 6. — Judin, Elvis and other young men of Pa' Dalih scalding the head of a wild pig (baka) of the species Sus barbatus Müller, 1838 prior to scraping off the hairs. Elvis holds Molly Janowski between his knees. Photo credit: Sally Greenhill, 1987.
FIG. 10 in Prey into kin: the cosmological role of the pig in the Kelabit Highlands, Sarawak
FIG. 10. — Participant who has been smeared with blood in ritual to establish new headhouse in Bidayuh village, Kampong Gumbang, 29 June 2017. Photo credit: Kaz Janowski.
FIG. 4 in Prey into kin: the cosmological role of the pig in the Kelabit Highlands, Sarawak
FIG. 4. — Kelabit hunting equipment and hunted meat from a wild pig (baka), probably Sus barbatus Müller, 1838. This includes a basket (bekang) containing the meat; a shotgun and cartridges; a quiver for blowpipe darts (selongan) together with small gourd (bua tabu kre) containing flights for the darts (ra'o); and a large forest knife (tongol). Photo credit: Monica Janowski, 1993.
FIG. 9. — Two young men distributing meat from a domestic pig Sus scrofa Linnaeus, 1758 in Prey into kin: the cosmological role of the pig in the Kelabit Highlands, Sarawak
FIG. 9. — Two young men distributing meat from a domestic pig Sus scrofa Linnaeus, 1758 (berak) at irau in Bario, 1987. Photo credit: Kaz Janowski.
FIG. 1 in Prey into kin: the cosmological role of the pig in the Kelabit Highlands, Sarawak
FIG. 1. — The longhouse community of Pa' Dalih, Kelabit Highlands in 1987. Photo credit: Kaz Janowski.
Cosmological Initial Conditions (3D magnetic fields for an alfa=1.0 magnetic spectrum) for 85Mpc^3
<p>Files representing the initial conditions at z=40 for ENZO-MHD cosmological simulation of a comoving 85Mpc^3 volume, for tangled magnetic fields from an alfaB=-1.0 initial spectrum of magnetic fluctuations. The simulation has 1024^3 cells and 1024^3 DM particles. These data are in binary format and can be read by the ENZO code.</p> <p>More details of the simulations and on it cosmological parameter can be found at:</p> <ul> <li>https://ui.adsabs.harvard.edu/abs/2021Galax...9..109V/abstract</li> <li>https://ui.adsabs.harvard.edu/abs/2021MNRAS.500.5350V/abstract</li> <li>https://ui.adsabs.harvard.edu/abs/2017CQGra..34w4001V/abstract</li> </ul>
Cosmological Initial Conditions (3D magnetic fields for an alfa=1.0 magnetic spectrum) for 85Mpc^3
<p>Files representing the initial conditions at z=40 for ENZO-MHD cosmological simulation of a comoving 85Mpc^3 volume, for tangled magnetic fields from an alfaB=1.0 initial spectrum of magnetic fluctuations. The simulation has 1024^3 cells and 1024^3 DM particles. These data are in binary format and can be read by the ENZO code.</p> <p>More details of the simulations and on it cosmological parameter can be found at:</p> <ul> <li>https://ui.adsabs.harvard.edu/abs/2021Galax...9..109V/abstract</li> <li>https://ui.adsabs.harvard.edu/abs/2021MNRAS.500.5350V/abstract</li> <li>https://ui.adsabs.harvard.edu/abs/2017CQGra..34w4001V/abstract</li> </ul>
Cosmological Initial Conditions (3D magnetic fields for an alfa=2.0 magnetic spectrum) for 85Mpc^3
<p>Files representing the initial conditions at z=40 for ENZO-MHD cosmological simulation of a comoving 85Mpc^3 volume, for tangled magnetic fields from an alfaB=2.0 initial spectrum of magnetic fluctuations. The simulation has 1024^3 cells and 1024^3 DM particles. These data are in binary format and can be read by the ENZO code.</p> <p>More details of the simulations and on it cosmological parameter can be found at:</p> <ul> <li>https://ui.adsabs.harvard.edu/abs/2021Galax...9..109V/abstract</li> <li>https://ui.adsabs.harvard.edu/abs/2021MNRAS.500.5350V/abstract</li> <li>https://ui.adsabs.harvard.edu/abs/2017CQGra..34w4001V/abstract</li> </ul>
Magnetogenesis Scenarios In Cosmological Simulations - Uniform Primordial B0=1nG
<p>One ENZO-MHD cosmological simulation of a comoving 85Mpc^3 volume, saved at z=0.</p> <p>The simulation features a primordial uniform magnetic field seed, 1nG B0=comoving.</p> <p>All datasets are written in HDF5 format, and they represent the physical fields (Gas Density, Temperature, Dark Matter Density, 3D velocity components and 3D magnetic components) on a uniform 1024^3 cartesian grid with uniform spacing.</p> <p>More details of the simulations and on the physical models of magnetism explored here can be found in:</p> <ul> <li>https://ui.adsabs.harvard.edu/abs/2021Galax...9..109V/abstract</li> <li>https://ui.adsabs.harvard.edu/abs/2021MNRAS.500.5350V/abstract</li> <li>https://ui.adsabs.harvard.edu/abs/2017CQGra..34w4001V/abstract</li> </ul>
Datasets for "Relic gravitational waves from the chiral plasma instability in the standard cosmological model"
<pre>This directory contains an index.html file with links to the run directories and idl plotting routines with secondary data for the other figures for the paper "Relic Gravitational Waves from the Chiral Plasma Instability in the Standard Cosmological Model". If anything turns out to be incomplete, please email brandenb@nordita.org.</pre>
A Test of the Cosmological Principle with Quasars
<p>Dataset, mask and code associated with</p> <p>https://inspirehep.net/literature/1820376</p> <p>(https://arxiv.org/abs/2009.14826)</p> <p>Code and README for selecting the sample from CatWISE can be found in Generatecode.tar.gz</p> <p>Code and README for masking the sample, evaluating the dipole, as well as the Monte Carlos for statistical significances can be found in Resultscode.tar.gz</p> <p>(This github repository: https://github.com/rameez3333/CatWISEdipole )</p> <p>Note that the final result is for the sample with W1 less than 16.4 cut applied, whereas this file includes objects with W1 less than 16.5.</p> <p>Additional code required to produce the catalog from scratch is available in "<a href="https://zenodo.org/api/files/6cb5d4a5-505a-4703-9351-958666e847f2/secrest%2B21_extra.tar.gz">secrest+21_extra.tar.gz</a>"</p> <p> </p> <p> </p>
Quantifying tensions in cosmological parameters: Interpreting the DES evidence ratio (supplementary inference products)
<p>These are the nested sampling inference products and input files that were used to compute results for <a href="https://arxiv.org/abs/1902.04029">arXiv:1902.04029</a> and <a href="https://arxiv.org/abs/1903.06682">arXiv:1903.06682</a></p> <p>An example plotting script and plots from the papers are included to demonstrate usage.</p> <p>Filename conventions:</p> <p>runs_default: default prior widths</p> <p>runs_narrow: narrowest prior widths</p> <p>runs_medium: intermediate prior widths</p> <p>planck: Planck 2018 baseline likelihoods</p> <p>SH0ES: Riess et al 2018 Hubble likelihood</p> <p>BAO: BOSS DR12 baryonic acoustic oscillations + redshift space distortion likelihood</p> <p>DES: Dark Energy Survey Y1 baseline</p> <p>Software used:</p> <p>CosmoChord <a href="https://github.com/williamjameshandley/CosmoChord/tree/e2f7020bd9d4254230097037fb6ebaee95a3d558">https://github.com/williamjameshandley/CosmoChord/tree/e2f7020bd9d4254230097037fb6ebaee95a3d558</a></p>
Data for 'Cosmology with Binary Neutron Stars: Does Mass-Redshift Correlation Matter?'
<p>The code is available at the following GitHub link: https://github.com/SoumendraRoy/RedevolBNS</p> <p>To generate the plots in the paper, see: https://github.com/SoumendraRoy/RedevolBNS/tree/main/Make_Plots</p> <p>A frozen version of the Make_Plots is included here.</p> <p>Description of the files:</p> <ol> <li><a href="https://zenodo.org/api/records/14704635/draft/files/Cosmo_Plots.ipynb/content" target="_blank" rel="noopener noreferrer">Cosmo_Plots.ipynb</a>, <a href="https://zenodo.org/api/records/14704635/draft/files/Pop_Plots.ipynb/content" target="_blank" rel="noopener noreferrer">Pop_Plots.ipynb</a> : Jupyter notebooks containing all plots in the main text.</li> <li><a href="https://zenodo.org/api/records/14704635/draft/files/Appendix_Plots.ipynb/content" target="_blank" rel="noopener noreferrer">Appendix_Plots.ipynb</a>, <a href="https://zenodo.org/api/records/14704635/draft/files/All_Contours.ipynb/content" target="_blank" rel="noopener noreferrer">All_Contours.ipynb</a> : Jupyter notebooks containing all plots in Appendix.</li> <li><a href="https://zenodo.org/api/records/14704635/draft/files/inference_marginal_fiducial.h5/content" target="_blank" rel="noopener noreferrer">inference_marginal_fiducial.h5</a>, <a href="https://zenodo.org/api/records/14704635/draft/files/inference_full_fiducial.h5/content" target="_blank" rel="noopener noreferrer">inference_full_fiducial.h5</a> : The samples of the Hubble constant and dark matter density for the fiducial injected population, with uncorrelated and correlated mass-redshift populations, respectively.</li> <li><a href="https://zenodo.org/api/records/14704635/draft/files/inference_marginal_MM.h5/content" target="_blank" rel="noopener noreferrer">inference_marginal_MM.h5</a>, <a href="https://zenodo.org/api/records/14704635/draft/files/inference_full_MM.h5/content" target="_blank" rel="noopener noreferrer">inference_full_MM.h5</a> : The samples of the Hubble constant and dark matter density for the Mandel-Müller injected population, with uncorrelated and correlated mass-redshift populations, respectively.</li> <li><a href="https://zenodo.org/api/records/14704635/draft/files/inference_full_result_Uncorrelated.h5/content" target="_blank" rel="noopener noreferrer">inference_full_result_Uncorrelated.h5</a>, <a href="https://zenodo.org/api/records/14704635/draft/files/inference_full_result_Injected.h5/content" target="_blank" rel="noopener noreferrer">inference_full_result_Injected.h5</a> : The samples of the Hubble constant and dark matter density for the fiducial injected population, with uncorrelated and correlated mass-redshift populations, respectively for varying number of detections.</li> <li><a href="https://zenodo.org/api/records/14704635/draft/files/simulation.h5/content" target="_blank" rel="noopener noreferrer">simulation.h5</a> : The injected mass, redshift samples for different population synthesis variations.</li> <li><a href="https://zenodo.org/api/records/14704635/draft/files/compare_pop.h5/content" target="_blank" rel="noopener noreferrer">compare_pop.h5</a>, <a href="https://zenodo.org/api/records/14704635/draft/files/variant_pop.h5/content" target="_blank" rel="noopener noreferrer">variant_pop.h5</a> : Comparison of different population synthesis variations.</li> <li><a href="https://zenodo.org/api/records/14704635/draft/files/gmm.h5/content" target="_blank" rel="noopener noreferrer">gmm.h5</a> : Gaussian mixture model fit of the fiducial and Mandel-Müller injected population.</li> </ol>
Inference products and plotting code for "Some Times in Standard Cosmology"
<p>This zip file contains the Monte Carlo Markov chains (MCMC), the plotting codes, and the figures for the paper "Some Times in Standard Cosmology" by Lukas Tobias Hergt and Douglas Scott (<a href="https://arxiv.org/abs/2411.07703">arXiv:2411.07703</a>):</p> <ul> <li>The folder <code>MCMC__LCDM__PR3_lowlTT_PR4_LoLLiPoP-lowlEE_HiLLiPoP-TTTEEE_lensing</code> contains the MCMC run generated with Cobaya. For details about theoretical model, input parameters, and likelihoods refer to the <code>.yaml</code> files therein or to information in the corresponding paper.</li> <li>The <code>some_times_in_standard_cosmology.py</code> file was used for the post-processing of the MCMC chains; specifically, to compute the physical times, which are not standard derived parameters.</li> <li>The <code>some_times_in_standard_cosmology.ipynb</code> file contains the plotting code and the <code>some_times_in_standard_cosmology_sympy.ipynb</code> file contains derivations of the 2-fluid solutions. We additinally provide the <code>some_times_in_standard_cosmology.html</code> and <code>some_times_in_standard_cosmology_sympy.html</code> files to allow for easy read access via a browser.</li> <li>The PDF files <code>some_times_in_standard_cosmology.pdf</code> and <code>some_times_in_standard_cosmology_2d.pdf</code> are the two figures published in the paper.</li> <li>The <code>.tex</code> files contain the data used for the tables in the paper.</li> </ul>
Images for "Analogue cosmological particle creation in an ultracold quantum fluid of light"
<p>The raw images used to create the plots shown in "Analogue cosmological particle creation in an ultracold quantum fluid of light".</p>
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OpenNeuro
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