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47 results for “Astrophysics”
Astrophysical S-factors for H-burning stars
<p> This dataset contains the latest recommendations of astrophysical S-factors for nuclear fusion reactions occurring in hydrogen-burning stars, included in the <strong><em>Solar Fusion III </em></strong>decadal review article (submitted for publication, e-print available at <a href="https://arxiv.org/abs/2405.06470" target="_blank" rel="noopener">arXiv:2405.06470</a>).</p> <p> The data includes S-factors and their derivatives at zero energy (where available). That is, <em>S(0)</em>,<em> S´(0)</em>, <em>S´´(0)</em>, in units of MeV·b, b, and b/MeV, respectively. Fractional uncertainties are also provided (marked as <em>fr_err</em>). Unavailable data are marked as <em>NA</em>.</p> <p> This data was used to compute the <a href="https://zenodo.org/records/10822316">Standard Solar Models B23 / SF-III</a>. </p> <p> For further information and references consult the <strong><em>Solar Fusion III </em></strong> article linked above.</p>
Joint Modelling of Astrophysical Systematics (JMAS) data
<p>This dataset is part of the Joint Modelling of Astrophysical Systematics (JMAS) project and includes redshift distributions (NZ), intrinsic alignment amplitudes (IA), parametric sweeps for NZ and IA, data vectors and Fisher matrices.</p> <p>The data is intended to support the findings published in [add]. The code to recreate the plots can be found on <a href="https://github.com/nikosarcevic/JMAS" target="_blank" rel="noopener">JMAS GH Repository</a>.</p>
Astrophysical constraints on neutron star f -modes with a nonparametric equation of state representation
<p>Data release for Mohanty et al. "<em>Astrophysical constraints on neutron star f-modes with a nonparametric equation of state representation"</em></p> <p>The data release consists of three files: </p> <ol> <li><a href="https://zenodo.org/api/records/13952437/draft/files/EoS_posterior_samples_PSR.h5/content" target="_blank" rel="noopener noreferrer">EoS_posterior_samples_PSR.h5</a> </li> <li><a href="https://zenodo.org/api/records/13952437/draft/files/EoS_posterior_samples_PSR+GW.h5/content" target="_blank" rel="noopener noreferrer">EoS_posterior_samples_PSR+GW.h5</a> </li> <li><a href="https://zenodo.org/api/records/13952437/draft/files/EoS_posterior_samples_PSR+GW+NICER.h5/content" target="_blank" rel="noopener noreferrer">EoS_posterior_samples_PSR+GW+NICER.h5</a> </li> </ol> <p>Each file contains 9,835 samples of EOS draws. The equation of state id's matches those of Legred et. al. 2022</p> <p>The data structure follows Legred, I. (2022) “<em>Impact of the PSR J0740+6620 radius constraint on the properties of high-density matter: Neutron star equation of state posterior samples</em>”. Zenodo. doi: 10.5281/zenodo.6502467.</p> <p>Samples were generated using stanspy, a general relativistic neutron star code written by Sailesh Ranjan Mohanty. </p> <p>Please see the readme (adapted from Legred et. al. 2022 Zenodo. doi: 10.5281/zenodo.6502467) </p>
Dataset for article Photodissociation of aliphatic PAH derivatives under relevant astrophysical conditions
<p>The experimental data are provided in subfolders by species, which contain each three files:<br> (i) the normalized intensities (Eq. 1 in the article) for the mass peaks corresponding to the parent cation and its fragments as a function of the VUV irradiation time,<br> (ii) the experimental error bars associated with these intensities,<br> (iii) the curves corresponding to the fitting functions that were derived with the procedure described in Sect. 2.4.</p> <p>Each folder is named by the parents species:<br> Pyr+ for pyrene (C16H10+),<br> H6-Pyr+ for 1,2,3,6,7,8-hexahydro-pyrene (C16H16+),<br> MePyr+ for 1-methylpyrene (C17H12+),<br> EtPyr+ for 4-ethyl-pyrene (C18H14+),<br> Cor+ for coronene (C24H12+),<br> MeCor+ for methyl-coronene (C25H14+),<br> EtCor+ for ethyl-coronene (C26H16+).</p> <p>In addition, the VUV_source folder contains the measurements corresponding to the VUV source calibration (see Fig. A.1 in the article appendix).</p> <p>The folder for TD-DFT calculations gathers the calculated photoabsorption cross-sections for all species of interest (see Fig. D.1 in the article appendix).</p>
US Department of Energy funded publications from Astrophysics Data System
<p>The John G. Wolbach Library, in collaboration with the NASA Astrophysics Data System (ADS), has compiled this bibliography of United States Department of Energy (DOE) funded publications. Grants were identified within the ADS by regular expression matching against article full text. There are over 70,000 articles in the bibliography, with bibliographic information for each publication. This bibliography is being released to explore its possible usage.</p> <p>Please note:</p> <p>Papers may include arXiv preprints (as non-refereed, with arXiv bibcode) and their subsequent journal articles (as refereed, with journal bibcode) as separate and unlinked records</p> <p>This compilation is a snapshot in time for DOE grants and ADS papers</p> <p>The method of data collection does not differentiate between grants credited with supporting projects and those supporting individuals contributing to projects.</p> <p>Results are based on available metadata which may be incomplete. This may include incomplete records of grant identifiers, due to limitations within the ADS. However, all articles in the bibliography acknowledge the support of the DOE in some way.</p> <p>Results have not been individually verified</p> <p>All abstracts and articles in the ADS are copyrighted by the publisher, and their use is free for personal use only. For more information, please read the Terms and Conditions regulating usage of resources.</p> <p>This dataset contains bibliographic information only, no information on the grants themselves is included. A potential application of the data could be to link the bibliographic information to grant information.</p> <p><br /> Links</p> <p>Harvard-Smithsonian Center for Astrophysics John G. Wolbach Library http://www.cfa.harvard.edu/lib/information/about.html</p> <p>NASA ADS http://labs.adsabs.harvard.edu/</p> <p>USA Spending: information on US government spending, including the Department of Energy: http://www.usaspending.gov</p> <p>Grants.gov, more information on US government grants: http://www.grants.gov</p> <p>Department of Energy: http://energy.gov/</p>
Astrophysical Templates for Crocker, Macias, et al. (2022)
<p>Astrophysical Templates for Crocker & Macias, et al. (2022)</p>
NMMA: A nuclear-physics and multi-messenger astrophysics framework to analyze binary neutron star mergers
<p>Data release associated with the preprint "<em>NMMA: A nuclear-physics and multi-messenger astrophysics framework to analyze binary neutron star mergers</em>"</p> <p>Data includes:</p> <p>EOS files:</p> <ul> <li>5000 eos files with radius (km), mass (Msun), and tidal deformability as columns stored under eos/eos_data</li> <li>prior probabilities for the EOSs are stored in eos/eos_prior_probability.dat</li> </ul> <p>Posterior samples:</p> <ul> <li>Posterior samples based on the analysis of GW170817 and AT2017gfo stored in posterior_samples/GW170817-AT2017gfo_posterior_samples.dat</li> <li>Posterior samples based on the analysis of GW170817, AT2017gfo, and the afterglow of GRB170817A are stored in posterior_samples/GW170817-AT2017gfo-GRB170817A_afterglow_posterior_samples.dat</li> </ul> <p> </p>
Further diagrams of the publication Schürmann & Langer 2024 (Astronomy & Astrophysics)
<h2>Content/Naming convention</h2> <p>Here are three groups of image files: HRD_??.png, AngMom_??.png, and WR?_b1_50.png. Each is an extension to one of the figures in Schürmann & Langer 2024.</p> <h3><br>HRD_??.png</h3> <p>Same as Fig. 1 (bottom), but for different initial masses (see file name) for various accretion rates (indicated by colour).</p> <h3><br>AngMom_??.png</h3> <p>Same as Fig. 8, but the ejected material carries either single (?=1) or double (?=2) the specific orbital angular momentum of the donor (AngMom_a?.png), of the accretor (AngMom_b?.png), of the orbit (AngMom_h?.png), or none (AngMom_h0.png).</p> <p>AngMom_a1.png: beta = eta = 0, alpha = - epsilon, A = 1<br>AngMom_a2.png: beta = eta = 0, alpha = - epsilon, A = 2<br>AngMom_b1.png: alpha = eta = 0, beta = - epsilon, B = 1<br>AngMom_b2.png: alpha = eta = 0, beta = - epsilon, B = 2<br>AngMom_h0.png: A = B = H = 0<br>AngMom_h1.png: alpha = beta = 0, eta = - epsilon, H = 1<br>AngMom_h2.png: alpha = beta = 0, eta = - epsilon, H = 2</p> <h3><br>WR?_b1_50.png</h3> <p>Same as Fig. 9, but for AB 3, AB 6, AB 7, AB 9. We assumed a WR progenitor mass of 50Msol, which is a typical number (see Table 3), and since the area of the contract-avoiding region varies not so strongly with mass. WR_key.png is the legend.</p>
Online example database generated representing nuclear astrophysics models predictions of correlations between stable/stable abundances of specific isotopes.
<p>Library of figures created using the SIMPLE code (Stellar Interpretation for Meteoritic data and PLotting). The SIMPLE stellar database includes 18 core-collapse supernova models with 3 different initial masses of 15, 20, 25 solar masses, all of solar metallicity and non-rotating stars. The 6 sets are the following:</p> <ul> <li>Rauscher et al. 2002 [Ra02]<br>(<a href="https://ui.adsabs.harvard.edu/abs/2002ApJ...576..323R/abstract">https://ui.adsabs.harvard.edu/abs/2002ApJ...576..323R/abstract</a>),</li> <li>Pignatari et al. 2016 [Pi16]<br>(<a href="https://ui.adsabs.harvard.edu/abs/2016ApJS..225...24P/abstract">https://ui.adsabs.harvard.edu/abs/2016ApJS..225...24P/abstract</a>),</li> <li>Sieverdin et al. 2018 [Si18]<br>(<a href="https://ui.adsabs.harvard.edu/abs/2018ApJ...865..143S/abstract">https://ui.adsabs.harvard.edu/abs/2018ApJ...865..143S/abstract</a>),</li> <li>Limongi & Chieffi 2018 [LC18]<br>(<a href="https://ui.adsabs.harvard.edu/abs/2018ApJS..237...13L/abstract">https://ui.adsabs.harvard.edu/abs/2018ApJS..237...13L/abstract</a>),</li> <li>Ritter et al. 2018 [Ri18]<br>(<a href="https://ui.adsabs.harvard.edu/abs/2018MNRAS.480..538R/abstract">https://ui.adsabs.harvard.edu/abs/2018MNRAS.480..538R/abstract</a>),</li> <li>Lawson et al. 2022 [La22]<br>(<a href="https://ui.adsabs.harvard.edu/abs/2022MNRAS.511..886L/abstract">https://ui.adsabs.harvard.edu/abs/2022MNRAS.511..886L/abstract</a>)</li> </ul> <p>The figures can be divided into two types. The first shows the structure of the ejecta and the abundance of the selected isotopes. The layers are automatically detected using SIMPLE based on the abundances of the main fuels (H-1, He-4, C-12, O-16, Ne-20, Si-28) from the supernova model ejecta. The code names the different layers based on the schematic diagram in Schofield et al. 2022 (<a href="https://ui.adsabs.harvard.edu/abs/2022MNRAS.517.1803S/abstract">https://ui.adsabs.harvard.edu/abs/2022MNRAS.517.1803S/abstract</a>). <br>Ni and Fe isotopes are plotted in the figures. The abundances shown include the radiogenic contribution from unstable isotopes.</p> <p>The SIMPLE code is designed to compare stellar data with measurements from meteorites. To achieve this, abundances in mass fractions need to be converted into isotopic ratios using specific units. See Lugaro et al. 2023 (<a href="https://ui.adsabs.harvard.edu/abs/2023EPJA...59...53L/abstract">https://ui.adsabs.harvard.edu/abs/2023EPJA...59...53L/abstract</a>) for details. For the specific case of Ni64 ratios, in comparison with model data we report the measured meteoritic anomaly by Steele et al 2012 (<a href="https://ui.adsabs.harvard.edu/abs/2012ApJ...758...59S/abstract">https://ui.adsabs.harvard.edu/abs/2012ApJ...758...59S/abstract</a>) as a continuous horizontal line. The same is done for the Fe54 ratios, with reference measurements by Hopp et al 2022 (<a href="https://ui.adsabs.harvard.edu/abs/2022E%26PSL.57717245H/abstract">https://ui.adsabs.harvard.edu/abs/2022E%26PSL.57717245H/abstract</a>). </p> <p>In the database the abundance plots are identified as <strong>structure_<model refe<em>rence>_<initial mass>_<element>_<decayed or undecayed>.png</em></strong><em>. In particular, the available reference model options are Ra02, Pi16, Si18, LC18, Ri18, La22; the initial mass of the progenitors are 15, 20 or 25 (solar masses). The third part of the filenames are the plotted elements (in this case Ni or Fe) and then if they are decayed or undecayed. In this database we only consider the decayed species, which means that the radioactive isotopes whose decay can add to the abundance of the selected isotopes were considered. In this plots the x-axis represents the total mass from the core and the y-axis is the mass fraction on a logarithmic scale. For the slopes the same name scheme applies, but they are identified as <strong>slopes_<model reference>_<initial mass>_<element>_<decayed or undecayed></strong></em><strong>.png,</strong> and on the y-axis there are the slope values insteas of abundances.</p>
Harvard-Smithsonian Center for Astrophysics
This is the Harvard-Smithsonian Center for Astrophysics (CfA) located in Cambridge (MA). It was founded from the merging of the Harvard College Observatory and the Smithsonian Astrophysical Observatory in 1973. CfA is a major institute for research, education and public outreach in astrophysics in the world and the headquarter of the NASA Chandra X-ray Observatory. https://www.cfa.harvard.edu/ Source: Objaverse 1.0 / Sketchfab
Simulations dataset and pre-trained models of "Deep learning in real-time on the astrophysical data obtained from the Čerenkov CTA Observatory" Ph.D. project
<p>Ph.D. project datasets and models release, <br><em>Deep learning in real-time on the astrophysical data obtained from the Čerenkov CTA Observatory.</em></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>
Modules for Experiments in Stellar Astrophysics (MESA): Planets, Oscillations, Rotation, and Massive Stars
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2013ApJS..208....4P">Modules for Experiments in Stellar Astrophysics (MESA): Planets, Oscillations, Rotation, and Massive Stars</a></p>
Modules for Experiments in Stellar Astrophysics (MESA): Convective Boundaries, Element Diffusion, and Massive Star Explosions
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/#abs/2018ApJS..234...34P/abstract">Modules for Experiments in Stellar Astrophysics (MESA): Convective Boundaries, Element Diffusion, and Massive Star Explosions</a></p>
Modules for Experiments in Stellar Astrophysics (MESA): Binaries, Pulsations, and Explosions
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2015ApJS..220...15P">Modules for Experiments in Stellar Astrophysics (MESA): Binaries, Pulsations, and Explosions</a></p>
Inference results from "No need to know: astrophysics-free gravitational-wave cosmology"
<p>Simulated GW data and inference results for all runs associated with the publication "No need to know: astrophysics-free gravitational-wave cosmology." This accompanies the code used to make the paper and run all analyses, hosted at: https://github.com/afarah18/spectral-sirens-with-GPs</p> <p> </p> <p>v4 and v5: updated after peer review changes</p>
Data package for paper "Transformer models for astrophysical time series and the GRB prompt-afterglow relation"
<p>This is a data package accompanying the paper "Transformer models for astrophysical time series and the GRB<br>prompt-afterglow relation". The code used to acquire the data is in the "data" folder. The code used to analyse the data is in the "analysis" folder.</p> <p>DOI paper: <a href="https://doi.org/10.1093/rasti/rzae026">10.1093/rasti/rzae026</a></p>
Appendix Figures B.1–B.7 from the article 'Core Prominence as a Signature of Restarted Jet Activity in the LOFAR Radio-Galaxy Population' (Accepted for publication in the journal Astronomy & Astrophysics on August 23, 2024)
<p><strong>Figure captions:</strong></p> <p> </p> <p><strong>Figs. B.1–B.5.</strong> Images of 69 candidate restarted galaxies selected based on high radio $\mathrm{CP_{1400}}$ combined with low SB of extended emission, a steep spectrum of the core, and USS extended emission coupled with a bright core and summarised in Tables A.1 and A.2. Radio contours from VLA FIRST maps (white, $5^{\prime\prime}$), LOFAR high-resolution maps (black, $6^{\prime\prime}$), and NVSS maps (purple, $45^{\prime\prime}$) are overlaid on the LOFAR low-resolution resolution maps (orange, $20^{\prime\prime}$). The contouring of all the maps is made at $\,\sigma_\mathrm{local}\times(-3,3,5,10,20,30,40,50,100,150,200)$ levels, with $\sigma_\mathrm{local}$ representing the local RMS noise of the corresponding maps. The host galaxy position is marked with a yellow cross.</p> <p> </p> <p><strong>Figs. B.6–B.7. </strong>Images of sources excluded from the sample of restarted candidates following the criteria discussed in Sect. 3.1, Sect. 3.2 and Sect. 3.3 and summarised in Tables A.3 and A.4. Radio contours from VLA FIRST maps (white, $5^{\prime\prime}$), LOFAR high-resolution maps (black, $6^{\prime\prime}$), and NVSS maps (purple, $45^{\prime\prime}$) are overlaid on the LOFAR low-resolution resolution maps (orange, $20^{\prime\prime}$). The contouring of all the maps is made at $\,\sigma_\mathrm{local}\times(-3,3,5,10,20,30,40,50,100,150,200)$ levels, with $\sigma_\mathrm{local}$ representing the local RMS noise of the corresponding maps. The host galaxy position is marked with a yellow cross.</p> <p> </p>
TAT: Timing Analysis Toolkit for high-energy pulsar astrophysics
<p>The TAT-pulsar (Timing Analysis Toolkit for Pulsars) package is a specialized toolkit designed for handling the scientific intricacies of pulsar timing. It provides a suite of Python-based utilities and scripts that facilitate the analysis, processing, and visualization of pulsar data. By leveraging observational data from pulsars, along with the associated physical processes and statistical characteristics, TAT-pulsar integrates a series of useful tools and data analysis scripts specifically developed for both isolated pulsars and binary systems. This enables swift analysis and the detailed presentation of timing properties in the high-energy pulsar field. Developed and implemented completely independently from other pulsar timing software such as Stingray (<a href="https://ascl.net/1608.001">ascl:1608.001</a>) and PINT (<a href="https://ascl.net/1902.007">ascl:1902.007</a>), TAT-pulsar serves as a valuable cross-checking and supplementary tool for data analysis.</p>
Single-atom catalysis in space: Computational exploration of Fischer–Tropsch reactions in astrophysical environments
<p>This supporting material contains:</p> <ul> <li>Cartesian coordinates of the PBE optimized minima and transition states for the reactions under study, in XYZ format.</li> <li>Inputs for the <a href="https://www.cp2k.org/">CP2K</a> and <a href="https://www.crystal.unito.it/">Crystal17</a> packages.</li> <li>Vibrational calculations with all the frequencies.</li> <li>Inputs and outputs for the benchmark study performed with the <a href="https://gaussian.com/">Gaussian16</a> package.</li> </ul>
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