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Dataset results
9 results for “millisecond pulsars”
A NICER View of the Massive Pulsar PSR J0740+6620 Informed by Radio Timing and XMM-Newton Spectroscopy: Nested Samples for Millisecond Pulsar Parameter Estimation
<p>Posterior sample files associated with the preprint "A <em>NICER</em> View of the Massive Pulsar PSR J0740+6620 Informed by Radio-Timing and <em>XMM-Newton</em> Spectroscopy" by Riley et al. (2021; <a href="https://arxiv.org/abs/2105.06980">arXiv:2105.06980 [astro-ph.HE]</a>; submitted to ApJL).</p> <p>Also included are: the data products; the numeric model files including the telescope calibration products; model modules in the Python language using the X-PSI framework; and Jupyter analysis notebooks.</p> <p>Please refer to the README for detailed information.</p> <p> </p> <p> </p>
A NICER View of PSR J0030+0451: Nested Samples for Millisecond Pulsar Parameter Estimation
<p>Posterior sample files associated with "A <em>NICER</em> View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation" by Riley et al. (2019; <a href="https://iopscience.iop.org/article/10.3847/2041-8213/ab481c">DOI: 10.3847/2041-8213/ab481c</a>).</p> <p>Also included are model modules and scripts in the Python language using the X-PSI framework.</p> <p>Please refer to the README for detailed information.</p>
Simulation of the Galactic field millisecond pulsar population and its gamma- and X-ray emission
<p>Monte Carlo simulation of the millisecond pulsar population in the Galactic field. The simulation includes four spatial components:</p> <ul> <li>the disk;</li> <li>the boxy bulge;</li> <li>the nuclear stellar cluster;</li> <li>the nuclear stellar disk.</li> </ul> <p>The last 3 components together form the Galactic bulge. There is one file per component, each containing at least 100 Monte Carlo simulations. Each line contains:</p> <ul> <li>the longitude L in deg;</li> <li>the latitude B in deg;</li> <li>the line of sight S in kpc;</li> <li>the 0.1-100 GeV gamma-ray flux in erg/cm^2/s;</li> <li>the X-ray spectral index;</li> <li>the gamma-to-X flux ratio, where the gamma-ray flux is the same as in the fourth column and the X-ray flux is the 2-10 keV unabsorbed one</li> </ul> <pre>of a simulated MSP. More information about the simulation can be found in the related paper. </pre>
Reproduction package for: 'A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715'
<div>Posterior sample files for the headline result associated with the publication "A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715" by Choudhury et al. (2024; <a href="https://doi.org/10.3847/2041-8213/ad5a6f" target="_blank" rel="noopener"><em>ApJL</em> <strong>971</strong> L20</a>; <a href="https://arxiv.org/abs/2407.06789" target="_blank" rel="noopener">arXiv:2407.06789</a>).</div> <div> </div> <div>Also included are: the data products; the numeric model files including the telescope calibration products; model modules in the Python language using the X-PSI framework; and Jupyter analysis notebooks.</div> <div> </div> <div> <div> <p>Please refer to the README for detailed information.</p> </div> </div>
Dataset for "Eight Millisecond Pulsars Discovered in the Arecibo PALFA Survey"
<p>This repository includes pulse profile templates (Pulsar Archive format; .sm files) presented in Figure 1 and TEMPO-readable ephemerides associated with the final timing solutions presented in Table 1 (text-readable format; .par files) of the manuscript, "<em>Eight Millisecond Pulsars Discovered in the Arecibo PALFA Survey</em>" accepted to the Astrophysical Journal.</p>
Constraining the Neutron Star Mass-Radius Relation and Dense Matter Equation of State with NICER. I. The Millisecond Pulsar X-Ray Data Set
<p>This deposit includes the cleaned, filtered and phase folded NICER event data set for the millisecond pulsar (MSP) PSR J0030+0451 in the 0.25-3 keV band. The data processing and filtering was performed using HEASoft 6.251 and NICERDAS version 5.0; the specific parameters and filtering criteria used are detailed in the ApJ Letter listed above. This event list was used to produce what is shown for PSR J0030+0451 in Figures 2, 3, and 4 in the accepted ApJ Letter listed above and was also used for the neutron star mass-radius and equation of state inference analyses presented in the companion papers (Miller et al. 2019, Riley et al. 2019, and Raaijmakers et al. 2019).</p> <p>The event file and its MD5 checksum is:<br> J0030+0451_merged_phase_0.25-3keV.fits (463bbac7203bb45bb02ea0deed49f083)<br> </p>
Data relating to "Millisecond Pulsars from Accretion Induced Collapse as the Origin of the Galactic Centre Gamma-ray Excess Signal"
<p>Data describe the evolution of a population of millisecond pulsars (MSPs) born from Accretion Induced Collapse.</p> <p>Data entries are comma-separated.</p> <p>The formation and subsequent evolution of 9194 MSPs have been modelled with code based on the BSE Code [see Hurley, J. R., Pols, O. R. & Tout, C. A. Comprehensive analytic formulae for stellar evolution as a function of mass and metallicity. Mon. Not. Roy. Astron. Soc. 315, 543–569 (2000)].</p> <p>For each MSP, the first row describes the magnetic field B (in Gauss) and the inclination angle (i, in radians) between magnetic & rotational axes.</p> <p>These quantities (B,i) do not evolve.</p> <p>Thus, every row containing only two entries indicates the beginning of the data covering a separate MSP.<br> For subsequent rows, there are seven entries in each row.</p> <p>The first entry in each row is the (discretised) time in units of Gyr since the star formation event when the MSP is formed. 0.1 is the minimum time possible time for which an MSP can be born. Subsequent discrete time steps are 0.1 Gyr. The last row for every MSP is for a time of 15.9 Gyr. </p> <p>Subsequent entries show (as a function of time)</p> <p>period (in s)</p> <p>period derivative dP/dt (s/s)</p> <p>NS mass (in units of solar masses)</p> <p>secondary mass (in units of solar masses)</p> <p>secondary type (for an explanation of secondary type label see Hurley, J. R., Pols, O. R. & Tout, C. A. Comprehensive analytic formulae for stellar evolution as a function of mass and metallicity. Mon. Not. Roy. Astron. Soc. 315, 543–569 (2000).</p> <p>orbital separation</p>
Evolution of Transient Low-mass X-Ray Binaries to Redback Millisecond Pulsars
<p>MESA inists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2015ApJ...814...74J">Jia & Li (2015)</a>. MESA version 7624.</p> <p>Publication DOI: <a href="https://doi.org/10.1088/0004-637X/814/1/74">10.1088/0004-637X/814/1/74</a></p>
Variable Scintillation Arcs in Millisecond Pulsars observed with the Large European Array for Pulsars
<p>Dynamic spectra used in "Variable Scintillation Arcs in Millisecond Pulsars observed with the Large European Array for Pulsars". </p> <p>The dynamic spectra are simple ascii (the same output produced by psrflux), produced as described in the manuscript. A function to read them in python is included on github: https://github.com/ramain/scintillation/blob/master/scintillation/dynspectools/dynspectools.py, and they should all be compatible with the scintools package.</p>
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