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89 results for “Pulsars”
Single-pulsar search for eccentric SMBHBs using NANOGrav 12.5-year data of PSR J1909--3744: Posterior samples
<p>This repository contains posterior samples for a Bayesian single-pulsar search for nanohertz gravitational waves originating from eccentric supermassive binaries, done using the NANOGrav 12.5-year dataset for PSR J1909-3744. The analysis is presented in Susobhanan 2023 [https://arxiv.org/abs/2210.11454].</p>
Additional evidence for a pulsar wind nebula in SN 1987A from multi-epoch X-ray data and MHD modelling
<p>This is a basic reproduction package for the paper "Additional evidence for a pulsar wind nebula in the hearth of sN 1987A from multi-epoch X-ray data and MHD modeling" by Greco et al. 2022. It aims to provide the most important data products to check and reproduce the main results of the paper.</p>
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>
Data and Software for: 'The Radius of the High-mass Pulsar PSR J0740+6620 with 3.6 yr of NICER Data'
<p>Posterior sample files associated with the publication "The Radius of the High-mass Pulsar PSR J0740+6620 with 3.6 yr of NICER Data" by Salmi et al. (2024; <a href="https://doi.org/10.48550/arXiv.2406.14466">arXiv.2406.14466</a>; <a href="https://doi.org/10.3847/1538-4357/ad5f1f">https://doi.org/10.3847/1538-4357/ad5f1f</a>).</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>
The Thousand-Pulsar-Array program on MeerKAT -- IX. The time-averaged properties of the observed pulsar population: data set
<p>This archive contains pulsar data presented as part of the MNRAS paper: <em>"The Thousand-Pulsar-Array program on MeerKAT -- IX. The time-averaged properties of the observed pulsar population"</em>.</p> <p>Folded, time-averaged pulse profiles (4 Stokes parameters, 8 frequency channels, 1024 time bins across the period) of the 1271 pulsars listed in Table 1 of the MNRAS paper are included in the ar_files.zip. Ephemerides of these pulsars (as used in the MNRAS paper) are included in the eph_files.zip. The pulsar data are readable by the PSRCHIVE package, see e.g. van Straten et al., Astronomical Research and Technology 9, 237 (2012).</p> <p>Tables 1, 5, and 6 from the MNRAS paper are included in tables_files.zip as .csv files. The file column_descriptions.txt describes the quantities in columns of these tables.<br> </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>
Catalog of GAIA eDR3 sources within 20 arcsec of pulsars
<p>Catalog of GAIA eDR3 sources within 20 arcsec of pulsars. Details on how the catalog was created can be found in <a href="https://arxiv.org/abs/2011.08075">Antoniadis (2021)</a></p> <p>The source code can be found <a href="https://zenodo.org/record/4378294#.X9-rR-lKjOQ">here</a></p>
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>
Data used in the "H-FISTA: A hierarchical algorithm for phase retrieval with application to pulsar dynamic spectra" publication
<p>Dynamic spectra used in the "A new approach to phase retrieval for pulsar dynamic spectra" publication. These data can be used to reproduce the results in the paper</p>
A highly magnetized environment in a pulsar binary system
<p>A highly magnetized environment in a pulsar binary system</p> <p><strong>Data availability:</strong></p> <ul> <li>IPV and DM, RM variations used for Fig 1 (Demo how to read the code and plot: plot_Fig1.py) <p>DM_Icut_60s_140114.txt, DM_Icut_60s_200621.txt, </p> <p>RM_140114_20s_rmfit.txt,RM_200621_20s_rmfit.txt, </p> <p>ILV_140114_20s.npy, ILV_200621_20s.npy</p> </li> <li>A full table of DM and RM variations (duplicated with the txt files, but with better readability): Li_DM_RM_Ter5A.xlsx</li> <li>Calibrated full stokes data with frequency information for Fig 2 (in psrfit format, can be read in with standard psrchive commands): VEGAS_Ter5A_200621_0001.zap.E2.calib.rot.f32</li> </ul> <p><strong>Code availability</strong></p> <ul> <li><em>The basic process of the raw data and DM, RM fitting:</em></li> </ul> <p>DSPSR (http://dspsr.sourceforge.net) PSRCHIVE (http://psrchive.sourceforge.net)</p> <ul> <li><em>Modeling and fitting:</em></li> </ul> <p>https://github.com/dongzili/Pol_prop_fitting</p> <p>NOTICE: If there are updated data due to new demands, the information or new URL will be posted in https://github.com/dongzili/Pol_prop_fitting</p>
Dataset for "Flickering of the Vela pulsar during its 2016 glitch"
<p>Dataset for the paper "Flickering of the Vela pulsar during its 2016 glitch". These files contain the summary statistics for each individual pulse around the glitch (kb_database_2016-12-12.h5) and during a period away from the glitch (kb_database_2016-09-18.h5). We additionally provide two scripts and a matplotlib stylefile to recreate Figures 1a and 1b from the publication.</p>
Testing strengths, limitations and biases of current Pulsar Timing Arrays detection analyses on realistic data
<p>In this project, we carried out an extensive investigation of the performance of current Pulsar Timing Arrays (PTA) analyses on simulated PTA datasets where we modeled the gravitational waves (GW) signal as the incoherent superposition of sinusoidal signals from a cosmic population of super-massive black hole binaries (SMBHBs). Here we publish the dataset referred to in the paper as the <em><strong>SMBHB_set</strong></em>: 100 realisations of PTA datasets with 25 pulsars and a GWB signal of nominal amplitude 2.4e-15. For each realisation, listed from 1001 to 1100, this repository contains the pulsars .par and .tim files, the mcmc chain (sampling over 66 parameters: 60 for pulsars intrinsic noise parameters and log amplitude and slope of a common red noise process), and the SMBHB details for that specific realisation of the GWB. The columns of the <em>MBHB_list.dat</em> files contain (from left to right): log10 MBH chirp mass (in solar masses in the source frame), mass ratio, source redshift, log10 of GW fundamental mode (n=2) in the observer frame, phi and theta angles in the sky, source inclination angle, source polarisation angle, source initial orbital phase, source initial direction of periastron and source initial eccentricity.</p> <p>If you make use of any of this data, please cite:<br><br></p> <div>@article{ refId0,</div> <div> author = {{Valtolina, Serena} and {Shaifullah, Golam} and {Samajdar, Anuradha} and {Sesana, Alberto}},</div> <div> title = {Testing strengths, limitations, and biases of current pulsar timing arrays’ detection analyses on realistic data},</div> <div> DOI= "10.1051/0004-6361/202348084",</div> <div> url= "https://doi.org/10.1051/0004-6361/202348084",</div> <div> journal = {A&A},</div> <div> year = 2024,</div> <div> volume = 683,</div> <div> pages = "A201",</div> <div>}</div>
Dataset for "Study of 72 pulsars discovered in the PALFA survey: Timing analysis, glitch activity, emission variability, and a pulsar in an eccentric binary"
<p>This repository includes TEMPO-readable ephemerides associated with the final timing solutions presented in Table 3 (text-readable format; .par files) of the manuscript, "<em>Study of 72 pulsars discovered in the PALFA survey: Timing analysis, glitch activity, emission variability, and a pulsar in an eccentric binary</em>" accepted to the Astrophysical Journal (October 2021).</p>
Utilizing cosmic-ray positron and electron observations to probe the averaged properties of Milky Way pulsars
<p>We include here the Milky Way pulsars simulations that were created and used in "Utilizing cosmic-ray positron and electron observations to probe the averaged properties of Milky Way pulsars" of Cholis & Krommydas 2021. We include both the simulations before fitting to the cosmic-ray observations and the simulations whose electron and positron fluxes have been fitted to the AMS, CALET and DAMPE observations. See paper for further details.</p>
Data supporting "Universality of Free Fall Shown by Orbital Motion of a Pulsar in a Stellar Triple System"
<p>This is a collection of data supporting the research paper "Orbital Motion of a Pulsar in a Stellar Triple System Shows Universality of Free Fall".</p> <p>The main data content (the ".tim" file) is a set of pulse arrival times, the primary input to the fitting process, in tempo2 format. These times are annotated with post-fit residuals and derivatives with respect to fit parameters using the tempo2 format's per-TOA flags.</p> <p>Additional files include the data that went into several figures, plus the above converted to CSV format - but note that the CSV format does not record the pulse arrival times with sufficient precision to permit fitting. Derivative and uncertainty information may permit reanalysis of the systematics.</p>
Radio emission from a pulsar's magnetic pole revealed by general relativity: a data archive
<p>This repository contains all pulsar data presented as part of the Science paper: "Radio emission from a pulsar's magnetic pole revealed by general relativity". These data consist of pulse profiles archives of PSR J1906+0746 observed by the Nancay and Arecibo radio telescopes between 2005 and 2018, that are readable by the PSRCHIVE package, see e.g. van Straten et al., Astronomical Research and Technology 9, 237 (2012).</p>
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>
Main-sequence pulsar: the peculiar subset of hot magnetic stars
<p>In my talk, I will describe some peculiar phenomena observed from a subset of hot magnetic stars, also known as 'main-sequnce pulsar's and discuss their usefulness. This class of stars is distinguished from the rest of the population by their ability to produce highly directed coherent radio emission via electron cyclotron maser emission (ECME) in their magnetospheres. The fundamental difference between the two classes is however still vague. I will describe our efforts to understand this difference; this includes a survey being carried out with the Giant Metrewave Radio telescope (GMRT) in order to find more hot magnetic stars that show coherent radio emission, and also wideband observations taken with two telescopes: the GMRT and the Very Large Array (VLA), of the already known coherent radio emitters to find out the bandwidth of the emission process. In this process, we have also come across certain new phenomena like the inversion of circular polarization and that of the sequence of ECME pulse arrival with frequency. I will discuss the implications of these new revelations and their potential to become tools for estimating plasma density close to the stellar surface, as well as constraining the inhomogeneity and asymmetry in the magnetosphere.</p>
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