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89 results for “pulsars”
The Thousand-Pulsar-Array programme on MeerKAT - VIII. The subpulse modulation of 1198 pulsars
<p>These datasets and document are online appendices beyond those provided in the main journal manuscript "The Thousand-Pulsar-Array programme on MeerKAT - VIII. The subpulse modulation of 1198 pulsars" by Song et al. published in Monthly Notices of the Royal Astronomical Society in 2023.</p> <p>File supplementary_appendices.pdf contains supplementary online appendices.</p> <p>Files appendix_a1_table_observationalparameters.pdf and appendix_a2_table_spectralmeasurements.pdf are two tables summarising the observational related parameters, and subpulse modulation measurements respectively. </p> <p>File appendix_spectralfigures.pdf contains spectral figures for all sources.</p> <p>Zip files (RA*_spectralfigures.zip) contain original and shuffled spectral figures for individual pulsars within a specific RA range.</p>
A Model-Independent Determination of Red Noise in Pulsar Timing Arrivals
<p>Data files for Reyes & Bernido, submitted, 2023, A Model-Independent Determination of Red Noise in Pulsar Timing Arrivals. </p> <p>In this work, we analyze the pulsar timing data from the North American Nanohertz Observatory for Gravitational Waves (NANOGrav; Arzoumanian et al 2018). For 23 pulsars with 820 MHz data, we show that an evaluation of the mean square deviation (MSD) and probability distribution (PDF) of timing residuals can provide a straightforward way of determining the presence of red noise. The model-free method presented could complement the normally more sophisticated model-dependent way of determining red noise in timing residuals.</p> <p>Data available here:</p> <p>- ts.zip - uniform time-series of timing residuals for the 23 pulsars</p> <p>- msd.zip - mean square deviation vs. lag time for the 23 pulsars</p> <p>- pdf.zip - probability distributions for lag times equal to 30, 150, 300, 900, and 1200 days for the 23 pulsars</p>
Radio Parallax of the Crab Pulsar Data Release
<p>This is the companion dataset to the publication <strong>"Radio Parallax of the Crab Pulsar: A First VLBI Measurement Calibrated with Giant Pulses" </strong>by <em>Lin, et al., (2023, submitted, preprint: <a href="https://arxiv.org/abs/2306.01617">https://arxiv.org/abs/2306.01617</a>)</em>.</p> <p>The FITS files contain images of the Crab Pulsar, SE_CAND3 and NE_CAND4 sources created from <a href="https://www.evlbi.org/">European VLBI Network</a> EK036A-D observations using the technique described in the paper. See the <strong>README.md</strong> and paper for more details.</p>
The second data release from the European Pulsar Timing Array III. Search for gravitational wave signals
<p>We present the results of the search for an isotropic stochastic gravitational wave background (GWB) at nanohertz frequencies using the second data release of the European Pulsar Timing Array (EPTA) for 25 millisecond pulsars and a combination with the first data release of the Indian Pulsar Timing Array (InPTA). A robust GWB detection is conditioned upon resolving the Hellings-Downs angular pattern in the pairwise cross-correlation of the pulsar timing residuals. Additionally, the GWB is expected to yield the same (common) spectrum of temporal correlations across pulsars, which is used as a null hypothesis in the GWB search. Such a common-spectrum process has already been observed in pulsar timing data. We analysed (i) the full 24.7-year EPTA data set, (ii) its 10.3-year subset based on modern observing systems, (iii) the combination of the full data set with the first data release of the InPTA for ten commonly timed millisecond pulsars, and (iv) the combination of the 10.3-year subset with the InPTA data. These combinations allowed us to probe the contributions of instrumental noise and interstellar propagation effects. With the full data set, we find marginal evidence for a GWB, with a Bayes factor of four and a false alarm probability of 4%. With the 10.3-year subset, we report evidence for a GWB, with a Bayes factor of 60 and a false alarm probability of about 0.1% (≳ 3σ significance). The addition of the InPTA data yields results that are broadly consistent with the EPTA-only data sets, with the benefit of better noise modelling. Analyses were performed with different data processing pipelines to test the consistency of the results from independent software packages. The latest EPTA data from new generation observing systems show non-negligible evidence for the GWB. At the same time, the inferred spectrum is rather uncertain and in mild tension with the common signal measured in the full data set. However, if the spectral index is fixed at 13/3, the two data sets give a similar amplitude of (2.5 ± 0.7) × 10−15 at a reference frequency of 1 yr−1 . Further investigation of these issues is required for reliable astrophysical interpretations of this signal. By continuing our detection efforts as part of the International Pulsar Timing Array (IPTA), we expect to be able to improve the measurement of spatial correlations and better characterise this signal in the coming years.</p>
Binary Pulsar PSR B1913+16 arrival time and associated files. Ref: Weisberg & Huang APJ 2016
<p>These files contain arrival time and associated data for PSR B1913+16, which are usable as input to the tempo software program. They were used for the paper "Relativistic Measurements from Timing the Binary Pulsar PSR B1913+16," Weisberg & Huang, Astrophysical Journal, 2016, in press. </p>
Pulsars detected in the GP survey in only Stokes I images
<p><span>The known pulsars detected in the GP survey in only Stokes I images. </span><span>The mean flux density of the pulsars from the Stokes I image from this work is </span><span>denoted by S</span><span>I</span><span> </span><span>and the flux density from the Stokes V image is denoted by S</span><span>V</span><span>.</span><span> </span><span>α </span><span>refers to the spectral index of the pulsars. Only two of the pulsars, PSRs J1614- </span><span>5048 and J1644-4559 have a previously recorded flux density below 300 MHz by </span><span>Frail et al. (2016). For the 14 remaining pulsars, this is the first low-frequency </span><span>detections below 300 MHz.</span></p>
The known pulsars detected in the GP survey in only beamformed searches.
<p><span>The known pulsars detected in the GP survey in only beamformed </span><span>searches. It shows the names and parameters of the pulsars. Detailed analysis of </span><span>these pulsars can be found in Xue et al. (2017) and Bhat et al. (2023b). As this </span><span>work is mainly focused on the imaging aspect of pulsar searching, these pulsars </span><span>are not included as part of the analysis done for this work.</span></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>
Software and data release for Fermi Pulsar Timing Array
<p>The archive include photon data from the Fermi Large Area Telescope, processed to enable its use for pulsar timing. It includes Python code for performing pulsar timing using Poisson likelihood and for producing pulse time-of-arrival measurements. It further includes code and scripts for constraining noise processes in the data, including the a signal from the nanohertz gravitational wave background.</p> <p> </p> <p>See README for more information.</p>
dataset for "A Scintillation Arc Survey of 22 Pulsars with Low to Moderate Dispersion Measures"
<p>These are the 54 Dynamic Spectrum files (.FITS format) behind the paper "A Scintillation Arc Survey of 22 Pulsars with Low to Moderate Dispersion Measures," submitted to the AAS Journals on 2022 April 06. We also include the Tables, Figures, and Text from the work, as well as some explanatory README files.</p>
Evolution of plasma properties in 2D particle-in-cell simulations of pulsar polar caps as function of dipole inclination angle
<p>The video shows the evolution of plasma properties in polar cap region of neutron stars from initial simulation conditions to the quasi-periodic pair creation. Three inclination angles of magnetic dipole axis to the star rotation axis are investigate \iota = 0°, 45°, and 90°.</p> <p>The presented quantities are (in rows): Parallel current density, parallel electric field, parallel and perpendicular Poynting flux, electron and positron plasma density, and electron and positron plasma bulk momenta.</p> <p> </p>
Database of simulated pulse profiles from X-ray accreting pulsar
<p>This database is a parquet file that stores a list of dictionary with the simulated pulse profiles from an X-ray accreting pulsar. Every dictionary contains 7 paframeters defining the pulsar and the associated pulse profile. It is highly recommended to check the GitHub repository containing instructions on how to read and use the data stored. </p> <p><a href="https://github.com/SimoneGalla/X-ray-accreting-pulsar/tree/main/pulse-Profile-X-ray-pulsars">X-ray-accreting-pulsar/pulse-Profile-X-ray-pulsars at main · SimoneGalla/X-ray-accreting-pulsar (github.com)</a></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>
Radio and gamma-ray timing of TRAPUM L-band Fermi pulsar survey discoveries - Supplementary material
<p>Timing ephemerides for the redback pulsar J1803-6707 (published in <em>"Radio and gamma-ray timing of TRAPUM L-band \textit{Fermi} pulsar survey discoveries"</em>, Burgay et al 2024, A&A) covering 15 years of Fermi data. The ephemeris are provided both in "ORBIFUNC" (to be used with timing software <a href="https://bitbucket.org/psrsoft/tempo2/src/master/" target="_blank" rel="noopener">tempo2</a>) and "ORBWAVES" (with <a href="https://github.com/nanograv/PINT" target="_blank" rel="noopener">PINT</a>) formats. The ORBIFUNC parameters are a time-domain interpolating function describing the orbital phase variations over time, while the ORBWAVES parameters are the Fourier-domain representation of the same function.</p>
Vela Pulsar Observation Files MJD 57985
<p>Files:</p> <ul> <li>579859820.dat (PRESTO time series format)</li> <li>579859820.inf (PRESTO time series format header)</li> <li>579859820.png (image of result of PRESTO 'prepfold' processing)</li> <li>579859820.ps (postscript result of PRESTO 'prepfold' processing)</li> <li>579859820.tim (SIGPROC time series format)</li> <li>579859820.prof (pulse profile output file of SIGPROC 'fold' processing)</li> <li>579859820.prof.png (image of pulse profile output file of SIGPROC 'fold' processing displayed in a spreadsheet)</li> <li>579859820.txt (information for processing command-line parameters)</li> </ul> <p>Observation Parameters</p> <ul> <li>Vela pulsar nominal topocentric period = 0.0893969312 seconds.</li> <li>Observation Start Time = MJD 57985.9820</li> <li>Duration = 120 minutes</li> <li>Frequency = 436 MHz</li> <li>Bandwidth = 2.4 MHz</li> <li>Antenna: 42-element circularly-polarised crossed Yagi (nominal gain 19 dBi)</li> <li>Location: 33.567 S, 150.745 E (Hawkesbury Radio Astronomy Observatory)</li> </ul>
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>
The second data release from the European Pulsar Timing Array II. Customised pulsar noise models for spatially correlated gravitational waves
<p>Aims: The nanohertz gravitational wave background (GWB) is expected to be an aggregate signal of an ensemble of gravitational waves emitted predominantly by a large population of coalescing supermassive black hole binaries in the centres of merging galaxies. Pulsar tiNanohertz ming arrays (PTAs), which are ensembles of extremely stable pulsars at approximately kiloparsec distances precisely monitored for decades, are the most precise experiments capable of detecting this background. However, the subtle imprints that the GWB induces on pulsar timing data are obscured by many sources of noise that occur on various timescales. These must be carefully modelled and mitigated to increase the sensitivity to the background signal. Methods: In this paper, we present a novel technique to estimate the optimal number of frequency coefficients for modelling achromatic and chromatic noise, while selecting the preferred set of noise models to use for each pulsar. We also incorporated a new model to fit for scattering variations in the Bayesian pulsar timing package temponest. These customised noise models enable a more robust characterisation of single-pulsar noise. We developed a software package based on tempo2 to create realistic simulations of European Pulsar Timing Array (EPTA) datasets that allowed us to test the efficacy of our noise modelling algorithms. Results: Using these techniques, we present an in-depth analysis of the noise properties of 25 millisecond pulsars (MSPs) that form the second data release (DR2) of the EPTA and investigate the effect of incorporating low-frequency data from the Indian Pulsar Timing Array collaboration for a common sample of ten MSPs. We used two packages, enterprise and temponest, to estimate our noise models and compare them with those reported using EPTA DR1. We find that, while in some pulsars we can successfully disentangle chromatic from achromatic noise owing to the wider frequency coverage in DR2, in others the noise models evolve in a much more complicated way. We also find evidence of long-term scattering variations in PSR J1600-3053. Through our simulations, we identify intrinsic biases in our current noise analysis techniques and discuss their effect on GWB searches. The analysis and results discussed in this article directly help to improve the sensitivity to the GWB signal and they are already being used as part of global PTA efforts.</p>
The second data release from the European Pulsar Timing Array I. The dataset and timing analysis
<p>Pulsar timing arrays offer a probe of the low-frequency gravitational wave spectrum (1−100 nanohertz), which is intimately connected to a number of markers that can uniquely trace the formation and evolution of the Universe. We present the dataset and the results of the timing analysis from the second data release of the European Pulsar Timing Array (EPTA). The dataset contains high-precision pulsar timing data from25 millisecond pulsars collected with the five largest radio telescopes in Europe, as well as the Large European Array for Pulsars. The dataset forms the foundation for the search for gravitational waves by the EPTA, presented in associated papers. We describe the dataset and present the results of the frequentist and Bayesian pulsar timing analysis for individual millisecond pulsars that have been observed over the last∼25 years.We discuss the improvements to the individual pulsar parameter estimates, as well as new measurements of the physical properties of these pulsars and their companions. This data release extends the dataset from EPTA Data Release 1 up to the beginning of 2021, with individual pulsar datasets with timespans ranging from 14 to 25 years. These lead to improved constraints on annual parallaxes, secular variation of the orbital period, and Shapiro delay for a number of sources. Based on these results, we derived astrophysical parameters that include distances, transverse velocities,binary pulsar masses, and annual orbital parallaxes.</p>
Investigational Device Exemption Study to Determine the Safety and Efficacy of the Astron and Pulsar Stents
ClinicalTrials.gov study NCT01319812. IPD Sharing: NO. Countries: 2. Publications: 1.
Data from: A pulsar-helium star compact binary system formed by common envelope evolution
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