S3PUL Overview
OERC logo SKADS logo

Overview

S3-PUL is a simulation of a Galactic population of pulsars. The database lists the position of the pulsars and includes an average pulse profile for each source. The population is derived using the PSRPOP package in collaboration with Roy Smits (Jodrell Bank Centre for Astrophysics) and with the help of D. R. Lorimer and J. Ridley (University of West Virginia). The pulsar profiles are generated using a stochastic model of the pulsar beam by Karastergiou & Johnston (2007), the viewing geometry from the population synthesis, and temporal smearing caused by interstellar scattering.

Database structure

The database consists of a simulated catalogue of 107829 normal (not millisecond) pulsars, and a simulated average pulse profile at 1.4 GHz for each pulsar.

The catalogue

This is a catalogue of simulated normal (not millisecond) pulsars, produced by the on-line version of the population synthesis code PSRPOP, with the help of D. R. Lorimer and J. Ridley. It is produced by executing a survey at 1.4 GHz, 512 MHz bandwidth, an exaggerated gain (larger than anticipated for the SKA) of 140 K/Jy, and an integration time of 1 hour. The catalogue therefore represents a very large Galactic population of normal pulsars, of which only a fraction will be found in typical SKA searches.

The pulsar profiles

One noiseless average pulse profile has been generated per pulsar of the catalogue, using a stochastic model of the pulsar beam by Karastergiou & Johnston (2007). The observing frequency of these profiles is 1.4 GHz, and DM dependent scattering effects have been included. The profiles are given as time resolved Stokes parameteres, with a temporal resolution of 1/1024 of the pulse period. The polarization has been computed assuming a dipole configuration for the magnetic field, and a stochastic manifestation of orthogonally polarized modes of emission. All 4 Stokes parameters have been scattered by the interstellar medium.

Future work

There are no interpulses (emission from both magnetic poles) in the simulation. This will be implemented in the next version.