Constraining the luminosity function parameters and population size of radio pulsars in globular clusters
Abstract
The luminosity distribution of Galactic radio pulsars is believed to be lognormal in form. Applying this functional form to populations of pulsars in globular clusters, we employ Bayesian methods to explore constraints on the mean and standard deviation of the function, as well as the total number of pulsars in the cluster. Our analysis is based on an observed number of pulsars down to some limiting flux density, measurements of flux densities of individual pulsars, as well as diffuse emission from the direction of the cluster. We apply our analysis to Terzan 5 and demonstrate, under reasonable assumptions, that the number of potentially observable pulsars is in a 95.45% credible interval of 133^{+101} _{58}. Beaming considerations would increase the true population size by approximately a factor of two.
 Publication:

Neutron Stars and Pulsars: Challenges and Opportunities after 80 years
 Pub Date:
 March 2013
 DOI:
 10.1017/S1743921312023794
 arXiv:
 arXiv:1210.5472
 Bibcode:
 2013IAUS..291..257C
 Keywords:

 methods: numerical  methods: statistical  globular clusters: general  globular clusters: individual: Terzan 5  stars: neutron  pulsars: general;
 Astrophysics  Solar and Stellar Astrophysics;
 Astrophysics  High Energy Astrophysical Phenomena
 EPrint:
 Proceedings of IAUS 291 "Neutron Stars and Pulsars: Challenges and Opportunities after 80 years", J. van Leeuwen (ed.)