Wide-band Timing of the Parkes Pulsar Timing Array UWL Data

In 2018 an ultra-wide-bandwidth low-frequency (UWL) receiver was installed on the 64 m Parkes Radio Telescope, enabling observations with an instantaneous frequency coverage from 704 to 4032 MHz. Here we present the analysis of a 3 yr data set of 35 ms pulsars observed with the UWL by the Parkes Pulsar Timing Array, using wide-band timing methods. The two key differences compared to typical narrowband methods are (1) generation of two-dimensional templates accounting for pulse shape evolution with frequency and (2) simultaneous measurements of the pulse time of arrival (TOA) and dispersion measure (DM). This is the first time that wide-band timing has been applied to a uniform data set collected with a single large fractional bandwidth receiver, for which such techniques were originally developed. As a result of our study, we present a set of profile evolution models and new timing solutions, including initial noise analysis. Precision of our TOA and DM measurements is in the range of 0.005-2.08 mu s and (0.043-14.24) x 10(-4) cm(-3) pc, respectively, with 94% of the pulsars achieving a median TOA uncertainty of less than 1 mu s.

Automated summary

This study used an ultra-wide-bandwidth low-frequency (UWL) receiver installed on the 64 m Parkes Radio Telescope to observe 35 ms pulsars, and analyzed the data using wide-band timing methods. The results include a set of profile evolution models and new timing solutions, with a precision of TOA and DM measurements ranging from 0.005 to 2.08 μs and (0.043-14.24) x 10(-4) cm(-3) pc, respectively. 94% of the pulsars achieved a median TOA uncertainty of less than 1 μs.