TY - JOUR
T1 - Wide-band timing of the Parkes Pulsar Timing Array UWL data
AU - Curyło, Małgorzata
AU - Pennucci, Timothy T.
AU - Bailes, Matthew
AU - Bhat, N. D. Ramesh
AU - Cameron, Andrew D.
AU - Dai, Shi
AU - Hobbs, George
AU - Kapur, Agastya
AU - Manchester, Richard N.
AU - Mandow, Rami
AU - Miles, Matthew T.
AU - Russell, Christopher J.
AU - Reardon, Daniel J.
AU - Shannon, Ryan M.
AU - Spiewak, Renée
AU - van Straten, Willem
AU - Zhu, Xing-Jiang
AU - Zic, Andrew
N1 - Copyright © 2023. The Author(s). Published by the American Astronomical Society. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.
PY - 2023/2/1
Y1 - 2023/2/1
N2 - 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 μs and (0.043-14.24) × 10−4 cm−3 pc, respectively, with 94% of the pulsars achieving a median TOA uncertainty of less than 1 μs.
AB - 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 μs and (0.043-14.24) × 10−4 cm−3 pc, respectively, with 94% of the pulsars achieving a median TOA uncertainty of less than 1 μs.
UR - http://www.scopus.com/inward/record.url?scp=85148665531&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/aca535
DO - 10.3847/1538-4357/aca535
M3 - Article
AN - SCOPUS:85148665531
SN - 0004-637X
VL - 944
SP - 1
EP - 22
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - 128
ER -