The Green Bank North Celestial Cap Survey. IX. Timing Follow-up for 128 Pulsars
Alexander McEwen, Joseph K. Swiggum, D. L. Kaplan, Chia Min Tan, Bradley W. Meyers, Emmanuel Fonseca, Gabriella Agazie, Pragya Chawla, Kathryn Crowter, Megan E. DeCesar, Timothy Dolch, Fengqiu Adam Dong, William Fiore, Emmanuel Fonseca, Deborah C. Good, Alina Istrate, V. M. Kaspi, V. I. Kondratiev, J. van Leeuwen, L. Levin, Evan F. Lewis, Ryan S. Lynch, Kiyoshi W. Masui, James W. McKee, M. A. McLaughlin, Hind Al Noori, E. Parent, S. M. Ransom, Xavier Siemens, R. Spiewak, I. H. Stairs
Abstract
Abstract The Green Bank North Celestial Cap survey is one of the largest and most sensitive searches for pulsars and transient radio objects. Observations for the survey have finished; priorities have shifted toward long-term monitoring of its discoveries. In this study, we have developed a pipeline to handle large data sets of archival observations and connect them to recent, high-cadence observations taken using the Canadian Hydrogen Intensity Mapping Experiment telescope. This pipeline handles data for 128 pulsars and has produced measurements of spin, positional, and orbital parameters that connect data over observation gaps as large as 2000 days. We have also measured glitches in the timing residuals for five of the pulsars included and proper motion for 19 sources (13 new). We include updates to orbital parameters for 19 pulsars, including nine previously unpublished binaries. For two of these binaries, we provide updated measurements of post-Keplerian binary parameters, which result in much more precise estimates of the total masses of both systems. For PSR J0509+3801, the much improved measurement of the Einstein delay yields much improved mass measurements for the pulsar and its companion, 1.399(6) M ⊙ and 1.412(6) M ⊙ , respectively. For this system, we have also obtained a measurement of the orbital decay due to the emission of gravitational waves, <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mover accent="true"> <mml:mrow> <mml:mi>P</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>̇</mml:mo> </mml:mrow> </mml:mover> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">B</mml:mi> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:mo>−</mml:mo> <mml:mn>1.37</mml:mn> <mml:mo stretchy="false">(</mml:mo> <mml:mn>7</mml:mn> <mml:mo stretchy="false">)</mml:mo> <mml:mo>×</mml:mo> <mml:msup> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>12</mml:mn> </mml:mrow> </mml:msup> </mml:math> , which is in agreement with the rate predicted by general relativity for these masses.