Long-term timing observations of 374 pulsars

By G. Hobbs, Andrew G. Lyne, Michael Kramer, C. Martin, C. Jordan. 2004

338 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Oceanography

View Paper: https://www.semanticscholar.org/paper/67dc0ec77845814f54009d4c62bfe115aaf5b03c

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Citations in the corpus

The International Pulsar Timing Array: First Data Release (2016, neutral): “…are as follows: (1) Lommen et al. (2000), (2) Abdo et al. (2009), (3) Lommen et al. (2006), (4) Bailes et al. (1994), (5) Abdo et al. (2010), (6) Hobbs et al. (2004b), (7) Toscano et al. (1998), (8) Navarro et al. (1995), (9) Kramer et al. (1998), (10) Du et al. (2014), (11) Verbiest & Lorimer…”
The Parkes Pulsar Timing Array Project (2006, background): “The exception, PSR J1824−2452A, is located in the globular cluster M28.”
The subpulse modulation properties of pulsars at 21 cm (2005, background): “It turns out that the correct pulse period of this pulsar has appeared in the literature (Hobbs et al. 2004) without a comment about this discrepancy.”
Pulsar timing analysis in the presence of correlated noise (2011, methodology): “The low frequencies have been removed by adding them to the timing model, either as a high order polynomial (e.g., Thorsett et al. 1999) or as a carefully chosen Fourier series (e.g., fitwaves in Tempo2; Hobbs et al. 2004).”
TEMPO2, a new pulsar-timing package - I. An overview (2006, methodology): “Except for the very youngest pulsars, the frequency second and higher derivatives are not believed to represent the secular spin-down of the pulsar, but rather timing irregularities known as timing noise (e.g. Hobbs et al. 2004).”
THE FIRST FERMI LARGE AREA TELESCOPE CATALOG OF GAMMA-RAY PULSARS (2009, methodology): “Jodrell Bank observations (Hobbs et al. 2004) were carried out at typical intervals of between 2 days and 10 days in a 64-MHz band centered on 1404 MHz, using an analog filterbank to provide the frequency resolution required to remove interstellar dispersive broadening.”
TIMING MEASUREMENTS OF THE RELATIVISTIC BINARY PULSAR PSR B1913+16 (2010, methodology): “Similar results were obtained by fitting multiple harmonically related sinusoids to the timing noise with the routine “FITWAVES” (Hobbs et al. 2004) of program TEMPO2 (Hobbs et al. 2006; Edwards et al. 2006), instead of the multiple frequency derivatives described above.”
A study of 315 glitches in the rotation of 102 pulsars (2011, neutral): “Observation procedures are described by Hobbs et al. (2004).”
An analysis of the timing irregularities for 366 pulsars (2009, neutral): “The basic observational parameters for the pulsars in our sample were provided by Hobbs et al. (2004); hereafter H04.”
The GMRT Epoch of Reionization experiment: a new upper limit on the neutral hydrogen power spectrum at z≈ 8.6 (2010, background): “This pulsar has a period of 0.53 seconds and an average flux of 350mJy at 150MHz (Hobbs et al. 2004).”
Getting Its Kicks: A VLBA Parallax for the Hyperfast Pulsar B1508+55 (2005, background): “8 While an estimate for P̈ exists for this pulsar (Hobbs et al. 2004), it is affected by timing noise and does not give a physically meaningful value for the braking index.”
FERMI LARGE AREA TELESCOPE OBSERVATIONS OF THE CRAB PULSAR AND NEBULA (2009, methodology): “The timing solution for the Crab Pulsar has been built using observations made with the Nançay radio telescope (France; Theureau et al. 2005) and the Jodrell Bank Observatory 42 foot MKIA telescope (England; Hobbs et al. 2004; Lyne et al. 1993).”
EIGHT γ-RAY PULSARS DISCOVERED IN BLIND FREQUENCY SEARCHES OF FERMI LAT DATA (2010, background): “This would be among the highest transverse velocities measured for any pul-337 sar (e.g. Hobbs et al. 2004).”
Avalanche Dynamics of Radio Pulsar Glitches (2007, neutral): “…(11) Hobbs et al. 2004a; (12) Downs 1981; (13) Wang et al. 2000; (14) Dodson et al. 2002; (15) Dodson et al. 2004; (16) Flanagan & Buchner 2006; (17) Hobbs et al. 2004b; (18) Camilo et al. 2000; (19) Camilo et al. 2004; (20) Torii et al. 2000; (21) Kaspi et al. 2000; (22) Kaspi & Gavriil 2003;…”