A 24 Hr Global Campaign to Assess Precision Timing of the Millisecond Pulsar J1713+0747

Dolch, Timothy; Lam, Michael T.; Cordes, J. M.; Chatterjee, Shami; Bassa, C. G.; Bhattacharyya, Bhaswati; Champion, D. J.; Cognard, I.; Crowter, Kathryn; Demorest, Paul; Hessels, J. W. T.; Janssen, G. H.; Jenet, F. A.; Jones, Glenn; Jordan, C.; Karuppusamy, R.; Keith, Michael; Kondratiev, V. I.; Krämer, M.; Lazarus, P.; Lazio, T. Joseph W.; Lee, K. J.; McLaughlin, M. A.; Roy, Jayanta; Shannon, R. M.; Stairs, I. H.; Stovall, K.; Verbiest, J. P. W.; Madison, D. R.; Palliyaguru, Nipuni; Perrodin, D.; Ransom, S. M.; Stappers, B. W.; Zhu, Weiwei; Dai, Shi; Desvignes, G.; Guillemot, L.; Liu, K.; Lyne, A. G.; Perera, B. B. P.; Petroff, Emily; Rankin, Joanna M.; Smits, R.

doi:10.1088/0004-637x/794/1/21

Cited by 42 publications

(41 citation statements)

References 68 publications

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“…Shannon & Cordes (2012) studied the pulse arrival times from a single long exposure of PSR J1713+0747, and found that this pulsarʼs single pulses showed random jitter of 26 s m  . A similar result of 27 s m  was found by Dolch et al (2014) from a more recent study using a 24 hr continuous observation of PSR J1713+0747 conducted with major telescopes around the globe. Therefore, by averaging many pulses collected in the typical ∼20 minutes NANOGrav observation, one expects 27 s 1200 m ñ = 51 ns of jitter noise.…”

Section: Noise Modelsupporting

confidence: 85%

Testing Theories of Gravitation Using 21-Year Timing of Pulsar Binary J1713+0747

Zhu

Stairs

Demorest

et al. 2015

ApJ

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125

119

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We report 21-year timing of one of the most precise pulsars: PSR J1713+0747. Its pulse times of arrival are well modeled by a comprehensive pulsar binary model including its three-dimensional orbit and a noise model that incorporates short-and long-timescale correlated noise such as jitter and red noise. Its timing residuals have weighted root mean square ∼92 ns. The new data set allows us to update and improve previous measurements of the system properties, including the masses of the neutron star (1.31 ± 0.11 M e ) and the companion white dwarf (0.286 ± 0.012 M e ) as well as their parallax distance 1.15 ± 0.03 kpc. We measured the intrinsic change in orbital period, P b Inṫ , is −0.20 ± 0.17 ps s −1 , which is not distinguishable from zero. This result, combined with the measured P bInṫ of other pulsars, can place a generic limit on potential changes in the gravitational constant G. We found that G Ġ is consistent with zero [(−0.6 ± 1.1) × 10 −12 yr −1 , 95% confidence] and changes at least a factor of 31 (99.7% confidence) more slowly than the average expansion rate of the universe. This is the best G Ġ limit from pulsar binary systems. The P b Inṫ of pulsar binaries can also place limits on the putative coupling constant for dipole gravitational radiation 0.9 3.3 10´-(95% confidence). Finally, the nearly circular orbit of this pulsar binary allows us to constrain statistically the strong-field post-Newtonian parameters Δ, which describes the violation of strong equivalence principle, and 3 a , which describes a breaking of both Lorentz invariance in gravitation and conservation of momentum. We found, at 95% confidence, 0.01 D < and 2 10 3 20 a <´-based on PSR J1713+0747.

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Section: Noise Modelsupporting

confidence: 85%

Testing Theories of Gravitation Using 21-Year Timing of Pulsar Binary J1713+0747

Zhu

Stairs

Demorest

et al. 2015

ApJ

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125

119

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“…The situation is likely to be significantly improved when coherent addition of the pulse signal is achieved with more telescopes, as also suggested in Dolch et al (2014). Eventually, the next generation of radio telescopes, e.g., the Square Kilometre Array and the Five hundred meter Aperture Spherical Telescope, will provide the best opportunity ever to study single pulse emission from MSPs.…”

Section: Conclusion and Discussionmentioning

confidence: 93%

Variability, polarimetry, and timing properties of single pulses from PSR J1713+0747 using the Large European Array for Pulsars

Liu¹,

Bassa²,

Janssen³

et al. 2016

Mon. Not. R. Astron. Soc.

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Single pulses preserve information about the pulsar radio emission and propagation in the pulsar magnetosphere, and understanding the behaviour of their variability is essential for estimating the fundamental limit on the achievable pulsar timing precision. Here we report the findings of our analysis of single pulses from PSR J1713+0747 with data collected by the Large European Array for Pulsars (LEAP). We present statistical studies of the pulse properties that include distributions of their energy, phase and width. Two modes of systematic sub-pulse drifting have been detected, with a periodicity of 7 and 3 pulse periods. The two modes appear at different ranges of pulse longitude but overlap under the main peak of the integrated profile. No evidence for pulse micro-structure is seen with a time resolution down to 140 ns. In addition, we show that the fractional polarisation of single pulses increases with their pulse peak flux density. By mapping the probability density of linear polarisation position angle with pulse longitude, we reveal the existence of two orthogonal polarisation modes. Finally, we find that the resulting phase jitter of integrated profiles caused by single pulse variability can be described by a Gaussian probability distribution only when at least 100 pulses are used for integration. Pulses of different flux densities and widths contribute approximately equally to the phase jitter, and no improvement on timing precision is achieved by using a sub-set of pulses with a specific range of flux density or width.

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“…We reanalyzed an 8 hr GBT observation from a 24 hr campaign targeting PSRJ1713+0747 (Dolch et al 2014). The increased observation length provided finer resolution but we did not see clear scintillation arcs; though, there is some notable power off the axis where conjugate time is zero.…”

Section: Changes In Flux and Scintillation Parametersmentioning

confidence: 99%

A Second Chromatic Timing Event of Interstellar Origin toward PSR J1713+0747

Lam

Ellis

Grillo

et al. 2018

ApJ

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The frequency dependence of radio pulse arrival times provides a probe of structures in the intervening media. Demorest et al. was the first to show a short-term (∼100-200 days) reduction in the electron content along the line of sight to PSRJ1713+0747 in data from 2008 (approximately MJD 54750) based on an apparent dip in the dispersion measure of the pulsar. We report on a similar event in 2016 (approximately MJD 57510), with average residual pulse-arrival times ≈−3.0, −1.3, and −0.7 μs at 820, 1400, and 2300MHz, respectively. Timing analyses indicate possible departures from the standard ν −2 dispersive-delay dependence. We discuss and rule out a wide variety of potential interpretations. We find the likeliest scenario to be lensing of the radio emission by some structure in the interstellar medium, which causes multiple frequency-dependent pulse arrival-time delays.

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A 24 Hr Global Campaign to Assess Precision Timing of the Millisecond Pulsar J1713+0747

Cited by 42 publications

References 68 publications

Testing Theories of Gravitation Using 21-Year Timing of Pulsar Binary J1713+0747

Testing Theories of Gravitation Using 21-Year Timing of Pulsar Binary J1713+0747

Variability, polarimetry, and timing properties of single pulses from PSR J1713+0747 using the Large European Array for Pulsars

A Second Chromatic Timing Event of Interstellar Origin toward PSR J1713+0747

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