Precision orbital dynamics from interstellar scintillation arcs for PSR J0437-4715

Reardon, Daniel J.; Coles, William A.; Bailes, Matthew; Bhat, N. D. Ramesh; Dai, Shi; Hobbs, George B.; Kerr, Matthew; Manchester, Richard N.; Oslowski, Stefan; Parthasarathy, Aditya; Russell, Christopher J.; Shannon, Ryan M.; Spiewak, Renee; Toomey, Lawrence; Tuntsov, Artem V.; van Straten, Willem; Walker, Mark A.; Wang, Jingbo; Zhang, Lei; Zhu, Xing-Jiang

doi:10.48550/arxiv.2009.12757

Cited by 5 publications

(5 citation statements)

References 34 publications

(83 reference statements)

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“…However, early studies by Hemberger and Stinebring [58] already showed how these phenomena can impact timing significantly. Turning this around, Reardon et al [121] showed how scintillation arcs can actually be useful for timing, as they can provide independent constraints on timing-model parameters. The study of how to use scintillation arcs, or what effects they really do have on PTA experiments, has only just begun, so at present their impact is not fully clear yet.…”

Section: Iism Studiesmentioning

confidence: 99%

Pulsar Timing Array Experiments

Verbiest,

Oslowski,

Burke-Spolaor

2021

Preprint

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Pulsar timing is a technique that uses the highly stable spin periods of neutron stars to investigate a wide range of topics in physics and astrophysics. Pulsar timing arrays (PTAs) use sets of extremely well-timed pulsars as a Galaxy-scale detector with arms extending between Earth and each pulsar in the array. These challenging experiments look for correlated deviations in the pulsars' timing that are caused by low-frequency gravitational waves (GWs) traversing our Galaxy. PTAs are particularly sensitive to GWs at nanohertz frequencies, which makes them complementary to other space-and ground-based detectors. In this chapter, we will describe the methodology behind pulsar timing; provide an overview of the potential uses of PTAs; and summarise where current PTA-based detection efforts stand. Most predictions expect PTAs to successfully detect a cosmological background of GWs emitted by supermassive black-hole binaries and also potentially detect continuouswave emission from binary supermassive black holes, within the next several years.

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Section: Iism Studiesmentioning

confidence: 99%

Pulsar Timing Array Experiments

Verbiest,

Oslowski,

Burke-Spolaor

2021

Preprint

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“…We have restricted this plot to source brightness temperatures in the range 10 11 − 10 12 K. 2013) that very similar screens could also be responsible for the parabolic arc phenomenon observed in the secondary spectra of certain radio pulsars (Cordes et al 2006;Walker et al 2004). It remains to be seen whether filamentary screens of the kind revealed in this paper can account for other properties of the parabolic arcs, such as their occurrence rate and the scattering anisotropy (Reardon et al 2020).…”

Section: Physical Propertiesmentioning

confidence: 79%

ASKAP observations of multiple rapid scintillators reveal a degrees-long plasma filament

Wang,

Tuntsov,

Murphy

et al. 2021

Preprint

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We present the results from an Australian Square Kilometre Array Pathfinder search for radio variables on timescales of hours. We conducted an untargeted search over a 30 deg 2 field, with multiple 10-hour observations separated by days to months, at a central frequency of 945 MHz. We discovered six rapid scintillators from 15-minute model-subtracted images with sensitivity of ∼ 200 𝜇Jy/beam; two of them are extreme intra-hour variables with modulation indices up to ∼ 40% and timescales as short as tens of minutes. Five of the variables are in a linear arrangement on the sky with angular width ∼ 1 arcmin and length ∼ 2 degrees, revealing the existence of a huge plasma filament in front of them. We derived kinematic models of this plasma from the annual modulation of the scintillation rate of our sources, and we estimated its likely physical properties: a distance of ∼ 4 pc and length of ∼ 0.1 pc. The characteristics we observe for the scattering screen are incompatible with published suggestions for the origin of intra-hour variability leading us to propose a new picture in which the underlying phenomenon is a cold tidal stream. This is the first time that multiple scintillators have been detected behind the same plasma screen, giving direct insight into the geometry of the scattering medium responsible for enhanced scintillation.

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“…Several scintillating pulsars show variability in their diffractive scintillation timescale, which can be modelled as in Rickett et al (2014) and Reardon et al (2019) to provide more precise measurements of 𝑖 and improve the mass constraints. Modulation in the curvature of scintillation arcs could also be detected in some pulsars and provide a more precise measurement of 𝑖 and Ω than the scintillation timescale (Reardon et al 2020).…”

Section: Discussionmentioning

confidence: 99%

The Parkes pulsar timing array second data release: Timing analysis

Reardon,

Shannon,

Cameron

et al. 2021

Preprint

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The main goal of pulsar timing array experiments is to detect correlated signals such as nanohertz-frequency gravitational waves. Pulsar timing data collected in dense monitoring campaigns can also be used to study the stars themselves, their binary companions, and the intervening ionised interstellar medium. Timing observations are extraordinarily sensitive to changes in path length between the pulsar and the Earth, enabling precise measurements of the pulsar positions, distances and velocities, and the shapes of their orbits. Here we present a timing analysis of 25 pulsars observed as part of the Parkes Pulsar Timing Array (PPTA) project over time spans of up to 24 yr. The data are from the second data release of the PPTA, which we have extended by including legacy data. We make the first detection of Shapiro delay in four Southern pulsars (PSRs J1017−7156, J1125−6014, J1545−4550, and J1732−5049), and of parallax in six pulsars. The prominent Shapiro delay of PSR J1125−6014 implies a neutron star mass of 𝑀 𝑝 = 1.5 ± 0.2 𝑀 (68% credibility interval). Measurements of both Shapiro delay and relativistic periastron advance in PSR J1600−3053 yield a large but uncertain pulsar mass of 𝑀 𝑝 = 2.06 +0.44 −0.41 M (68% credibility interval). We measure the distance to PSR J1909−3744 to a precision of 10 lyr, indicating that for gravitational wave periods over a decade, the pulsar provides a coherent baseline for pulsar timing array experiments.

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Precision orbital dynamics from interstellar scintillation arcs for PSR J0437-4715

Cited by 5 publications

References 34 publications

Pulsar Timing Array Experiments

Pulsar Timing Array Experiments

ASKAP observations of multiple rapid scintillators reveal a degrees-long plasma filament

The Parkes pulsar timing array second data release: Timing analysis

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