Sri Lanka: Compiled and introduced by <b>S.W. Perera</b>

Perera, S.W.

doi:10.1177/0021989411424839

Cited by 2 publications

(2 citation statements)

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“…In principle, one can get the position vectors of a pulsar in two different DCRFs at any given reference epochs. Since the transformation results are determined by the position accuracy, which is positively correlated with the timing accuracy, and the residuals of J0437 − 4715 become worse in the 2nd release of IPTA because of the missing the additional noise terms to optimize its noise analysis (Perera et al 2019), we prefer to choose the 1st release of IPTA. Since IPTA DR1 adopts DE421, which is only sub‐mas away from the ephemerides of subsequent versions, including DE436 and DE440 (Wang et al 2017), even for the closest previous ephemerides DE405, the transformation angle between them is only in the order of sub‐mas, which indicates low reliability of the result, and therefore earlier versions of ephemerides need to be considered.…”

Section: Calculation Principle and Methods Of The Transformation Betw...mentioning

confidence: 99%

An application of pulsar timing in dynamic reference frame transformation of solar system

et al. 2023

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The establishment of pulsar space-time reference frame is of great significance for X-ray pulsar deep space navigation. To demonstrate that the pulsar parameters are accurate enough to be used as a spatial reference, the transformation parameters, that is, 𝛼, 𝛽, and 𝛾, of different reference frames determined based on pulsar timing are shown and compared with that of the heliocentric coordinates of Earth-Moon barycenter. The JPL ephemerides such as DE421, DE200 and INPOP series, are mainly selected for conversion parameter calculation. For the best-determined parameter 𝛾, the discrepancy between the two different data is 0.38 mas/1.33𝜎. The timing positions of pulsars clearly show the frame-tie of different ephemerides, indicating that MSPs have the potential to be a candidate for constructing time-space standard. It is also found that the rotation angles change linearly with time, and PSR J0437 − 4715 plays a critical role in the fitting of 𝛼. By employing a few high-quality MSPs, the transformation precision of the right ascension is evaluated to be on the order of sub-milliarcsecond, which is an order of magnitude higher than that of the declination.

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Section: Calculation Principle and Methods Of The Transformation Betw...mentioning

confidence: 99%

An application of pulsar timing in dynamic reference frame transformation of solar system

et al. 2023

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“…The IPTA data release 2 (Perera et al. 2019) was formed by combining a subset of PPTA Data Release 2 (Kerr et al. 2020) with the EPTA DR1 (Desvignes et al.…”

Section: Introductionmentioning

confidence: 99%

The Parkes Pulsar Timing Array third data release

Zic

Reardon

Kapur

et al. 2023

Publ. Astron. Soc. Aust.

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We present the third data release from the Parkes Pulsar Timing Array (PPTA) project. The release contains observations of 32 pulsars obtained using the 64-m Parkes “Murriyang” radio telescope. The data span is up to 18 years with a typical cadence of 3 weeks. This data release is formed by combining an updated version of our second data release with ∼ 3 years of more recent data primarily obtained using an ultra-wide-bandwidth receiver system that operates between 704 and 4032 MHz. We provide calibrated pulse profiles, flux-density dynamic spectra, pulse times of arrival, and initial pulsar timing models. We describe methods for processing such wide-bandwidth observations, and compare this data release with our previous release.

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Sri Lanka: Compiled and introduced by S.W. Perera

Cited by 2 publications

References 1 publication

An application of pulsar timing in dynamic reference frame transformation of solar system

An application of pulsar timing in dynamic reference frame transformation of solar system

The Parkes Pulsar Timing Array third data release

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