Astrometric VLBI Observation of PSR 0329+54

Sekido, Mamoru; Imae, Michito; Hanado, Yuko; Ilyasov, Yuri P.; Орешко, В В; Rodin, A. E.; Hama, S.; Nakajima, Jun; Kawai, Eiji; Koyama, Yasuhiro; Kondo, Tetsuro; Kurihara, Noriyuki; Hosokawa, Mizuhiko

doi:10.1093/pasj/51.5.595

Cited by 9 publications

(4 citation statements)

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“…3, we plot the localization result of every individual single pulse and average positions given by two methods. To evaluate the absolute localization precision of the whole data processing pipeline, we also present two reference positions (Sekido et al 1999;Brisken et al 2002, see Tab. 2 for details).…”

Section: Localizationmentioning

confidence: 99%

“…in standard geodetic and astrometric VLBI measurement (Thompson et al 2001;Takahashi 2000). Actually there is already work that tries to obtain the high precision pulsar position in a geodetic VLBI approach: Sekido et al (1999) obtain the position of B0329+54 and further derive its proper motion by first deriving the group delay with Japanese bandwidth synthesis software "KOMB" (Takahashi et al 1991), then carrying out analysis with CALC/SOLVE. However, their approach is still quite different from our work: they treat the pulsar as a normal radio source.…”

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confidence: 99%

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The Localization of the Single Pulse in VLBI Observation

Liu

Jiang

Zheng

et al. 2019

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In our previous work, we propose a cross spectrum based method to extract single pulse signals from RFI contaminated data, which is originated from geodetic VLBI postprocessing. This method fully utilizes fringe phase information of the cross spectrum and hence maximizes the signal power. However, the localization has not been discussed in that work yet. As the continuation of that work, in this paper, we further study how to localize single pulses using astrometric solving method. Assuming that the burst is a point source, we derive the burst position by solving a set of linear equations given the relation between the residual delay and the offset to a priori position. We find that the single pulse localization results given by both astrometric solving and radio imaging are consistent within 3 σ level. Therefore we claim that it is possible to derive the position of a single pulse with reasonable precision based on only 3 or even 2 baselines with 4 milliseconds integration. The combination of cross spectrum based detection and the localization proposed in this work then provide a thorough solution for searching single pulse in VLBI observation. According to our calculation, our pipeline gives comparable accuracy as radio imaging pipeline. Moreover, the computational cost of our pipeline is much smaller, which makes it more practical for FRB search in regular VLBI observation. The pipeline is now publicly available and we name it as "VOLKS", which is the acronym of "VLBI Observation for frb Localization Keen Searcher".

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Section: Localizationmentioning

confidence: 99%

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confidence: 99%

The Localization of the Single Pulse in VLBI Observation

Liu

Jiang

Zheng

et al. 2019

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“…Radio pulses from the Crab pulsar inevitably pass through the nebula plasma and the effect there in the acceleration site is possibly seen as fluctuation of the dispersion measure (DM). We can utilize the 34 m radio antenna in Kashima, Japan [8] which has a good record with precise…”

Section: Pos(icrc2015)887mentioning

confidence: 99%

A 3-Meter Atmospheric Cherenkov Telescope as a Test Bench for Very High Energy Gamma-Ray Astrophysics Projects

Yoshikoshi¹

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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We have been setting up a 3-meter diameter atmospheric Cherenkov telescope in Akeno, Japan, for various R & D studies mainly on very high energy gamma-ray astrophysics. This Davies-Cotton type telescope (Akeno telescope, hereafter) was manufactured in 1998 and has been recommissioned at low cost. A low power consumption imaging camera system has been developed for a future gamma-ray astrophysics observatory with "mobile" imaging atmospheric Cherenkov telescopes, which can flexibly change the array configuration for a number of science targets, and has been installed to the Akeno telescope for test observations. We present performances of the optics and the drive system of the Akeno telescope, as well as the status of the imaging camera system. Some other R & D plans including test observations using a prototype imaging camera for CTA and simultaneous observations of the optical and radio Crab pulsar are also presented.

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“…With steady progress of VLBI observations, correlation and data processing techniques (Bartel et al 1985;Deller et al 2007), astrometry observations of more and more pulsars have been successfully accomplished with the VLBI (Gwinn et al 1986;Sekido et al 1999;Brisken et al 2003;Chatterjee et al 2009;Deller et al 2009Deller et al , 2019. The precision of VLBI measurements is getting higher and higher.…”

Section: Introductionmentioning

confidence: 99%

New timing measurement results of 16 pulsars

Liu,

Yan,

Shen

et al. 2020

Preprint

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Pulsar's position, proper motion and parallax are important parameters in timing equations.It is a really challenging work to fit astrometric parameters accurately through pulsar timing, especially for pulsars that show irregular timing properties. As the fast development of related techniques, it is possible to measure astrometric parameters of more and more pulsars in a model-independent manner with the Very Long Baseline Interferometry (VLBI). In this work, we select 16 normal pulsars, whose parallax and proper motion have not been successfully fitted with timing observations or show obvious differences with corresponding latest VLBI solutions, and do further studies on their timing properties. After updating astrometric parameters in pulsar ephemerides with the latest VLBI measurements, we derive the latest rotation solutions of these pulsars with observation data at S and C-band obtained from the Shanghai Tian Ma Radio Telescope (TMRT). Compared with spin frequency ν inferred from previous rotation solutions, the newly-fitted ν show differences larger than 10 −9 Hz for most pulsars. The contribution of the Shklovsky effect to period derivative Ṗ can be properly removed taking advantages of accurate proper motion and distance of target pulsars measured 1 by VLBI astrometry. This further leads to a precise estimate of intrinsic characteristic age τ c . Differences between the newly-measured τ c and corresponding previous results are as large as 2% for some pulsars. VLBI astrometric parameter solutions also lead to better measurements of timing irregularities. For PSR B0154+61, the glitch epoch (MJD 58279.5) measured with previous ephemeris is about 13 d later than the result (MJD 58266.4) obtained with VLBI astrometric parameter solutions.

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Astrometric VLBI Observation of PSR 0329+54

Cited by 9 publications

References 0 publications

The Localization of the Single Pulse in VLBI Observation

The Localization of the Single Pulse in VLBI Observation

A 3-Meter Atmospheric Cherenkov Telescope as a Test Bench for Very High Energy Gamma-Ray Astrophysics Projects

New timing measurement results of 16 pulsars

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