Richard Dodson

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Pulsar timing at the Mt Pleasant observatory has focused on Vela, which can be tracked for 18 hours of the day. These nearly continuous timing records extend over 24 years allowing a greater insight into details of timing noise, micro glitches and other more exotic effects. In particular we report the glitch parameters of the 2004 event, along with the(More)
We report on Chandra ACIS imaging of the pulsar wind nebula (PWN) of the young Vela-like PSR B1706−44, which shows the now common pattern of an equatorial wind and polar jets. The structure is particularly rich, showing a relativistically boosted termination shock, jets with strong confinement, a surrounding radio/X-ray PWN and evidence for a quasi-static(More)
Relative astrometry of the J=1→0, v=1 and v=2 SiO masers towards R Leonis Minoris using VERA Abstract Oxygen-rich Asymptotic Giant Branch (AGB) stars are intense emitters of SiO and H 2 O maser lines at 43 (J=1→0, v=1 and 2) and 22 GHz, respectively. VLBI observations of the maser emission provides a unique tool to sample the innermost layers of the(More)
The first accurate measurements of Vela's proper motion were produced using the Parkes-Tidbinbilla Interferometer (PTI) (Bailes et al 1989). This 275 km baseline at 1.6 GHz gave a resolution of 140 mas and detected the proper motion and thus, by extrapolation, the birth site. We have extended this work to allow the third dimension to be derived via the(More)
The SKA will be capable of producing a stream of science data products that are Exa-scale in terms of their storage and processing requirements. This Google-scale enterprise is attracting considerable international interest and excitement from within the industrial and academic communities. In this chapter we examine the data flow, storage and processing(More)
Pulsar timing at the Mt Pleasant observatory focused on Vela, which could be tracked for 18 hours of the day. These nearly continuous timing records extend over 24 years allowing a great insight into details of timing noise, micro glitches and other more exotic effects. It has been found that the spin up for the Vela pulsar occurs instantaneously to within(More)
  • María J Rioja, Richard Dodson, Richard W Porcas, Dick Ferris, John Reynolds, Tetsuo Sasao +2 others
  • 2009
We revisit the " Cluster-Cluster " or multi-view VLBI technique from the perspective of its syner-gy with the multi-beam features inherent in the Australian Square Kilometer Array Pathfinder (ASKAP) and its potential to improve the outcomes of VLBI observations with ASKAP. We include a list of candidate VLBI sites that already support or can be upgraded to(More)
Work has been ongoing for the development of the required code for full polarisation processing of VLBI data using some new antennae mounts. The extensions of AIPS allows the support of two new mount types; the left-handed and right-handed Nasmyth antennae (Pico Veleta in the GMVA and Yebes-40m in the EVN) and the EW-mount (Hobart in the LBA). The data(More)
We have combined high resolution VLBI Space Observatory Programme (VSOP) data at 1.6 and 4.8 GHz with Very Long Baseline Array (VLBA) data at higher frequencies and with similar resolutions to study the spectral properties of the core of M87 with milliarcsecond resolution. The VSOP data allow a more accurate measurement of the turnover frequency, and hence(More)
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