ORCID Profile
0000-0002-4594-3438
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In Research Link Australia (RLA), "Research Topics" refer to ANZSRC FOR and SEO codes. These topics are either sourced from ANZSRC FOR and SEO codes listed in researchers' related grants or generated by a large language model (LLM) based on their publications.
Astronomy And Astrophysics | Information Systems Organisation | Astronomical and Space Sciences | Archaeology | Computer Software | Information Systems | Archaeology of Asia Africa and the Americas | Software Engineering | Distributed and Grid Systems | Concurrent Programming | Global Information Systems
Physical sciences | Information processing services | Technological and organisational innovation | Application Software Packages (excl. Computer Games) | Expanding Knowledge in the Physical Sciences | Expanding Knowledge in the Information and Computing Sciences |
Publisher: American Astronomical Society
Date: 29-11-2011
Publisher: Cambridge University Press (CUP)
Date: 2009
DOI: 10.1071/AS08025
Abstract: We demonstrate how interactive, three-dimensional (3D) scientific visualizations can be efficiently interchanged between a variety of mediums. Through the use of an appropriate interchange format, and a unified interaction interface, we minimize the effort to produce visualizations appropriate for undertaking knowledge discovery at the astronomer's desktop, as part of conference presentations, in digital publications or as Web content. We use ex les from cosmological visualization to address some of the issues of interchange and to describe our approach to adapting s2plot desktop visualizations to the Web 2 .
Publisher: Oxford University Press (OUP)
Date: 17-08-2010
Publisher: Springer International Publishing
Date: 2017
Publisher: Springer Science and Business Media LLC
Date: 23-10-2018
DOI: 10.1007/S12024-017-9915-0
Abstract: A gunfight between police and a gang of men led by the self-styled "Captain Moonlite", a.k.a. George Scott, occurred on 16th November 1879 at a farmhouse near Wantabadgery Station in the colony of New South Wales. The skirmish resulted in the deaths of two bushrangers and one police officer. As a result, Captain Moonlite and Thomas Rogan were hung in Sydney's Darlinghurst Gaol on 20 January 1880 for the murder of Constable Edward Webb-Bowen. Culpability for firing the fatal shot, however, has remained a source of controversy. Information obtained from an analysis of historical records was used to guide an archeological excavation at the scene of the shooting in which Terrestrial Laser Scanning (TLS) technology was employed to produce a digital (3D) terrain model of the siege location. Utilizing the terrain model, the relative positions of Moonlite, Webb-Bowen, and the other gang members were established with possible projectile trajectories plotted. This, in combination with inquest evidence from a gun maker and the medical practitioner who examined Constable Webb-Bowen's wound, indicates that the most likely shooter was Gus Warnicke, aged 15 years, the youngest member of the gang, who was also killed in the exchange of fire.
Publisher: Society for Imaging Science & Technology
Date: 14-02-2016
Publisher: American Astronomical Society
Date: 08-2002
DOI: 10.1086/341582
Publisher: Oxford University Press (OUP)
Date: 04-01-2013
DOI: 10.1093/MNRAS/STS513
Publisher: American Astronomical Society
Date: 05-03-2007
DOI: 10.1086/511068
Publisher: American Astronomical Society
Date: 06-2003
DOI: 10.1086/374944
Publisher: Oxford University Press (OUP)
Date: 11-04-2001
Publisher: American Astronomical Society
Date: 07-2001
DOI: 10.1086/321453
Publisher: Cambridge University Press (CUP)
Date: 2006
DOI: 10.1071/AS06009
Abstract: We present a new, three-dimensional (3D) plotting library with advanced features, and support for standard and enhanced display devices. The library — s2plot — is written in c and can be used by c , c++ , and fortran programs on GNU/Linux and Apple/OSX systems. s2plot draws objects in a 3D ( x , y , z ) Cartesian space and the user interactively controls how this space is rendered at run time. With a pgplot -inspired interface, s2plot provides astronomers with elegant techniques for displaying and exploring 3D data sets directly from their program code, and the potential to use stereoscopic and dome display devices. The s2plot architecture supports dynamic geometry and can be used to plot time-evolving data sets, such as might be produced by simulation codes. In this paper, we introduce s2plot to the astronomical community, describe its potential applications, and present some ex le uses of the library.
Publisher: IEEE
Date: 04-2017
Publisher: Cambridge University Press (CUP)
Date: 2011
DOI: 10.1071/AS10019
Abstract: General-purpose computing on graphics processing units (GPGPU) is dramatically changing the landscape of high performance computing in astronomy. In this paper, we identify and investigate several key decision areas, with a goal of simplifying the early adoption of GPGPU in astronomy. We consider the merits of OpenCL as an open standard in order to reduce risks associated with coding in a native, vendor-specific programming environment, and present a GPU programming philosophy based on using brute force solutions. We assert that effective use of new GPU-based supercomputing facilities will require a change in approach from astronomers. This will likely include improved programming training, an increased need for software development best practice through the use of profiling and related optimisation tools, and a greater reliance on third-party code libraries. As with any new technology, those willing to take the risks and make the investment of time and effort to become early adopters of GPGPU in astronomy, stand to reap great benefits.
Publisher: IEEE
Date: 12-2010
Publisher: Elsevier BV
Date: 2010
Publisher: Oxford University Press (OUP)
Date: 21-06-1997
Publisher: Public Library of Science (PLoS)
Date: 14-09-2015
Publisher: Elsevier BV
Date: 11-2008
Publisher: Oxford University Press (OUP)
Date: 07-2005
Publisher: American Astronomical Society
Date: 08-2012
Publisher: Public Library of Science (PLoS)
Date: 24-07-2013
Publisher: SPIE
Date: 16-09-2004
DOI: 10.1117/12.551030
Publisher: Frontiers Media SA
Date: 27-02-2017
Publisher: Springer Netherlands
Date: 2008
Publisher: American Astronomical Society
Date: 10-2002
DOI: 10.1086/342546
Publisher: Oxford University Press (OUP)
Date: 07-2001
Publisher: IEEE
Date: 09-2013
Publisher: Elsevier BV
Date: 02-2011
Publisher: Cambridge University Press (CUP)
Date: 2012
DOI: 10.1071/AS12025
Abstract: We present a framework to volume-render three-dimensional data cubes interactively using distributed ray-casting and volume-bricking over a cluster of workstations powered by one or more graphics processing units (GPUs) and a multi-core central processing unit (CPU). The main design target for this framework is to provide an in-core visualization solution able to provide three-dimensional interactive views of terabyte-sized data cubes. We tested the presented framework using a computing cluster comprising 64 nodes with a total of 128 GPUs. The framework proved to be scalable to render a 204 GB data cube with an average of 30 frames per second. Our performance analyses also compare the use of NVIDIA Tesla 1060 and 2050 GPU architectures and the effect of increasing the visualization output resolution on the rendering performance. Although our initial focus, as shown in the ex les presented in this work, is volume rendering of spectral data cubes from radio astronomy, we contend that our approach has applicability to other disciplines where close to real-time volume rendering of terabyte-order three-dimensional data sets is a requirement.
Publisher: Oxford University Press (OUP)
Date: 09-2002
Publisher: Oxford University Press (OUP)
Date: 06-2004
Publisher: American Geophysical Union (AGU)
Date: 04-2011
DOI: 10.1029/2009RS004323
Publisher: Elsevier BV
Date: 2018
DOI: 10.1016/J.NEUROIMAGE.2017.10.049
Abstract: To improve the accuracy of automated vein segmentation by combining susceptibility-weighted images (SWI), quantitative susceptibility maps (QSM), and a vein atlas to produce a resultant image called a composite vein image (CV image). An atlas was constructed in common space from manually traced MRI images from ten volunteers. The composite vein image was derived for each subject as a weighted sum of three inputs an SWI image, a QSM image and the vein atlas. The weights for each input and each anatomical location, called template priors, were derived by assessing the accuracy of each input over an independent data set. The accuracy of vein segmentations derived automatically from each of the CV image, SWI, and QSM image sets was assessed by comparison with manual tracings. Three different automated vein segmentation techniques were used, and ten performance metrics evaluated. Vein segmentations using the CV image were comprehensively better than those derived from SWI or QSM images (mean Cohen's d = 1.1). Sixty permutations of performance metric, benchmark image, and automated segmentation technique were evaluated. Vein identification improvements that were both large and significant (Cohen's d > 0.80, p < 0.05) were found in 77% of the permutations, compared to no improvement in 5%. The accuracy of automated vein segmentations derived from the composite vein image was overwhelmingly superior to segmentations derived from SWI or QSM alone.
Publisher: Oxford University Press (OUP)
Date: 05-12-2011
Publisher: Oxford University Press (OUP)
Date: 10-2006
Publisher: American Astronomical Society
Date: 16-09-2013
Publisher: American Astronomical Society
Date: 20-03-2003
DOI: 10.1086/344477
Publisher: American Astronomical Society
Date: 02-2002
DOI: 10.1086/338088
Publisher: Springer Science and Business Media LLC
Date: 08-1998
DOI: 10.1038/29466
Publisher: Cambridge University Press (CUP)
Date: 2003
DOI: 10.1071/AS03039
Abstract: We describe the first distributed data implementation of the perspective shear-warp volume rendering algorithm and explore its applications to large astronomical data cubes and simulation realisations. Our system distributes sub-volumes of 3-dimensional images to leaf nodes of a Beowulf-class cluster, where the rendering takes place. Junction nodes composite the sub-volume renderings together and pass the combined images upwards for further compositing or display. We demonstrate that our system out-performs other software solutions and can render a 'worst-case' 512 × 512 × 512 data volume in less than four seconds using 16 rendering and 15 compositing nodes. Our system also performs very well compared with much more expensive hardware systems. With appropriate commodity hardware, such as Swinburne's Virtual Reality Theatre or a 3Dlabs Wildcat graphics card, stereoscopic display is possible.
Publisher: Public Library of Science (PLoS)
Date: 25-09-2013
Publisher: PeerJ
Date: 05-2014
DOI: 10.7717/PEERJ.355
Publisher: Institute of Electrical and Electronics Engineers (IEEE)
Date: 06-1997
DOI: 10.1109/42.585760
Abstract: Methods for optimizing the acquisition, reconstruction and analysis of positron emission tomography (PET) images for functional brain mapping have been investigated. The scatter fraction and noise-equivalent count rate characteristics were measured for the ECAT 951/31R PET scanner operating in septa-extended two-dimensional (2-D) and septa-retracted three-dimensional (3-D) modes. The 3-D mode is shown to provide higher signal-to-noise images than the 2-D mode at specific activities less than 30 kBq/ml. To enable increased temporal resolution in dynamic 3-D PET activation studies, a parallel version of the 3-D reconstruction algorithm was developed. Implementation of the reprojection algorithm on an 88 processor 1860 supercomputer resulted in a more than tenfold increase in reconstruction speed compared to a single 1860 processor system. An investigation of the optimal duration for imaging brain activations was undertaken in 12 normal subjects using repeated H2(15)O slow infusions and a visually presented lexical decision task. The significance of change in regional cerebral blood flow (CBF) was determined using statistical parametric maps for images acquired during stimulation, immediately after stimulation, and commencing 1 min after cessation of the stimulus. Regions of CBF change were detected in all three images. Dynamic 3-D, or four-dimensional (4-D), PET activation scanning is shown to be practical and likely to further improve the sensitivity of PET for detection of subtle regional CBF changes in functional brain mapping research.
Publisher: Elsevier BV
Date: 09-2018
Publisher: Cambridge University Press (CUP)
Date: 2014
DOI: 10.1017/PASA.2013.36
Abstract: Archival data from the HI Parkes All-Sky Survey (HIPASS) and the HI Zone of Avoidance (HIZOA) survey have been carefully reprocessed into a new 1.4 GHz continuum map of the sky south of δ = +25°. The wide sky coverage, high sensitivity of 40 mK (limited by confusion), resolution of 14.4 arcmin (compared to 51 arcmin for the Haslam et al. 408 MHz and 35 arcmin for the Reich et al. 1.4 GHz surveys), and low level of artefacts make this map ideal for numerous studies, including: merging into interferometer maps to complete large-scale structures decomposition of thermal and non-thermal emission components from Galactic and extragalactic sources and comparison of emission regions with other frequencies. The new map is available for download.
Publisher: Oxford University Press (OUP)
Date: 06-2004
Publisher: Oxford University Press (OUP)
Date: 09-03-2012
Publisher: Springer Netherlands
Date: 2007
Publisher: American Astronomical Society
Date: 20-06-2007
DOI: 10.1086/517986
Publisher: American Astronomical Society
Date: 23-06-2004
DOI: 10.1086/423239
Publisher: American Astronomical Society
Date: 14-12-1970
DOI: 10.1086/519444
Publisher: Springer Science and Business Media LLC
Date: 22-02-2015
Publisher: Oxford University Press (OUP)
Date: 11-1999
Publisher: Oxford University Press (OUP)
Date: 2005
Publisher: Cambridge University Press (CUP)
Date: 2004
DOI: 10.1071/AS03048
Abstract: The H I content of Hickson Compact Groups in the southern hemisphere is measured using data from the H I Parkes All-Sky Survey (HIPASS), and dedicated observations using the narrow band filter on the Multibeam instrument on the Parkes telescope. The expected H I mass of these groups was estimated using the luminosity, diameter, and morphological types of the member galaxies, calibrated from published data. Taking careful account of non-detection limits, the results show that the compact group population that has been detected by these observations has an H I content similar to that of galaxies in the reference field s le. The upper limits for the undetected groups lie within the normal range improvement of these limits will require a large increase in sensitivity.
Publisher: Oxford University Press (OUP)
Date: 21-12-2009
Publisher: Cambridge University Press (CUP)
Date: 2015
DOI: 10.1017/PASA.2015.5
Abstract: The Murchison Widefield Array is a Square Kilometre Array Precursor. The telescope is located at the Murchison Radio–astronomy Observatory in Western Australia. The MWA consists of 4 096 dipoles arranged into 128 dual polarisation aperture arrays forming a connected element interferometer that cross-correlates signals from all 256 inputs. A hybrid approach to the correlation task is employed, with some processing stages being performed by bespoke hardware, based on Field Programmable Gate Arrays, and others by Graphics Processing Units housed in general purpose rack mounted servers. The correlation capability required is approximately 8 tera floating point operations per second. The MWA has commenced operations and the correlator is generating 8.3 TB day −1 of correlation products, that are subsequently transferred 700 km from the MRO to Perth (WA) in real-time for storage and offline processing. In this paper, we outline the correlator design, signal path, and processing elements and present the data format for the internal and external interfaces.
Publisher: Springer Berlin Heidelberg
Date: 2007
Publisher: Cambridge University Press (CUP)
Date: 10-2016
DOI: 10.1017/S1743921317001399
Abstract: Radio survey datasets comprise an increasing number of in idual observations stored as sets of multidimensional data. In large survey projects, astronomers commonly face limitations regarding: 1) interactive visual analytics of sufficiently large subsets of data 2) synchronous and asynchronous collaboration and 3) documentation of the discovery workflow. To support collaborative data inquiry, we present encube , a large-scale comparative visual analytics framework. encube can utilise advanced visualization environments such as the CAVE2 (a hybrid 2D and 3D virtual reality environment powered with a 100 Tflop/s GPU-based supercomputer and 84 million pixels) for collaborative analysis of large subsets of data from radio surveys. It can also run on standard desktops, providing a capable visual analytics experience across the display ecology. encube is composed of four primary units enabling compute-intensive processing, advanced visualisation, dynamic interaction, parallel data query, along with data management. Its modularity will make it simple to incorporate astronomical analysis packages and Virtual Observatory capabilities developed within our community. We discuss how encube builds a bridge between high-end display systems (such as CAVE2) and the classical desktop, preserving all traces of the work completed on either platform – allowing the research process to continue wherever you are.
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Start Date: 2005
End Date: 06-2008
Amount: $235,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 02-2012
End Date: 05-2015
Amount: $320,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 01-2004
End Date: 12-2003
Amount: $10,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 12-2023
End Date: 12-2028
Amount: $513,598.00
Funder: Australian Research Council
View Funded Activity