ORCID Profile
0000-0002-6620-7421
Current Organisation
Australian National University
Does something not look right? The information on this page has been harvested from data sources that may not be up to date. We continue to work with information providers to improve coverage and quality. To report an issue, use the Feedback Form.
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.
Astronomical and Space Sciences | Astronomy And Astrophysics | Cosmology and Extragalactic Astronomy | Other Plasma Physics | Fluid Physics | Numerical Computation
Expanding Knowledge in the Physical Sciences | Physical sciences | Expanding Knowledge in the Information and Computing Sciences | Application packages | Mathematical sciences |
Publisher: Oxford University Press (OUP)
Date: 10-1998
Publisher: American Astronomical Society
Date: 18-11-2019
Publisher: EDP Sciences
Date: 12-09-2006
Publisher: Oxford University Press (OUP)
Date: 30-06-2017
Publisher: American Astronomical Society
Date: 02-03-2015
Publisher: American Astronomical Society
Date: 1990
DOI: 10.1086/185630
Publisher: American Astronomical Society
Date: 10-04-2017
Publisher: American Astronomical Society
Date: 10-04-2017
Publisher: American Astronomical Society
Date: 10-12-2001
DOI: 10.1086/323836
Publisher: Wiley
Date: 06-2017
DOI: 10.1111/JOSP.12188
Publisher: AIP
Date: 2005
DOI: 10.1063/1.1913936
Publisher: American Astronomical Society
Date: 09-07-2015
Publisher: American Astronomical Society
Date: 12-1995
DOI: 10.1086/176596
Publisher: AIP
Date: 2005
DOI: 10.1063/1.1913939
Publisher: Oxford University Press (OUP)
Date: 15-04-1999
Publisher: American Astronomical Society
Date: 07-1998
DOI: 10.1086/300399
Publisher: American Astronomical Society
Date: 20-06-2001
DOI: 10.1086/321417
Publisher: Cambridge University Press (CUP)
Date: 2003
DOI: 10.1071/AS02042
Abstract: We review theoretical ideas that seem to be currently important for the physics of GPS and CSS radio sources. These include models for their evolution, the production of emission lines, and the origin of the low frequency turnover. We also describe the initial phases of a program of simulations that is aimed at understanding the radiative interactions between jets, lobes, and dense clouds in the nuclei of these objects.
Publisher: American Astronomical Society
Date: 07-2003
DOI: 10.1086/375294
Publisher: American Astronomical Society
Date: 28-03-2018
Publisher: American Astronomical Society
Date: 24-03-2015
Publisher: Oxford University Press (OUP)
Date: 13-12-2016
Publisher: Wiley
Date: 02-2016
Abstract: Powerful relativistic jets in radio galaxies are capable of driving strong outflows but also inducing star‐formation by pressure‐triggering collapse of dense clouds. We review theoretical work on negative and positive active galactic nuclei feedback, discussing insights gained from recent hydrodynamical simulations of jet‐driven feedback on galaxy scales that are applicable to compact radio sources. The simulations show that the efficiency of feedback and the relative importance of negative and positive feedback depend strongly on interstellar medium properties, especially the column depth and spatial distribution of clouds. Negative feedback is most effective if clouds are distributed spherically and in idual clouds have small column depths, while positive feedback is most effective if clouds are predominantly in a disc‐like configuration. (© 2016 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Publisher: American Astronomical Society
Date: 20-02-2000
DOI: 10.1086/308397
Publisher: American Astronomical Society
Date: 20-08-2000
DOI: 10.1086/309241
Publisher: Annual Reviews
Date: 18-08-2019
DOI: 10.1146/ANNUREV-ASTRO-081817-051832
Abstract: We review the use of emission lines for understanding galaxy evolution, focusing on excitation source, metallicity, ionization parameter, ISM pressure, and electron density. We discuss the physics, benefits, and caveats of emission line diagnostics, including the effects of theoretical model uncertainties, diffuse ionized gas, and s le selection bias. In anticipation of upcoming telescope facilities, we provide new self-consistent emission line diagnostic calibrations for complete spectral coverage from the UV to the IR. These diagnostics can be used in concert to understand how fundamental galaxy properties have changed across cosmic time. We conclude the following: ▪ The UV, optical, and IR contain complementary diagnostics that can probe the conditions within different nebular ionization zones. ▪ Accounting for complex density gradients and temperature profiles is critical for reliably estimating the fundamental properties of Hii regions and galaxies. ▪ Diffuse ionized gas can raise metallicity estimates, flatten metallicity gradients, and introduce scatter in ionization parameter measurements. ▪ New 3D emission line diagnostics successfully separate the contributions from star formation, AGN, and shocks using integral field spectroscopy. We summarize with a discussion of the challenges and major opportunities for emission line diagnostics in the coming years.
Publisher: Oxford University Press (OUP)
Date: 12-10-2020
Abstract: Local ex les of jet-induced star formation lend valuable insight into its significance in galaxy evolution and can provide important observational constraints for theoretical models of positive feedback. Using optical integral field spectroscopy, we present an analysis of the ISM conditions in Minkowski’s object (z = 0.0189), a peculiar star-forming dwarf galaxy located in the path of a radio jet from the galaxy NGC 541. Full spectral fitting with ppxf indicates that Minkowski’s object primarily consists of a young stellar population $\\sim \\! 10\\, \\rm Myr$ old, confirming that the bulk of the object’s stellar mass formed during a recent jet interaction. Minkowski’s object exhibits line ratios largely consistent with star formation, although there is evidence for a low level ($\\lesssim \\! 15 \\, \\rm per \\, cent$) of contamination from a non-stellar ionizing source. Strong-line diagnostics reveal a significant variation in the gas-phase metallicity within the object, with $\\log \\left(\\rm O / H \\right) + 12$ varying by $\\sim \\! 0.5\\, \\rm dex$, which cannot be explained by in-situ star formation, an enriched outflow from the jet, or enrichment of gas in the stellar bridge between NGC 541 and NGC 545/547. We hypothesize that Minkowski’s object either (i) was formed as a result of jet-induced star formation in pre-existing gas clumps in the stellar bridge, or (ii) is a gas-rich dwarf galaxy that is experiencing an elevation in its star formation rate due to a jet interaction, and will eventually redden and fade, becoming an ultradiffuse galaxy as it is processed by the cluster.
Publisher: American Astronomical Society
Date: 06-11-2013
Publisher: American Astronomical Society
Date: 10-03-2006
DOI: 10.1086/499762
Publisher: American Astronomical Society
Date: 20-07-2001
DOI: 10.1086/321545
Publisher: SPIE
Date: 29-06-2000
DOI: 10.1117/12.390130
Publisher: American Astronomical Society
Date: 27-03-2019
Publisher: Cambridge University Press (CUP)
Date: 02-2013
DOI: 10.7120/09627286.22.1.095
Abstract: Collar-worn deterrents reduce predation by cats while collar-mounted ID enhances return of lost animals. A perception that collars are hazardous limits their use. We defined cases as ‘collar incidents’ (cat snagged its collar or caught a paw), ‘collar injuries’ (veterinary treatment needed for a collar incident), and ‘collar deaths’ (cat died), before integrating data from veterinarians, owners from the general public and owners from a welfare society. Despite biases associated with each of these groups, taken together, the results from these indicated that collar injuries or deaths are rare. Interviews with one hundred and seven veterinarians indicated an average rate of one collar injury observed per 2.3 years of veterinary practice. At one practice, over three years, only 0.33% of 4,460 cat cases were collar injuries, while 180 cat cases at four clinics during August and November 2011 included none. The 63 owners from the general public reported only one collar injury and no deaths in a lifetime of ownership, although 27% experienced collar incidents. In contrast, 22% reported cats needing treatment following road accidents, 53% reported cats needing treatment for fighting injuries and 62% had owned cats killed on the road. Most (62%) of the 55 respondents from a cat welfare society had experienced a collar incident, but only two cats needed treatment. One died. In contrast, 31 and 58% reported cats needing treatment for road accidents and fighting, respectively, and 41% had owned cats killed on the road. Fighting and road accidents are greater hazards to roaming cats than collars, which offer the compensatory benefits of mounting predation deterrents and ID tags.
Publisher: American Astronomical Society
Date: 09-2023
Publisher: American Astronomical Society
Date: 03-11-2015
Publisher: Oxford University Press (OUP)
Date: 19-11-2016
Publisher: American Astronomical Society
Date: 1999
DOI: 10.1086/300666
Publisher: American Astronomical Society
Date: 20-11-1997
DOI: 10.1086/304862
Publisher: Springer Science and Business Media LLC
Date: 12-07-2011
Publisher: Springer International Publishing
Date: 2016
Publisher: SPIE
Date: 02-2002
DOI: 10.1117/12.456509
Publisher: Springer Science and Business Media LLC
Date: 13-01-2016
Publisher: Informa UK Limited
Date: 02-10-2014
Publisher: Oxford University Press (OUP)
Date: 14-07-2017
Publisher: Oxford University Press (OUP)
Date: 15-02-2016
DOI: 10.1093/MNRAS/STW330
Publisher: American Astronomical Society
Date: 11-2007
DOI: 10.1086/520640
Publisher: American Astronomical Society
Date: 27-03-2019
Publisher: American Astronomical Society
Date: 02-2005
DOI: 10.1086/423948
Publisher: Oxford University Press (OUP)
Date: 10-01-2018
DOI: 10.1093/MNRAS/STY070
Publisher: American Astronomical Society
Date: 10-07-2000
DOI: 10.1086/309077
Publisher: Springer Science and Business Media LLC
Date: 02-08-2007
Publisher: Oxford University Press (OUP)
Date: 27-02-2015
DOI: 10.1093/MNRAS/STV081
Publisher: Cambridge University Press (CUP)
Date: 06-2019
DOI: 10.1017/S174392131900841X
Abstract: Accurate predictions of the physics of interstellar medium (ISM) are vital for understanding galaxy formation and evolution. Modelling photoionized regions with complex geometry produces realistic ionization structures within the nebulae, providing the necessary physical predictions to interpret observational data. 3D photoionization codes built with Monte Carlo techniques provide powerful tools to produce the ionizing radiation field with fractal geometry. We present a high-resolution Monte Carlo modelling of a nebula with fractal geometry, and will further show how nebular geometry influences the emission-line behaviours. Our research has important implications for studies of emission-line ratios in high redshift galaxies.
Publisher: American Astronomical Society
Date: 04-09-2013
Publisher: American Astronomical Society
Date: 07-07-2014
Publisher: American Astronomical Society
Date: 14-01-2019
Publisher: American Astronomical Society
Date: 02-2021
Abstract: We present the Stromlo Stellar Tracks, a set of stellar evolutionary tracks, computed by modifying the Modules for Experiments in Stellar Astrophysics (MESA) 1D stellar evolution package, to fit the Galactic Concordance abundances for hot ( T 8000 K) massive (≥10 M ⊙ ) main-sequence (MS) stars. Until now, all stellar evolution tracks have been computed at solar, scaled-solar, or α -element-enhanced abundances, and none of these models correctly represent the Galactic Concordance abundances at different metallicities. This paper is the first implementation of Galactic Concordance abundances to the stellar evolution models. The Stromlo tracks cover massive stars (10 ≤ M / M ⊙ ≤ 300) with varying rotations ( v / v crit = 0.0, 0.2, 0.4) and a finely s led grid of metallicities (−2.0 ≤ [Z/H] ≤ +0.5 Δ[Z/H] = 0.1) evolved from the pre-main sequence to the end of 12 C burning. We find that the implementation of Galactic Concordance abundances is critical for the evolution of MS, massive hot stars in order to estimate accurate stellar outputs ( L , T eff , g ), which, in turn, have a significant impact on determining the ionizing photon luminosity budgets. We additionally support prior findings of the importance that rotation plays on the evolution of massive stars and their ionizing budget. The evolutionary tracks for our Galactic Concordance abundance scaling provide a more empirically motivated approach than simple uniform abundance scaling with metallicity for the analysis of H ii regions and have considerable implications for determining nebular emission lines and metallicity. Therefore, it is important to refine existing stellar evolutionary models for comprehensive high-redshift extragalactic studies. The Stromlo tracks are available to the astronomical community.
Publisher: American Astronomical Society
Date: 15-07-2013
Publisher: American Astronomical Society
Date: 04-1997
DOI: 10.1086/303802
Publisher: American Astronomical Society
Date: 05-03-2013
Publisher: Oxford University Press (OUP)
Date: 29-08-2014
Publisher: American Astronomical Society
Date: 09-1993
DOI: 10.1086/191823
Publisher: American Astronomical Society
Date: 10-09-2000
DOI: 10.1086/309343
Publisher: American Astronomical Society
Date: 11-1994
DOI: 10.1086/187603
Publisher: Oxford University Press (OUP)
Date: 11-05-2005
Publisher: American Chemical Society (ACS)
Date: 06-1989
DOI: 10.1021/ED066P506
Publisher: American Astronomical Society
Date: 08-06-2016
Publisher: Cambridge University Press (CUP)
Date: 09-2015
DOI: 10.1017/S174392131500201X
Abstract: Feedback provided by relativistic jets may be effective in shaping the galaxy luminosity function. The quenching mode (quasar mode) at redshifts ~2-3 potentially disperses gas in star-forming galaxies. The maintenance mode (radio mode) heats the gas in galaxy clusters counteracting cooling flows. A number of authors have examined the effect of relativistic jets in dispersing clouds in the kpc-scale inhomogeneous interstellar medium of evolving galaxies. We have also investigated a particular case of maintenance-mode feedback in our simulation of the iconic radio galaxy / cooling flow cluster Hydra A. Modelling of the knots produced by the jets in the inner 10 kpc provides an estimate of 0.8 – 0.9 c for the velocities of the jets in agreement with other velocity estimates for FR1 jets. The addition of jet precession provides realistic simulations of the morphology of the Hydra A radio source and raises interesting questions as to the role of black hole and disk precession, in general, in galaxy formation.
Publisher: American Astronomical Society
Date: 06-06-2019
Publisher: American Astronomical Society
Date: 07-05-2015
Publisher: Oxford University Press (OUP)
Date: 10-06-2019
Abstract: In the optical spectra of galaxies, the separation of line emission from gas ionized by star formation and an active galactic nucleus (AGN), or by star formation and shocks, are very well-understood problems. However, separating line emission between AGN and shocks has proven difficult. With the aid of a new three-dimensional diagnostic diagram, we show the simultaneous separation of line emission from star formation, shocks, and AGN in NGC 1068, and quantify the ratio of star formation, shocks, and AGN in each spaxel. The AGN, shock, and star formation luminosity distributions across the galaxy accurately align with X-ray, radio, and CO(3–2) observations, respectively. Comparisons with previous separation methods show that the shocked emission heavily mixes with the AGN emission. We also show that if the H α flux is to be used as a star formation rate indicator, separating line emission from as many sources as possible should be attempted to ensure accurate results.
Publisher: American Astronomical Society
Date: 12-1991
DOI: 10.1086/186244
Publisher: American Astronomical Society
Date: 16-09-2014
Publisher: Springer Science and Business Media LLC
Date: 11-03-2010
Publisher: Oxford University Press (OUP)
Date: 08-06-2016
Publisher: Cambridge University Press
Date: 28-10-2010
Publisher: Springer Science and Business Media LLC
Date: 05-06-2007
Publisher: Oxford University Press (OUP)
Date: 17-05-2017
Publisher: Wiley
Date: 03-02-2006
Abstract: In the past, extragalactic radio jets have been modelled as interacting with a smooth, hot interstellar medium. However, it is likely that the precursors of radio sources are major or minor mergers and the resultant debris from such an event will interact with the jets that result from the fuelling of the black hole. We describe here some recent work on the interactions of jets with clumpy interstellar media consisting of a log normal distribution of dense clouds. Important features of the simulations include radio morphologies typical of powerful radio galaxies at various stages of their evolution and persistent X‐ray emission from shocked clouds which are the remnant of a circumnuclear disk. (© 2006 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Publisher: IOP Publishing
Date: 28-01-2020
Publisher: IOP Publishing
Date: 11-1996
DOI: 10.1086/133825
Publisher: EDP Sciences
Date: 2011
DOI: 10.1051/EAS/1148087
Publisher: American Astronomical Society
Date: 30-10-2014
Publisher: Elsevier BV
Date: 05-2006
Publisher: Cambridge University Press (CUP)
Date: 03-2004
Publisher: American Astronomical Society
Date: 07-10-2014
Publisher: American Astronomical Society
Date: 09-2008
DOI: 10.1086/589652
Publisher: American Astronomical Society
Date: 27-07-2016
Publisher: American Astronomical Society
Date: 12-2006
DOI: 10.1086/508261
Publisher: American Astronomical Society
Date: 06-2008
DOI: 10.1086/528711
Publisher: American Astronomical Society
Date: 26-06-2018
Publisher: American Astronomical Society
Date: 11-2002
DOI: 10.1086/342679
Publisher: Oxford University Press (OUP)
Date: 22-01-2018
DOI: 10.1093/MNRAS/STY067
Publisher: AIP Publishing LLC
Date: 2015
DOI: 10.1063/1.4937705
Publisher: American Astronomical Society
Date: 10-08-2006
DOI: 10.1086/505418
Publisher: EDP Sciences
Date: 10-2002
Publisher: American Astronomical Society
Date: 07-2004
DOI: 10.1086/421114
Publisher: American Astronomical Society
Date: 1995
DOI: 10.1086/175180
Publisher: EDP Sciences
Date: 10-2003
Publisher: American Astronomical Society
Date: 21-08-2013
Publisher: American Astronomical Society
Date: 1995
DOI: 10.1086/175181
Publisher: American Astronomical Society
Date: 10-02-2008
DOI: 10.1086/524918
Publisher: Springer Science and Business Media LLC
Date: 23-06-2007
Publisher: American Astronomical Society
Date: 07-2004
DOI: 10.1086/421113
Publisher: Oxford University Press (OUP)
Date: 04-06-2015
Publisher: Oxford University Press (OUP)
Date: 05-07-2018
Publisher: American Astronomical Society
Date: 07-2003
DOI: 10.1086/374795
Publisher: American Astronomical Society
Date: 1996
DOI: 10.1086/192255
Publisher: American Astronomical Society
Date: 08-1996
DOI: 10.1086/118031
Publisher: American Astronomical Society
Date: 27-08-2009
Publisher: American Astronomical Society
Date: 27-01-2015
Publisher: Oxford University Press (OUP)
Date: 02-04-2020
Abstract: The evolutionary paths taken by massive stars with M ≳ 60 M⊙ remain substantially uncertain. They begin their lives as main-sequence (MS) O stars. Depending on their masses, rotation rates, and metallicities, they can then encounter a wide range of evolutionary states with an equally broad set of possible surface compositions and spectral classifications. We present a new grid of calculations for the evolution of such stars that covers a broad range in mass, M/M⊙ = 60–150, rotation rate, $v/v_{\\rm crit} = 0$–0.6, metallicity, [Fe/H] = −4 to 0, and α-element enhancement, [α/Fe] = 0–0.4. We show that rotating stars undergo rotationally induced dredge-up of nucleosynthetic products, mostly He and N, to their surfaces while still on the MS. Non-rotating metal-rich stars also reveal the products of nucleosynthesis on their surfaces because even modest amounts of mass-loss expose their ‘fossil’ convective cores: regions that are no longer convective, but were part of the convective core at an early stage in the star’s evolution. Thus, surface enhancement of He and N is expected for rotating stars at all metallicities, and for non-rotating stars if they are relatively metal-rich. We calculate a stellar atmosphere for a representative model from our grid, properly accounting for He and N enhancement, and show that the resulting spectrum provides a good match to observed WNL stars, strongly suggesting that the physical mechanisms we have identified are the ultimate cause of the WNL phase.
Publisher: American Astronomical Society
Date: 02-2003
DOI: 10.1086/345448
Publisher: American Astronomical Society
Date: 21-11-2003
DOI: 10.1086/381190
Publisher: American Astronomical Society
Date: 02-1999
DOI: 10.1086/306718
Publisher: Elsevier BV
Date: 10-2003
Publisher: Cambridge University Press (CUP)
Date: 07-2014
DOI: 10.1017/S1743921314009661
Abstract: Here we present the first results from the Siding Spring Southern Seyfert Spectroscopic Snapshot Survey (S7) which aims to investigate the physics of ∼140 radio-detected southern active Galaxies with z .02 through Integral Field Spectroscopy using the Wide Field Spectrograph (WiFeS). This instrument provides data cubes of the central 38×25 arc sec. of the target galaxies in the waveband 340–710nm with the unusually high resolution of R =7000 in the red (530–710nm), and R =3000 in the blue (340–560nm). These data provide the morphology, kinematics and the excitation structure of the extended narrow-line region, probe relationships with the black hole characteristics and the host galaxy, measures host galaxy abundance gradients and the determination of nuclear abundances from the HII regions. From photoionisation modelling, we may determine the shape of the ionising spectrum of the AGN, discover whether AGN metallicities differ from nuclear abundances determined from HII regions, and probe grain destruction in the vicinity of the AGN. Here we present some preliminary results and modelling of both Seyfert galaxies observed as part of the survey.
Publisher: American Astronomical Society
Date: 03-2022
Abstract: The Messenger Interface Monte Carlo Mappings V (M 3 ) is a photoionization code adopting the fully self-consistent Monte Carlo radiative transfer (MCRT) technique, which presents a major advance over previous photoionization models with simple geometries. M 3 is designed for modeling nebulae in arbitrary three-dimensional geometries. In this paper, we describe the MCRT technique and the microphysics implemented in M 3 , including photoionization, collisional ionization, free–free and free–bound recombination, and two-photon radiation. We put M 3 through the Lexington/Meudon benchmarks to test the reliability of the new code. We apply M 3 to three H ii region models with fiducial geometries, demonstrating that M 3 is capable of dealing with nebulae with complex geometries. M 3 is a promising tool for understanding emission-line behavior in the era of SDSS-V/LVM and James Webb Space Telescope, which will provide high-quality data of spatially resolved nearby H ii regions and highly turbulent local and high-redshift H ii regions.
Publisher: American Astronomical Society
Date: 18-07-2019
Publisher: American Astronomical Society
Date: 11-1996
DOI: 10.1086/118189
Publisher: Oxford University Press (OUP)
Date: 27-06-2017
Publisher: American Astronomical Society
Date: 02-11-2007
DOI: 10.1086/524657
Publisher: American Astronomical Society
Date: 30-07-2014
Publisher: Cambridge University Press (CUP)
Date: 03-2004
Publisher: Oxford University Press (OUP)
Date: 20-07-2016
Publisher: Springer Berlin Heidelberg
Date: 1993
Publisher: American Astronomical Society
Date: 10-06-2016
Publisher: EDP Sciences
Date: 06-2014
Publisher: American Astronomical Society
Date: 10-07-2018
Publisher: American Astronomical Society
Date: 07-2022
Abstract: We create a photoionization model embedded in the turbulent interstellar medium (ISM) by using the state-of-the-art Messenger Monte Carlo MAPPINGS V code (M 3 ) in conjunction with the CMFGEN stellar atmosphere model. We show that the turbulent ISM causes the inhomogeneity of electron temperature and density within the nebula. The fluctuation in the turbulent ISM creates complex ionization structures seen in nearby nebulae. The inhomogeneous density distribution within the nebula creates a significant scatter on the spatially resolved standard optical diagnostic diagrams, which cannot be represented by the spherical constant-density photoionization model. We analyze the dependence of different optical emission lines on the complexity of nebular geometry, finding that the emission lines residing on the nebular boundary are highly sensitive to the complexity of nebular geometry, while the emission lines produced throughout the nebula are sensitive to the density distribution of the ISM within the nebula. Our fractal photoionization model demonstrates that a complex nebular geometry is required for the accurate modeling of H ii regions and emission-line galaxies, especially for the high-redshift galaxies, where the ISM is highly turbulent based on increasing observational evidence.
Publisher: American Astronomical Society
Date: 09-1993
DOI: 10.1086/173099
Publisher: AIP
Date: 1998
DOI: 10.1063/1.55879
Publisher: Cambridge University Press (CUP)
Date: 03-2004
Publisher: Oxford University Press (OUP)
Date: 09-12-2018
Publisher: American Astronomical Society
Date: 25-04-2014
Publisher: Journal of the Physical Society of Japan
Date: 19-03-2014
Publisher: American Astronomical Society
Date: 10-03-1998
DOI: 10.1086/305336
Publisher: American Astronomical Society
Date: 20-06-2002
DOI: 10.1086/340429
Publisher: American Astronomical Society
Date: 06-06-2012
Publisher: American Astronomical Society
Date: 10-10-2000
DOI: 10.1086/309538
Start Date: 09-2016
End Date: 04-2021
Amount: $422,200.00
Funder: Australian Research Council
View Funded ActivityStart Date: 2002
End Date: 12-2005
Amount: $400,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 2006
End Date: 12-2011
Amount: $440,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 2014
End Date: 12-2017
Amount: $399,231.00
Funder: Australian Research Council
View Funded Activity