ORCID Profile
0000-0001-7289-1998
Current Organisation
Armagh Observatory and Planetarium
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 | Galactic Astronomy | Cosmology and Extragalactic Astronomy | Astronomical and Space Instrumentation | Instruments And Techniques | High Energy Astrophysics; Cosmic Rays | Turbulent Flows | Astrobiology | Tropospheric and Stratospheric Physics | Stellar Astronomy and Planetary Systems | Atmospheric Sciences Not Elsewhere Classified
Physical sciences | Expanding Knowledge in the Physical Sciences | Scientific instrumentation | Higher education | Expanding Knowledge in Technology | Atmospheric processes | Education and Training Systems not elsewhere classified | Education and Training not elsewhere classified | Air quality | Earth sciences |
Publisher: Oxford University Press (OUP)
Date: 03-2016
DOI: 10.1093/MNRAS/STW473
Publisher: Cambridge University Press (CUP)
Date: 2009
DOI: 10.1071/AS08027
Abstract: Since the recent upgrades to the Australia Telescope National Facility (ATNF) Mopra telescope back-end and receiver system, it has risen from an under-subscribed facility to a sought-after instrument with heavy international competition to gain time. Furthermore, the introduction of the on-the-fly mapping capability in 2004 has made this technique one of Mopra's most popular observing modes. In addition, the recent upgrade of the NANTEN millimetre-wavelength telescope to the sub-millimetre NANTEN2 instrument, has provided a complementary, higher-frequency facility to Mopra. A two-day workshop was held at Swinburne University in June 2008 to disseminate the current state of ongoing large-scale mapping projects and associated spin-offs that the telescopes' upgrades have facilitated, and to decide upon future research directions. Here, we provide a summary of the result-oriented talks as a record of the state of Australian-access single-dish millimetre science in 2008.
Publisher: Cambridge University Press (CUP)
Date: 2016
DOI: 10.1017/PASA.2016.38
Abstract: The high Antarctic plateau provides exceptional conditions for infrared observations on account of the cold, dry and stable atmosphere above the ice surface. This paper describes the scientific goals behind the first program to examine the time-varying universe in the infrared from Antarctica — the Kunlun Infrared Sky Survey (KISS). This will employ a 50cm telescope to monitor the southern skies in the 2.4μm K dark window from China's Kunlun station at Dome A, on the summit of the Antarctic plateau, through the uninterrupted 4-month period of winter darkness. An earlier paper discussed optimisation of the K dark filter for sensitivity (Li et al. 2016). This paper examines the scientific program for KISS. We calculate the sensitivity of the camera for the extrema of observing conditions that will be encountered. We present the parameters for s le surveys that could then be carried out for a range of cadences and sensitivities. We then discuss several science programs that could be conducted with these capabilities, involving star formation, brown dwarfs and hot Jupiters, exoplanets around M dwarfs, the terminal phases of stellar evolution, fast transients, embedded supernova searches, reverberation mapping of AGN, gamma ray bursts and the detection of the cosmic infrared background.
Publisher: Oxford University Press (OUP)
Date: 14-07-2016
Publisher: SPIE
Date: 12-2002
DOI: 10.1117/12.456999
Publisher: Cambridge University Press (CUP)
Date: 2004
DOI: 10.1071/AS03018
Abstract: We have developed a 350 μm radiometer to perform automated site testing in remote regions of Antarctica. In summer 2000–2001 the instrument operated at Concordia, a new station under construction at Dome C on the Antarctic Plateau. We present the results, and compare them with the atmospheric opacity measured at the South Pole in the same five-week period. During these five weeks, observing conditions at Dome C were, on average, substantially better than those at the South Pole.
Publisher: Oxford University Press (OUP)
Date: 30-08-2010
Publisher: Cambridge University Press (CUP)
Date: 08-2006
DOI: 10.1017/S1743921307002177
Abstract: We are studying the molecular clouds in the region around G333.6-0.2 in a number of 3-mm transitions from different molecular species, to probe, among other things, the turbulent properties. The observations are being made by on-the-fly mapping with the 22-m diameter single-dish Mopra radio telescope. See Bains et al . (2006) and Cunningham et al . (2006 in these proceedings) for more details. During 2004 and 2005 we obtained 13 CO (1 – 0), C 18 O, CS (2 – 1) and C 34 S data. Using the different molecular tracers gives complementary information about the gas density structure, due to the different critical densities, and different isotopomers allows correction for optical depth effects.
Publisher: Oxford University Press (OUP)
Date: 12-02-2016
DOI: 10.1093/MNRAS/STW121
Publisher: American Astronomical Society
Date: 03-2021
Abstract: We report the most detailed 1–3 GHz radio continuum emission map of the nearest region of massive-star formation, the Carina Nebula. As part of a large program with the Australia Telescope Compact Array, we have covered ∼12 deg 2 , achieving an angular resolution of ∼16″, representing the largest and most complete map of the radio continuum to date. Our continuum map shows a spectacular and complex distribution of emission across the nebula, with multiple structures such as filaments, shells, and fronts across a wide range of size scales. The ionization fronts have advanced far into the southern and northern region of the Galactic plane, as fronts are clearly detected at distances of ∼80 pc from the stellar clusters in the center. We estimated an ionization photon luminosity Q H = (7. 8 ± 0.8) × 10 50 s −1 , which corresponds to ∼85% of the total value obtained from stellar population studies. Thus, approximately 15% of the ionizing flux has escaped from the nebula into the diffuse Galactic interstellar medium. Comparison between radio continuum and the hydrogen atomic and molecular gas maps offers a clear view of the bipolar outflow driven by the energy released by the massive stellar clusters that also affects the fraction of molecular gas across the nebula. Comparison between 8 μ m and 70 μ m emission maps and the radio continuum reveals how the hot gas permeates through the molecular cloud shapes the material into features such as pillars, small shells, and arc-like structures and ultimately escapes.
Publisher: American Astronomical Society
Date: 06-04-2011
Publisher: Oxford University Press (OUP)
Date: 21-03-2009
Publisher: AIP
Date: 2012
DOI: 10.1063/1.4772298
Publisher: Cambridge University Press (CUP)
Date: 2001
DOI: 10.1071/AS01007
Abstract: The Near-infrared Integral Field Spectrograph (NIFS) will beAustralia’s first Gemini instrument. NIFS is a near-infrared, imaging spectrograph that will be used with the ALTAIR facility adaptive optics system on Gemini North to perform near-diffraction-limited imaging spectroscopy over a 3·0″ × 3·0″ field of view with 0·1″ wide slitlets and a spectral resolving power of ˜5300. NIFS will operate in the wavelength range from 0·94–2·50 µm where ALTAIR delivers its greatest gains. Its primary purpose is to study moderate-surface-brightness structures around discrete objects that are revealed at high spatial resolution by ALTAIR. NIFS will address a wide range of science from studies of Galactic star formation and the Galactic centre to the nature of disk galaxies at z ˜ 1. Studies of the demographics of massive black holes in galactic nuclei and studies of the excitation conditions in the inner narrow-line regions of Seyfert galaxies have been identified as two core NIFS programs. These and other science drivers for NIFS are discussed.
Publisher: Wiley
Date: 09-2003
Publisher: Cambridge University Press (CUP)
Date: 10-2013
DOI: 10.1017/S1743921314000283
Abstract: We present maps of a large number of dense molecular gas tracers across the central molecular zone of our Galaxy. The data were taken with the CSIRO/CASS Mopra telescope in Large Projects in the 1.3 cm, 7 mm, and 3 mm wavelength regimes. Here, we focus on the brightness of the shock tracers SiO and HNCO, molecules that are liberated from dust grains under strong (SiO) and weak (HNCO) shocks. The shocks may have occurred when the gas enters the bar regions and the shock differences could be due to differences in the moving cloud masses. Based on tracers of ionizing photons, it is unlikely that the morphological differences are due to selective photo-dissociation of the molecules. We also observe direct heating of molecular gas in strongly shocked zones, with high SiO/HNCO ratios, where temperatures are determined from the transitions of ammonia. Strong shocks appear to be the most efficient heating source of molecular gas, apart from high energy emission emitted by the central supermassive black hole Sgr A* and the processes within the extreme star formation region Sgr B2.
Publisher: Oxford University Press (OUP)
Date: 25-02-2010
DOI: 10.1093/PASJ/62.1.51
Publisher: SPIE
Date: 12-2002
DOI: 10.1117/12.456503
Publisher: Springer Berlin Heidelberg
Date: 2009
Publisher: American Astronomical Society
Date: 11-09-2015
Publisher: Cambridge University Press (CUP)
Date: 07-2016
DOI: 10.1017/S1743921316012035
Abstract: We present an update on the Mopra Central Molecular Zone Carbon Monoxide (CO) survey, with data taken in 2016 extending the original 3.5° ≥ l ≥ 358.5°, +1.0° ≥ b ≥ -0.5° to 4.0° ≥ l ≥ 358.0°, +1.0° ≥ b ≥ -1.0°. Using the four simultaneously observed lines of 12 CO, 13 CO, C 18 O, and C 17 O Nyquist s led at 0.6′ spatial and 0.1 km/s spectral resolution, we are building an optical-thickness-corrected three-dimensional model of the diffuse gas, and making cloud mass estimates. This data, as part of the Mopra Southern Galactic Plane CO Survey (Braiding et al . (2015), Burton et al . (2013)), is at the highest resolution available across such a widespread region, and includes the Sagittarius A, Sagittarius B2, Sagittarius C, and G1.3 cloud complexes, as well as Bania’s Clump 2.
Publisher: Oxford University Press (OUP)
Date: 07-03-2016
DOI: 10.1093/MNRAS/STW525
Publisher: Oxford University Press (OUP)
Date: 02-01-2019
Publisher: SPIE
Date: 21-08-1998
DOI: 10.1117/12.317242
Publisher: Cambridge University Press (CUP)
Date: 2005
DOI: 10.1071/AS04077
Abstract: The cold, dry, and stable air above the summits of the Antarctic plateau provides the best ground-based observing conditions from optical to sub-millimetre wavelengths to be found on the Earth. Pathfinder for an International Large Optical Telescope (PILOT) is a proposed 2 m telescope, to be built at Dome C in Antarctica, able to exploit these conditions for conducting astronomy at optical and infrared wavelengths. While PILOT is intended as a pathfinder towards the construction of future grand-design facilities, it will also be able to undertake a range of fundamental science investigations in its own right. This paper provides the performance specifications for PILOT, including its instrumentation. It then describes the kinds of projects that it could best conduct. These range from planetary science to the search for other solar systems, from star formation within the Galaxy to the star formation history of the Universe, and from gravitational lensing caused by exo-planets to that produced by the cosmic web of dark matter. PILOT would be particularly powerful for wide-field imaging at infrared wavelengths, achieving near diffraction-limited performance with simple tip–tilt wavefront correction. PILOT would also be capable of near diffraction-limited performance in the optical wavebands, as well be able to open new wavebands for regular ground-based observation, in the mid-IR from 17 to 40 μm and in the sub-millimetre at 200 μm.
Publisher: Oxford University Press (OUP)
Date: 11-05-2009
Publisher: SPIE
Date: 21-08-1998
DOI: 10.1117/12.317241
Publisher: EDP Sciences
Date: 11-2018
DOI: 10.1051/0004-6361/201833183
Abstract: Using high-resolution data of the 12 CO and 13 CO ( J = 1 – 0) line emission from the Mopra Southern Galactic Plane CO Survey in conjunction with neutral hydrogen observations from the Southern Galactic Plane Survey (SGPS) and mid-infrared Spitzer data, we have explored the large-scale environment of the supernova remnant Kes 41. On the basis of these data, we identified for the first time the parent cloud of Kes 41 in its whole extension and surveyed the HII regions, masers, and the population of massive young stellar objects in the cloud. The whole unveiled giant cloud, located at the kinematic distance of 12.0 ± 3.6 kpc, whose average total mass and size are ~10–30 × 10 5 M ⊙ and ~ 26′, also shines in γ -rays, as revealed by the Large Area Telescope on board the Fermi satellite. We determined a high average proton density ~500–1000 cm −3 in the large molecular complex, of which protons from the neutral atomic and ionised gases comprise only ~15%.
Publisher: EDP Sciences
Date: 2011
DOI: 10.1051/EAS/1152021
Publisher: Oxford University Press (OUP)
Date: 04-02-2013
DOI: 10.1093/MNRAS/STT061
Publisher: Oxford University Press (OUP)
Date: 1998
Publisher: Oxford University Press (OUP)
Date: 08-2007
Publisher: Cambridge University Press (CUP)
Date: 2009
DOI: 10.1071/AS08048
Abstract: PILOT (the Pathfinder for an International Large Optical Telescope) is a proposed 2.5-m optical/infrared telescope to be located at Dome C on the Antarctic plateau. Conditions at Dome C are known to be exceptional for astronomy. The seeing (above ∼30 m height), coherence time, and isoplanatic angle are all twice as good as at typical mid-latitude sites, while the water-vapour column, and the atmosphere and telescope thermal emission are all an order of magnitude better. These conditions enable a unique scientific capability for PILOT, which is addressed in this series of papers. The current paper presents an overview of the optical and instrumentation suite for PILOT and its expected performance, a summary of the key science goals and observational approach for the facility, a discussion of the synergies between the science goals for PILOT and other telescopes, and a discussion of the future of Antarctic astronomy. Paper II and Paper III present details of the science projects ided, respectively, between the distant Universe (i.e. studies of first light, and the assembly and evolution of structure) and the nearby Universe (i.e. studies of Local Group galaxies, the Milky Way, and the Solar System).
Publisher: Cambridge University Press (CUP)
Date: 2009
DOI: 10.1071/AS08049
Abstract: PILOT (the Pathfinder for an International Large Optical Telescope) is a proposed 2.5-m optical/infrared telescope to be located at Dome C on the Antarctic plateau. The atmospheric conditions at Dome C deliver a high sensitivity, high photometric precision, wide-field, high spatial resolution, and high-cadence imaging capability to the PILOT telescope. These capabilities enable a unique scientific potential for PILOT, which is addressed in this series of papers. The current paper presents a series of projects dealing with the distant (redshift ) Universe, that have been identified as key science drivers for the PILOT facility. The potential for PILOT to detect the first populations of stars to form in the early Universe, via infrared projects searching for pair-instability supernovae and gamma-ray burst afterglows, is investigated. Two projects are proposed to examine the assembly and evolution of structure in the Universe: an infrared survey searching for the first evolved galaxies at high redshift, and an optical survey aimed at characterising moderate-redshift galaxy clusters. Finally, a large-area weak-lensing survey and a program to obtain supernova infrared light-curves are proposed to examine the nature and evolution of dark energy and dark matter.
Publisher: Oxford University Press (OUP)
Date: 11-05-2007
Publisher: Oxford University Press (OUP)
Date: 24-05-2017
Publisher: Oxford University Press (OUP)
Date: 09-11-2011
Publisher: Cambridge University Press (CUP)
Date: 08-2012
DOI: 10.1017/S1743921312016973
Abstract: While the summit of the Antarctic Plateau has long been expected to harbor the best ground-based sites for terahertz (THz) frequency astronomical investigations, it is only recently that direct observations of exceptional THz atmospheric transmission and stability have been obtained. These observations, in combination with recent technological advancements in astronomical instrumentation and autonomous field platforms, make the recognition and realization of terahertz observatories on the high plateau feasible and timely. Here, we will explore the context of terahertz astronomy in the era of Herschel , and the crucial role that observatories on the Antarctic Plateau can play. We explore the important scientific questions to which observations from this unique environment may be most productively applied. We examine the importance and complementarity of Antarctic THz astronomy in the light of contemporary facilities such as ALMA, CCAT, SOFIA and (U)LDB ballooning. Finally, building from the roots of THz facilities in Antarctica to present efforts, we broadly highlight future facilities that will exploit the unique advantages of the Polar Plateau and provide a meaningful, lasting astrophysical legacy.
Publisher: EDP Sciences
Date: 03-2003
Publisher: Cambridge University Press (CUP)
Date: 03-2007
DOI: 10.1017/S1743921307012665
Abstract: We present the results of spectral energy distribution analysis for 162 of the 405 sources reported in the SIMBA survey of Hill et al . (2005). The fits reveal source specific parameters including: the luminosity, mass, temperature, H 2 number density, the surface density and the luminosity-to-mass ratio. Each of these parameters are examined with respect to the four classes of source present in the s le. Obvious luminosity and temperature distinctions exist between the mm-only cores and those cores with methanol maser and/or radio continuum emission, with the former cooler and less luminous than the latter. The evidence suggests that the mm-only cores are a precursor to the methanol maser in the formation of massive stars. The mm-only cores comprise two distinct populations distinguished by temperature. Analysis and conclusions about the nature of the cool-mm and warm-mm cores comprising the mm-only population are drawn.
Publisher: Cambridge University Press (CUP)
Date: 05-2005
Publisher: Oxford University Press (OUP)
Date: 13-04-2006
Publisher: Oxford University Press (OUP)
Date: 07-12-2018
Publisher: Cambridge University Press (CUP)
Date: 08-2006
DOI: 10.1017/S1743921307001925
Abstract: Any successful model of star formation must be able to explain the low star forming efficiency of molecular clouds in our Galaxy. If the collapse of gas is regulated only by gravity, then the star formation rate should be orders of magnitude larger than the 1 M per year within our galaxy. The standard model invokes magnetic fields to slow down the rate of collapse, but does not explain star formation in cluster mode, or the lack of observed variations in the chemistry of molecular clouds if they are long-lived entities.
Publisher: Oxford University Press (OUP)
Date: 03-12-2018
Publisher: Oxford University Press (OUP)
Date: 19-03-2012
Publisher: EDP Sciences
Date: 2005
Publisher: Oxford University Press (OUP)
Date: 21-03-2009
Publisher: Oxford University Press (OUP)
Date: 11-2017
Publisher: Springer-Verlag
Date: 2005
DOI: 10.1007/10828557_19
Publisher: Oxford University Press (OUP)
Date: 21-10-2005
Publisher: Oxford University Press (OUP)
Date: 14-08-2017
Publisher: EDP Sciences
Date: 2005
DOI: 10.1051/EAS:2005003
Publisher: Oxford University Press (OUP)
Date: 03-2010
Publisher: Oxford University Press (OUP)
Date: 04-09-2015
Publisher: Oxford University Press (OUP)
Date: 06-07-2018
Publisher: Cambridge University Press (CUP)
Date: 2001
DOI: 10.1071/AS01026
Abstract: Over the past few years, site-testing at the South Pole has revealed conditions that are uniquely favourable for infrared astronomy. In particular, the exceptionally low sky brightness throughout the near and mid-infrared leads to the possibility of a modest-sized telescope achieving comparable sensitivity to that of existing 8–10 metre class telescopes. An 8 metre Antarctic telescope, if constructed, would yield performance that would be unrivalled until the advent of the NGST. In this paper we review the scientific potential of infrared telescopes in Antarctica, and discuss their complementarity with existing 8–10 metre class telescopes and future proposed space telescopes. In particular, we discuss the role that a 2 metre class infrared telescope plays in future plans for the development of an observatory on the Antarctic plateau.
Publisher: American Astronomical Society
Date: 20-10-2001
DOI: 10.1086/322496
Publisher: SPIE
Date: 12-07-2008
DOI: 10.1117/12.788858
Publisher: Cambridge University Press (CUP)
Date: 2009
DOI: 10.1071/AS08051
Abstract: PILOT (the Pathfinder for an International Large Optical Telescope) is a proposed 2.5-m optical/infrared telescope to be located at Dome C on the Antarctic plateau. The atmospheric conditions at Dome C deliver a high sensitivity, high photometric precision, wide-field, high spatial resolution, and high-cadence imaging capability to the PILOT telescope. These capabilities enable a unique scientific potential for PILOT, which is addressed in this series of papers. The current paper presents a series of projects dealing with the nearby Universe that have been identified as key science drivers for the PILOT facility. Several projects are proposed that examine stellar populations in nearby galaxies and stellar clusters in order to gain insight into the formation and evolution processes of galaxies and stars. A series of projects will investigate the molecular phase of the Galaxy and explore the ecology of star formation, and investigate the formation processes of stellar and planetary systems. Three projects in the field of exoplanet science are proposed: a search for free-floating low-mass planets and dwarfs, a program of follow-up observations of gravitational microlensing events, and a study of infrared light-curves for previously discovered exoplanets. Three projects are also proposed in the field of planetary and space science: optical and near-infrared studies aimed at characterising planetary atmospheres, a study of coronal mass ejections from the Sun, and a monitoring program searching for small-scale Low Earth Orbit satellite debris items.
Publisher: SPIE
Date: 09-08-2016
DOI: 10.1117/12.2233317
Publisher: Oxford University Press (OUP)
Date: 19-10-2016
Publisher: EDP Sciences
Date: 2008
DOI: 10.1051/EAS:0831015
Publisher: Oxford University Press (OUP)
Date: 08-2014
Publisher: Oxford University Press (OUP)
Date: 13-07-2017
Publisher: SPIE
Date: 30-09-2004
DOI: 10.1117/12.552354
Publisher: EDP Sciences
Date: 2005
DOI: 10.1051/EAS:2005051
Publisher: Cambridge University Press (CUP)
Date: 1996
DOI: 10.1017/S132335800002049X
Abstract: Conditions on the high Antarctic Plateau would appear to be extremely favourable for a wide range of astronomical research. Before a decision can be made on constructing an observatory, data are required on site conditions at the most promising locations. To enable these data to be collected, a Lockheed Automated Geophysical Observatory is being purchased. This facility will be fitted with a suite of astronomical site-testing instruments, and deployed to several sites on the Antarctic Plateau. This program will allow a definitive assessment of the site conditions to be made by the end of this century.
Publisher: Cambridge University Press (CUP)
Date: 2018
DOI: 10.1017/PASA.2018.18
Abstract: We present observations of 50 deg 2 of the Mopra carbon monoxide (CO) survey of the Southern Galactic Plane, covering Galactic longitudes l = 300–350° and latitudes | b | ⩽ 0.5°. These data have been taken at 0.6 arcmin spatial resolution and 0.1 km s −1 spectral resolution, providing an unprecedented view of the molecular clouds and gas of the Southern Galactic Plane in the 109–115 GHz J = 1–0 transitions of 12 CO, 13 CO, C 18 O, and C 17 O. We present a series of velocity-integrated maps, spectra, and position-velocity plots that illustrate Galactic arm structures and trace masses on the order of ~10 6 M ⊙ deg −2 , and include a preliminary catalogue of C 18 O clumps located between l = 330–340°. Together with the information about the noise statistics of the survey, these data can be retrieved from the Mopra CO website and the PASA data store.
Publisher: Cambridge University Press (CUP)
Date: 05-2005
Publisher: American Astronomical Society
Date: 29-01-2014
Publisher: Oxford University Press (OUP)
Date: 06-09-2017
Publisher: SPIE
Date: 12-2002
DOI: 10.1117/12.457000
Publisher: Oxford University Press (OUP)
Date: 16-03-1999
Publisher: AIP
Date: 2012
DOI: 10.1063/1.4772245
Publisher: Cambridge University Press (CUP)
Date: 2015
DOI: 10.1017/PASA.2015.20
Abstract: We present observations of the first 10° of longitude in the Mopra CO survey of the southern Galactic plane, covering Galactic longitude l = 320–330° and latitude b = ±0.5°, and l = 327–330°, b = +0.5–1.0°. These data have been taken at 35-arcsec spatial resolution and 0.1 km s −1 spectral resolution, providing an unprecedented view of the molecular clouds and gas of the southern Galactic plane in the 109–115 GHz J = 1–0 transitions of 12 CO, 13 CO, C 18 O, and C 17 O. Together with information about the noise statistics from the Mopra telescope, these data can be retrieved from the Mopra CO website and the CSIRO-ATNF data archive.
Publisher: Oxford University Press (OUP)
Date: 06-05-2011
Publisher: Cambridge University Press (CUP)
Date: 03-2007
DOI: 10.1017/S1743921307012720
Abstract: We report the results of a blind search for 22 GHz water masers in two regions, covering approximately half a square degree, within the G 333.2–0.6 giant molecular cloud. The complete search of the two regions was carried out with the 26 m Mount Pleasant radio telescope and resulted in the detection of nine water masers, five of which are new detections. Australia Telescope Compact Array (ATCA) observations of these detections have allowed us to obtain positions with arcsecond accuracy, allowing meaningful comparison with infrared and molecular data for the region. We find that for the regions surveyed there are more water masers than either 6.7 GHz methanol, or main-line OH masers. The water masers are concentrated towards the central axis of the star formation region, in contrast to the 6.7 GHz methanol masers which tend to be located near the periphery. The colours of the GLIMPSE point sources associated with the water masers are slightly less red than those associated with methanol masers. Statistical investigation of the properties of the 13 CO and 1.2 mm dust clumps with and without associated water masers shows that the water masers are associated with the more massive, denser and brighter 13 CO and 1.2 mm dust clumps. We present statistical models that can predict those 13 CO and 1.2 mm dust clumps likely to have associated water masers.
Publisher: Cambridge University Press (CUP)
Date: 08-2015
DOI: 10.1017/S1743921316007717
Abstract: We present spectral data cubes of the [CI] 809 GHz, 12 CO 115 GHz, 13 CO 110 GHz and HI 1.4 GHz line emission from a ~1° region along the l = 328° (G328) sightline in the Galactic Plane. The [CI] data comes from the High Elevation Antarctic Terahertz telescope at Ridge A on the summit of the Antarctic plateau, where the extremely low levels of precipitable water vapour open atmospheric windows for THz observations. The CO data comes from the Southern Galactic Plane Survey being conducted with the Mopra telescope. Emission arises principally from gas in three spiral arm crossings along the sight line. The distribution of the emission in the CO and [CI] lines is found to be similar, with the [CI] slightly more extended, and both are enveloped in extensive HI. Spectral line ratios are similar across the entire extent of the Galaxy. However, towards the edges of the molecular clouds the [CI]/ 13 CO and 12 CO/ 13 CO line ratios rise by ~ 50%, and the [CI]/H i ratio falls by ~ 10%. We attribute this to sightlines passing predominantly through the surfaces of photodissociation regions (PDRs), where the carbon is found mainly as C or C + rather than CO, while the gas is mostly molecular. This is the signature of dark molecular gas.
Publisher: American Astronomical Society
Date: 23-06-2015
Publisher: American Astronomical Society
Date: 20-06-2019
Publisher: EDP Sciences
Date: 24-12-2009
DOI: 10.1051/EAS/1040004
Publisher: Oxford University Press (OUP)
Date: 11-01-2009
Publisher: Oxford University Press (OUP)
Date: 17-02-2017
DOI: 10.1093/MNRAS/STX369
Publisher: Oxford University Press (OUP)
Date: 17-04-2017
DOI: 10.1093/MNRAS/STX887
Publisher: EDP Sciences
Date: 02-11-2007
Publisher: American Astronomical Society
Date: 21-02-2019
Publisher: Cambridge University Press (CUP)
Date: 2017
DOI: 10.1017/PASA.2017.59
Abstract: HESS J1614–518 and HESS J1616–508 are two tera-electron volt γ-ray sources that are not firmly associated with any known counterparts at other wavelengths. We investigate the distribution of interstellar medium towards the tera-electron volt γ-ray sources using results from a 7-mm-wavelength Mopra study, the Mopra Southern Galactic Plane CO Survey, the Millimetre Astronomer’s Legacy Team-45 GHz survey and [C i ] data from the HEAT telescope. Data in the CO(1–0) transition lines reveal diffuse gas overlapping the two tera-electron volt sources at several velocities along the line of sight, while observations in the CS(1–0) transition line reveal several interesting dense gas features. To account for the diffuse atomic gas, archival H i data was taken from the Southern Galactic Plane Survey. The observations reveal gas components with masses ~10 3 to 10 5 M ⊙ and with densities ~10 2 to 10 3 cm −3 overlapping the two tera-electron volt sources. Several origin scenarios potentially associated with the tera-electron volt γ-ray sources are discussed in light of the distribution of the local interstellar medium. We find no strong convincing evidence linking any counterpart with HESS J1614–518 or HESS J1616–508.
Publisher: WORLD SCIENTIFIC
Date: 26-02-2018
DOI: 10.1142/10986
Publisher: Springer Berlin Heidelberg
Date: 1997
Publisher: Cambridge University Press (CUP)
Date: 03-2007
DOI: 10.1017/S1743921307012677
Abstract: Methanol maser emission has proven to be an excellent signpost of regions undergoing massive star formation (MSF). To investigate their role as an evolutionary tracer, we have recently completed a large observing program with the ATCA to derive the dynamical and physical properties of molecular/ionised gas towards a s le of MSF regions traced by 6.7GHz methanol maser emission. We find that the molecular gas in many of these regions breaks up into multiple sub-clumps which we separate into groups based on their association with/without methanol maser and cm continuum emission. The temperature and dynamic state of the molecular gas is markedly different between the groups. Based on these differences, we attempt to assess the evolutionary state of the cores in the groups and thus investigate the role of class II methanol masers as a tracer of MSF.
Publisher: EDP Sciences
Date: 10-2003
Publisher: EDP Sciences
Date: 2012
Publisher: Oxford University Press (OUP)
Date: 29-07-2014
Publisher: Oxford University Press (OUP)
Date: 09-01-2023
Abstract: We present the first high spatial resolution radio continuum survey of the southern Galactic plane. The CORNISH project has mapped the region defined by 295° & l & 350° |b| & 1° at 5.5 GHz, with a resolution of 2.5 arcsec (FWHM). As with the CORNISH-North survey, this is designed to primarily provide matching radio data to the Spitzer GLIMPSE survey region. The CORNISH-South survey achieved a root mean square noise level of ∼0.11 mJy beam−1, using the 6A configuration of the Australia Telescope Compact Array (ATCA). In this paper, we discuss the observations, data processing and measurements of the source properties. Above a 7σ detection limit, 4701 sources were detected, and their ensemble properties show similar distributions with their northern counterparts. The catalogue is highly reliable and is complete to 90 per cent at a flux density level of 1.1 mJy. We developed a new way of measuring the integrated flux densities and angular sizes of non-Gaussian sources. The catalogue primarily provides positions, flux density measurements, and angular sizes. All sources with IR counterparts at 8 μm have been visually classified, utilizing additional imaging data from optical, near-IR, mid-IR, far-IR, and sub-millimetre galactic plane surveys. This has resulted in the detection of 524 H ii regions of which 255 are ultra-compact H ii regions, 287 planetary nebulae, 79 radio stars, and 6 massive young stellar objects. The rest of the sources are likely to be extragalactic. These data are particularly important in the characterization and population studies of compact ionized sources such as UCHII regions and PNe towards the Galactic mid-plane.
Publisher: Oxford University Press (OUP)
Date: 05-2008
Publisher: Cambridge University Press (CUP)
Date: 1998
DOI: 10.1071/AS98228
Abstract: We describe the specifications, characteristics, calibration, and analysis of data from the University of New South Wales Infrared Fabry–Perot (UNSWIRF) etalon. UNSWIRF is a near-infrared tunable imaging spectrometer, used primarily in conjunction with IRIS on the AAT, but suitable for use as a visitor instrument at other telescopes. The etalon delivers a resolving power in excess of 4000 (corresponding to a velocity resolution ∼75 km s −1 ), and allows imaging of fields up to 100″ in diameter on the AAT at any wavelength between 1·5 and 2·4 μ m for which suitable blocking filters are available.
Publisher: American Association for the Advancement of Science (AAAS)
Date: 20-03-1992
DOI: 10.1126/SCIENCE.255.5051.1538
Abstract: In late December 1990, a new radio source appeared near the center of our galaxy rivaling the intensity of Sgr A(*) (the compact radio source at the galactic center). Following its first detection, the flux density of the galactic center transient (GCT) increased rapidly to a maximum 1 month later, and then declined gradually with a time scale of about 3 months. Surprisingly, the GCT maintained a steep radio spectrum during both its rising and decay phases. The neutral hydrogen (HI) absorption shows similar absorption to that in front of Sgr A(*) this indicates that the GCT lies near the galactic center. Furthermore, both HI and OH observations show an additional deep absorption at +20 kilometers per second with respect to the local standard of rest. Thus, the GCT is either embedded in or located behind a molecular cloud moving with that velocity. The cloud can be seen on infrared images. Its opacity is shown to be inadequate to conceal a supernova near the galactic center. It is argued that the GCT was probably transient radio emission from synchrotron-radiating plasma associated with an x-ray binary system.
Publisher: Oxford University Press (OUP)
Date: 26-07-2013
Publisher: IOP Publishing
Date: 10-1996
DOI: 10.1086/133815
Publisher: American Astronomical Society
Date: 07-11-2019
Publisher: Oxford University Press (OUP)
Date: 11-08-1997
Publisher: Oxford University Press (OUP)
Date: 18-11-2011
Publisher: Oxford University Press (OUP)
Date: 05-2008
Publisher: Cambridge University Press (CUP)
Date: 11-2010
DOI: 10.1017/S1743921310011294
Abstract: Several lines of evidence suggest that planet formation may be well underway within the circumstellar disk of the enigmatic Herbig Be star HD100546, including a cleared inner cavity, spiral structure, and similar dust mineralogy as seen in our own solar system. To learn more about the processes occurring in this disk we have conducted a multi-frequency observing program with the Australia Telescope Compact Array (ATCA).
Publisher: Oxford University Press (OUP)
Date: 25-11-2011
Publisher: Cambridge University Press (CUP)
Date: 2005
DOI: 10.1071/AS04037
Abstract: We examine the historical development of astrophysical science in Antarctica from the early 20th century until today. We find three temporally overlapping eras, each having a rather distinct beginning. These are the astrogeological era of meteorite discovery, the high energy era of particle detectors, and the photon astronomy era of microwave, submillimetre, and infrared telescopes, sidelined by a few niche experiments at optical wavelengths. The favourable atmospheric and geophysical conditions are briefly examined, followed by an account of the major experiments and a summary of their results.
Publisher: Oxford University Press (OUP)
Date: 10-2007
Publisher: Elsevier BV
Date: 04-2007
Publisher: Oxford University Press (OUP)
Date: 25-11-2010
Publisher: Cambridge University Press (CUP)
Date: 2013
DOI: 10.1017/PASA.2013.22
Abstract: We present the first results from a new carbon monoxide (CO) survey of the southern Galactic plane being conducted with the Mopra radio telescope in Australia. The 12 CO, 13 CO, and C 18 O J = 1–0 lines are being mapped over the $l = 305^{\\circ }\\text{--} 345^{\\circ }, b = \\pm 0.5^{\\circ }$ portion of the fourth quadrant of the Galaxy, at 35 arcsec spatial and 0.1 km s −1 spectral resolution. The survey is being undertaken with two principal science objectives: (i) to determine where and how molecular clouds are forming in the Galaxy and (ii) to probe the connection between molecular clouds and the ‘missing’ gas inferred from gamma-ray observations. We describe the motivation for the survey, the instrumentation and observing techniques being applied, and the data reduction and analysis methodology. In this paper, we present the data from the first degree surveyed, $l = 323^{\\circ } \\text{--} 324^{\\circ }, b = \\pm 0.5^{\\circ }$ . We compare the data to the previous CO survey of this region and present metrics quantifying the performance being achieved the rms sensitivity per 0.1 km s −1 velocity channel is ~1.5 K for ${\\rm ^{12}CO}$ and ~0.7 K for the other lines. We also present some results from the region surveyed, including line fluxes, column densities, molecular masses, ${\\rm ^{12}CO/^{13}CO}$ line ratios, and ${\\rm ^{12}CO}$ optical depths. We also examine how these quantities vary as a function of distance from the Sun when averaged over the 1 square degree survey area. Approximately 2 × 10 6 M ⊙ of molecular gas is found along the G323 sightline, with an average H 2 number density of $n_{\\text{H}_2} \\sim 1$ cm −3 within the Solar circle. The CO data cubes will be made publicly available as they are published.
Publisher: Wiley
Date: 10-2004
Abstract: The high plateau that covers half of the continent of Antarctica contains the best astronomical observing sites on Earth. The infrared sky background is low, the precipitable water vapour is low, the sub‐millimetre sky opacity is low, the winds are low, the atmosphere is exceedingly clear and stable, it never rains, there is no dust, it is geological stable, and the seeing at some sites, notably Dome C, is superb. The turbulence profile in the atmosphere is beneficial for adaptive optics, with fewer actuators and fewer deformable mirrors being required, and with significant correction being possible at visible wavelengths. For projects that require continuous monitoring, e.g., planet detection through micro‐lensing, a single robotic telescope in Antarctica can replace a network of 4–6 telescopes placed around the world at mid‐latitude sites. For many projects requiring large apertures, a given size telescope in Antarctica will outperform a telescope of 2–3 times the aperture at a mid‐latitude site. We review what is known about the site conditions, and outline some of the issues involved with designing robotic telescopes to work in Antarctica. (© 2004 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Publisher: American Astronomical Society
Date: 29-04-2011
Publisher: Author(s)
Date: 2017
DOI: 10.1063/1.4968938
Publisher: Oxford University Press (OUP)
Date: 10-2004
Publisher: Oxford University Press (OUP)
Date: 07-2001
Publisher: Cambridge University Press (CUP)
Date: 2019
DOI: 10.1017/PASA.2019.7
Abstract: We investigate the interstellar medium towards seven TeV gamma-ray sources thought to be pulsar wind nebulae using Mopra molecular line observations at 7 mm [CS(1–0), SiO(1–0, v = 0)], Nanten CO(1–0) data and the Southern Galactic Plane Survey/GASS H i survey. We have discovered several dense molecular clouds co-located to these TeV gamma-ray sources, which allows us to search for cosmic rays coming from progenitor SNRs or, potentially, from pulsar wind nebulae. We notably found SiO(1–0, v = 0) emission towards HESS J1809–193, highlighting possible interaction between the adjacent supernova remnant SNR G011.0–0.0 and the molecular cloud at d ∼ 3.7 kpc. Using morphological features, and comparative studies of our column densities with those obtained from X-ray measurements, we claim a distance d ∼ 8.6 − 9.7kpc for SNR G292.2–00.5, d ∼ 3.5 − 5.6 kpc for PSR J1418–6058 and d ∼ 1.5 kpc for the new SNR candidate found towards HESS J1303–631. From our mass and density estimates of selected molecular clouds, we discuss signatures of hadronic/leptonic components from pulsar wind nebulae and their progenitor SNRs. Interestingly, the molecular gas, which overlaps HESS J1026–582 at d ∼ 5 kpc, may support a hadronic origin. We find however that this scenario requires an undetected cosmic-ray accelerator to be located at d 10 pc from the molecular cloud. For HESS J1809–193, the cosmic rays which have escaped SNR G011.0–0.0 could contribute to the TeV gamma-ray emission. Finally, from the hypothesis that at most 20% the pulsar spin down power could be converted into CRs, we find that among the studied pulsar wind nebulae, only those from PSR J1809–1917 could potentially contribute to the TeV emission.
Publisher: Oxford University Press (OUP)
Date: 15-02-2022
Abstract: HESS J1804−216 is one of the brightest yet most mysterious TeV γ-ray sources discovered to date. Previous arc-minute scale studies of the interstellar medium (ISM) surrounding this TeV γ-ray source revealed HESS J1804−216 is likely powered by a mature supernova remnant (SNR) or pulsar, hence its origin remains uncertain. In this paper, we focus on the diffusive escape of cosmic ray protons from potential SNR accelerators. These cosmic rays interact with the ISM to produce TeV γ-rays. We utilize the isotropic diffusion equation solution for particles escaping from a shell, to model the energy-dependent escape and propagation of protons into the ISM. This work is the first attempt at modelling the spatial morphology of γ-rays towards HESS J1804−216, using arc-minute ISM observations from both Mopra and the Southern Galactic Plane Survey. The spectral and spatial distributions of γ-rays for the two nearby potential SNR counterparts, SNR G8.7−0.1 and the progenitor SNR of PSR J1803−2137, are presented here. We vary the diffusion parameters and particle spectrum and use a grid search approach to find the best combination of model parameters. We conclude that moderately slow diffusion is required for both candidates. The most promising candidate to be powering the TeV γ-rays from HESS J1804−216 in a hadronic scenario is the progenitor SNR of PSR J1803−2137.
Publisher: Oxford University Press (OUP)
Date: 02-11-2011
Publisher: EDP Sciences
Date: 16-06-2008
Publisher: Cambridge University Press (CUP)
Date: 10-2005
Publisher: SPIE
Date: 14-06-2006
DOI: 10.1117/12.672159
Publisher: EDP Sciences
Date: 09-07-2009
Publisher: Oxford University Press (OUP)
Date: 21-04-2006
Publisher: Oxford University Press (OUP)
Date: 11-12-2008
Publisher: American Astronomical Society
Date: 09-05-2017
Publisher: Oxford University Press (OUP)
Date: 13-08-2015
Publisher: Cambridge University Press (CUP)
Date: 11-2009
DOI: 10.1017/S1743921310011786
Abstract: The methanol multi-beam (MMB) survey has produced the largest and most complete catalogue of Galactic 6.7-GHz methanol masers to date. 6.7-GHz methanol masers are exclusively associated with high-mass star formation, and as such provide invaluable insight into the Galactic distribution and properties of high-mass star formation regions. I present the statistical properties of the MMB catalogue and, through the calculation of kinematic distances, investigate the resolution of distance ambiguities and explore the Galactic distribution.
Publisher: Cambridge University Press (CUP)
Date: 2002
DOI: 10.1071/AS02020
Abstract: The near infrared sky spectral brightness has been measured at the South Pole with the Near Infrared Sky Monitor (NISM) throughout the 2001 winter season. The sky is found to be typically more than an order of magnitude darker than at temperate latitude sites, consistent with previous South Pole observations. Reliable robotic operation of the NISM, a low power, autonomous instrument, has been demonstrated throughout the Antarctic winter. Data analysis yields a median winter value of the 2.4μm (K dark ) sky spectral brightness of ˜120μJy arcsec −2 and an average of 210 ± 80μJy arcsec −2 . The 75%, 50%, and 25% quartile values are 270 ± 100, 155 ± 60, and 80 ± 30μJy arcsec −2 , respectively.
Publisher: Oxford University Press (OUP)
Date: 18-06-2018
Publisher: Oxford University Press (OUP)
Date: 17-03-2015
DOI: 10.1093/MNRAS/STV173
Publisher: American Astronomical Society
Date: 10-08-2009
Publisher: EDP Sciences
Date: 2008
DOI: 10.1051/EAS:0831003
Publisher: EDP Sciences
Date: 2008
DOI: 10.1051/EAS:0833026
Publisher: Cambridge University Press (CUP)
Date: 2013
DOI: 10.1017/PASA.2013.35
Abstract: We present results from a Mopra 7 mm-wavelength survey that targeted the dense gas-tracing CS(1-0) transition towards the young γ-ray-bright supernova remnant, RX J1713.7–3946 (SNR G 347.3−0.5). In a hadronic γ-ray emission scenario, where cosmic ray (CR) protons interact with gas to produce the observed γ-ray emission, the mass of potential CR target material is an important factor. We summarise newly discovered dense gas components, towards Cores G and L, and Clumps N1, N2, N3, and T1, which have masses of 1 – 10 4 M ⊙ . We argue that these components are not likely to contribute significantly to γ-ray emission in a hadronic γ-ray emission scenario. This would be the case if RX J1713.7–3946 were at either the currently favoured distance of ~1 kpc or an alternate distance (as suggested in some previous studies) of ~6 kpc. This survey also targeted the shock-tracing SiO molecule. Although no SiO emission corresponding to the RX J1713.7–3946 shock was observed, vibrationally excited SiO(1-0) maser emission was discovered towards what may be an evolved star. Observations taken 1 yr apart confirmed a transient nature, since the intensity, line-width, and central velocity of SiO(J = 1-0,v = 1,2) emission varied significantly.
Publisher: Cambridge University Press (CUP)
Date: 08-1994
DOI: 10.1017/S1323358000019809
Abstract: Our knowledge of the universe comes from recording the photon and particle fluxes incident on the Earth from space. We thus require sensitive measurement across the entire energy spectrum, using large telescopes with efficient instrumentation located on superb sites. Technological advances and engineering constraints are nearing the point where we are recording as many photons arriving at a site as is possible. Major advances in the future will come from improving the quality of the site. The ultimate site is, of course, beyond the Earth’s atmosphere, such as on the Moon, but economic limitations prevent our exploiting this avenue to the degree that the scientific community desires. Here we describe an alternative, which offers many of the advantages of space for a fraction of the cost: the Antarctic Plateau.
Publisher: EDP Sciences
Date: 2007
DOI: 10.1051/EAS:2007104
Publisher: Oxford University Press (OUP)
Date: 07-06-2006
Publisher: SPIE
Date: 17-09-2012
DOI: 10.1117/12.925514
Publisher: Oxford University Press (OUP)
Date: 31-12-2015
Publisher: Oxford University Press (OUP)
Date: 22-05-2013
DOI: 10.1093/MNRAS/STT717
Publisher: Oxford University Press (OUP)
Date: 03-2002
Publisher: Oxford University Press (OUP)
Date: 27-02-2015
DOI: 10.1093/MNRAS/STV178
Publisher: Oxford University Press (OUP)
Date: 07-09-2007
Publisher: IOP Publishing
Date: 08-1996
DOI: 10.1086/133792
Location: United Kingdom of Great Britain and Northern Ireland
Start Date: 2004
End Date: 12-2009
Amount: $550,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 07-2003
End Date: 12-2007
Amount: $37,300.00
Funder: Australian Research Council
View Funded ActivityStart Date: 2007
End Date: 12-2009
Amount: $47,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 01-2003
End Date: 03-2004
Amount: $222,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 02-2002
End Date: 12-2006
Amount: $587,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 2006
End Date: 12-2007
Amount: $10,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 06-2015
End Date: 12-2017
Amount: $760,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 2016
End Date: 12-2016
Amount: $150,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 11-2021
End Date: 10-2025
Amount: $1,680,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 2015
End Date: 12-2015
Amount: $270,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 05-2013
End Date: 09-2017
Amount: $330,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 07-2003
End Date: 12-2006
Amount: $193,035.00
Funder: Australian Research Council
View Funded ActivityStart Date: 12-2011
End Date: 12-2012
Amount: $150,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 2008
End Date: 12-2010
Amount: $50,400.00
Funder: Australian Research Council
View Funded ActivityStart Date: 07-2007
End Date: 03-2011
Amount: $100,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 03-2008
End Date: 12-2011
Amount: $201,224.00
Funder: Australian Research Council
View Funded ActivityStart Date: 03-2008
End Date: 02-2013
Amount: $281,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 06-2012
End Date: 06-2016
Amount: $315,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 03-2010
End Date: 02-2011
Amount: $200,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 07-2017
End Date: 07-2023
Amount: $1,390,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 04-2012
End Date: 07-2018
Amount: $750,000.00
Funder: Australian Research Council
View Funded Activity