ORCID Profile
0000-0002-0742-379X
Current Organisation
Macquarie University
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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.
Astronomical and Space Sciences | Astronomical and Space Instrumentation | Cosmology and Extragalactic Astronomy | Photonics, Optoelectronics and Optical Communications | Galactic Astronomy | Stellar Astronomy and Planetary Systems |
Expanding Knowledge in the Physical Sciences | Scientific Instruments | Physical sciences | Scientific instrumentation | Expanding Knowledge in Technology
Publisher: American Astronomical Society
Date: 30-06-2010
Publisher: SPIE
Date: 29-08-2022
DOI: 10.1117/12.2639961
Publisher: Oxford University Press (OUP)
Date: 02-2012
Publisher: The Optical Society
Date: 27-06-2017
DOI: 10.1364/OE.25.015868
Publisher: SPIE
Date: 03-01-2020
DOI: 10.1117/12.2539594
Publisher: Optica Publishing Group
Date: 27-04-2021
DOI: 10.1364/AO.421383
Abstract: Near-infrared wavelength observations are crucial for understanding numerous fields of astrophysics, such as supernova cosmology and positronium annihilation detection. However, current ground-based observations suffer from an enormous background due to OH emission in the upper atmosphere. One promising way to solve this problem is to use ring-resonator filters to suppress OH emission lines. In this work, we discuss our optimization of ring-resonator filter performance from five perspectives: resonance wavelength matching, polarization-independent operation, low insertion loss, low-loss coupling to astronomical instruments, and broadband operation. In the end, we discuss next steps needed for reliable supernova and positronium observations, thus providing a roadmap for future advances in near-infrared astronomy.
Publisher: SPIE
Date: 29-08-2022
DOI: 10.1117/12.2630348
Publisher: SPIE
Date: 13-12-2020
DOI: 10.1117/12.2561967
Publisher: SPIE
Date: 13-09-2012
DOI: 10.1117/12.924874
Publisher: MyJove Corporation
Date: 20-04-2016
DOI: 10.3791/53326
Publisher: Oxford University Press (OUP)
Date: 09-11-2018
Publisher: SPIE
Date: 13-09-2012
DOI: 10.1117/12.925923
Publisher: OSA
Date: 2010
Publisher: SPIE
Date: 13-09-2012
DOI: 10.1117/12.925804
Publisher: SPIE
Date: 29-08-2022
DOI: 10.1117/12.2630275
Publisher: Optica Publishing Group
Date: 20-04-2021
DOI: 10.1364/AO.423439
Abstract: Integrated photonic spectrographs offer an avenue to extreme miniaturization of astronomical instruments, which would greatly benefit extremely large telescopes and future space missions. These devices first require optimization for astronomical applications, which includes design, fabrication, and field testing. Given the high costs of photonic fabrication, multi-project wafer (MPW) silicon nitride (SiN) offerings, where a user purchases a portion of a wafer, provide a convenient and affordable avenue to develop this technology. In this work, we study the potential of two commonly used SiN waveguide geometries by MPW foundries, i.e., square and rectangular profiles, to determine how they affect the performance of mid/high-resolution arrayed waveguide grating (AWG) spectrometers around 1.5 µm. Specifically, we present results from detailed simulations on the mode sizes, shapes, and polarization properties, and on the impact of phase errors on the throughput and cross talk as well as some laboratory results of coupling and propagation losses. From the MPW run tolerances and our phase-error study, we estimate that an AWG with R ∼ 10,000 can be developed with the MPW runs, and even greater resolving power is achievable with more reliable, dedicated fabrication runs. Depending on the fabrication and design optimizations, it is possible to achieve throughputs ∼ 60 % using the SiN platform. Thus, we show that SiN MPW offerings are highly promising and will play a key role in integrated photonic spectrograph developments for astronomy.
Publisher: SPIE
Date: 22-07-2016
DOI: 10.1117/12.2231924
Publisher: SPIE
Date: 28-07-2014
DOI: 10.1117/12.2057108
Publisher: Cambridge University Press (CUP)
Date: 2006
DOI: 10.1071/AS05037
Abstract: We present H -band observations of the elliptical galaxy NGC 4696, the brightest member of the Centaurus cluster of galaxies. We have measured its light profile, using a two-dimensional fitting algorithm, out to a radius of 180 arcsec (37 h 70 −1 kpc). The profile is well described by a de Vaucouleurs law, with an effective radius of 35.3 ± 1.0 h 70 −1 kpc. There is no need for the extra free parameter allowed by a Sérsic law. Allowing for a variation of 0.3% in the sky level, the profile obtained is compatible with data from the Two-Micron All Sky Survey (2MASS). The profile shows no sign of either a truncation or an extended halo.
Publisher: American Astronomical Society
Date: 16-01-2013
Publisher: SPIE
Date: 12-07-2008
DOI: 10.1117/12.788527
Publisher: American Astronomical Society
Date: 20-03-2006
DOI: 10.1086/499939
Publisher: IEEE
Date: 05-2011
Publisher: Springer Science and Business Media LLC
Date: 2018
Publisher: Optica Publishing Group
Date: 17-06-2021
DOI: 10.1364/JOSAB.423905
Abstract: Photonic devices (e.g., optical fibers, 2D waveguides) are commonly used on telescopes worldwide and have been hugely successful in terms of their scientific impact. Coupling light efficiently into photonic devices is critical because most astronomical sources generate low photon count rates at the detector, even when coupled to large telescope apertures. Recent developments in adaptive optics have helped to improve the coupling to optical fibers, although efficient coupling to single-mode fibers remains a challenge. We appraise the theoretical limits to this coupling efficiency in both diffraction limited and seeing limited conditions, and we review methods to improve coupling efficiency with a view to recent advances in astrophotonics.
Publisher: Oxford University Press (OUP)
Date: 17-08-2012
Publisher: SPIE
Date: 13-12-2020
DOI: 10.1117/12.2561930
Publisher: SPIE
Date: 30-09-2004
DOI: 10.1117/12.550980
Publisher: Optica Publishing Group
Date: 10-2009
DOI: 10.1364/OE.17.018643
Publisher: Oxford University Press (OUP)
Date: 05-2006
Publisher: Oxford University Press (OUP)
Date: 13-01-2015
Publisher: Oxford University Press (OUP)
Date: 11-05-2006
Publisher: SPIE
Date: 07-05-2015
DOI: 10.1117/12.2178427
Publisher: American Astronomical Society
Date: 23-11-2009
Publisher: SPIE
Date: 06-01-2020
DOI: 10.1117/12.2539883
Publisher: IEEE
Date: 08-2011
Publisher: Springer Science and Business Media LLC
Date: 06-12-2011
DOI: 10.1038/NCOMMS1584
Abstract: A long-standing and profound problem in astronomy is the difficulty in obtaining deep near-infrared observations due to the extreme brightness and variability of the night sky at these wavelengths. A solution to this problem is crucial if we are to obtain the deepest possible observations of the early Universe, as redshifted starlight from distant galaxies appears at these wavelengths. The atmospheric emission between 1,000 and 1,800 nm arises almost entirely from a forest of extremely bright, very narrow hydroxyl emission lines that varies on timescales of minutes. The astronomical community has long envisaged the prospect of selectively removing these lines, while retaining high throughput between them. Here we demonstrate such a filter for the first time, presenting results from the first on-sky tests. Its use on current 8 m telescopes and future 30 m telescopes will open up many new research avenues in the years to come.
Publisher: SPIE
Date: 24-09-2012
DOI: 10.1117/12.925812
Publisher: SPIE
Date: 28-07-2014
DOI: 10.1117/12.2055597
Publisher: Oxford University Press (OUP)
Date: 10-10-2005
Publisher: Oxford University Press (OUP)
Date: 03-2002
Publisher: SPIE
Date: 06-07-2018
DOI: 10.1117/12.2311898
Publisher: WORLD SCIENTIFIC (EUROPE)
Date: 20-06-2022
DOI: 10.1142/Q0391
Publisher: Springer Netherlands
Date: 2009
Publisher: Springer Netherlands
Date: 2009
Publisher: SPIE
Date: 02-01-2018
DOI: 10.1117/12.2283353
Publisher: Wiley
Date: 03-2010
Publisher: Wiley
Date: 29-10-2012
Publisher: SPIE
Date: 16-07-2010
DOI: 10.1117/12.857007
Publisher: SPIE
Date: 03-01-2020
DOI: 10.1117/12.2539772
Publisher: IEEE
Date: 08-2011
Publisher: American Astronomical Society
Date: 11-2005
DOI: 10.1086/491790
Publisher: Optica Publishing Group
Date: 23-06-2021
DOI: 10.1364/AO.421560
Abstract: Celestially, positronium (Ps) has been observed only through gamma-ray emission produced by its annihilation. However, in its triplet state, a Ps atom has a mean lifetime long enough for electronic transitions to occur between quantum states. This produces a recombination spectrum observable in principle at near IR wavelengths, where angular resolution greatly exceeding that of the gamma-ray observations is possible. However, the background in the near IR is dominated by extremely bright atmospheric hydroxyl (OH) emission lines. In this paper, we present the design of a diffraction-limited spectroscopic system using novel photonic components—a photonic lantern, OH fiber Bragg grating filters, and a photonic TIGER 2D pseudo-slit—to observe the Ps Balmer alpha line at 1.3122 µm for the first time, to our knowledge.
Publisher: SPIE
Date: 10-07-2018
DOI: 10.1117/12.2312360
Publisher: Sissa Medialab
Date: 09-05-2012
DOI: 10.22323/1.147.0064
Publisher: SPIE
Date: 12-07-2008
DOI: 10.1117/12.788629
Publisher: SPIE
Date: 08-07-2014
DOI: 10.1117/12.2055588
Publisher: Oxford University Press (OUP)
Date: 10-2009
Publisher: American Astronomical Society
Date: 05-12-2012
Publisher: SPIE
Date: 14-03-2019
DOI: 10.1117/12.2511917
Publisher: SPIE
Date: 13-12-2020
DOI: 10.1117/12.2561990
Publisher: SPIE
Date: 12-07-2008
DOI: 10.1117/12.788549
Publisher: The Optical Society
Date: 12-12-2014
DOI: 10.1364/OE.22.031575
Publisher: Oxford University Press (OUP)
Date: 02-2004
Publisher: SPIE
Date: 09-08-2016
DOI: 10.1117/12.2232115
Publisher: SPIE
Date: 12-07-2008
DOI: 10.1117/12.788650
Publisher: SPIE
Date: 17-05-2017
DOI: 10.1117/12.2265958
Publisher: Oxford University Press (OUP)
Date: 05-2008
Publisher: SPIE
Date: 24-09-2012
DOI: 10.1117/12.926483
Publisher: SPIE
Date: 16-07-2010
DOI: 10.1117/12.856348
Publisher: Oxford University Press (OUP)
Date: 07-02-2013
DOI: 10.1093/MNRAS/STT030
Publisher: Oxford University Press (OUP)
Date: 11-05-2007
Publisher: EDP Sciences
Date: 20-07-2012
Publisher: SPIE
Date: 10-07-2018
DOI: 10.1117/12.2312895
Publisher: American Physical Society (APS)
Date: 03-06-2015
Publisher: Oxford University Press (OUP)
Date: 02-03-2011
Publisher: SPIE
Date: 28-07-2014
DOI: 10.1117/12.2054570
Publisher: American Astronomical Society
Date: 15-07-2022
Abstract: The sky observed by space telescopes in Low Earth Orbit (LEO) can be dominated by stray light from multiple sources including Earth, Sun, and Moon. This stray light presents a significant challenge to missions that aim to make a secure measurement of the extragalactic background light (EBL). In this work, we quantify the impact of stray light on sky observations made by the Hubble Space Telescope (HST) Advanced Camera for Surveys. By selecting on orbital parameters, we successfully isolate images with sky that contain minimal and high levels of earthshine. In addition, we find weather observations from CERES satellites correlate with the observed HST sky surface brightness indicating the value of incorporating such data to characterize the sky. Finally, we present a machine-learning model of the sky trained on the data used in this work to predict the total observed sky surface brightness. We demonstrate that our initial model is able to predict the total sky brightness under a range of conditions to within 3.9% of the true measured sky. Moreover, we find that the model matches the stray-light-free observations better than current physical zodiacal light models.
Publisher: Oxford University Press (OUP)
Date: 04-2006
Publisher: OSA
Date: 2011
Publisher: Oxford University Press (OUP)
Date: 08-01-2020
Abstract: Ground-based near-infrared (NIR) astronomy is severely h ered by the forest of atmospheric emission lines resulting from the rovibrational decay of OH molecules in the upper atmosphere. The extreme brightness of these lines, as well as their spatial and temporal variability, makes accurate sky subtraction difficult. Selectively filtering these lines with OH suppression instruments has been a long standing goal for NIR spectroscopy. We have shown previously the efficacy of fibre Bragg gratings (FBGs) combined with photonic lanterns for achieving OH suppression. Here we report on PRAXIS, a unique NIR spectrograph that is optimized for OH suppression with FBGs. We show for the first time that OH suppression (of any kind) is possible with high overall throughput (18 per cent end-to-end), and provide ex les of the relative benefits of OH suppression.
Publisher: The Optical Society
Date: 27-01-2011
DOI: 10.1364/OE.19.002649
Publisher: SPIE
Date: 16-07-2010
DOI: 10.1117/12.856345
Publisher: SPIE
Date: 09-08-2016
DOI: 10.1117/12.2232107
Publisher: Optica Publishing Group
Date: 07-2021
DOI: 10.1364/JOSAB.434565
Abstract: Astrophotonics is an emerging field that focuses on the development of photonic components for astronomical instrumentation. With ongoing advancements, astrophotonic solutions are already becoming an integral part of existing instruments. A recent ex le is the €60M ESO GRAVITY instrument at the Very Large Telescope Interferometer, Chile, that makes heavy use of photonic components. We envisage far-reaching applications in future astronomical instruments, especially those intended for the new generation of extremely large telescopes and in space. With continued improvements in extreme adaptive optics, the case becomes increasingly compelling. The joint issue of JOSA B and Applied Optics features more than 20 state-of-the-art papers in erse areas of astrophotonics. This introduction provides a summary of the papers that cover several important topics, such as photonic lanterns, beam combiners and interferometry, spectrographs, OH suppression, and coronagraphy.
Publisher: EDP Sciences
Date: 22-06-2009
Publisher: Oxford University Press (OUP)
Date: 16-05-2013
DOI: 10.1093/MNRAS/STT677
Publisher: IOP Publishing
Date: 10-2023
Abstract: Photonic technologies offer numerous functionalities that can be used to realize astrophotonic instruments. The most spectacular ex le to date is the ESO Gravity instrument at the Very Large Telescope in Chile that combines the light-gathering power of four 8-m telescopes through a complex photonic interferometer. Fully integrated astrophotonic devices offer critical advantages for instrument development, including extreme miniaturization when operating at the diffraction-limit, plus integration, superior thermal and mechanical stabilization owing to the small footprint, and high replicability offering significant cost savings. Numerous astrophotonic technologies have been developed to address shortcomings of conventional instruments to date, including the development of photonic lanterns to convert from multimode inputs to single mode outputs, complex aperiodic fiber Bragg gratings to filter OH emission from the atmosphere, beam combiners enabling long baseline interferometry with for ex le, ESO Gravity, and laser frequency combs for high precision spectral calibration of spectrometers. Despite these successes, the facility implementation of photonic solutions in astronomical instrumentation is currently limited because of 1) low throughputs from coupling to fibers, coupling fibers to chips, propagation and bend losses, device losses, etc., 2) difficulties with scaling to large channel count devices needed for large bandwidths and high resolutions, and 3) efficient integration of photonics with detectors. In this roadmap, we identify 23 key areas that need further development. We outline the challenges and advances needed across those areas covering design tools, simulation capabilities, fabrication processes, the need for entirely new components, integration and hybridization and the characterization of devices. To realize these advances the astrophotonics community will have to work cooperatively with industrial partners who have more advanced manufacturing capabilities. With the advances described herein, multi-functional integrated instruments will be realized leading to novel observing capabilities for both ground and space based platforms, enabling new scientific studies and discoveries.
Publisher: Oxford University Press (OUP)
Date: 22-01-2019
DOI: 10.1093/MNRAS/STZ217
Start Date: 11-2022
End Date: 12-2023
Amount: $1,749,940.00
Funder: Australian Research Council
View Funded ActivityStart Date: 01-2021
End Date: 01-2022
Amount: $632,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 11-2010
End Date: 11-2010
Amount: $500,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 02-2013
End Date: 01-2014
Amount: $300,000.00
Funder: Australian Research Council
View Funded Activity