ORCID Profile
0000-0001-5185-9876
Current Organisations
Gdański Uniwersytet Medyczny
,
Australian Astronomical Observatory
,
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 | Cosmology and Extragalactic Astronomy | Astronomical and Space Instrumentation | Photonics, Optoelectronics and Optical Communications | Galactic Astronomy |
Expanding Knowledge in the Physical Sciences | Expanding Knowledge in Technology | Expanding Knowledge in Engineering | Food Safety
Publisher: American Astronomical Society
Date: 09-01-2017
Publisher: American Astronomical Society
Date: 08-02-2018
Publisher: Springer Science and Business Media LLC
Date: 04-2017
DOI: 10.1038/NATURE21680
Abstract: Finding massive galaxies that stopped forming stars in the early Universe presents an observational challenge because their rest-frame ultraviolet emission is negligible and they can only be reliably identified by extremely deep near-infrared surveys. These surveys have revealed the presence of massive, quiescent early-type galaxies appearing as early as redshift z ≈ 2, an epoch three billion years after the Big Bang. Their age and formation processes have now been explained by an improved generation of galaxy-formation models, in which they form rapidly at z ≈ 3-4, consistent with the typical masses and ages derived from their observations. Deeper surveys have reported evidence for populations of massive, quiescent galaxies at even higher redshifts and earlier times, using coarsely s led photometry. However, these early, massive, quiescent galaxies are not predicted by the latest generation of theoretical models. Here we report the spectroscopic confirmation of one such galaxy at redshift z = 3.717, with a stellar mass of 1.7 × 10
Publisher: Oxford University Press (OUP)
Date: 08-02-2023
Abstract: The distribution of galaxies and clusters of galaxies on the mega-parsec scale of the Universe follows an intricate pattern now famously known as the Large-Scale Structure or the Cosmic Web. To study the environments of this network, several techniques have been developed that are able to describe its properties and the properties of groups of galaxies as a function of their environment. In this work, we analyse the previously introduced framework: 1-Dimensional Recovery, Extraction, and Analysis of Manifolds (1-dream) on N-body cosmological simulation data of the Cosmic Web. The 1-DREAM toolbox consists of five Machine Learning methods, whose aim is the extraction and modelling of one-dimensional structures in astronomical big data settings. We show that 1-DREAM can be used to extract structures of different density ranges within the Cosmic Web and to create probabilistic models of them. For demonstration, we construct a probabilistic model of an extracted filament and move through the structure to measure properties such as local density and velocity. We also compare our toolbox with a collection of methodologies which trace the Cosmic Web. We show that 1-DREAM is able to split the network into its various environments with results comparable to the state-of-the-art methodologies. A detailed comparison is then made with the public code disperse, in which we find that 1-DREAM is robust against changes in s le size making it suitable for analysing sparse observational data, and finding faint and diffuse manifolds in low-density regions.
Publisher: American Astronomical Society
Date: 07-03-2011
Publisher: American Astronomical Society
Date: 31-08-2022
Abstract: The discovery in deep near-infrared surveys of a population of massive quiescent galaxies at z 3 has given rise to the question of how they came to be quenched so early in the history of the universe. Measuring their molecular gas properties can distinguish between physical processes where they stop forming stars due to a lack of fuel versus those where the star formation efficiency is reduced and the gas is retained. We conducted Atacama Large Millimeter/submillimeter Array observations of four quiescent galaxies at z = 3.5–4.0 found by the Fourstar Galaxy Evolution Survey and a serendipitous optically dark galaxy at z = 3.71. We aim to investigate the presence of dust-obscured star formation and their gas content by observing the dust continuum emission at Band 7 and the atomic carbon [C i ]( 3 P 1 – 3 P 0 ) line at 492.16 GHz. Among the four quiescent galaxies, only one source is detected in the dust continuum at λ obs = 870 μ m. The submillimeter observations confirm their passive nature, and all of them are located more than four times below the main sequence of star-forming galaxies at z = 3.7. None of the targets are detected in [C i ], constraining their gas-mass fractions to be %. These gas-mass fractions are more than 3 times lower than the scaling relation for star-forming galaxies at z = 3.7. These results support scenarios where massive galaxies at z = 3.5–4.0 quench by consuming/expelling all the gas rather than by reducing the efficiency of the conversion of their gas into stars.
Publisher: Oxford University Press (OUP)
Date: 21-03-2010
Publisher: American Astronomical Society
Date: 05-01-2017
Publisher: American Astronomical Society
Date: 11-03-2010
Publisher: American Astronomical Society
Date: 24-03-2017
Publisher: Oxford University Press (OUP)
Date: 14-03-2017
DOI: 10.1093/MNRAS/STX605
Publisher: American Astronomical Society
Date: 28-10-2020
Publisher: American Astronomical Society
Date: 17-08-2018
Publisher: American Astronomical Society
Date: 04-10-2010
Publisher: American Astronomical Society
Date: 30-09-2019
Publisher: EDP Sciences
Date: 07-2014
Publisher: American Astronomical Society
Date: 05-03-2019
Publisher: American Astronomical Society
Date: 03-10-2017
Publisher: Oxford University Press (OUP)
Date: 09-10-2018
Publisher: Oxford University Press (OUP)
Date: 06-07-2008
Publisher: Oxford University Press (OUP)
Date: 16-06-2011
Publisher: Oxford University Press (OUP)
Date: 04-09-2008
Publisher: American Astronomical Society
Date: 10-10-2016
Publisher: Cambridge University Press (CUP)
Date: 07-2007
DOI: 10.1017/S1743921308017912
Abstract: Globular Clusters provide a unique method for tracing the formation and evolution of their host galaxies. As single stellar populations they are far easier to interpret than the multi-population complexity of galaxy field stars. The scaling properties of globular clusters provide important constraints on the hierarchical assembly history of galaxies. Here we briefly review recent progress using the Hubble Space Telescope for imaging and the Keck plus Gemini telescopes for spectroscopy. We argue that the red, or metal-rich, subpopulation of GCs is associated with the bulge/spheroid component of galaxies. As one of the oldest stellar systems available for study, we discuss how globular clusters can be used to constrain the formation of galaxy bulges, in particular the role of mergers vs secular evolution. We conclude that metal-rich GCs, and hence bulges, formed very early in the Universe with more recent mergers having a small effect at most.
Publisher: Oxford University Press (OUP)
Date: 09-10-2012
Publisher: American Astronomical Society
Date: 03-05-2018
Publisher: Oxford University Press (OUP)
Date: 30-03-2023
Abstract: Using very deep, high spectral resolution data from the SAMI Integral Field Spectrograph, we study the stellar population properties of a s le of dwarf galaxies in the Fornax Cluster, down to a stellar mass of 107 M⊙, which has never been done outside the Local Group. We use full spectral fitting to obtain stellar population parameters. Adding massive galaxies from the ATLAS3D project, which we re-analysed, and the satellite galaxies of the Milky Way, we obtained a galaxy s le that covers the stellar mass range 104–1012 M⊙. Using this large range, we find that the mass–metallicity relation is not linear. We also find that the [α/Fe]-stellar mass relation of the full s le shows a U-shape, with a minimum in [α/Fe] for masses between 109 and 1010 M⊙. The relation between [α/Fe] and stellar mass can be understood in the following way: when the faintest galaxies enter the cluster environment, a rapid burst of star formation is induced, after which the gas content is blown away by various quenching mechanisms. This fast star formation causes high [α/Fe] values, like in the Galactic halo. More massive galaxies will manage to keep their gas longer and form several bursts of star formation, with lower [α/Fe] as a result. For massive galaxies, stellar populations are regulated by internal processes, leading to [α/Fe] increasing with mass. We confirm this model by showing that [α/Fe] correlates with clustercentric distance in three nearby clusters and also in the halo of the Milky Way.
Publisher: Oxford University Press (OUP)
Date: 04-2014
DOI: 10.1093/PASJ/PSU022
Publisher: American Astronomical Society
Date: 12-03-2012
Publisher: Oxford University Press (OUP)
Date: 29-04-2015
DOI: 10.1093/MNRAS/STV677
Publisher: American Astronomical Society
Date: 12-2022
Abstract: Large and less-biased s les of star-forming galaxies are essential to investigate galaxy evolution. H α emission line is one of the most reliable tracers of star-forming galaxies because its strength is directly related to recent star formation. However, it is observationally expensive to construct large s les of H α emitters by spectroscopic or narrowband imaging survey at high redshifts. In this work, we demonstrate a method to extract H α fluxes of galaxies at z = 2.1–2.5 from K s broadband photometry of ZFOURGE catalog. Combined with 25–39 other filters, we estimate the emission-line fluxes by SED fitting with stellar population models that incorporate emission-line strengths. 2005 galaxies are selected as H α emitters by our method and their fluxes show good agreement with previous measurements in the literature. On the other hand, there are more H α luminous galaxies than previously reported. The discrepancy can be explained by extended H α profiles of massive galaxies and a luminosity dependence of dust attenuation, which are not taken into account in the previous work. We also find that there are a large number of low-mass galaxies with a much higher specific star formation rate (sSFR) than expected from the extrapolated star formation main sequence. Such low-mass galaxies exhibit larger ratios between H α and UV fluxes compared to more massive high sSFR galaxies. This result implies that a “starburst” mode may differ among galaxies: low-mass galaxies appear to assemble their stellar mass via short-duration bursts, while more massive galaxies tend to experience longer-duration ( Myr) bursts.
Publisher: American Astronomical Society
Date: 21-07-2016
Publisher: Oxford University Press (OUP)
Date: 25-09-2013
Publisher: American Astronomical Society
Date: 07-07-2011
Publisher: Cambridge University Press (CUP)
Date: 12-2007
Publisher: American Astronomical Society
Date: 02-09-2015
Publisher: American Astronomical Society
Date: 19-01-2016
Publisher: American Astronomical Society
Date: 16-02-2017
Publisher: American Astronomical Society
Date: 04-11-0004
Abstract: The mission of the 2000 kg Cassini spacecraft concluded on 2017 September 15, by its deliberate entry into Saturn’s atmosphere at some 31.1 km s −1 . Observations, using Hubble and groundbased observatories, to attempt optical detection of this 0.25 kT “artificial meteor” are summarized. No signatures were identified. A challenge with observing the event is that due to atmospheric drag, its timing was not completely deterministic months or even days in advance, a particular problem for space observatories. While imaging observations needed no geometric specification more than “Saturn,” observations with spectrometers required pointing the instrument aperture or slit at the specific impact site. Since giant planet longitude systems are not always familiar, distribution of an unambiguous “finder chart” showing the location of the predicted entry site on the disk is essential, as is clarity on whether stated times are spacecraft event time, or Earth received time (light-travel time, 83 minutes, later).
Publisher: American Astronomical Society
Date: 22-09-2010
Publisher: American Astronomical Society
Date: 03-11-2018
Abstract: Deep near-infrared photometric surveys are efficient in identifying high-redshift galaxies, however, they can be prone to systematic errors in photometric redshift. This is particularly salient when there is limited s ling of key spectral features of a galaxy’s spectral energy distribution (SED), such as for quiescent galaxies where the expected age-sensitive Balmer/4000 Å break enters the K -band at z 4. With single-filter s ling of this spectral feature, degeneracies between SED models and redshift emerge. A potential solution to this comes from splitting the K band into multiple filters. We use simulations to show an optimal solution is to add two medium-band filters, K blue ( λ cen = 2.06 μ m, Δ λ = 0.25 μ m) and K red ( λ cen = 2.31 μ m, Δ λ = 0.27 μ m), that are complementary to the existing K s filter. We test the impact of the K -band filters with simulated catalogs comprised of galaxies with varying ages and signal-to-noise. The results suggest that the K -band filters do improve photometric redshift constraints on z 4 quiescent galaxies, increasing precision and reducing outliers by up to 90%. We find that the impact from the K -band filters depends on the signal-to-noise, the redshift, and the SED of the galaxy. The filters we designed were built and used to conduct a pilot of the FLAMINGOS-2 Extragalactic Near-Infrared K -band Split survey. While no new z 4 quiescent galaxies are identified in the limited area pilot, the K blue and K red filters indicate strong Balmer/4000 Å breaks in existing candidates. Additionally, we identify galaxies with strong nebular emission lines, for which the K -band filters increase photometric redshift precision and in some cases indicate extreme star formation.
Publisher: Oxford University Press (OUP)
Date: 25-11-0088
Publisher: Oxford University Press (OUP)
Date: 11-03-2006
Publisher: Oxford University Press (OUP)
Date: 17-09-2022
Abstract: We explore the kinematic scaling relations of 38 dwarf galaxies in the Fornax Cluster using observations from the SAMI integral field spectrograph. We focus on the Fundamental Plane (FP), defined by the physical properties of the objects (scale length, surface brightness, and velocity dispersion) and the Stellar Mass (Fundamental) Plane, where surface brightness is replaced by stellar mass, and investigate their dynamical-to-stellar-mass ratio. We confirm earlier results that the Fornax dEs are significantly offset above the FP defined by massive, hot stellar systems. For the Stellar Mass (Fundamental) Plane, which shows much lower scatter, we find that young and old dwarf galaxies lie at about the same distance from the plane, all with comparable scatter. We introduce the perpendicular deviation of dwarf galaxies from the Stellar Mass Plane defined by giant early-types as a robust estimate of their DM fraction, and find that the faintest dwarfs are systematically offset above the plane, implying that they have a higher dark matter fraction. This result is confirmed when estimating the dynamical mass of our dEs using a virial mass estimator, tracing the onset of dark matter domination in low mass stellar systems. We find that the position of our galaxies on the Stellar Mass FP agrees with the galaxies in the Local Group. This seems to imply that the processes determining the position of dwarf galaxies on the FP depend on the environment in the same way, whether the galaxy is situated in the Local Group or in the Fornax Cluster.
Publisher: American Astronomical Society
Date: 09-09-2010
Publisher: EDP Sciences
Date: 12-2016
Publisher: American Astronomical Society
Date: 29-04-2015
Publisher: American Astronomical Society
Date: 05-2022
Abstract: Extremely metal-poor (EMP) stars provide a valuable probe of early chemical enrichment in the Milky Way. Here we leverage a large s le of ∼600,000 high-resolution stellar spectra from the GALAH survey plus a machine-learning algorithm to find 54 candidates with estimated [Fe/H] ≤−3.0, six of which have [Fe/H] ≤−3.5. Our s le includes ∼20% main-sequence EMP candidates, unusually high for EMP star surveys. We find the magnitude-limited metallicity distribution function of our s le is consistent with previous work that used more complex selection criteria. The method we present has significant potential for application to the next generation of massive stellar spectroscopic surveys, which will expand the available spectroscopic data well into the millions of stars.
Publisher: Oxford University Press (OUP)
Date: 22-08-2011
Publisher: Springer Science and Business Media LLC
Date: 19-12-2016
Publisher: Oxford University Press (OUP)
Date: 21-12-2012
Publisher: American Astronomical Society
Date: 2006
DOI: 10.1086/509124
Publisher: Oxford University Press (OUP)
Date: 25-10-2013
DOI: 10.1093/MNRAS/STS029
Publisher: American Astronomical Society
Date: 03-03-2016
Publisher: American Astronomical Society
Date: 11-05-2018
Publisher: American Astronomical Society
Date: 03-2021
Abstract: In order to shed light on how galactic properties depend on the intergalactic medium (IGM) environment traced by the Ly α forest, we observationally investigate the IGM–galaxy connection using the publicly available 3D IGM tomography data (CLAMATO) and several galaxy catalogs in the COSMOS field. We measure the cross-correlation function (CCF) for 570 galaxies with spec- z measurements and detect a correlation with the IGM up to 50 h −1 comoving Mpc. We show that galaxies with stellar masses of 10 9 −10 10 M ⊙ are the dominant contributor to the total CCF signal. We also investigate CCFs for several galaxy populations: Ly α emitters (LAEs), H α emitters (HAEs), [O iii ] emitters (O3Es), active galactic nuclei (AGNs), and submillimeter galaxies (SMGs), and we detect the highest signal in AGNs and SMGs at large scales ( r ≥ 5 h −1 Mpc), but in LAEs at small scales ( r 5 h −1 Mpc). We find that they live in various IGM environments—HAEs trace the IGM in a similar manner to the continuum-selected galaxies, but LAEs and O3Es tend to reside in higher-density regions. Additionally, LAEs’ CCF is flat up to r ∼ 3 h −1 Mpc, indicating that they tend to avoid the highest-density regions. For AGNs and SMGs, the CCF peak at r = 5−6 h −1 Mpc implies that they tend to be in locally lower-density regions. We suspect that it is due to the photoionization of IGM H i by AGNs, i.e., the proximity effect.
Publisher: Springer Science and Business Media LLC
Date: 09-2014
DOI: 10.1038/NATURE13762
Abstract: Ultra-compact dwarf galaxies are among the densest stellar systems in the Universe. These systems have masses of up to 2 × 10(8) solar masses, but half-light radii of just 3-50 parsecs. Dynamical mass estimates show that many such dwarfs are more massive than expected from their luminosity. It remains unclear whether these high dynamical mass estimates arise because of the presence of supermassive black holes or result from a non-standard stellar initial mass function that causes the average stellar mass to be higher than expected. Here we report adaptive optics kinematic data of the ultra-compact dwarf galaxy M60-UCD1 that show a central velocity dispersion peak exceeding 100 kilometres per second and modest rotation. Dynamical modelling of these data reveals the presence of a supermassive black hole with a mass of 2.1 × 10(7) solar masses. This is 15 per cent of the object's total mass. The high black hole mass and mass fraction suggest that M60-UCD1 is the stripped nucleus of a galaxy. Our analysis also shows that M60-UCD1's stellar mass is consistent with its luminosity, implying a large population of previously unrecognized supermassive black holes in other ultra-compact dwarf galaxies.
Publisher: American Astronomical Society
Date: 18-12-2019
Publisher: American Astronomical Society
Date: 15-04-2013
Publisher: Oxford University Press (OUP)
Date: 10-2012
Publisher: American Astronomical Society
Date: 22-02-2021
Publisher: Oxford University Press (OUP)
Date: 04-2017
DOI: 10.1093/MNRAS/STX678
Publisher: American Astronomical Society
Date: 13-04-2017
Publisher: American Astronomical Society
Date: 21-08-2014
Publisher: SPIE
Date: 29-07-2016
DOI: 10.1117/12.2232467
Publisher: American Astronomical Society
Date: 27-01-2016
Publisher: Elsevier BV
Date: 12-2016
Publisher: American Astronomical Society
Date: 12-09-2006
DOI: 10.1086/507328
Publisher: American Astronomical Society
Date: 03-06-2015
Publisher: American Astronomical Society
Date: 07-11-2012
Publisher: Oxford University Press (OUP)
Date: 11-09-2013
Publisher: Oxford University Press (OUP)
Date: 2009
Publisher: American Astronomical Society
Date: 18-02-2014
Publisher: American Astronomical Society
Date: 24-04-2012
Publisher: American Astronomical Society
Date: 24-08-2016
Publisher: American Astronomical Society
Date: 02-04-2015
Publisher: Springer Science and Business Media LLC
Date: 25-05-2020
Publisher: American Astronomical Society
Date: 12-2011
Publisher: American Astronomical Society
Date: 11-10-2016
Publisher: American Astronomical Society
Date: 28-09-2018
Publisher: Oxford University Press (OUP)
Date: 05-2012
Publisher: American Astronomical Society
Date: 17-04-2017
Publisher: Oxford University Press (OUP)
Date: 08-03-2011
Publisher: Oxford University Press (OUP)
Date: 13-04-2011
Publisher: Oxford University Press (OUP)
Date: 22-01-2016
Publisher: American Astronomical Society
Date: 18-07-2016
Publisher: Oxford University Press (OUP)
Date: 16-07-2013
Publisher: AIP
Date: 2010
DOI: 10.1063/1.3458528
Publisher: American Astronomical Society
Date: 20-05-2014
Publisher: Springer Science and Business Media LLC
Date: 07-02-2015
Publisher: Oxford University Press (OUP)
Date: 05-2010
Publisher: Oxford University Press (OUP)
Date: 24-07-2015
Publisher: Springer Berlin Heidelberg
Date: 2009
Publisher: Oxford University Press (OUP)
Date: 10-06-2014
DOI: 10.1093/MNRAS/STU940
Publisher: American Astronomical Society
Date: 06-05-2009
Publisher: American Astronomical Society
Date: 22-03-2016
Publisher: Cambridge University Press (CUP)
Date: 2015
DOI: 10.1017/PASA.2015.49
Abstract: The first observations by a worldwide network of advanced interferometric gravitational wave detectors offer a unique opportunity for the astronomical community. At design sensitivity, these facilities will be able to detect coalescing binary neutron stars to distances approaching 400 Mpc, and neutron star–black hole systems to 1 Gpc. Both of these sources are associated with gamma-ray bursts which are known to emit across the entire electromagnetic spectrum. Gravitational wave detections provide the opportunity for ‘multi-messenger’ observations, combining gravitational wave with electromagnetic, cosmic ray, or neutrino observations. This review provides an overview of how Australian astronomical facilities and collaborations with the gravitational wave community can contribute to this new era of discovery, via contemporaneous follow-up observations from the radio to the optical and high energy. We discuss some of the frontier discoveries that will be made possible when this new window to the Universe is opened.
Publisher: American Astronomical Society
Date: 23-07-2015
Publisher: Oxford University Press (OUP)
Date: 21-09-2008
Publisher: EDP Sciences
Date: 05-04-2016
Publisher: American Astronomical Society
Date: 2022
Abstract: Star-forming galaxies are the sources likely to have reionized the universe. As we cannot observe them directly due to the opacity of the intergalactic medium at z ≳ 5, we study z ∼ 3–5 galaxies as proxies to place observational constraints on cosmic reionization. Using new deep Hubble Space Telescope rest-frame UV F336W and F435W imaging (30 orbits, ∼40 arcmin 2 , ∼29–30 mag depth at 5 σ ), we attempt to identify a s le of Lyman continuum galaxies (LCGs). These are in idual sources that emit ionizing flux below the Lyman break ( Å). This population would allow us to constrain cosmic reionization parameters such as the number density and escape fraction ( f esc ) of ionizing sources. We compile a comprehensive parent s le that does not rely on the Lyman-break technique for redshifts. We present three new spectroscopic candidates at z ∼ 3.7–4.4 and 32 new photometric candidates. The high-resolution multiband HST imaging and new Keck/Low Resolution Imaging Spectrometer (LRIS) redshifts make these promising spectroscopic LCG candidates. Using both a traditional and a probabilistic approach, we find that the most likely f esc values for the three spectroscopic LCG candidates are % and therefore not physical. We are unable to confirm the true nature of these sources with the best available imaging and direct blue Keck/LRIS spectroscopy. More spectra, especially from the new class of 30 m telescopes, will be required to build a statistical s le of LCGs to place firm observational constraints on cosmic reionization.
Publisher: Oxford University Press (OUP)
Date: 21-01-2010
Publisher: Oxford University Press (OUP)
Date: 23-06-2015
DOI: 10.1093/PASJ/PSV044
Publisher: American Astronomical Society
Date: 21-07-2020
Publisher: American Astronomical Society
Date: 16-09-2015
Publisher: Oxford University Press (OUP)
Date: 23-02-2016
Publisher: American Astronomical Society
Date: 02-03-2012
Publisher: IOP Publishing
Date: 07-2012
DOI: 10.1086/666528
Publisher: Oxford University Press (OUP)
Date: 21-03-2009
Publisher: Oxford University Press (OUP)
Date: 09-2009
Publisher: American Astronomical Society
Date: 27-07-2016
Publisher: Oxford University Press (OUP)
Date: 19-02-2008
Publisher: Oxford University Press (OUP)
Date: 21-08-2009
Publisher: EDP Sciences
Date: 06-2015
Publisher: American Astronomical Society
Date: 17-10-2014
Publisher: American Astronomical Society
Date: 13-12-2011
Publisher: EDP Sciences
Date: 20-07-2015
Publisher: American Astronomical Society
Date: 20-02-2014
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: American Astronomical Society
Date: 22-06-2016
Publisher: Oxford University Press (OUP)
Date: 19-12-2012
Publisher: EDP Sciences
Date: 09-2016
Publisher: American Association for the Advancement of Science (AAAS)
Date: 23-09-2011
Abstract: Timing observations of a millisecond pulsar reveal a planet that is far denser than any known planet.
Publisher: American Astronomical Society
Date: 11-02-2016
Start Date: 05-2016
End Date: 12-2017
Amount: $175,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 04-2015
End Date: 12-2016
Amount: $560,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 01-2019
End Date: 12-2023
Amount: $330,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 2017
End Date: 12-2018
Amount: $400,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 2015
End Date: 12-2015
Amount: $430,000.00
Funder: Australian Research Council
View Funded Activity