Established within the School of Physics, the Sydney Institute for Astronomy (SIfA) is a national and international leader in astronomy and physics research. We are also committed to excellence in postgraduate training and research-led undergraduate training.
The University owns the:
The development and application of new technology for the next generation of instruments and telescopes is enabled through state-of-the-art Sydney Astrophotonic Instrumentation Laboratories (SAIL).
Our Institute has leadership or key involvement in several major surveys including the:
The CAASTRO Centre of Excellence is housed within the School of Physics and engages about half of the students and staff within SIfA. Through our leading role in the Physics Equity and Access Committee (PEAC), we aim to provide an environment that is equitable and supportive for all staff and students, free of conscious and unconscious bias, with access to facilities, learning and work open to all.
We also have access to a number of astronomy facilities.
We undertake research in several key areas:
Our recent work on flares includes the construction of a model for particle acceleration in flares based on inertial Alfven waves, which attempts to account for the flare 'number problem' - the difficulty in reconciling the large inferred numbers of accelerated electrons in flares with the low density of the background solar plasma.
For more information contact Mike Wheatland or Don Melrose.
Despite the recent avalanche of discovery, the exoplanetary systems discovered by Astronomy's newest field have so far raised far more questions than they have answered. To get a more representative picture of exoplanetary populations, including greater sensitivity to those in the habitable zone, we need new techniques to illuminate the unknown areas beyond the reach of our present instruments.
Researchers at SIfA have very strong linkages with NASA's Kepler mission and we are also engaged in opening entirely new windows onto the planetary realm, including advanced projects in both the optical and the radio attempting to capture the faint signals betraying the presence of a planet against the noise and glare of their host star.
Among the most fundamental areas underpinning of the entire field of astronomy is a quantitative understanding of the basic properties of stars. In recent years, observational astronomy has developed new technologies to deliver exquisite new studies of stellar surfaces, their immediate surroundings, and even probes of their interior structure. By revolutionising our view of the stars themselves, we are able to see the interplay between them and the galaxies that host them, the families of planets that they harbor, and the extreme physics of the weird remnants left behind after they die.
We host one of the world's leading asteroseismology groups and are pioneers in the use of the highly complementary technology of high resolution interferometry. The information obtained from using both atereoseismology and interferometry combined can help us study fascinating physics under the extreme conditions in stars such as mapping their internal rotational profile and from that the transport of angular momentum as they grow old. This combined approach turns out to be a particularly powerful way to gain a nearly complete observationally-based physical understanding of a star, for the first time free from simplifying assumptions and model parameters derived from theory.
Magnetism plays a critical role in many areas of astrophysics, because it controls both the bulk flow properties of interstellar gas as well as the motion of individual charged particles. However, we know surprisingly little about the properties of the Galactic magnetic field. We are making a concerted effort to redress this situation, using the Faraday rotation of the diffuse polarised radio background as a new way to study structure and turbulence in magnetized gas.
Some of our current projects include:
Such data represent a whole new way of studying the ISM, and can allow a comprehensive study of interstellar magnetic fields on scales ranging from sub-parsec turbulence up to global galactic structure.
What can we learn about the formation processes of galaxies from studying the present structure of our own Milky Way, and nearby galaxies? Members of our group participate in international collaborations to observe structures in the outskirts of both the Milky Way and the Andromeda galaxies, thought to be remnants of interactions with smaller systems. Combining such observations with numerical simulations is an effective way for galaxy formation and evolutionary models to be tested.
Galactic cannibalism occurs throughout the universe but, close to home, small dwarf galaxies are torn apart by the much more massive Milky Way and Andromeda Galaxy. Using telescopes from around the world, including the 10-m Keck telescope in Hawaii, we have mapped the tell-tale signs of tidal disruption and destruction, providing important clues to how large galaxies have grown over time.
For more information contact Geraint Lewis.
The twinkling of stars, called scintillation, is due to fluctuations in the density of the air along the line of sight through the earth's atmosphere. Point-like radio sources, such as pulsars and quasars, also scintillate due to fluctuations in the electron density along the line of sight through the interstellar medium. Scintillation can lead to a change in the intensity of the source, a change in its apparent position, or both.
Jean-Pierre Macquart and Don Melrose have developed a model for scintillations of radio sources based on scattering by discrete structures in the interstellar medium. This differs from the usual model that assumes a statistical fluctuation in density. Their approach was motivated by the thought that the rather large discrete structures required to explain Extreme Scattering Events (ESEs) may be extreme examples of a range of discrete structures common in the ISM.
For more information contact Don Melrose.
We don't yet fully understand how stars explode and constraints on the many complicated processes which occur during core collapse are desperately needed. Since we rarely see a nearby star go supernova, our focus is on studying the aftermaths of supernova explosions, namely supernova remnants and young neutron stars, and in using these objects to infer the properties of the supernova, the progenitor star, and their surroundings.
This work is providing new insights into the micro- and macro-physics of the core-collapse process, on the properties of supernova progenitors, and on the mechanisms which produce the diversity we see in the resulting compact objects.
For more information contact Anne Green, Dick Hunstead or Tara Murphy.
This research aims to place the nearest galaxies, members of the Local Group, within a cosmological context. A physical model is being developed describing the formation and evolution of the Local Group, with attention to radiative and gaseous processes, combining radiative hydrodynamics code with multiwavelength data.
For more information contact Joss Bland-Hawthorn
We are building large data-sets containing thousands of quasars and radio galaxies with the express aim of measuring how they evolve and what the physical processes are which drive the evolution. We can do this by studying how individual sub-populations evolve, what their environments are and the how the black holes interact with their host galaxy. We will build on this with a broad range of multi-wavelength observations (from X-ray to radio) using state-of-the-art astronomical facilities in Australia and overseas.
For more information contact Scott Croom, Dick Hunstead or Elaine Sadler.
The multi-parameter nature of galaxy formation has meant that much progress has been made over the last decade by conducting massive surveys of up to one million galaxies to be constructed. These have, in turn, allowed detailed statistical analyses to be made, where the correlation between the multitudes of physical parameters can be studied.
All of these major surveys use a single optical fibre to collect the light from each galaxy. Yet, galaxies are intrinsically complex, multi-component systems with multiple structural components (eg. disks, bulges, halos) and elaborate interactions between the dark matter, stars, gas and super-massive black holes they contain. The use of single apertures thus loses valuable information and adds confusing biases.
We are leading the SAMI Galaxy Survey to survey thousands of galaxies in 3D measuring the way gas and stars move with these galaxies as well as where star formation is currently ongoing and how and why accretion onto super-massive black holes is important. Key questions we hope to answer include:
The University of Sydney is also a key partner in new deep spectroscopic surveys such as the Galaxy And Mass Assembly (GAMA) project. This aims to get redshifts for hundreds of thousands of galaxies and combine this with multi-wavelength data to understand how galaxies are distributed and grouped within dark matter halos and measure the structural properties of galaxies.
For more information contact Scott Croom or Joss Bland-Hawthorn.
Gravitational lensing is the bending of light by the gravitational field of a massive object. This phenomenon has a variety of astronomical applications. For example, it can be used as a natural telescope, magnifying distant sources into view or to probe the density profile of galaxies and galaxy clusters, testing dark matter theories.
The related field of microlensing has been used to search for low mass extrasolar planets, and to investigate the structure of quasars. Members of our group carry out computer simulations and observations of gravitational lensing.
Quasars, also known as quasi-stellar objects or QSOs, are luminous objects that are so distant that they appear pointlike in our images. When they are gravitationally lensed by an intervening galaxy, they can be multiply imaged. Often, assuming that the lens has a smooth mass distribution is adequate. However, in reality, galaxies are composed of stars and other compact objects, and are lumpy on small scales. Amazingly, this can actually change the brightnesses of the images, and these can vary with time in rather funky ways. We investigate these phenomena through the use of computational simulations.
For more information contact Geraint Lewis.
The WiggleZ team is using the Anglo-Australian Telescope to construct a huge redshift survey of ~400,000 galaxies at redshifts z~0.5-1.3.
The goal of this survey is to measure the "equation of state" of dark energy at high redshift. This is done by making high-precision measurements of the clustering of galaxies which ought to reveal the baryon acoustic oscillations (BAOs or baryon wiggles), a relic feature from the primordial Big Bang.
This encodes a fundamental physical scale whose size we can measure from the cosmic microwave background. Measuring this standard ruler at z=0.75 will give us the first high-precision measurement of dark energy independent of previous supernovae determinations.
For more information contact Scott Croom.
The theory of General Relativity is close to 100 years old and has been the preferred theory of gravity since its formulation by Einstein. Despite this, the understanding of General Relativity is not as advanced as might be expected, with few formal solutions existing and the physical interpretation of some of the mathematical results being unclear.
The Gravitational Astrophysics group conducts research into fundamental concepts in GR including the meaning and nature of expanding space and accelerated paths into black holes.
For more information contact Geraint Lewis.
Members of our group study the implications of various dark energy models, primarily through N-body simulations, in order to increase the theoretical understanding of dark energy physics required in order to maximise the effectiveness of future surveys and instruments.
For more information contact Geraint Lewis.
|Prof. Tim Bedding||official | personal|
|Prof. Joss Bland-Hawthorn||Director, SIfA, ARC Laureate Fellow||official | personal|
|A/Prof. Scott Croom||official | personal|
|Prof. Anne Green||official|
|Prof. Dick Hunstead||official|
|Dr Helen Johnston||official | personal|
|Dr Sergio Leon-Saval||Director, SAIL Labs||official|
|Prof. Geraint Lewis||official | personal|
|Prof. Don Melrose||official | personal|
|A/Prof. Tara Murphy||ARC Future Fellow||official | personal|
|A/Prof. John O'Byrne||official | personal|
|Prof. Elaine Sadler||Director, CAASTRO||official|
|Prof. Peter Tuthill||ARC Future Fellow||official | personal|
|A/Prof. Mike Wheatland||official | personal
|Dr Chris Betters||official|
|Dr Krzysztof Bolejko||ARC Future Fellow||official|
|Dr Shari Breen||official|
|Dr Julia Bryant||official|
|Dr Gayandhi De Silva||official|
|Dr Caroline Foster||ASTRO 3D Fellow||official | personal|
|Dr Magda Guglielmo||official|
|Dr Michael Hayden||Sydney Stromlo Fellowship||official|
|Dr Janez Kos||official|
|Dr Tanda Li||official|
|Dr Alpha Mastrano||official|
|Dr Seong-Sik Min||official|
|Dr Simon Murphy||DECRA||official|
|Dr Barnaby Norris||official|
|Dr Nic Scott||official|
|Dr Sanjib Sharma||official|
|Dr Adam Stewart
|Dr Thorsten Tepper Garcia||official|
|Dr Jesse Van de Sande||official | personal|
|Dr Timothy Van Reeth||official|
|Eromanga Adermann||Cosmic Voids in Evolving and Interacting Dark Sector Cosmologies|
|Rebecca Brown||Next generation 3D spectroscopy for the Anglo-Australian Telescope|
|Filip Chatys||Period-luminosity relations of red giants and supergiants|
|Isabel Colman||Asteroseismology using Kepler pixel data, with a focus on binary phenomena and red giants|
|Douglas Compton||Asteroseismology of Red Giant Stars|
|Jason Drury||Asteroseismology of Open Clusters: Ensembles and Kepler|
|Marcin Glowacki||Study of HI Absorption Against Distant Radio Sources through ASKAP|
|Asger Gronnow||The effect of the Galactic magnetic field on the accretion and survival of gas clouds|
|Daniel Hey||Binaries and pulsating stars|
|Nikolas Iwanus||Dark Matter Annihilation in Cosmological Simulations|
|Apsem Jibrail||The Growth of Angular Momentum in Non-Standard Cosmological Models|
|Alexey Latyshev||Interferometric image recovery in astronomy|
|Gang Li||Asteroseismology of gamma Doradus stars|
|Ralph Morgan||High angular resolution imaging of Galactic microquasar SS 433 and various stellar objects|
|Harry Qiu||Detection and classification of Fast Radio Bursts|
|Katazhyna Redzikultsava||Testing Non-Standard Cosmological Models With Supernova Data
|Zhen Wan||Galaxy Archeology|
|Jie Yu||Asteroseimology of 16,000 oscillating red giants observed by Kepler|
Seminars are held weekly typically on Fridays at 11am to 12pm in LT5 at the School of Physics building (A28). If you wish to give a talk or presentation please email Nic Scott.
Unfortunately, we do not have general funds available to cover travel or accommodation costs. If you would like to give a talk or are scheduled at a time that you will be away please let us know ASAP. If you have students or visitors that are going to have interesting topics to talk about please dob them in. Let us know if you will be giving a long (45min) or short (20min) talk, so we can have either two short talks or one long talk each week.
|May 31||11am LT5||Aman Khalid, Hillary Davis||SSP Project student talks|
|Jun 7||11am LT5||Peter Cottrell||
Interpreting stellar spectra or
The life of a spectroscopist
|Jul 2||11am LT5||Alan McConnachie||The Mauna Kea Spectroscopic Explorer|
|Jul 5||11am LT5||Guillaume Drouart||TBC|
|Nov 1||11am LT5||Ortwin Gerhard & Magda Aenaboldi||TBC|
|Jan 25||11am LT5||Lucia Armillotta||Metal mixing during star cluster formation|
|Feb 1||11am LT5||Andrew Hopkins||Measuring the stellar initial mass function|
|Feb 8||11am LT5||Matthew Baring||A Multiwavelength Perspective on Acceleration and Radiation in Extragalactic Jets|
|Feb 15||11am LT5||Toshi Futamese||Possible constraints on neutrino mass and dark energy from the lensing dispersion of the magnitude-redshift relation of Type Ia supernovae|
|Mar 1||11am LT5||Chris Tinney||VELOCE|
|Mar 8||11am LT5||Ahmed Elagali||Studies of Interacting Galaxies & the Environmental Effects on Their Evolution|
|Mar 15||11am LT5||Robert Jedicke||Super catastrophic asteroid disruption|
|Mar 22||11am LT5||Jo Dawson||Shining Light on the Dark ISM|
|Mar 29||11am LT5||Robert Jedicke||Super catastrophic asteroid disruption|
|Apr 5||11am LT5||Maria Cunningham||Radio Astronomy in the Era of Large surveys: Interpreting the results of large, multi-molecular-line datasets of the molecular ISM|
|Apr 9||11am LT5||Nicholas Martin||Mining and mapping the first generations of stars with the Pristine CaH&K survey|
|Apr 12||11am LT5||Amelia Fraser-Mckelvie||The complicated lives of disk galaxies|
|May 3||11am LT5||Nichole Barry||The Future of EoR Structure Limits|
|May 10||11am LT5||Nell Byler||Ultraviolet spectral diagnostics for star forming galaxies at high redshift|
|May 16||11am LT5||Kim Venn||Data Analysis and Machine Learning in Astrophysical Stellar Spectroscopic Surveys|
|May 17||11am LT5||Mahavir Sharma||Cosmic Reionization and its fossils in the Milky Way|
The State of the Universe
Professor Brian Schmidt
5 June 2018
Nobel Laureate Professor Brian Schmidt looks at the Universe's vital statistics and what we do (and don't) know about the past, present and future.