Eventos

The AAO is a consortium of three Australian instrumentation groups, based at Macquarie University, University of Sydney, and the Australian National University. Collectively, the consortium has delivered hundreds of instrument projects for astronomy, for our own telescopes and internationally.

Solar atmosphere and solar wind provide a unique laboratory for understanding the nonlinear dynamics of space and astrophysical plasmas.

The Cherenkov Telescope Array (CTA), currently in construction, shall be the Cherenkov Telescope Observatory for VHE Gamma Ray Astronomy, and shall provide crucial data for the understanding of the extreme universe in the recently open multimessenger era.

In the context of the upcoming SRG/eROSITA survey, I will present in this talk a methodology to construct mock catalogs for X-ray selected AGN samples based on dark matter only N-body simulations.

In this seminar I will describe the results of a large study designed to determine the input rate of cosmic dust to the terrestrial atmosphere, using a self-consistent treatment of cosmic dust from the outer solar system to the Earth’s surface.

Long γ-ray bursts are associated with energetic, broad-lined, stripped-envelope supernovae that are characterised by an high-velocity ejecta, of the order of 30,000 km/s.

We are entering a golden age for radio astronomy. New and existing facilities operating at submm-to-m wavelengths are shedding new light on the formation of planets, black holes, and even the first galaxies.

The central region of our Galaxy contains a huge amount of molecular gas. This region is often referred to as the "central molecular zone (CMZ)". High-velocity compact clouds (HVCC) are a peculiar population of molecular clouds found in the CMZ of our Galaxy.

Life, planets, exoplanetary systems, stars, and our galaxy evolve with time, and the best and sometimes only way for understanding this evolution is dating stars. THOT is a Marie Curie Project devted to gathering and updating all the stellar dating techniques into a single computational tool.

The habitability of a planet depends on various factors, such as delivery of water during the formation, the coevolution of the interior and the atmosphere, as well as the stellar irradiation which changes in time.

The first trans-Neptunian object was discovered in 1930 and we waited over 60 years to discover the second one. The discovery of Albion (a.k.a. 1992QB1) enticed the minor bodies community to characterize the new population, called collectively as trans-Neptunian objects (TNOs).

The Hubble (HST) and Spitzer telescopes were the first instruments to unveil the presence of rings and arcs around evolved low-mass stars (AGB stars, proto-PNe and PNe) in great detail. Since the mid-2000s it was suggested that these structures were ubiquitous around evolved low-mass stars.

Sagittarius A* (Sgr A*) is the variable radio, infrared (IR), and X-ray source associated with accretion onto  the massive black hole (MBH) at the center of the Milky Way.

The analysis of the UV atmospheric emissions arising from Mars' upper atmosphere has been used since the Mariner missions in the 60s to obtain information about this region, very difficult to sound by other means.

The RadioAstron active galactic nuclei (AGN) polarization Key Science Project (KSP) aims at exploiting the unprecedented angular resolution provided by RadioAstron to study jet launching/collimation and magnetic-field configuration in AGN jets.

We have imaged the shadow of the central black hole in the radiogalaxy M87. This required assembling the Event Horizon Telescope, a global VLBI array observing at a wavelength of 1.3 mm capable of achieving an angular resolution of 20 microarcsecond (uas).

In this talk I will show you a study on the detectability of the emission associated with the AGN dusty structure at sub-mm wavelengths using ALMA, in a theoretical and observational way. Theoretically, we use the Clumpy models from Nenkova et al.

In only four years, ALMA has radically changed the field of planet formation. We are currently obtaining very detailed images of the dust emission in protoplanetary disks with an unprecedent sensitivity and high angular resolution.

The results and products derived from the third and final release of data from the Planck mission will be reviewed with emphasis on the implications for cosmology.

I will divide my talk into three parts, starting with an overview of CSIRO’s Australia Telescope National Facility (ATNF), especially our telescopes (ASKAP & ATCA radio interferometers and the 64-m Parkes Dish), their receiving systems and key science projects.

The Earth’s northern winter polar vortex is a highly variable region. Sometimes, it becomes a beautiful demonstration of atmospheric coupling. Enhanced planetary waves, originated down in the troposphere, interact with the stratospheric mean flow and weaken or even break the vortex.

Planetary nebulae, the descendants of low- and intermediate-mass stars, have characteristic onion-like ionization structure, with the highest ionization species closer to the central star. This is true for all planetary nebulae, but HuBi 1, which shows an inverted ionization inner shell.

The Balmer emission originated in the broad line region (BLR) of active galactic nuclei (AGNs) could be either weak and difficult to detect, or even absent, for low luminosity AGNs,  as low ionization nuclear emission-line regions (LINERs).

Tidal disruption events (TDEs) are transient flares produced when a star is ripped apart by the gravitational field of a supermassive black hole (SMBH).