I will present an update on the status of CTA, an overview Australia's involvements in CTA, and future funding plans for Australia's contributions moving towards the operational phase of CTA.
Optical polarimetry is an identified area in which Australia can contribute to CTA. We are planning to construct a prototype polarimeter to be installed on one or more Australian optical telescopes.
We report on CTA-pol progress: Parts have been selected, purchasing is ongoing, and we will shortly start design, prototyping and construction.
An Imaging Air Cherenkov Telescope (IACT) site in Australia, as part of a worldwide network of IACTs, would be crucial for achieving 24-hour all-sky coverage of the GeV to TeV sky for transient followup and continuous source monitoring. These sources of interest are typically brighter at comparatively low energies, so it’s valuable to study methods to reduce a telescope’s energy threshold. To...
The Cherenkov Telescope Array (CTA) is poised to revolutionise gamma-ray astronomy. One of the key science goals of CTA is the detection of gamma rays from dark matter annihilation. In this talk, I will describe a new Bayesian pipeline for the detection of dark matter using CTA data. The pipeline builds on top of the popular Gammapy package. The dark matter signal model is described in terms...
The Southern Wide-field Gamma-ray Observatory (SWGO) will be built in South America to survey the Southern sky for gamma-ray sources from hundreds of GeVs to beyond PeV energies. The candidate site will be decided by the end of 2023 and construction will start in 2024. It is expected that SWGO would be fully built by the end of 2026. SWGO will deploy 6500 particle detectors (Water Cherenkov...
Mixed-morphology supernova remnants (SNRs) are unique in that the exhibit X-ray and Gamma-ray properties, which are unexpected considering their advanced age. They tend to be rich in stellar ejecta, while they are some of the brightest gamma-ray remnants in our Galaxy. Currently, there has not been a consistent systematic study of the gamma-ray properties of these objects to understand why...
I will present detection of one of the largest Galactic SNR - G288.8-6.3 that we found in the new ASKAP EMU survey.
High-energy gamma-ray sources can be produced away from the supernova remnant (SNR), due to diffused hadronic cosmic-rays interacting with the interstellar medium (ISM). In order to find the corresponding accelerator, one possible approach is the modelling of gamma-ray emission from this process. The observation of gamma-ray sources can then be compared with the obtained model. In modelling,...
Simulating the propagation of particles can be very expensive when scattering lengths and detector sizes are small. I will present a MCMC method to speed up these simulations using the motivating example of propagating light in the IceCube detector.
In November 2022 we presented a Likelihood-Free Inference (LFI) method for gamma-ray reconstruction at CTA. Since then, we have proceeded an updated dataset in order to fully test the capabilities of the LFI algorithm. Unfortunately, not everything always goes as planned. In this talk we will provide an update on the project and highlight how the choice of training and testing data can have...
High-energy gamma rays and neutrinos can be produced due to the hadronic interactions between protons escaping particle accelerators such as supernova remnants (SNRs) and nearby target material such as molecular clouds (MCs). By modelling the diffusion of protons escaping SNRs and interacting with nearby MCs in our Galaxy, we can predict the resulting gamma-ray and neutrino fluxes at Earth....
SNRs are believed to be a likely sources of Galactic cosmic-ray protons with energies of PeV and above. High-energy protons, escaped from the shock front, diffuse in the ambient ISM and produce gamma rays as products of neutral pion decay from proton-proton interactions.
Current models use a constant diffusion coefficient over the whole map to describe cosmic rays travelling through the...
We have simulated the diffuse cosmic-ray sea and gamma-ray emission with GALPROP using a time-dependent solution to the transport equation to ensure the IC emissions are computed accurately. Our predictions are compared to the diffuse emission estimated by the H.E.S.S. telescope array, and the future prospects for detections with CTA will be discussed.
I will provide an update on the analysis of gas data towards RXJ1713 and compare them to data obtained from the GOT C Survey.
In this presentation, I report an optical feature associated with the Scutum Supershell utilising [SII] and H alpha observations. The morphology of the optical structure resembles the outflow that is currently under investigation. Furthermore, we conducted a X-ray analysis to determine the flux using PIMSS, incorporating ROSAT PSPC and MAXI SSC observations of the region.
