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We present here radiosed , a Bayesian inference framework tailored to modelling and classifying broad-band radio spectral energy distributions (SEDs) using only data from publicly released, large-area surveys. We outline the functionality of radiosed , with its focus on broad-band radio emissions that can trace kiloparsec-scale absorption within both the radio jets and the circumgalactic medium of active galactic nuclei (AGN). In particular, we discuss the capability of radiosed to advance our understanding of AGN physics and composition within youngest and most compact sources, for which high-resolution imaging is often unavailable. These young radio AGN typically manifest as peaked spectrum sources that, before radiosed , were difficult to identify owing to the large, broad-band frequency coverage typically required, and yet they provide an invaluable environment for understanding AGN evolution and feedback. We discuss the implementation details of radiosed , and we validate our approach against both synthetic and observational data. Since the surveys used are drawn from multiple epochs of observation, we also consider the output from radiosed in the context of AGN variability. Finally, we show that radiosed recovers the expected SED shapes for a selection of well-characterized radio sources from the literature, and we discuss avenues for further study of these and other sources using radio SED fitting as a starting point. The scalability and modularity of this framework make it an exciting tool for multiwavelength astronomers as next-generation telescopes begin several all-sky surveys. Accordingly, we make the code for radiosed , which is written in python , available on GitHub. [ABSTRACT FROM AUTHOR]

Exhibition booths provide a platform for organisations to showcase their specialities but are often limited by space and prohibitive costs for transporting large or fragile equipment. To address this, we developed a three-dimensional virtual exhibit that allows visitors to explore the technology and research behind the ASKAP radio telescope through interactive models of antennas and other components of the telescope array, including 360-degree visuals and animations. People can meet inside the virtual space regardless of their physical location to tour the exhibit and engage in discussions. The exhibition can be accessed through nearly any internet-accessible device, including a virtual reality (VR) headset, computer, or smartphone. The virtual exhibit was demonstrated at three in-person conferences by using a VR headset to access the exhibit from a conference booth, with both in-person and online team members to support the space. Participants were markedly impressed by the sense of presence in the 3D space and the ability to meet with experts who were not attending the conference. Such virtual spaces can be constructed relatively simply and have the potential to bridge online and in-person participants, as well as demonstrate facilities impossible to carry to event locations. [ABSTRACT FROM AUTHOR]

When low- and intermediate-mass stars evolve off the main sequence, they expand and cool into the red giant stages of evolution, which include those associated with shell H burning (the red giant branch), core He burning (the red clump), and shell He burning (the asymptotic giant branch). The majority of red giants have masses <2 M⊙, and red giants more massive than this are often excluded from major studies. Here, we present a study of the highest mass stars (M > 3.0 M⊙) in the Kepler sample of 16 000 red giants. We begin by re-estimating their global seismic properties with new light curves, highlighting the differences between using the simple aperture photometry and presearch data conditioning of simple aperture photometry light curves provided by Kepler. We use the re-estimated properties to derive new mass estimates for the stars, ending with a final sample of 48 confirmed high-mass stars. We explore their oscillation envelopes, confirming the trends found in recent works such as low mean mode amplitude and wide envelopes. We find, through probabilistic means, that our sample is likely all core He burning stars. We measure their dipole and quadrupole mode visibilities and confirm that the dipole mode visibility tends to decrease with mass. [ABSTRACT FROM AUTHOR]