Astronomy is now very much a big-data science.
Gaia has had its second data release and is on track to measure the brightness, position and kinematics of close to 10e9 stars.
TESS and PLATO will observe pulsations in > 10e5 targets. They will add to the approximately 2 x10e5 stars that have had their oscillations monitored by
Kepler and CoRoT. To exploit such large data sets the tools of analysis devised must demonstrate speed, accuracy and versatility.
Speed and accuracy are required to process the sheer volume of data collected.
Versatility is necessary because although there will be overlap in the many surveys, not all stars will have the same quantities measured.
It is paramount that methods are designed to handle missing or inhomogeneous data sets -- we must maximize the information extracted from the available observations.
I will discuss the Stellar Parameters in an Instant Pipeline (SPI) which is a machine learning algorithm that makes use of detailed asteroseismic observations to rapidly and robustly determine stellar parameters. Stellar parameters are important for both exoplanet and galactic astrophysics.

Garry's 30-month (pre-submission) review. Note earlier time.

Our Mahalo-Subaru project, a systematic narrow-band line emitter survey,
has been mapping out star forming galaxies in and around galaxy clusters at 0.4and revealing the inside-out quenching of star formation activities from cluster
cores to the surrounding regions as time progresses.
In the dense cores of the highest redshift cluster, we see an enhancement of star
forming activities, which are likely driven by ample gas that is supplied by massive
gas inflow through the filamentary structures. It is consistent with strong Lya line
attenuations with respect to the Ha emission lines as indicated by dual narrow-band
imaging (Lya and Ha), and also with higher molecular gas mass fraction as observed
by ALMA.
These results are different from recent studies of X-ray clusters at similar
redshifts (z=2-2.5) where they find a deficit of gas while star formation efficiency
tends to be higher in the cluster cores. Such discrepancy implies that the gas
accretion mode may be changed from the cold accrtetion mode accompanied by high star
formation activity, to the hot mode where gas cooling and thus accretion to galaxies
become inefficient, resulting in the quenching of the cluster cores.
If time allows, I will also touch on our on-going and future programs with Subaru
and TAO.

Neutron stars unite many extremes of physics and can serve as astrophysical laboratories that allow us to probe states of matter at densities which cannot be reached on Earth.
One exciting example is the presence of superfluid and superconducting components in mature neutron stars. When developing mathematical models to describe these large-scale
quantum condensates, physicists tend to focus on the interface between astrophysics and nuclear physics. Connections with low-temperature physics are generally ignored.
However, there has been dramatic progress in understanding and experimenting with laboratory condensates (from the different phases of superfluid helium to the entire range
of superconductors and ultra-cold gases). In this talk, I will provide an overview of what we know about superfluid and superconducting components in neutron stars, and
suggest novel ways that we may make progress in understanding neutron star physics using the connections to terrestrial low-temperature condensates.

Type Ia supernovae play a key role in understanding nucleosynthesis, galactic chemical evolution, and constraining the nature of dark energy (Nobel Prize in Physics, 2011). Despite all their importance, we still do not know which type(s) of binary stars make Type Ia supernovae. This is an unsolved puzzle in astrophysics known as 'the progenitor problem'. To uncover the origin of Type Ia progenitors, one must understand how close binary stars evolve and interact. I will show how calculations that combine binary star evolution, explosion models, and radiative transfer spectral synthesis have been successful in linking different theoretical formation channels of Type Ia progenitors to their explosion mechanism(s). These predictions ultimately help us to make predictions for the elemental yields arising from different SN Ia subclasses, and bring us closer to understanding the nature of their progenitors.

On the 13th of July this year, two years after its first light, the MeerKAT telescope, was inaugurated by the South African deputy president in Carnavon, in the remote Northern Cape of South Africa. The inauguration showcased the first science quality data flowing out of the full 64 antenna interferometeric array, operating in 4096 channel mode at L-band, by unveiling a detailed panorama of the Galactic Centre. This important milestone has exhibited both the sensitivity and the potential of the MeerKAT telescope, which is increasingly "open for business". To get the instrument working at its full capacity, much commissioning work remains to be done. As a member of the beamformer commissioning team, I will provide an overview of the MeerKAT telescope and the goals achieved in the run up to the inauguration event. I will also map the road ahead -- pointing to exciting developments since the inauguration and the remaining challenges.

At present, the LIGO and Virgo collaborations have announced the detection of gravitational waves from seven compact binaries. The analysis of data from LIGO’s second observing run is ongoing, and updated results are expected soon. As the sensitivity of the detector network improves, detections will become routine. At design sensitivity, LIGO may detect several events every week. The growing catalog of gravitational-waves events records the masses and spins of merging black holes, which, in turn, provide clues about the life and death of the stars that formed them. In this talk I describe how Bayesian parameter estimation is used to infer the population properties of binary black holes. I discuss how upcoming results from LIGO/Virgo will shed light on phenomena such as pulsational pair instability supernova and binary black hole formation.

The chemical composition of the interstellar medium of galaxies continuously evolves as a function of time because of many environmental physical processes. Restitution of metals from dying stars, astration of metals due to the star formation activity, gas inflows and outflows, radial mixing of both gas and stars are all fundamental mechanisms which drive the chemical evolution of galaxies. Starting from the observed present-day chemical abundances in the stars and interstellar medium, chemical evolution models aim to reconstructing the past chemical enrichment history of galaxies, in a typical “astro-archaeological” approach. In the first part of the talk, I will introduce the basic concepts behind chemical evolution models and present my original contribution in the foundations of this field. In the second part, I will show how cosmological hydrodynamical simulations can be effectively used to study the evolution of the radial (gas-phase and stellar) C, N and O chemical abundance gradients in galaxies, presenting also new results from high-resolution zoom-in simulations, where a target galaxy is selected at low redshift from a reference large-scale cosmological simulation and then re-simulated with a larger number of resolution elements, starting from the initial conditions of the early Universe. Finally, I will present some preliminary results from the chemodynamical simulation of a Milky Way-like galaxy, that we have developed to characterise the different chemical evolution histories of the thin and thick disc stellar components of our Galaxy.

Astronomers will increasingly rely on AI and machine learning code to sift and sort through the mountains of data that are now upon us, growing in volume and complexity by the day. As the diamonds in the rough are identified, it will still come down to careful and close inspection to disentangle the natural secrets within. Astrophysical data is inherently multi-parameter, with the spatial dimensions at the core centre of imaging, spectral, time-domain and simulation data. With the dawn of powerful GPUs and virtual-reality (VR) technology we are no longer limited to flat screens to emulate 3-D cosmic views. Leveraging the significantly improved VR headsets with the powerful programming tools developed for visualisation gaming, the time is right for astronomers to deploy such technology to interrogate and interact with complex multi-dimensional data. Here I will present the development work in our visualisation laboratory - using HTC VIVE-PRO and Samsung Odyssey VR tech, the Unreal Engine C++ and Unity programming C# foundations - that supports our research on galaxy evolution, cosmic web large scale structure, galaxy-galaxy interaction simulations, and gas/kinematics of nearby galaxies. The Big Data Era ushered in by the SKA and its Pathfinders challenges our storage, calibration, reduction and refinement methods, and it also demands innovative ways to interrogate the data at intuitive -visualisation - levels necessary for new discovery.

The observation of gravitational waves from merging compact objects has marked the beginnings of gravitational waves astrophysics for ground-based gravitational-wave observatories like LIGO and Virgo. However, these instruments are also searching for other gravitational wave sources. Continuous gravitational waves from rotating neutron stars are persistent, long duration signals at close to monochromatic frequencies. Noise sources can also introduce monochromatic signals into LIGO data, which proves challenging if searching for a continuous gravitational wave signal near to the affected frequencies. One such noise source in the LIGO observatories originates from the 60Hz American electricity grid. Here we investigate how and whether signal processing techniques (similar to those used in noise-cancelling headphones) can be used to help continuous gravitational wave searches.

Confirmation of Candidature on exploring the pollution of the early universe by high redshift galaxies in Aurora.

Sara Webb's 6-month review

Measurements of the angular momentum and spin of galaxies are becoming widely available thanks to the new generation of extragalactic IFU surveys. This is opening a new window in which to investigate galaxies and specifically the connection between their mass growth, quenching, morphological and kinematic transformation. Simulations of galaxy formation provide us with a unique opportunity to study causality in all the emerging correlations, such as the specific angular momentum-mass, spin-ellipticity, among other relations. I'll be discussing how we have used the EAGLE and Hydrangea cosmological hydrodynamical simulation suites to investigate the connection between gas accretion, angular momentum, mass growth and environment in galaxies, and the main conclusions we have reached so far. I will also discuss how we are using the new semi-analytic model Shark to study the halo-galaxy angular momentum connection and how different physical processes work towards breaking it down.

With a single confirmed joint observation of the gravitational waves (GW) emitted from a binary neutron star system with an electromagnetic (EM) counterpart, the era of multimessenger astronomy was born overnight. With only a few detectors online, the poor directional resolution of the GW antennae network leaves hundreds of square degrees to be searched for associated transients. The large number of false-positives which simultaneously litter the sky represent a major challenge to reliably identify and link potential EM counterparts to GW events. In this talk, I will discuss the Gravitational-Wave Optical Transient Observatory (GOTO) which is dedicated to the follow-up of GW event triggers; as well as the ways in which we automatically detect and classify potential astrophysical transients using unsupervised and supervised machine learning algorithms on image-subtracted data. I will also discuss exciting research avenues with routine joint GW-EM observations, such as GW-EM parameter estimation, which may provide further constraints on the Hubble constant independent of the cosmological distance-ladder.

Thesis confirmation talk

As the physical prescriptions, resolution, and volume of hydrodynamic cosmological simulations continue to improve, so too do their ability to meaningfully describe the gas properties of galaxies in various phases. Nevertheless, ‘state of the art’ simulations still require significant post-processing to separate gas into its atomic and molecular components. This is crucial for comparing to observations, where data are most abundant for HI (atomic hydrogen). In this presentation, I will showcase the latest results from the IllustrisTNG simulations regarding HI in galaxies. I will make close comparisons to recently completed HI surveys, namely xGASS and ALFALFA. Focus will be given to the effect environment has on satellite galaxies. While the simulations predict the HI content of satellites to change with environment at fixed stellar mass and specific star formation rate (in line with observations), the effect appears to be far weaker for fixed HI size or disc specific angular momentum. While the former predictions agree with semi-analytic models of galaxy formation (namely Dark Sage), the latter are at odds. By dissecting the assumptions that different models/simulations make and therefore why their predictions differ, we gain insight into the key physical processes that impact HI in galaxies.

Transient sources of gravitational waves, such as coalescing black holes
and neutron stars, have obviously been at the forefront of gravitational
wave astronomy. But, there are still many intriguing sources that have
yet to be detected, and these include continuous quasi-monochromatic
signals from individual rapidly-rotating neutron stars. Known pulsars
therefore are intriguing targets for searches for such signals. In this
talk I will give an overview of searches for gravitational waves from
pulsars using the LIGO and Virgo detectors. I will describe some recent
work that may provide some evidence that millisecond pulsars have a
minimum ellipticity, which makes detection of these sources more
plausible with future gravitational detectors. I will also describe how
hierarchical Bayesian inference can potentially be used to detect
signals from an ensemble of pulsars and infer the distribution of pulsar
ellipticities.

The Galaxy's supermassive black hole is a hundred times closer than any other massive singularity. It is surrounded by a highly unstable gas disk so why is the black hole so peaceful at the present time? This mystery has led to a flurry of models in order to explain why Sgr A* is radiating far below (1 part in 10⁸) the Eddington accretion limit. But has this always been so? Evidence is gathering that Sgr A* has been far more active in the recent past, on timescales of thousands of years and longer. The bipolar wind discovered by MSX, the x-ray/gamma-ray bubbles discovered by ROSAT/Fermi, the WMAP haze, the positronium flash confirmed by INTEGRAL, and new UV spectroscopy from HST are suggestive of something truly spectacular in the recent past. We present new evidence that the Galactic Centre was a full blown "active galaxy" just a few million years ago. The echo of this incredible event can be seen today imprinted across the Galaxy. This leads us to a developing paradigm for Sgr A* activity over billions of years.

As near-infrared instrumentation comes into widespread use in extragalactic astronomy, we can observe the rest-frame properties of galaxies in over-dense or proto-cluster environments. These observations provide valuable information on the early affects of environmental density on galaxy evolution, and provide constraints on advanced cosmological simulations such as FIRE and Illustris-TNG. The ZFIRE survey has spectroscopically confirmed two such proto-clusters, at z=2.095 in COSMOS, and at z=1.65 in UDS, using the MOSFIRE instrument on Keck 1. We measure gas kinematics from the Hydrogen alpha emission line, and find no cluster-wide effects on kinematics, and a minor correlation between irregular morphology and angular momentum. In addition, we measure gas-phase metallicity on the group scale, attempting to measure indications of gas accretion or metal enrichment in the merging groups that define this proto-cluster. We determine if and when environmental density plays a role in early galaxy properties, which evolutionary processes are affected, and at what scale these processes act on members of over-dense regions at z~2

Absorption systems in the emission spectra of quasi-stellar objects (QSOs) provide an opportunity to study the distribution of metals in the Universe without the direct detection of the galaxies which have processed them. I study the spectra of four QSOs with emission redshifts 5.79=4.77, the comoving mass density (Ω) of MgII exceeds an expectation from the global metallicity of damped Lyα absorbers (DLAs) paired with the comoving mass density of HI.

I provide the first statistical study of SiIV beyond redshift 5 and I classify the CIV population by the presence of other ions and their velocity width. I find that all CIV systems with v>200km/s have associated low ionisation systems. I find that two such systems, separated by 550 physical kpc along the line of sight, are most likely tracing a multi-phase medium where hot and cold gas is mixing at the interface between the circumgalactic and intergalactic medium. I connect these observational discoveries to cosmological simulations and future investigations as well as the opportunity for future such observational studies.

I will present findings from our ongoing UK KMOS GTO programme that has measured the spatially-resolved gas properties for over 1000 emission-line galaxies at z~0.6–2. Combining this sample with ~800 galaxies at z~0 from the SAMI Galaxy Survey and ~400 more at intervening redshifts (z~0.4) observed with MUSE, we are able to probe the dynamics of star-forming galaxies over an interval of ~10 Gyr. This period encompasses ~70 percent of cosmic history and includes key epochs for galaxy growth and evolution. I will highlight recent results from our programme, including a measure of the redshift evolution of the Tully-Fisher relation since z~1 and an examination of the shapes of galaxy rotation curves between z~0.6-2. I will discuss how these analyses provide insights into the processes governing galaxy evolution in our Universe.

The outer halos of galaxies are a fantastic laboratory to study
several important physical processes that shape the appearance of galaxies
in the universe. While dominated by the dark matter component, the outer
halos also harbor small galaxies orbiting around the main galaxy, and
often a faint stellar halo. Low surface brightness observations of these
stellar halos, as done for example using the Dragonfly telescope, often
reveal streams, shells, and several other indicators of merger events,
providing a unique insight into the formation pathways of individual
galaxies. Additionally, metallicity and stellar population gradients in
the smooth parts of the stellar halos provide information about the early
formation times of the galaxies. Such global outer stellar halos are
commonly observed in galaxy cluster environments, but only recently became
available for less massive galaxies. Using the hydrodynamical cosmological
simulation set Magneticum Pathfinder, as well as isolated merger
simulations, I will demonstrate how to decipher the information hidden in
the various components of these outer halos, and what we can learn from
that.

It is now well established that the star-formation activity of our Universe increased from the very early epochs, peaked around z=2, and then decreased by an order of magnitude until present age. However, the exact contribution of different galaxy populations to the total SFR budget is not yet well-defined. Further progress in this area requires both a better understanding (or calibration) of SFR tracers used as well as deep observations of such tracers. The international panchromatic Cosmic Evolution Survey (COSMOS), is the only single survey large enough to study the coupled evolution of the large-scale structure of the Universe, galaxies, star formation, and active galactic nuclei across cosmic time. The 2 sq deg area of sky covered by COSMOS has the most extensive set of multi-wavelength observations of any deep field sufficient to probe the high mass end of galaxy populations out to high redshift, spanning the entire electromagnetic spectrum from X-ray, UV, optical, infrared to the radio. In this talk I will cover two topics from my PhD work: 1) the evolution of galaxy opacity and dust distributions since z~1 and 2) the evolution of specific star formation since z~5 using radio continuum as a star formation rate tracer.

"Localising the source of Fast Radio Bursts with UTMOST-2D", 6 month review talk.

UV diagnostics are critical for the study of high-redshift galaxies, given that commonly-used optical emission line diagnostics become observationally unavailable as they redshift out of wavelength regimes accessible from the ground. UV emission in galaxies is dominated by flux produced by young massive stars, along with line and continuum emission from ionized gas in the ISM. In this work, I assess the diagnostic potential of both absorption and emission features in the UV, using models that simultaneously and self-consistently consider stellar and nebular emission. I measure the metallicity sensitivity of established UV stellar absorption indices, and identify those that include a significant contribution from nebular emission. I identify combinations of strong emission lines that constrain metallicity and ionization parameter, and develop UV versions of the canonical “BPT” diagram. For nebular emission lines that overlap with known stellar wind features like C IV λλ1548,1551, I quantify the relative contribution from nebular and stellar emission to line ratios. I evaluate the diagnostics against observations of local galaxies and galaxies at high redshift and summarize the best diagnostic choices and the associated redshift range for low-, mid-, and high-resolution rest-UV spectroscopy in preparation for the launch of JWST.

In this talk I’ll present the "HI KOALA IFS Dwarf galaxy Survey" (Hi-KIDS). Hi-KIDS, which is part of ASTRO-3D, uses KOALA+AAOmega at the Anglo-Australian Telescope (AAT) to get good-quality IFS data of a sample of nearby dwarf and irregular galaxies for which we already have 21cm HI interferometric data, exploring a parameter space which is not studied by current IFS galaxy surveys. Hi-KIDS studies the global and local properties of the ionized gas (metallicity, SFR, kinematics) and the stellar component (star-formation history, kinematics) of nearby dwarf galaxies. It also compares the combined IFS+radio data with theoretical predictions of chemical evolution models to investigate the efficiency of the conversion of gas into stars. Hi-KIDS will provide a comprehensive picture of the physical processes ruling dwarf galaxies. In this talk I’ll present the motivations for conducting the Hi-KIDS survey, the status of the observations, and some preliminary results.

As the experiments looking to detect dark matter close in (coming from different directions on the Feynman Diagram), a small fraction of the baryon community is quietly anticipating a window on the universe (21cm neutral hydrogen) to de-fog a little. While theoretical simulators continue to grapple with the challenges of “mocking the universe”, observers can focus on refining (or even just beginning to understand) the prescriptive, previously sub-grid, physics and chemistry that made the universe great. I will talk about how star formation and stellar mass in galaxy groups can possibly make more sense if we can see the faint stuff (stars and gas) that everyone assumed was unimportant.

Connecting planetary systems at different stages of stellar evolution helps us understand their formation, evolution and fate, as well as provides us with crucial insights about their dynamics and chemistry. Post-main-sequence stars -- pulsars, white dwarfs and giant branch stars -- all host planetary systems, which often include remnant debris discs. Here I provide a review of our current knowledge of these systems. I show how this interdisciplinary field incorporates several facets of stellar physics and chemistry as well as solar system physics and chemistry, and detail simulation-based efforts to understand the big picture.

Confirmation of Candidature

High-performing deformable secondary mirrors, and powerful, robust sodium lasers guide stars are becoming standard technology on the world's largest telescopes. This is enabling a new level of reliability, sky coverage, and precision for adaptive optics (AO), with multiple configuration options for different science applications. In particular, wide field, high-strehl AO performance has been demonstrated at infrared wavelengths through the use of Multi-Conjugate Adaptive Optics (MCAO). The high actuator density possible with deformable secondary mirrors is also enabling diffraction-limited performance at optical wavelengths, as demonstrated by recent observations at various 8m-class telescopes. MAVIS proposes to combine these two developments, exploiting the full capabilities of the European Southern Observatory's 4-laser guide star Adaptive Optics Facility, providing near-diffraction limited spatial resolution of an 8m telescope across a relatively large field of view. This Australian-led instrument will provide HST-like (or better) resolution from the ground, but with the light-gathering power of the Very Large Telescope (VLT), making it a powerful complement to future facilities like the space-based JWST and the 30-40m class ground-based telescopes currently under construction. We will present an overview of the foreseen MAVIS technical and scientific capabilities, and describe ways in which you can get involved in developing the science case for this exciting new instrument.

MAVIS factsheet

The intergalactic medium (IGM) plays a unique role in constraining the (small scale) matter power spectrum, since the low-density, high redshift IGM filaments are particularly sensitive to the small scale properties of dark matter. The main observable manifestation of the IGM, the Lyman-alpha forest, has provided important constraints on the linear matter power spectrum, especially when combined with cosmic microwave background data. This includes, most notably, the tightest constraints on warm dark matter (WDM) and fuzzy dark matter (FDM) models, that I will present in this talk.

Primordial non-Gaussianity (PNG) is one of the most promising probes to distinguish between different models of inflation, a theory to describe an era of exponential expansion of the very early universe that was first introduced to solve problems within the Big Bang model. Inflation can solve the horizon problem as well as the flatness problem, and can also explain the origin of structure formation through the creation of initial fluctuations. Currently, the best constraints on PNG are provided by measurements of the cosmic microwave background (CMB) with the Planck satellite. Even though current constraints from large scale structure (LSS) data are weaker than the CMB results, future galaxy surveys have the potential to significantly improve upon these limits by constraining the scale dependent halo bias induced by PNG. To fully exploit the information from galaxy surveys, optimal analysis methods need to be developed and applied to the data. I will present an optimal technique to directly constrain local non-Gaussianity from galaxy clustering by applying redshift weights to the galaxies and present preliminary results from the extended Baryon acoustic Oscillation Spectroscopic Survey (eBOSS).

Quasars play a key role in our understanding of the physical universe and its major constituents. Variability is one of their key observable characteristics, and it is present at all wavelengths and at all time scales probed so far. It reflects directly the physics of their fueling and beaming, and offers a spectrum-independent method for quasar discovery that bypasses many selection effects. The field is being transformed by the large synoptic sky surveys and the resulting archives of light curves, that offer unprecedented opportunities for the systematic studies of quasar variability. I will describe several such projects, based mainly on the CRTS survey archive, including: a novel characterization of the stochastic variability of quasars, a discovery of a population of quasars with a periodic variability interpreted as a signature of the long-predicted supermassive black hole binaries, the most efficient method to date for a selection of quasar candidates, the discovery of megaflares in their light curves, a search for outliers in the variability parameter space that revealed interesting phenomena, including a population of type-changing quasars, etc.

Renee Spiewak 18 month review.

Searching for and timing millisecond pulsars.

The evolution of galaxies is linked to the growth and accretion histories of their host dark matter haloes. Weak gravitational lensing allows us to measure the evolution of their dark matter haloes, as well as the larger cosmic web that these haloes inhabit. I will review recent results from weak gravitational lensing and other methods that allow us to probe the dark matter content of the Universe on the scale of galaxies and so provide new insight into the processes that shape the evolution of galaxies. I will also discuss our recent detection of dark matter in the filaments of the cosmic web between galaxies. I will conclude by highlighting prospects from upcoming ground-surveys, and satellite missions.

Ellert vd Velden 6 month PhD Review / Confirmation of Canditature

The magnifying power of gravitational lensing allows us to study distant galaxies in unprecedented detail. At moderate redshifts (1 < z < 5) the spatial magnification allows us to examine the kinematics and morphologies of ‘normal’ star-forming galaxies, revealing the processes that lead to the clumpy star formation observed in this epoch. At the highest redshifts (6 < z < 10), the flux magnification from lensing allows us to directly observe dwarf galaxies in the first billion years of the Universe, probing the faint end of the luminosity function where the majority of the ionizing photons that contribute to reionization originate. I will also discuss prospects for JWST in studying the first galaxies and the epoch of reionization.

Aditya 18 month review.

The Multi-Unit Spectroscopic Explorer (MUSE) is an integral field spectrograph with unique capabilities on the Very Large Telescope. With its high sensitivity and by providing a complete view of the optical spectrum over 1 arcmin2 it has been a tremendous breakthrough in the way galactic and extragalactic observations are performed. We will present a few examples where MUSE's transformational science capabilities are demonstrated. The success of MUSE calls for new ideas for the next generation of VLT instruments, and we will present the concept of a blue-MUSE: a wider field of view, higher resolution, blue-optimised version of MUSE.

Slides: Keynote
Slides: PDF

Confirmation of Candidature

In the quest for identifying pop-III stars, the most sought-after emission line is He II, however, stellar population models are unable to accurately predict the He II features while being consistent with other emission line diagnostics. To produce He II ionizing photons, stellar populations require sources of hard ionizing radiation with energies >= 54.4 eV and sources such as AGN, shocks, X-Ray binaries, stellar rotation and/or binary stellar evolution, and post-AGB stars have been suggested as possible contributors. To accurately identify relative contributions from these wide variety of sources, high signal-to-noise spectra with rest-frame UV/optical coverage and advanced stellar population/photoionization models are required.

The VLT/MUSE GTO program has obtained deep ~10-30h exposures of the Hubble legacy fields yielding rest-UV spectra of galaxies at z~2-6. In this talk I will present recent results of the MUSE program, where we compare the z=2-4 He II emitters with expectations from photoionization modelling to explore their stellar population and ISM conditions. I will compare our results with recent results from local samples of high-redshift "analogues" to show the different parameter spaces probed by local and high-redshift galaxies in the rest-UV. I will address the necessity to obtain high signal-to-noise spectra of individual galaxies to model rest UV emission and absorption systems along with auxiliary rest-NIR lines to constrain stellar population properties of galaxies at high-z, which will be aided by combined studies by MUSE and JWST in future.

Fast radio bursts (FRBs), bright millisecond duration radio transients, are quickly becoming a subject of intense interest in time-domain astronomy. FRBs have the exciting potential to be used as cosmological probes of both matter and fundamental parameters, but such studies require large populations. Advances in FRB detection using current and next-generation radio telescopes will enable the growth of the population in the next few years from 30 to hundreds. Real-time discovery and follow-up, and new studies of the FRB population will provide us with some of the greatest insights in the coming years. I will discuss many observational aspects of the FRB population, including polarisation, searches for multi-wavelength emission, localisation, and repeating FRBs. I will also discuss how our response to these events can inform next generation surveys and pave the way for the enormous number of FRB discoveries expected in the SKA era.