The Melbourne Astro group has weekly colloquia, group meetings, and journal clubs. Normal times and places can be found on the calendar here.
A list of recent colloquia, with slides in some cases, can be found here
The Melbourne Astro group has weekly colloquia, group meetings, and journal clubs. Normal times and places can be found on the calendar here.
A list of recent colloquia, with slides in some cases, can be found here
Wednesday 19 May 2021 @ 11:00 a.m., David Caro building, Level 2, Hercus Theatre (+Zoom)
A Prof Duane Hamacher, University of Melbourne; Email: duane.hamacher[at]unimelb.edu.au
Australia’s First People developed complex knowledge systems that are committed to memory and passed to successive generations through oral tradition. The length of time oral traditions can be passed down while maintaining vitality is a topic of ongoing debate. Scientific techniques have been utilised to date natural events described in oral tradition, such as volcanic eruptions, tsunamis, and meteorite impacts to provide a terminus ante quem for the origin or development of these oral traditions. In this talk, we analyse Tasmanian Aboriginal (palawa) oral traditions recorded in the early nineteenth century that describe the flooding of the Bassian Land Bridge connecting Tasmania to mainland Australia, as well as the presence of a culturally significant “Great South Star”. Using astro-chronological and geo-chronological techniques, we show that these traditions have a terminus ante quem of approximately 12,000 years.
Wednesday 12 May 2021 @ 12:00 p.m., David Caro building, Level 2, Hercus Theatre (+Zoom)
James Esdaile, Swinburne University; Email: jesdaile[at]swin.edu.au
In the early Universe one might expect only star-forming galaxies but there is now substantial evidence that some massive galaxies have quenched star-formation within the first billion years of galaxy evolution. These massive quiescent galaxies (MQG) have proven difficult to reproduce in sufficient numbers in cosmological hydrodynamical simulations. While the latest generation of simulations have begun to achieve more consistent number densities through detailed prescriptions of AGN feedback, the observed quenched galaxies still appear to quench at earlier epochs. This begs the question: how early in the Universe can we still find quiescent galaxies? Additionally, high redshift MQGs host old stellar populations that can provide insights into the star-formation conditions during the epoch of reionisation. The intense star-bursts that likely formed MQGs are expected to have a different distribution of stellar masses, the initial-mass function (IMF), compared to local elliptical galaxie
s. I present work done to identify these rare MQGs at high redshift based on the FENIKS survey and determine some of their physical properties using a combination of deep HST imaging and MOSFIRE spectra.
Wednesday 28 Apr 2021 @ 12 p.m., David Caro building, Level 2, Hercus Theatre (+Zoom)
Dr Nikole M. Nielsen, Swinburne University; Email: nikolenielsen[at]swin.edu.au
The star formation history of the universe reveals that galaxies most actively build their stellar mass at “cosmic noon” (z=1-3). The gas accreting onto galaxies to drive their construction and the resulting metal-enriched material ejected from these galaxies due to feedback must pass through the circumgalactic medium (CGM). The CGM is a massive reservoir of diffuse, multiphase gas out to ~200 kpc and is the interface between the intergalactic medium and the galaxy. While the CGM is well-studied at z<1, little attention has been paid to the reservoir when star formation is most active, due to the difficulty in identifying host galaxies at cosmic noon. The installation of the Keck Cosmic Web Imager (KCWI), a sensitive integral field spectrograph, on Keck II has opened a new window to quickly identify galaxies via their Lyman alpha emission at cosmic noon as well as to directly image the CGM in emission. I will introduce two new surveys with KCWI aiming to study the CGM in (1) absorpti
on around galaxies at z=2-3 and (2) emission around local starbursting galaxies (cosmic noon analogues). These surveys are still in progress, but first results reveal strong outflows at cosmic noon and tantalising sub-kiloparsec structure in the CGM.
Wednesday 05 May 2021 @ 12:00 p.m., David Caro building, Level 2, Hercus Theatre (+Zoom)
Dr Steven Murray, Arizona State University; Email: steven.g.murray[at]asu.edu
21cm cosmology is growing in momentum. New low-frequency radio telescopes able to probe the neutral hydrogen in the high-redshift Universe (z~6-30) come in two flavours: single-antennas that probe the average thermal history of the Universe (such as EDGES, SARAS and REACH), and interferometers that measure the spatial fluctuations of 21cm emission (such as HERA, MWA and SKA).
Both come with an extraordinary challenge: bright foregrounds amplify small spectral “features” in the instrument, obscuring the background signal unless calibrated to one part in 10^5. Accounting for these effects is susceptible to inadvertant removal of part of the signal, which has led to several retractions of published upper-limits over the past decade. Add to this the extremely surprising results from EDGES in 2018, and we must ask: how much can we trust the results of 21cm experiments, and how can we build confidence amongst the community?
In this talk, I will discuss my role in answering
these questions with two current 21cm experiments — EDGES and HERA.
EDGES is working to verify its result from 2018 using new and improved data and improved analysis techniques. I will describe our new effort to forward-model systematics, starting with receiver calibration and simple models for the antenna reflection coefficients, showing the effects of propagating their full correlated uncertainties on the cosmological estimates.
Concerning HERA, I will report on the work of the Validation team (Aguirre et al., 2021), in support of our recent first upper limit (Kern et al., 2021). We produced a sophisticated end-to-end simulation of the full observation, including thermal noise, realistic foregrounds and many instrumental systematics. This simulation was processed with the exact analysis pipeline used for the data. I will discuss our philosophy and findings, with special regards for future improvements.
Wednesday 21 Apr 2021 @ 12:00 p.m., David Caro building, Level 2, Hercus Theatre (+Zoom)
Dr Jielai Zhang, Swinburne University; Email: jielaizhang[at]swin.edu.au
Fast radio bursts (FRBs) are millisecond bursts in the radio, so bright that we observe them in distant galaxies at a rate of over 1000/day over the whole sky with large radio facilities. Despite their frequency and high energy output, what causes these bursts have eluded astronomers since their discovery over a decade ago. FRBs may result from magnetar bursts, binary neutron star mergers (producing kilonovae), neutron stars collapsing to black holes (blitzars) or several other theories. Information on emission coherent with the radio burst in other wavelengths can help reveal the physical processes that create these bursts. I present results from an observational program that can do this called the Deeper Faster Wider (DWF) program. A key part of the DWF program is coordinating ~10 multi-wavelength observatories to perform deep, wide-field, fast cadence observations on the same field simultaneously to collect possible imaging on fast-evolving transients before they fade. Important
ly, DWF can collect data before, during and after fast transients. Typically, a DWF observing run goes for a week. In particular, I present results from DWF operation run 8 (DWF-O8). During DWF-O8, two FRBs were detected with the Murriyang Radio Telescope (formerly known as the Parkes Radio Telescope). Simultaneously observing with Murriayng was the Neil Gehrels Swift Observatory , Hard X-ray Modulation Telescope, AstroSat, the Korea Microlensing Telescope Network, the Huntsman Telescope, Murriyang and the Molonglo Observatory Synthesis Telescope, amongst others.
Wednesday 24 Mar 2021 @ 12:00 p.m., David Caro building, Level 2, Hercus Theatre (+Zoom)
Dr Nicha Leethochawalit, University of Melbourne; Email: firstname.lastname@example.org
Having accurate completeness functions (and/or determining the survey effective volume) is crucial to the determination of the rest-frame ultraviolet luminosity functions (UVLFs) all the way back to the epoch of reionization. Most studies use injection-recovery simulations to determine completeness functions. Although conceptually the same, these simulations have subtle but important differences in their definition of the completeness function across existing studies. In turn, this requires implementation of different methods to obtain the final determination of the UVLFs. Here, we discuss the advantages and limitations of existing methods using a reference set of mock observations, and then compare the methods when applied to the same set of Hubble Legacy Field (HLF) images. We find that some methods may suffer limitations in a presence of substantial photometric scatter and/or steep luminosity functions.
Wednesday 17 Mar 2021 @ 12:00 p.m., David Caro building, Level 2, Hercus Theatre (+Zoom) Prof. David Jamieson, University of Melbourne Email: email@example.com
Galileo’s prolific letters to friends, colleagues, patrons and other associates are valuable treatises in their own right. A letter he wrote on 21 December 1613 to a former student in Prague sets out his forthright views on the relationship between religious doctrine and science. Galileo’s letter found its way into the hands of the Inquisition in Rome and this ultimately led to Galileo’s conviction of “vehement suspicion of heresy”. Galileo must have realised his letter would cause trouble because he claimed the letter passed to the authorities in Rome had been altered by malevolent forces out to damage him and strengthen their case for heresy. He released a new version of the letter with much less inflammatory language which he claimed was the original. In a sensational discovery in the library of the Royal Society in London UK, Galileo’s claim of alteration is shown to be false. Incorrectly filed for 250 years, the original of the inflammatory letter was accidentally rediscov
ered in 2018, with edits in Galileo’s own handwriting to tone down the language. This is a remarkable piece of history about a physicist facing dire consequences at the hands of the authorities. A particular passage in the letter has captured my attention. Galileo wrote “This (scientific knowledge) applies especially to those sciences about which one can read only very small phrases and scattered conclusions in the Scripture as is particularly the case for astronomy, of which it contains such a small portion that one does not even find in it the names of all the planets.” I will link this statement back to Galileo’s observations of the planet Neptune that occurred in December 1612 to January 1613 just on one year before he wrote his inflammatory letter. We may be able to glean new insights into his thinking at the time.
Tuesday 08 Dec 2020 @ 12:00 p.m., Zoom colloquium
Mahsa Rahimi, University of Melbourne (Completion Seminar) Email: firstname.lastname@example.org
Wednesday December 2nd 2020 @12pm, Zoom Colloquium
Dr Sam Vaughan The University of Sydney
Nearby galaxies can be divided into two broad categories: those which have blue colours, disc-like morphologies and are forming stars; and those which are red, have spheroidal morphologies and have ceased their star formation. Explaining why this is the case is a key challenge of galaxy evolution theories, but a comprehensive theory of what causes galaxies to quench their star formation is still missing. I will discuss a toy model of quenching which successfully reproduces a number of important differences between quiescent and star-forming galaxies at redshift 0, including their different mass-metallicity relations and mass-size planes. This model was born out of my studies of stellar metallicities in the SAMI galaxy survey, and I will also give a brief summary of my metallicity measurements and some of the powerful statistical tools I’ve used in my analysis.
Wednesday November 25th 2020 @12pm, Zoom Colloquium
Dr Neil Goeckner-Wald KIPAC
Precision measurements of the anisotropies in the Cosmic Microwave Background (CMB) have become one of the cornerstones of modern cosmology. One major objective of current CMB experiments is the discovery of a stochastic background of gravitational waves generically produced by theories of cosmic inflation. Such a signal could be detected as an excess of odd-parity polarization in the CMB at degree angular scales. The South Pole Observatory is a coordinated effort between the South Pole Telescope (SPT) and the BICEP/Keck collaborations that will use the synergies of the two experiments to search for this signal in the presence of galactic and gravitational lensing foregrounds with unprecedented sensitivity. In this talk I will discuss some recent and upcoming results from both projects focusing on the search for inflationary gravitational waves in the CMB.
Wednesday November 18th 2020 @12pm, Zoom Colloquium
Prof Chris Tinney UNSW
Breakthrough discoveries in astronomy invariably come through one of two routes – applying established techniques to new classes of objects discovered from new classes of surveys, or pushing established techniques to new levels of precision to make available previously unexplored observational phase space. Examples of the former include the discovery of T and Y-class brown dwarfs from surveys like 2MASS or WISE, or higher and higher redshift QSOs from larger and larger surveys.
Opening new phase space through higher measurement precision has been particularly prominent lately – exoplanets being first discovered by increasing precise Doppler measurements, more exoplanets being discovered by increasing precise photometry from space, or gravitation waves being confirmed by increasingly precise strain meters.
The Veloce instrument on the AAT seeks to push the boundaries of increasingly precise Doppler velocity measurement at a fraction of the cost of competing instruments. I’ll describe what it takes to make your instrument more precise, at lower cost, than other leading brands.
Wednesday November 11th 2020 @12pm, Zoom Colloquium
Dr Jordan Mirocha McGill University
A relatively simple model has emerged in recent years that can explain the bulk properties of high redshift galaxies: star formation is fueled by the inflow of pristine material from the intergalactic medium, and proceeds with an efficiency that depends strongly on the mass of a galaxy’s parent dark matter halo but not obviously on cosmic time. We generally interpret this mass dependence as a signature of stellar feedback despite the fact that stellar feedback models also predict time evolution in the star formation efficiency. In this talk, I’ll focus on this apparent tension, and show that to remain in agreement with observations, competing feedback scenarios require qualitatively different assumptions about the properties of dust and the duty cycle of star formation in galaxies. As a result, I’ll discuss the prospects for distinguishing models based on the ‘dustiness’ and ‘burstiness’ of galaxies found in upcoming galaxy surveys with JWST and ALMA, and potentially via constraints on reionization from future 21-cm experiments.
Wednesday October 21st 2020 @12pm, Zoom Colloquium
Poojan Agrawal Swinburne University
Recent observations of galaxies and star clusters have highlighted the need for systematic studies dedicated to exploring the impact of uncertain parameters of stellar evolution on the properties of stellar populations. While the use of fitting formulae to stellar tracks remains a popular choice for modelling stellar evolution in population synthesis codes, they are not adaptable to changes in the stellar tracks. In this talk, I will present results from an alternative approach, METISSE, which uses interpolation between sets of pre-computed stellar tracks to approximate evolution parameters for a population of stars. It can readily make use of stellar models computed with different stellar evolution codes and can compare their predictions for populations of stars. Using METISSE with the data from two different stellar evolution codes, I will show how different physical ingredients used in the evolution of massive stars, such as the treatment of their radiation dominated envelopes, can lead to differences in their evolutionary properties. These differences are important as they can help us account for observations of the stellar populations and the formation of gravitational wave progenitors.
Wednesday October 14th 2020 @12pm, Zoom Colloquium
Dorota Bayer Swinburne University
While a direct detection of the dark-matter particle remains very challenging, the nature of dark matter can potentially be constrained indirectly — by comparing the properties of substructure in galactic haloes with predictions from the phenomenological dark-matter models, such as the cold, warm or hot dark matter. Whereas these models are practically indistinguishable with respect to the predicted characteristics of high-mass substructure, the critical difference lies in the abundance and statistical properties of low-mass galactic substructure. Galaxy-galaxy strong gravitational lensing provides a unique opportunity to search for gravitational signatures of such low-mass substructure in lens galaxies beyond the Local Group. In this talk, I will present a novel approach to observationally constrain the statistical nature of low-mass sub-galactic structure in the inner regions of massive elliptical lens galaxies, based on the power spectrum of surface-brightness anomalies measured in highly-magnified galaxy-scale Einstein rings and gravitational arcs. A future comparison of these results with the predictions from hydrodynamical simulations might either verify the CDM paradigm or require its substantial revision.
Wednesday September 30th 2020 @12pm, Zoom Colloquium
Dr Lilian Garratt-Smithson University of Western Australia
Simulations are now allowing us to probe the scales of the CGM (circumgalactic medium) around galaxies in order to look at the influence of realistic galaxy formation processes. However, it is apparent that the properties of the multi-phase CGM are not yet converged in simulations (e.g. Van de Voort et al., 2019; Hummels et al., 2019), hence their reliability to make predictions is still in question. It is also clear the CGM plays a key role in the evolution of a galaxy; it is a supply of gas for star formation and a key site for feedback-generated outflows, along with the recycling of baryons (for a recent review see Tumlinson et al., 2017).
During this talk I will discuss the results of my recent paper (Garratt-Smithson et al. 2020 – available on astro-ph) and in particular the significant mass of HI seen in the CGM of EAGLE galaxies between redshift 2 and 0. I will explore the physical conditions of this HI, and discuss whether or not we can constrain the fraction existing in the cold neutral medium. I will also discuss the physical processes we can constrain by studying the detailed properties of this CGM HI gas; in particular I link my results back to AGN and stellar feedback, along with how this is modelled in simulations. Finally, I will discuss my current projects, which aim to explore the CGM in greater detail using a mix of idealised and cosmological zoom simulations.
Wednesday September 16th 2020 @12pm, Zoom Colloquium
Pol Gurri Perez Swinburne University
Weak gravitational lensing provides an observational avenue to determine the relation between the halo mass and stellar mass of a galaxy. While we expect two galaxies with the same stellar mass to have different halos, at the moment, existing weak lensing studies are only sensitive to an average halo mass. In this talk, I will present an end-to-end methodology to measure the effects of weak lensing on individual galaxy-galaxy systems exploiting their kinematic information. I will present the results of analysing 21 weakly lensed systems and present ways to overcome weak lensing limitations and be sensitive to the dispersion in halo masses.
Wednesday September 9th 2020 @12pm, Zoom Colloquium
Dr Rob Bassett Swinburne University
Understanding the sources responsible for driving reionization has been a major goal in astrophysics for many years. One critical measurement required is the ionizing (or Lyman continuum, LyC) escape fraction from observed galaxy samples. A major difficulty arises from the level of transmission of LyC through the intergalactic medium (IGM), an unknown (but essential) quantity in the calculation of LyC escape from individual sources. The typical method is to assume an average transmission value based on consideration of HI column density distribution functions, but is this appropriate? In general, observational surveys at high redshift are strongly biased towards the brightest objects as these are the easiest to detect. Given the fact that LyC emission is remarkably faint, we should expect to only detect those galaxies with the highest emergent LyC flux. This, in turn, suggests that detections of LyC in surveys will be biased towards IGM sightlines with higher than average transmission of ionizing photons. In this talk I discuss the quantification of this IGM transmission bias for LyC detections and explore the implications when considering the recovered LyC escape values from current surveys. Careful consideration of such biases will be critical in understanding how LyC escape depends on galaxy properties, which ultimately colours our understanding of how reionization proceeds.
Wednesday August 26th 2020 @12pm, Zoom Colloquium
Dr Colin Jacobs Swinburne University
Neural Networks are finding increasing use in many areas of astronomy, but often act as “black boxes”. Many techniques exist to probe in the internals of neural networks but not all are relevant to scientists. In this talk I discuss some of the techniques developed in computer vision to investigate what neural networks are learning, and discuss some of their benefits and problems when applied to astronomy. I introduce a simple technique to probe what neural networks have learned and apply it to networks trained to find strong gravitational lenses.
Wednesday July 22nd 2020 @12pm, Zoom Colloquium
Melanie Hampel Monash University
The quest for the origin of the elements in the universe combines different fields of physics and astronomy, from the smallest scales of nuclear reactions to large scales of giant stars. To understand the chemical history of our universe the abundances of elements heavier than iron are observed in the photospheres of old stars. The vast majority of heavy elements are formed by the slow (s) and rapid (r) neutron-capture processes. However, some observations of heavy-element abundance patterns of old stars are incompatible with either of these processes or even a combination of both.
I will show that these puzzling heavy-element patterns can be explained as the result of a separate neutron-capture process operating at neutron densities intermediate to the s and r process: the i process. Comparing theoretical predictions of i-process nucleosynthesis with the observed abundance patterns gives us new insights into uncertain phases of stellar evolution and will ultimately help us understand the origin of the elements in our universe.
Wednesday June 17th 2020 @12pm, Zoom Colloquium
Nikhil Sarin Monash University
The first neutron star merger observed with gravitational waves and in electromagnetic radiation confirmed that binary neutron star mergers are the progenitors of at least some short gamma-ray bursts. The multi-messenger observations have been used to a probe a lot of fundamental physics, however, despite the wealth of observations the fate of the remnant of GW170817 is still uncertain. I will give an overview of binary neutron star mergers focussing on the nature of the remnant from observations of short gamma-ray bursts and theoretical considerations. I will discuss the implications of these observations on the nuclear equation of state, neutron star dynamics and gamma-ray bursts.
Wednesday May 6th 2020 @12pm, Zoom Colloquium
Prof. Chris Blake Swinburne University
The physics of gravity on cosmological scales affects both the rate of assembly of galaxy large-scale structure, and the gravitational lensing of background light through this cosmic web. By comparing the amplitude of these different observational signatures, we can construct tests that can distinguish General Relativity from its potential modifications. We use the latest weak gravitational lensing dataset from the Kilo-Degree Survey, KiDS-1000, in conjunction with overlapping galaxy redshift surveys, to perform the most accurate existing amplitude ratio test on projected scales up to 100 Mpc/h. The scale-independence and redshift-dependence of these measurements are consistent with the theoretical expectation of General Relativity in a Universe with matter density Omega_m = 0.27 +/- 0.04. We demonstrate that our results are robust against different analysis choices, including schemes for correcting the effects of source photometric redshift errors.
(postponed due to Covid-19 pandemic social distancing measures) , level 7 Conference Room, David Caro Building
Dr Katie Auchettl The University of Melbourne
One of the most uncertain aspects related to our understanding of the end points of stellar evolution is the link between the progenitor star and the nature of the supernova explosion that the progenitor will undergo. Even though hundreds of supernovae are discovered each year by optical surveys, these sources are usually too distance to resolve the ejecta and immediate surrounding of the exploded star. However, due to their long lifetimes and close proximity, supernova remnants which are the long lived structures that results from the supernova explosion of either a white dwarf or a massive star, provide us with a unique opportunity to study supernova explosion and dynamics up close and in detail. In this talk, I will highlight some recent advances that have been made in the understanding of supernovae and their progenitors using wavelength studies of supernova remnants.
Wed 11th March 2020 @2:15 PM, level 7 Conference Room, David Caro Building
Dr Matus Rybak Leiden University
Sub-millimeter galaxies (SMGs) play a key role in the early Universe and are an important laboratory for understanding the most extreme star formation. However, our understanding of SMGs — what drives their intense star-formation? what are the physical properties of their star-forming ISM? – requires high angular resolution, long unavailable in mm/FIR wavelengths.
The start of ALMA operations in 2011 was a quantum leap from barely resolved SMGs to kpc-scales studies, matching or even exceeding the resolution achieved for present-day galaxies. A further order-of-magnitude jump in resolution – down to ~100-parcsec scales – has been provided by strong gravitational lensing.
I will showcase recent results from resolved multi-tracer (FIR, CO, C+) studies of dust and gas in z>2 SMGs at (k)pc resolution. Combining the superb angular resolution and high-frequency capabilities of ALMA, gravitational lensing and radiative transfer modelling, our results provide an unprecedented view of the conditions in these extreme star factories down to 50-pc scales .
Wed 4th March 2020 @12:00 PM, level 7 Conference Room, David Caro Building
Dr Camila Correa University of Amsterdam
In this talk I will summarise recent results of the dependence of the galaxy stellar-to-halo mass relation on galaxy morphology. We use data from the Sloan Digital Sky Survey DR7 with morphological classifications from Galaxy Zoo, and also compare with the EAGLE cosmological simulation, to draw a coherent physical picture of the different evolutionary paths of discs and ellipticals. I will also explore possible scenarios of galaxies undergoing morphological transformation and quenching. To finalise I will discuss the limitations of current simulations such as EAGLE, and introduce the ongoing simulation project of EAGLE-2.
Wed 26th Feb 2020 @12:00 PM, level 7 Conference Room, David Caro Building
Coen Neijssel University of Birmingham
Population synthesis codes enable us to simulate large populations of massive stars to compare to different types of observations. In this talk I will focus on the predictions for black hole masses both in high mass X-ray binaries and gravitational wave mergers. I will give a brief overview of basic stellar evolution and the prediction of remnant masses in the context of rapid population synthesis codes. Binary evolution can significantly alter the evolution of stars through events such as mass transfer and supernovae. I show what we believe is the most common formation channel for the binary black mergers we detect with current gravitational wave detectors. I will try to highlight what the critical assumptions are and which newer observations might contest previous results of the population synthesis community
Wed 19th Feb 2020 @12:00 PM, level 7 Conference Room, David Caro Building
Prof. Sukyoung Yi Yonsei University
I will present new results on the formation and fate of discs of spiral galaxies from the New Horizon and Galactica simulations. The high-resolution simulations (>40pc) reveal the history of disc settling, build-up, and fading in great detail and provide hints to the origin of the thin and thick discs.
Wed 5th Feb 2020 @12:00 PM, level 7 Conference Room, David Caro Building
Dr Chiaki Kobayashi University of Hertfordshire
Stars are fossils that retain the history of their host galaxies. At the end of their lives, some explode as supernovae, producing heavy elements that are distributed into the surrounding interstellar gas. New stars that are created from this gas contain the elements that were produced from the previous generations of stars. From the spatial distribution of elements, it is therefore possible to constrain the star formation and chemical enrichment histories of the galaxies. This approach, Galactic Archaeology, has been popularly used for our Milky Way Galaxy. It can also be applied to external galaxies thanks to the recent and future observations with integral field units (extra-galactic archaeology). My team has been running hydrodynamical simulations from cosmological initial conditions including detailed chemical enrichment. By comparing with observations, I will discuss the roles of metal flows, i.e., gas infall, outflow, radial flow, and stellar migration, in the evolution of Milky Way Galaxy and galaxies in general.
Wed 29th Jan 2020 @12:00 PM, level 7 Conference Room, David Caro Building
Dr James D Rhodes NASA Jet Propulsion Laboratory
The top recommendation for a large space mission in the US 2010 Decadal Survey was the Wide Field Infrared Survey Telescope (WFIRST). Similarities in hardware requirements between proposed dark energy, exoplanet microlensing, and near infrared surveyor missions allowed for a single mission that would accomplish all three goals. The gift of an existing 2.4 meter telescope to NASA by another US government agency allowed for the addition of a coronagraph that will take images and spectra of nearby exoplanets; this instrument will be a technological stepping stone to imaging other Earths in the 2030s. I will give an overview of WFIRST’s proposed instrumentation, science goals, and implementation plan.
Wed 18th Dec 2019 @2:15 PM, level 7 Conference Room, David Caro Building
George Howitt The University of Melbourne (Completion Seminar)
Neutron stars are famously steady rotators, but some occasionally undergo sudden changes in their spin frequency known as glitches. I will discuss the theoretical and observational considerations for the origin of glitches in the superfluid interior of neutron stars, and present the results of simulations which show how interacting superfluid vortices in a model of a neutron star can produce similar behaviour to glitches in pulsars.
Wed 27th Nov 2019 @2:15 PM, level 7 Conference Room, David Caro Building
Dr Serena Vinciguerra Max Planck Institute for Gravitational Physics
Be X-ray binaries (BeXBs) consist of rapidly rotating Be stars with neutron star companions accreting from the emission disk. We compare the observed population of BeXBs in the Small Magellanic Cloud to simulated populations of BeXB-like systems produced with the COMPAS population synthesis code. We focus on the apparently higher minimal mass of Be stars in BeXBs than in the Be population at large. Assuming that BeXBs experienced only dynamical stable mass transfer, their mass distribution suggests that the efficiency of accretion rarely drops below ~30%. We also investigate the observed orbital period distribution and number of observed systems, looking for further constraints on our mass transfer models. Finally, we argue if ultra stripped stars could lead to fast rotating neutron stars in BeXBs. We expect our findings to affect our previous predictions on the population of double compact mergers.
Number of posts found: 148