ORCID Profile
0000-0003-1925-4302
Current Organisation
Los Alamos National Laboratory
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Research Topics
In Research Link Australia (RLA), "Research Topics" refer to ANZSRC FOR and SEO codes. These topics are either sourced from ANZSRC FOR and SEO codes listed in researchers' related grants or generated by a large language model (LLM) based on their publications.
Top 5 Research Topics
ANZSRC Field of Research (FoR)
Astronomical and Space Sciences | Astronomy And Astrophysics | Cosmology and Extragalactic Astronomy | Astronomical and Space Instrumentation | Information Storage, Retrieval And Management | Information Systems Development Methodologies | Galactic Astronomy | Computer Hardware | Neural Networks, Genetic Alogrithms And Fuzzy Logic | Artificial Intelligence and Image Processing | Astronomical and Space Sciences not elsewhere classified | Stellar Astronomy and Planetary Systems | Information Systems | Computer Hardware not elsewhere classified | Quantum Physics not elsewhere classified | Instruments And Techniques | Communications Technologies | Information Systems Organisation | Computer Hardware Not Elsewhere Classified | Microwave and Millimetrewave Theory and Technology | Particle Physics | Global Information Systems
ANZSRC Socio-Economic Objective (SEO)
Physical sciences | Expanding Knowledge in the Physical Sciences | Information processing services | Library and related information services | Expanding Knowledge in Technology | Application tools and system utilities | Technological and organisational innovation | Higher education | Data, image and text equipment | Scientific instrumentation | Information services not elsewhere classified | Information and Communication Services not elsewhere classified | Expanding Knowledge in Engineering | Computer hardware and electronic equipment not elsewhere classified |
Related Links
Publications
Galaxy Groups: Proceedings from a Swinburne University Workshop
Publisher: Cambridge University Press (CUP)
Date: 2005
DOI: 10.1071/AS05030
Abstract: We present the proceedings from a two-day workshop held at Swinburne University on 2005 May 24–25. The workshop participants highlighted current Australian research on both theoretical and observational aspects of galaxy groups. These proceedings include short one-page summaries of a number of the talks presented at the workshop. The talks presented ranged from reconciling N -body simulations with observations, to the Hı content of galaxies in groups and the existence of ‘dark galaxies’. The formation and existence of ultra-compact dwarfs in groups, and a new supergroup in Eridanus were also discussed.
The SAMI Galaxy Survey: The cluster redshift survey, target selection and cluster properties
Publisher: Oxford University Press (OUP)
Date: 08-03-2017
DOI: 10.1093/MNRAS/STX562
Galaxy and Mass Assembly (GAMA): formation and growth of elliptical galaxies in the group environment
Publisher: Oxford University Press (OUP)
Date: 22-02-2017
DOI: 10.1093/MNRAS/STX441
Galaxy And Mass Assembly (GAMA): galaxy environments and star formation rate variations
Publisher: Oxford University Press (OUP)
Date: 06-06-2012
Evidence for a nonuniform initial mass function in the local universe
Publisher: American Astronomical Society
Date: 04-2009
Erratum: Choirs, H i galaxy groups: catalogue and detection of star-forming dwarf group members
Publisher: Oxford University Press (OUP)
Date: 21-07-2017
The WiggleZ Dark Energy Survey: Direct constraints on blue galaxy intrinsic alignments at intermediate redshifts
Publisher: Oxford University Press (OUP)
Date: 05-10-2011
AN UPPER LIMIT TO THE DRY MERGER RATE AT ⟨z⟩ ∼ 0.55
Publisher: American Astronomical Society
Date: 14-01-2010
Using a complete spectroscopic survey to find red quasars and test the KX method
Publisher: Oxford University Press (OUP)
Date: 10-12-2007
The WiggleZ Dark Energy Survey: Survey design and first data release
Publisher: Oxford University Press (OUP)
Date: 21-01-2010
Galaxy And Mass Assembly (GAMA): the unimodal nature of the dwarf galaxy population
Publisher: Oxford University Press (OUP)
Date: 02-12-2014
The spectra of red quasars
Publisher: Cambridge University Press (CUP)
Date: 2001
DOI: 10.1071/AS01039
Abstract: We measure the spectral properties of a representative sub-s le of 187 quasars, drawn from the Parkes Half-Jansky, Flat-radio-spectrum S le (PHFS). Quasars with a wide range of rest-frame optical/UV continuum slopes are included in the analysis: their colours range over 2 B – K 7. We present composite spectra of red and blue sub-s les of the PHFS quasars, and tabulate their emission line properties. The median Hβ and [O III] emission line equivalent widths of the red quasar sub-s le are a factor of ten weaker than those of the blue quasar sub-s le. No significant differences are seen between the equivalent width distributions of the C IV, C III] and Mg II lines. Both the colours and the emission line equivalent widths of the red quasars can be explained by the addition of a featureless red synchrotron continuum component to an otherwise normal blue quasar spectrum. The red synchrotron component must have a spectrum at least as red as a power-law of the form F υ α υ −2.8 . The relative strengths of the blue and red components span two orders of magnitude at rest-frame 500 nm. The blue component is weaker relative to the red component in low optical luminosity sources. This suggests that the fraction of accretion energy going into optical emission from the jet is greater in lowluminosity quasars. This correlation between colour and luminosity may be of use in cosmological distance scale work. This synchrotron model does not, however, fit ˜10% of the quasars, which have both red colours and high equivalent width emission lines.We hypothesise that these red, strong-lined quasars have intrinsically weak Big Blue Bumps. There is no discontinuity in spectral properties between the BL Lac objects in our s le and the other quasars. BL Lac objects appear to be the red, low equivalent width tail of a continuous distribution. The synchrotron emission component only dominates the spectrum at longer wavelengths, so existing BL Lac surveys will be biased against high redshift objects. This will affect measurements of BL Lac evolution. The blue PHFS quasars have significantly higher equivalent width C IV, Hβ and [O III] emission than a matched s le of optically selected QSOs.
Examination of the α-ω two-phase shock-induced microstructure in zirconium and titanium
Publisher: Author(s)
Date: 2017
DOI: 10.1063/1.4971658
The WiggleZ Dark Energy Survey: the growth rate of cosmic structure since redshift z=0.9
Publisher: Oxford University Press (OUP)
Date: 07-06-2011
The WiggleZ Dark Energy Survey: testing the cosmological model with baryon acoustic oscillations at z= 0.6
Publisher: Oxford University Press (OUP)
Date: 23-06-2011
The WiggleZ Dark Energy Survey: constraining galaxy bias and cosmic growth with three-point correlation functions
Publisher: Oxford University Press (OUP)
Date: 24-05-2013
DOI: 10.1093/MNRAS/STT520
The WiggleZ Dark Energy Survey: joint measurements of the expansion and growth history atz< 1
Publisher: Oxford University Press (OUP)
Date: 19-07-2012
The WiggleZ dark energy survey: The selection function and z = 0.6 galaxy power spectrum
Publisher: Oxford University Press (OUP)
Date: 05-2010
The WiggleZ Dark Energy Survey: probing the epoch of radiation domination using large-scale structure
Publisher: Oxford University Press (OUP)
Date: 04-01-2013
DOI: 10.1093/MNRAS/STS431
GAMA/WiggleZ: the 1.4 GHz radio luminosity functions of high- and low-excitation radio galaxies and their redshift evolution toz= 0.75
Publisher: Oxford University Press (OUP)
Date: 20-04-2016
DOI: 10.1093/MNRAS/STW910
The stellar masses of ̃ 40 000 UV selected Galaxies from the WiggleZ survey at 0.3
Publisher:
Oxford University Press (OUP)
Date:
20-03-2013
DOI:
10.1093/MNRAS/STT320
Publisher: Oxford University Press (OUP)
Date: 20-03-2013
DOI: 10.1093/MNRAS/STT320
The neutral hydrogen properties of galaxies in gas-rich groups
Publisher: Oxford University Press (OUP)
Date: 29-12-2018
The SAMI Galaxy Survey: Cubism and covariance, putting round pegs into square holes
Publisher: Oxford University Press (OUP)
Date: 20-11-2015
The WiggleZ Dark Energy Survey: improved distance measurements to z = 1 with reconstruction of the baryonic acoustic feature
Publisher: Oxford University Press (OUP)
Date: 31-05-2014
DOI: 10.1093/MNRAS/STU778
Testing the tidal stripping scenario of ultracompact dwarf galaxy formation by using internal properties
Publisher: Oxford University Press (OUP)
Date: 02-07-2021
Abstract: We use the hydrodynamical EAGLE simulation to test if ultracompact dwarf galaxies (UCDs) can form by tidal stripping by predicting the ages and metallicities of tidally stripped galaxy nuclei in massive galaxy clusters, and compare these results to compiled observations of age and metallicities of observed UCDs. We further calculate the colours of our s le of simulated stripped nuclei using single stellar population models and compare these colours to observations of UCDs in the Virgo Cluster. We find that the ages of observed UCDs are consistent with simulated stripped nuclei, with both groups of objects having a mean age & Gyr. Both stripped nuclei and UCDs follow a similar mass–metallicity relationship, and the metallicities of observed UCDs are consistent with those of simulated stripped nuclei for objects with M & 107 M⊙. The colours of observed UCDs are also consistent with our simulated stripped nuclei, for objects with M & 107 M⊙, with more massive objects being redder. We find that the colours of stripped nuclei exhibit a bimodal red and blue distribution that can be explained by the dependency of colour on age and metallicity, and by the mass–colour relation. We additionally find that our low-mass stripped nuclei s le is consistent with the colour of blue globular clusters. We conclude that the internal properties of simulated nuclei support the tidal stripping model of UCD formation.
Erratum: The stellar masses of ̃40 000 UV-selected galaxies from the WiggleZ survey at 0.3 < z < 1.0: analogues of Lyman break galaxies?
Publisher: Oxford University Press (OUP)
Date: 15-12-2015
The 2df SDSS LRG and QSO survey: evolution of the luminosity function of luminous red galaxies toz= 0.6
Publisher: Oxford University Press (OUP)
Date: 21-10-2006
The 2dF-SDSS LRG and QSO Survey: the LRG 2-point correlation function and redshift-space distortions
Publisher: Oxford University Press (OUP)
Date: 10-2007
The WiggleZ Dark Energy Survey: Final data release and cosmological results
Publisher: American Physical Society (APS)
Date: 16-11-2012
The WiggleZ Dark Energy Survey: High-resolution kinematics of luminous star-forming galaxies
Publisher: Oxford University Press (OUP)
Date: 19-09-2011
The SAMI Galaxy Survey
Publisher: Oxford University Press (OUP)
Date: 08-08-2016
The SAMI Galaxy Survey: instrument specification and target selection
Publisher: Oxford University Press (OUP)
Date: 13-01-2015
Galaxy And Mass Assembly: evolution of the Hα luminosity function and star formation rate density up to z < 0.35
Publisher: Oxford University Press (OUP)
Date: 29-06-2013
DOI: 10.1093/MNRAS/STT890
Foreword
Publisher: Springer Science and Business Media LLC
Date: 26-09-2014
A LARGE POPULATION OF ULTRA-COMPACT DWARFS AND BRIGHT INTRACLUSTER GLOBULARS IN THE FORNAX CLUSTER
Publisher: American Astronomical Society
Date: 19-12-2008
The 2dF-SDSS LRG and QSO Survey: the spectroscopic QSO catalogue
Publisher: Oxford University Press (OUP)
Date: 2009
WiggleZ Dark Energy Survey: Cosmological neutrino mass constraint from blue high-redshift galaxies
Publisher: American Physical Society (APS)
Date: 23-04-2012
Galaxy And Mass Assembly (GAMA): Data Release 4 and the z < 0.1 total and z < 0.08 morphological galaxy stellar mass functions
Publisher: Oxford University Press (OUP)
Date: 02-03-2022
Abstract: In Galaxy And Mass Assembly Data Release 4 (GAMA DR4), we make available our full spectroscopic redshift s le. This includes 248 682 galaxy spectra, and, in combination with earlier surveys, results in 330 542 redshifts across five sky regions covering ∼250 deg2. The redshift density, is the highest available over such a sustained area, has exceptionally high completeness (95 per cent to rKiDS = 19.65 mag), and is well-suited for the study of galaxy mergers, galaxy groups, and the low redshift (z & 0.25) galaxy population. DR4 includes 32 value-added tables or Data Management Units (DMUs) that provide a number of measured and derived data products including GALEX, ESO KiDS, ESO VIKING, WISE, and HerschelSpace Observatory imaging. Within this release, we provide visual morphologies for 15 330 galaxies to z & 0.08, photometric redshift estimates for all 18 million objects to rKiDS ∼ 25 mag, and stellar velocity dispersions for 111 830 galaxies. We conclude by deriving the total galaxy stellar mass function (GSMF) and its sub- ision by morphological class (elliptical, compact-bulge and disc, diffuse-bulge and disc, and disc only). This extends our previous measurement of the total GSMF down to 106.75 M$_{\\odot } \\, h_{70}^{-2}$ and we find a total stellar mass density of ρ* = (2.97 ± 0.04) × 108 M$_{\\odot } \\, h_{70}$ Mpc−3 or $\\Omega _*=(2.17 \\pm 0.03) \\times 10^{-3} \\, h_{70}^{-1}$. We conclude that at z & 0.1, the Universe has converted 4.9 ± 0.1 per cent of the baryonic mass implied by big bang Nucleosynthesis into stars that are gravitationally bound within the galaxy population.
The HIPASS catalogue - III. Optical counterparts and isolated dark galaxies
Publisher: Oxford University Press (OUP)
Date: 07-2005
The 2dF-SDSS LRG and QSO (2SLAQ) Luminous Red Galaxy Survey
Publisher: Oxford University Press (OUP)
Date: 11-10-2006
Kinematics of dwarf galaxies in gas-rich groups, and the survival and detectability of tidal dwarf galaxies
Publisher: Oxford University Press (OUP)
Date: 23-11-2015
Galaxy tagging: photometric redshift refinement and group richness enhancement
Publisher: Oxford University Press (OUP)
Date: 18-06-2018
Confronting cold dark matter predictions with observed galaxy rotations
Publisher: American Astronomical Society
Date: 15-03-2013
Near-identical star formation rate densities from Hα and FUV at redshift zero
Publisher: Oxford University Press (OUP)
Date: 12-06-2018
No evidence for intermediate-mass black holes in the globular clusters ω Cen and NGC 6624
Publisher: Oxford University Press (OUP)
Date: 27-07-2019
Abstract: We compare the results of a large grid of N-body simulations with the surface brightness and velocity dispersion profiles of the globular clusters ω Cen and NGC 6624. Our models include clusters with varying stellar-mass black hole retention fractions and varying masses of a central intermediate-mass black hole (IMBH). We find that an $\\sim 45\\, 000$ M⊙ IMBH, whose presence has been suggested based on the measured velocity dispersion profile of ω Cen, predicts the existence of about 20 fast-moving, m & 0.5 M⊙, main-sequence stars with a (1D) velocity v & 60 km s−1 in the central 20 arcsec of ω Cen. However, no such star is present in the HST/ACS proper motion catalogue of Bellini et al. (2017), strongly ruling out the presence of a massive IMBH in the core of ω Cen. Instead, we find that all available data can be fitted by a model that contains 4.6 per cent of the mass of ω Cen in a centrally concentrated cluster of stellar-mass black holes. We show that this mass fraction in stellar-mass BHs is compatible with the predictions of stellar evolution models of massive stars. We also compare our grid of N-body simulations with NGC 6624, a cluster recently claimed to harbour a 20 000 M⊙ black hole based on timing observations of millisecond pulsars. However, we find that models with MIMBH & 1000 M⊙ IMBHs are incompatible with the observed velocity dispersion and surface brightness profile of NGC 6624, ruling out the presence of a massive IMBH in this cluster. Models without an IMBH provide again an excellent fit to NGC 6624.
The WiggleZ Dark Energy Survey: Galaxy Evolution at 0.25 <= z <= 0.75 Using the Second Red-Sequence Cluster Survey
Publisher: American Astronomical Society
Date: 17-02-2012
The WiggleZ Dark Energy Survey: measuring the cosmic growth rate with the two-point galaxy correlation function
Publisher: Oxford University Press (OUP)
Date: 07-02-2013
DOI: 10.1093/MNRAS/STS608
How Is Science Being Taught? Measuring Evidence-Based Teaching Practices across Undergraduate Science Departments
Publisher: American Society for Cell Biology (ASCB)
Date: 03-2017
Abstract: While there is a wealth of research evidencing the benefits of active-learning approaches, the extent to which these teaching practices are adopted in the sciences is not well known. The aim of this study is to establish an evidential baseline of teaching practices across a bachelor of science degree program at a large research-intensive Australian university. Our purpose is to contribute to knowledge on the adoption levels of evidence-based teaching practices by faculty within a science degree program and inform our science curriculum review in practical terms. We used the Teaching Practices Inventory (TPI) to measure the use of evidence-based teaching approaches in 129 courses (units of study) across 13 departments. We compared the results with those from a Canadian institution to identify areas in need of improvement at our institution. We applied a regression analysis to the data and found that the adoption of evidence-based teaching practices differs by discipline and is higher in first-year classes at our institution. The study demonstrates that the TPI can be used in different institutional contexts and provides data that can inform practice and policy.
THE SAMI GALAXY SURVEY: TOWARD A UNIFIED DYNAMICAL SCALING RELATION FOR GALAXIES OF ALL TYPES
Publisher: American Astronomical Society
Date: 29-10-2014
The Gigaparsec WiggleZ simulations: characterizing scale-dependant bias and associated systematics in growth of structure measurements
Publisher: Oxford University Press (OUP)
Date: 24-03-2015
DOI: 10.1093/MNRAS/STV314
Ultrafast X-ray Diffraction Study of a Shock-Compressed Iron Meteorite above 100 GPa
Publisher: MDPI AG
Date: 26-05-2021
DOI: 10.3390/MIN11060567
Abstract: Natural kamacite s les (Fe92.5Ni7.5) from a fragment of the Gibeon meteorite were studied as a proxy material for terrestrial cores to examine phase transition kinetics under shock compression for a range of different pressures up to 140 GPa. In situ time-resolved X-ray diffraction (XRD) data were collected of a body-centered cubic (bcc) kamacite section that transforms to the high-pressure hexagonal close-packed (hcp) phase with sub-nanosecond temporal resolution. The coarse-grained crystal of kamacite rapidly transformed to highly oriented crystallites of the hcp phase at maximum compression. The hcp phase persisted for as long as 9.5 ns following shock release. Comparing the c/a ratio with previous static and dynamic work on Fe and Fe-rich Fe-Ni alloys, it was found that some shots exhibit a larger than ideal c/a ratio, up to nearly 1.65. This work represents the first time-resolved laser shock compression structural study of a natural iron meteorite, relevant for understanding the dynamic material properties of metallic planetary bodies during impact events and Earth’s core elasticity.
The galaxy morphology–density relation in the EAGLE simulation
Publisher: Oxford University Press (OUP)
Date: 08-12-2022
Abstract: The optical morphology of galaxies is strongly related to galactic environment, with the fraction of early-type galaxies increasing with local galaxy density. In this work, we present the first analysis of the galaxy morphology–density relation in a cosmological hydrodynamical simulation. We use a convolutional neural network, trained on observed galaxies, to perform visual morphological classification of galaxies with stellar masses $M_\\ast \\gt 10^{10} \\, \\rm {M}_{\\odot }$ in the EAGLE simulation into elliptical, lenticular and late-type (spiral/irregular) classes. We find that EAGLE reproduces both the galaxy morphology–density and morphology–mass relations. Using the simulations, we find three key processes that result in the observed morphology–density relation: (i) transformation of disc-dominated galaxies from late-type (spiral) to lenticular galaxies through gas stripping in high-density environments, (ii) formation of lenticular galaxies by merger-induced black hole feedback in low-density environments, and (iii) an increasing fraction of high-mass galaxies, which are more often elliptical galaxies, at higher galactic densities.
The SAMI Galaxy Survey
Publisher: American Astronomical Society
Date: 21-07-2017
The WiggleZ Dark Energy Survey: measuring the cosmic expansion history using the Alcock-Paczynski test and distant supernovae
Publisher: Oxford University Press (OUP)
Date: 04-10-2011
The HIPASS catalogue - I. Data presentation
Publisher: Oxford University Press (OUP)
Date: 06-2004
Searches for ultracompact dwarf galaxies in galaxy groups
Publisher: Oxford University Press (OUP)
Date: 06-06-2007
The SAMI–Fornax Dwarfs Survey I: sample, observations, and the specific stellar angular momentum of dwarf elliptical galaxies
Publisher: Oxford University Press (OUP)
Date: 13-07-2020
Abstract: Dwarf ellipticals are the most common galaxy type in cluster environments however, the challenges associated with their observation mean that their formation mechanisms are still poorly understood. To address this, we present deep integral field observations of a s le of 31 low-mass (107.5 & M⋆ & 109.5 M⊙) early-type galaxies in the Fornax cluster with the SAMI instrument. For 21 galaxies, our observations are sufficiently deep to construct spatially resolved maps of the stellar velocity and velocity dispersion – for the remaining galaxies, we extract global velocities and dispersions from aperture spectra only. From the kinematic maps, we measure the specific stellar angular momentum λR of the lowest mass dE galaxies to date. Combining our observations with early-type galaxy data from the literature spanning a large range in stellar mass, we find that λR decreases towards lower stellar mass, with a corresponding increase in the proportion of slowly rotating galaxies in this regime. The decrease of λR with mass in our s le dE galaxies is consistent with a similar trend seen in somewhat more massive spiral galaxies from the CALIFA survey. This suggests that the degree of dynamical heating required to produce dEs from low-mass starforming progenitors may be relatively modest and consistent with a broad range of formation mechanisms.
Contribution of stripped nuclei to the ultracompact dwarf galaxy population in the Virgo cluster
Publisher: Oxford University Press (OUP)
Date: 03-12-2020
Abstract: We use the hydrodynamical EAGLE simulation to predict the numbers, masses, and radial distributions of tidally stripped galaxy nuclei in massive galaxy clusters, and compare these results to observations of ultracompact dwarf galaxies (UCDs) in the Virgo cluster. We trace the merger trees of galaxies in massive galaxy clusters back in time and determine the numbers and masses of stripped nuclei from galaxies disrupted in mergers. The spatial distribution of stripped nuclei in the simulations is consistent with those of UCDs surrounding massive galaxies in the Virgo cluster. Additionally, the numbers of stripped nuclei are consistent with the numbers of M & 107 M⊙ UCDs around in idual galaxies and in the Virgo cluster as a whole. The mass distributions in this mass range are also consistent. We find that the numbers of stripped nuclei surrounding in idual galaxies correlate better with the stellar or halo mass of in idual galaxies than the total cluster mass. We conclude that most high mass (M & 107 M⊙) UCDs are likely stripped nuclei. It is difficult to draw reliable conclusions about low mass (M & 107 M⊙) UCDs because of observational selection effects. We additionally predict that a few hundred stripped nuclei below a mass of 2 × 106 M⊙ should exist in massive galaxies that will overlap in mass with the globular cluster population. Approximately 1–3 stripped nuclei in the process of forming also exist per massive galaxy.
The Northern HIPASS catalogue - Data presentation, completeness and reliability measures
Publisher: Oxford University Press (OUP)
Date: 10-2006
CHOIRS H I GALAXY GROUPS: THE METALLICITY OF DWARF GALAXIES
Publisher: American Astronomical Society
Date: 23-01-2014
Choirs, H i galaxy groups: catalogue and detection of star-forming dwarf group members
Publisher: Oxford University Press (OUP)
Date: 21-05-2013
DOI: 10.1093/MNRAS/STT747
The 2QDES Pilot: the luminosity and redshift dependence of quasar clustering
Publisher: Oxford University Press (OUP)
Date: 15-03-2016
DOI: 10.1093/MNRAS/STW616
Self-consistent Bulge/Disk/Halo Galaxy Dynamical Modeling Using Integral Field Kinematics
Publisher: American Astronomical Society
Date: 17-11-2017
ERRATUM: “CHOIRS H I GALAXY GROUPS: THE METALLICITY OF DWARF GALAXIES” (2014, ApJ, 782, 35)
Publisher: American Astronomical Society
Date: 16-04-2014
The SAMI Galaxy Survey: the third and final data release
Publisher: Oxford University Press (OUP)
Date: 02-2021
Abstract: We have entered a new era where integral-field spectroscopic surveys of galaxies are sufficiently large to adequately s le large-scale structure over a cosmologically significant volume. This was the primary design goal of the SAMI Galaxy Survey. Here, in Data Release 3, we release data for the full s le of 3068 unique galaxies observed. This includes the SAMI cluster s le of 888 unique galaxies for the first time. For each galaxy, there are two primary spectral cubes covering the blue (370–570 nm) and red (630–740 nm) optical wavelength ranges at spectral resolving power of R = 1808 and 4304, respectively. For each primary cube, we also provide three spatially binned spectral cubes and a set of standardized aperture spectra. For each galaxy, we include complete 2D maps from parametrized fitting to the emission-line and absorption-line spectral data. These maps provide information on the gas ionization and kinematics, stellar kinematics and populations, and more. All data are available online through Australian Astronomical Optics Data Central.
The SAMI–Fornax Dwarfs Survey – II. The Stellar Mass Fundamental Plane and the dark matter fraction of dwarf galaxies
Publisher: Oxford University Press (OUP)
Date: 17-09-2022
Abstract: We explore the kinematic scaling relations of 38 dwarf galaxies in the Fornax Cluster using observations from the SAMI integral field spectrograph. We focus on the Fundamental Plane (FP), defined by the physical properties of the objects (scale length, surface brightness, and velocity dispersion) and the Stellar Mass (Fundamental) Plane, where surface brightness is replaced by stellar mass, and investigate their dynamical-to-stellar-mass ratio. We confirm earlier results that the Fornax dEs are significantly offset above the FP defined by massive, hot stellar systems. For the Stellar Mass (Fundamental) Plane, which shows much lower scatter, we find that young and old dwarf galaxies lie at about the same distance from the plane, all with comparable scatter. We introduce the perpendicular deviation of dwarf galaxies from the Stellar Mass Plane defined by giant early-types as a robust estimate of their DM fraction, and find that the faintest dwarfs are systematically offset above the plane, implying that they have a higher dark matter fraction. This result is confirmed when estimating the dynamical mass of our dEs using a virial mass estimator, tracing the onset of dark matter domination in low mass stellar systems. We find that the position of our galaxies on the Stellar Mass FP agrees with the galaxies in the Local Group. This seems to imply that the processes determining the position of dwarf galaxies on the FP depend on the environment in the same way, whether the galaxy is situated in the Local Group or in the Fornax Cluster.
The 2dF-SDSS LRG and QSO (2SLAQ) Survey: thez< 2.1 quasar luminosity function from 5645 quasars tog= 21.85
Publisher: Oxford University Press (OUP)
Date: 07-2005
Galaxy And Mass Assembly (GAMA): Panchromatic Data Release (far-UV–far-IR) and the low-zenergy budget
Publisher: Oxford University Press (OUP)
Date: 03-12-2015
The SAMI Galaxy Survey: Data Release Two with absorption-line physics value-added products
Publisher: Oxford University Press (OUP)
Date: 31-08-2018
The WiggleZ Dark Energy Survey: the transition to large-scale cosmic homogeneity
Publisher: Oxford University Press (OUP)
Date: 26-07-2012
The WiggleZ Dark Energy Survey: mapping the distance-redshift relation with baryon acoustic oscillations
Publisher: Oxford University Press (OUP)
Date: 04-10-2011
The SAMI Galaxy Survey: Early Data Release
Publisher: Oxford University Press (OUP)
Date: 20-11-2015
The SAMI galaxy survey
Publisher: Oxford University Press (OUP)
Date: 02-07-2020
Abstract: It has been proposed that S0 galaxies are either fading spirals or the result of galaxy mergers. The relative contribution of each pathway and the environments in which they occur remain unknown. Here, we investigate stellar and gas kinematics of 219 S0s in the SAMI Survey to look for signs of multiple formation pathways occurring across the full range of environments. We identify a large range of rotational support in their stellar kinematics, which correspond to ranges in their physical structure. We find that pressure-supported S0s with v/σ below 0.5 tend to be more compact and feature misaligned stellar and gas components, suggesting an external origin for their gas. We postulate that these S0s are consistent with being formed through a merger process. Meanwhile, comparisons of ellipticity, stellar mass, and Sérsic index distributions with spiral galaxies show that the rotationally supported S0s with v/σ above 0.5 are more consistent with a faded spiral origin. In addition, a simulated merger pathway involving a compact elliptical and gas-rich satellite results in an S0 that lies within the pressure-supported group. We conclude that two S0 formation pathways are active, with mergers dominating in isolated galaxies and small groups, and the faded spiral pathway being most prominent in large groups ($10^{13}\\lt \\rm {M_{halo}}\\lt 10^{14}$).
Galaxy And Mass Assembly (GAMA): spectroscopic analysis
Publisher: Oxford University Press (OUP)
Date: 07-02-2013
DOI: 10.1093/MNRAS/STT030
The WiggleZ Dark Energy Survey: final data release and the metallicity of UV-luminous galaxies
Publisher: Oxford University Press (OUP)
Date: 21-11-2018
The HIPASS catalogue - II. Completeness, reliability and parameter accuracy
Publisher: Oxford University Press (OUP)
Date: 06-2004
The WiggleZ Dark Energy Survey: Small-scale clustering of Lyman-break galaxies at z < 1
Publisher: Oxford University Press (OUP)
Date: 05-2009
Galaxy And Mass Assembly (GAMA): galaxy close pairs, mergers and the future fate of stellar mass
Publisher: Oxford University Press (OUP)
Date: 18-09-2014
Galaxy And Mass Assembly: the evolution of the cosmic spectral energy distribution from z = 1 to z = 0
Publisher: Oxford University Press (OUP)
Date: 25-05-2017
The 2dF-SDSS LRG and QSO Survey: evolution of the clustering of luminous red galaxies sincez= 0.6
Publisher: Oxford University Press (OUP)
Date: 07-2008
The 2dF-SDSS LRG and QSO Survey: the star formation histories of luminous red galaxies
Publisher: Oxford University Press (OUP)
Date: 21-11-2006
The SAMI Galaxy Survey: Data Release One with emission-line physics value-added products
Publisher: Oxford University Press (OUP)
Date: 11-12-2017
Measuring the 2D baryon acoustic oscillation signal of galaxies in WiggleZ: cosmological constraints
Publisher: Oxford University Press (OUP)
Date: 23-10-2017
Galaxy and Mass Assembly (GAMA): survey diagnostics and core data release
Publisher: Oxford University Press (OUP)
Date: 02-03-2011
The two formation pathways of S0 galaxies
Publisher: Oxford University Press (OUP)
Date: 30-09-2021
Abstract: Despite their ubiquity throughout the Universe, the formation of S0 galaxies remains uncertain. Recent observations have revealed that S0 galaxies make up a erse population that is difficult to explain with a single formation pathway, suggesting that the picture of how these galaxies form is more complicated than originally envisioned. Here, we take advantage of the latest hydrodynamical cosmological simulations and follow up these studies with an investigation into the formation histories of S0s in IllustrisTNG. We first classify IllustrisTNG galaxies in a way that is fully consistent with the observations, and reproduce the observed photometric and environmental distributions seen for the S0 population. We then trace the formation histories of S0 galaxies back through time, identifying two main distinct pathways: those that experienced gas stripping via group infalls (37 per cent of S0s) or significant merger events (57 per cent). We find that those forming via mergers feature a transient star-forming ring, whose present-day occurrence rate matches observations. We find that these formation pathways together can reproduce the range in rotational support in observed S0s, concluding that there are two main formation pathways for S0 galaxies.
Galaxy And Mass Assembly (GAMA): the effect of close interactions on star formation in galaxies
Publisher: Oxford University Press (OUP)
Date: 08-07-2015
Erratum: Kinematics of dwarf galaxies in gas-rich groups, and the survival and detectability of tidal dwarf galaxies
Publisher: Oxford University Press (OUP)
Date: 14-01-2016
The WiggleZ Dark Energy Survey: star formation in UV-luminous galaxies from their luminosity functions
Publisher: Oxford University Press (OUP)
Date: 09-07-2013
Galaxy And Mass Assembly (GAMA): the life and times of L★ galaxies
Publisher: Oxford University Press (OUP)
Date: 08-03-2013
DOI: 10.1093/MNRAS/STT156
NGC 922 - a new drop-through ring galaxy★
Publisher: Oxford University Press (OUP)
Date: 07-07-2006
Galaxy And Mass Assembly (GAMA): the absence of stellar mass segregation in galaxy groups and consistent predictions from GALFORM and EAGLE simulations
Publisher: Oxford University Press (OUP)
Date: 12-09-2016
Improved constraints on possible variation of physical constants from H I 21-cm and molecular QSO absorption lines
Publisher: Oxford University Press (OUP)
Date: 11-11-2001
The SAMI Galaxy Survey
Publisher: Oxford University Press (OUP)
Date: 16-01-2018
DOI: 10.1093/MNRAS/STY127
The formation pathways of compact elliptical galaxies
Publisher: Oxford University Press (OUP)
Date: 02-08-2023
Abstract: Compact elliptical (cE) galaxies remain an elusively difficult galaxy class to study. Recent observations have suggested that isolated and host-associated cEs have different formation pathways, while simulation studies have also shown different pathways can lead to a cE galaxy. However, a solid link has not been established, and the relative contributions of each pathway in a cosmological context remains unknown. Here, we combine a spatially resolved observational s le of cEs taken from the Sydney-AAO Multi-object Integral field spectrograph Galaxy Survey with a matched s le of galaxies within the IllustrisTNG cosmological simulation to establish an overall picture of how these galaxies form. The observed cEs located near a host galaxy appear redder, smaller, and older than isolated cEs, supporting previous evidence for multiple formation pathways. Tracing the simulated cEs back through time, we find two main formation pathways 32 ± 5 per cent formed via the stripping of a spiral galaxy by a larger host galaxy, while 68 ± 4 per cent formed through a gradual build-up of stellar mass in isolated environments. We confirm that cEs in different environments do indeed form via different pathways, with all isolated cEs in our s le having formed via in situ formation (i.e. none were ejected from a previous host), and 77 ± 6 per cent of host-associated cEs having formed via tidal stripping. Separating them by their formation pathway, we are able to reproduce the observed differences between isolated and host-associated cEs, showing that these differences can be fully explained by the different formation pathways dominating in each environment.
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