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Articles by CSIRO Space
EGUsphere - First demonstration of the combination of observations and datasets from diverse instruments (in a coordinated experiment using KAIRA, EISCAT, GNSS) that enables the extraction of new information about the ionosphere
The plasma of the Earth’s ionosphere introduces effects on radio waves that traverse it. Propagation effects reflect the presence of the bulk ionisation along the ray path as well as the presence of inhomogeneities (or irregularities) in the spatial distribution of the plasma (or electron) density.
Relevance of Murchison Widefield Array Interplanetary Scintillation Observations to Heliospheric Transient Catalogs
1 Introduction Interplanetary scintillation (IPS) is the amplitude and phase scintillation at radio frequencies from compact sources caused by density irregularities in the solar wind (Coles, 1978). IPS has an extensive history of capturing and studying heliospheric structures (Hewish, 1989), such as stream interaction regions (SIR, Dennison & Wiseman, 1968; Hewish & Bravo, 1986).
Measurements of the temperature and $E$-mode polarization of the cosmic microwave background from the full 500-square-degree SPTpol dataset
F. Bianchini27, L. E. Bleem5,2, J. E. Carlstrom2,6,5,1,7, C. L. Chang2,5,1, P. Chaubal28, H. C. Chiang29,30, R. Citron8, C. Corbett Moran31, T. M. Crawford2,1, A. T. Crites2,1,32,33, T. de Haan34,35,36, M. A. Dobbs29,37, D. Dutcher9, W. Everett10, J. Gallicchio2,11, E. M. George38,34, N. Gupta12, N. W. Halverson10,25, G. P. Holder39,40, W. L. Holzapfel34, J. D. Hrubes8, N. Huang34, J. Hubmayr4, K. D. Irwin27,41, L. Knox13, A. T. Lee34,35, D. Li4,27, A. Lowitz1,42, J. J. McMahon2,6,1, J. Montgomery29, T. Natoli1,2,14, J. P. Nibarger4, G. I.
FEASTS: the fate of gas and star formation in interacting galaxies
Galaxies in our Universe are not ideally isolated. A large fraction of them reside in groups and clusters with neighbours at low redshift (e.g. Wetzel et al. 2013). In groups and clusters, central galaxies accrete less massive infalling galaxies. And satellites galaxies themselves also interact and even merge with each other. The cold dark matter ( CDM) cosmology predicts that the halo–halo merger is one of the major channel of mass and structure assembly.
Searching for short-time-scale radio anomalies using non-linear dimensionality reduction techniques
Radio astronomy is a subject full of surprises. From 1933 to 1997, 17 key discoveries in radio astronomy were found (Wilkinson et al. 2004). These discoveries can be divided into two classes: seven were made by testing a theory prediction (these were the ‘known–unknowns’), and 10 were unexpected results found by chance (the ‘unknown–unknowns’) (Norris 2017). One unexpected highlight in the 21st century was the discovery of fast radio bursts (FRBs).
Radio Galaxy Zoo data release 1: 100185 radio source classifications from the FIRST and ATLAS surveys
Radio galaxies, a subset of Active Galactic Nuclei (AGNs), may be single compact structures, simple doubles, or large, multicomponent structures with complex morphologies. Identifying which discrete radio components belong to a single source, and which optical or infrared galaxy is their host, can thus be a complex task.
Discovery of Perun (G329.9-0.5): A New, Young, Galactic SNR
We present the discovery of possibly the youngest Galactic supernova remnant (SNR) with associated pulsar-wind nebula (PWN), which we name Perun (G329.9-0.5).
Discovery of Perun (G329.9−0.5): a new, young, Galactic SNR
Supernova (SN) explosions are one of the most violent and spectacular events in the universe. They occur when massive stars reach the end of their lives and are responsible for most of the chemical enrichment in galaxies (Lee et al. 2009; Mernier et al. 2020). An SN explosion belongs to one of two broad categories.
Probing the magnetised gas distribution in galaxy groups and the cosmic web with POSSUM Faraday Rotation Measures
We present initial results from the Polarisation Sky Survey of the Universe’s Magnetism (POSSUM), analyzing 22,817 Faraday Rotation Measures (RMs) with median uncertainties of 1.2 rad m−2 across 1,520 square degrees to study magnetised gas associated with 55 nearby galaxy groups (z ≲ 0.025) with halo masses between 1012.5 and 1014.0 M .
Probing the magnetized gas distribution in galaxy groups and the cosmic web with POSSUM Faraday rotation measures
Most galaxies in the local universe reside in galaxy groups, which are themselves embedded in the sparse gaseous filaments that form the large-scale structure of the Cosmos (Bond, Kofman & Pogosyan 1996; Eke et al. 2004; Haan & Braun 2014; Rost et al. 2024).
ASKAP reveals the radio tail structure of the Corkscrew Galaxy shaped by its passage through the Abell 3627 cluster
Among the bent tail radio galaxies common in galaxy clusters are some with long, collimated tails (so-called head-tail galaxies) shaped by their interactions with the intracluster medium (ICM). Here we report the discovery of intricate filamentary structure in and beyond the ∼28′ (570 kpc) long, helical radio tail of the Corkscrew Galaxy (1610–60.5, ESO 137-G007), which resides in the X-ray bright cluster Abell 3627 (D = 70 Mpc).
RadioSED I: Bayesian inference of radio SEDs from inhomogeneous surveys
We present here RadioSED, a Bayesian inference framework tailored to modelling and classifying broadband radio spectral energy distributions (SEDs) using only data from publicly-released, large-area surveys. We outline the functionality of RadioSED, with its focus on broadband radio emissions which can trace kiloparsec-scale absorption within both the radio jets and the circumgalactic medium of Active Galactic Nuclei (AGN).
The UTMOST-NS: a fully digital, wide-field transient search facility operating at a centre frequency of 831 MHz
Fast radio transients are extreme events exhibiting brightness variations on ≲ millisecond time-scales in the radio spectrum. They include some of the most interesting astrophysical objects, such as pulsars, magnetars, rotating radio transients, and fast radio bursts (FRBs, Hewish et al. 1968; McLaughlin et al. 2006; Lorimer et al. 2007).
The thousand-pulsar-array programme on MeerKAT XIII: Timing, flux density, rotation measure and dispersion measure timeseries of 597 pulsars
We report here on the timing of 597 pulsars over the last four years with the MeerKAT telescope. We provide Times-of-Arrival, pulsar ephemeris files and per-epoch measurements of the flux density, dispersion measure (DM) and rotation measure (RM) for each pulsar. In addition we use a Gaussian process to model the timing residuals to measure the spin frequency derivative at each epoch. We also report the detection of 11 glitches in 9 individual pulsars.
The Thousand-Pulsar-Array programme on MeerKAT – XIV. On the high linearly polarized pulsar signals
Radhakrishnan & Cooke (1969) first observed the characteristic S-shaped swing of the linear polarization position angle (PPA) across the pulse profile in the Vela pulsar and proposed the rotating vector model (RVM) to explain the observations. In the RVM, the PPA swing results due to an emission mechanism where the linearly polarized emission traces the variation in the dipolar magnetic field line planes.
A serendipitous discovery of H i-rich galaxy groups with MeerKAT
Galaxy groups occupy up to ∼50 per cent of the local Universe (z ∼ 0; Eke et al. 2004; Robotham et al. 2011) and are important parts of the hierarchical structure of the Universe (Springel et al. 2018) where they trace filamentary large-scale structure, as they lie between the low-density environments of the field and high-density clusters. Galaxy systems form through episodic mergers, with groups thought to act as the building blocks for the more massive clusters.
Milliarcsecond localization of the hyperactive repeating FRB 20220912A
Fast radio bursts (FRBs) are flashes of coherent radio emission that have durations of microseconds to seconds (for a recent review see Petroff, Hessels & Lorimer 2022). Some of them are known to repeat (Spitler et al. 2016).
The highest mass Kepler red giants – I. Global asteroseismic parameters of 48 stars
Red giants are a late-stage evolutionary phase for most low- to intermediate-mass stars. When these stars evolve off the main sequence after core hydrogen exhaustion, they begin shell hydrogen burning and expand to large radii as they move upwards on the red giant branch (RGB). However, once they become hot enough to ignite helium in their cores, either in a flash or not, they shrink down slightly for core He burning (CHeB) in what we sometimes call the red clump phase.
The Thousand-Pulsar-Array programme on MeerKAT – XII. Discovery of long-term pulse profile evolution in 7 young pulsars
A number of pulsars are known to have profile evolution on timescales of months, often correlated with spin-down rate changes. Here, we present the first result from 3 years of monitoring observations from MeerKAT as part of the Thousand Pulsar Array programme. This programme obtains high-fidelity pulse profiles for ∼ 500 pulsars, which enabled the detection of subtle changes in seven sources not previously known to exhibit long-term profile evolution.
MUSE-ALMA Haloes X: the stellar masses of gas-rich absorbing galaxies
One of the key questions in galaxy evolution is how galaxies interact and connect to their immediate environment, called the circumgalactic medium (CGM; Tumlinson, Peeples & Werk 2017). Once stars are formed, galaxies expel ionizing photons and heavy elements formed in stars and supernovae into their surrounding environment through galactic winds (Pettini et al. 2008; Shull, Danforth & Tilton 2014).
WALLABY pilot survey: An ‘Almost’ dark cloud near the hydra cluster
We explore the properties of an ‘almost’ dark cloud of neutral hydrogen (H i) using data from the Widefield ASKAP L-band Legacy All-sky Survey (WALLABY). Until recently, WALLABY J103508-283427 (also known as H1032-2819 or LEDA 2793457) was not known to have an optical counterpart, but we have identified an extremely faint optical counterpart in the DESI Legacy Imaging Survey Data Release 10. We measured the mean g-band surface brightness to be 27.0 ± 0.3 mag arcsec−2.
Multi-epoch sampling of the radio star population with the Australian SKA Pathfinder
A wide variety of stellar systems produce magnetically driven non-thermal radio emission, featuring a high degree of fractional circular polarization and large brightness temperatures. In analogy to solar radio activity, K- and M-type dwarfs produce slowly varying or ‘quiescent’ emission as well as stochastic bursts associated with magnetic reconnection and space weather (e.g. Villadsen & Hallinan 2019; Zic et al. 2020).
An off-axis relativistic jet seen in the long lasting delayed radio flare of the TDE AT 2018hyz
The Tidal Disruption Event (TDE) AT 2018hyz exhibited a delayed radio flare almost three years after the stellar disruption. Here we report new radio observations of the TDE AT 2018hyz with the AMI-LA and ATCA spanning from a month to more than four years after the optical discovery and 200 days since the last reported radio observation.
The physical origins of gas in the circumgalactic medium using observationally motivated TNG50 mocks
The discovery of extragalactic absorption lines (e.g. Burbidge, Lynds & Burbidge 1966; Lynds & Stockton 1966; Stockton & Lynds 1966) shortly followed the discovery of the first quasar/quasi-stellar object (QSO) 3C 273 (Schmidt 1963). At the time, it was suggested that the absorption arose from discrete clouds of gas found in galaxies located along the line of sight (LOS) towards the background source (Bahcall & Salpeter 1965).
Resolving Moving Heliospheric Structures Using Interplanetary Scintillation Observations With the Murchison Widefield Array
1 Introduction Interplanetary scintillation (IPS) was discovered in 1964 (Clarke, 1964; Hewish et al., 1964). It was observed as amplitude scintillation at radio wavelengths as radiation from compact objects (0.3 arcsec for 162 MHz) traverse through the irregularities of the solar wind (Coles, 1978). IPS, as a general technique, has been used to study the solar wind, solar wind transients, and for inner-heliospheric observations for over 55 years.
Spectropolarimetric variability in the repeating fast radio burst source FRB 20180301A
As the sample size of repeating fast radio bursts (FRBs) has grown, an increasing diversity of phenomenology has emerged. Through long-term multi-epoch studies of repeating FRBs, it is possible to assess which phenomena are common to the population and which are unique to individual sources. We present a multi-epoch monitoring campaign of the repeating FRB source 20180301A using the ultra-wideband low (UWL) receiver observations with Murriyang, the Parkes 64-m radio telescope.
The FAST Galactic Plane Pulsar Snapshot survey – IV. Discovery of five fast radio bursts
Since the discovery of the first fast radio burst (FRB) by Lorimer et al. (2007), hundreds of FRBs have been reported,1 with the majority being one-off events (CHIME/FRB Collaboration 2021), and a few dozen are repeaters (Spitler et al. 2016; CHIME/FRB Collaboration 2019, 2023; Fonseca et al. 2020). Notable among the repeaters are FRB 20121102A, which was the first repeater identified (Spitler et al. 2016), and FRB 20201124A, which displays heightened activity during specific episodes (Xu et al.
The FAST Galactic Plane Pulsar Snapshot survey – IV. Discovery of five fast radio bursts
We report five new fast radio bursts (FRBs) discovered from the Galactic Plane Pulsar Snapshot (GPPS) survey by the Five-hundred-meter Aperture Spherical radio Telescope (FAST): FRB 20210126, FRB 20210208, FRB 20210705, FRB 20211005, and FRB 20220306. To date, no repeating bursts from these FRB sources have been detected in the follow-up monitoring observations, leading to their classification as potential one-off events.
Ultraluminous Quasars At High Redshift Show Evolution In Their Radio-Loudness Fraction In Both Redshift And Ultraviolet Luminosity
We take a sample of 94 ultraluminous, optical quasars from the search of over 14,486 deg2 by Onken et al. (2022) in the range 4.4 <redshift<5.2 and match them against the Rapid ASKAP Continuum Survey (RACS) observed on the Australian Square Kilometre Array Pathfinder (ASKAP). From this most complete sample of the bright end of the redshift ∼5 quasar luminosity function, there are 10 radio continuum detections of which 8 are considered radio-loud quasars.
On the spatial distribution of electron energy loss due to gyro-cooling in hot star magnetospheres
Hot magnetic stars often exhibit incoherent circularly polarized radio emission thought to arise from gyro-synchrotron emission by energetic electrons trapped in the circumstellar magnetosphere. Theoretical scalings for electron acceleration by magnetic reconnection driven by centrifugal breakout match well the empirical scalings for observed radio luminosity with both the magnetic field strength and the stellar rotation rate.
The unseen host galaxy and high dispersion measure of a precisely localized fast radio burst suggests a high-redshift origin
FRB 20210912A is a fast radio burst (FRB), detected and localized to subarcsecond precision by the Australian Square Kilometre Array Pathfinder. No host galaxy has been identified for this burst despite the high precision of its localization and deep optical and infrared follow-up, to 5σ limits of R = 26.7 mag and K = 24.9 mag with the Very Large Telescope.
A ‘MeerKAT-meets-LOFAR’ study of Abell 1413: A moderately disturbed non-cool-core cluster hosting a ∼500 kpc ‘mini’-halo
Many relaxed cool-core clusters host diffuse radio emission on scales of hundreds of kiloparsecs: mini-haloes. However, the mechanism responsible for generating them, as well as their connection with central active galactic nuclei, is elusive and many questions related to their physical properties and origins remain unanswered.
Systematic performance of the ASKAP Fast Radio Burst search algorithm
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Rapid radio brightening of GRB 210702A
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The LOFAR Two-metre Sky Survey: the radio view of the cosmic star formation history
We present a detailed study of the cosmic star formation history over 90 per cent of cosmic time (0 ≲ z ≲ 4), using deep, radio continuum observations that probe star formation activity independent of dust. The Low Frequency Array Two Metre Sky Survey has imaged three well-studied extragalactic fields, Elais-N1, Boötes and the Lockman Hole, reaching |$\sim 20\, \mu \rm {Jy/beam}$| rms sensitivity at |$150\, \rm {MHz}$|.
WALLABY Pilot Survey: H i in the Host Galaxy of a Fast Radio Burst
To date, we do not know the origin of fast radio bursts (FRBs; Lorimer et al. 2007), the highly energetic radio pulses occurring on timescales of milliseconds and found to originate at extragalactic distances. While several theories exist (see the review by Cordes & Chatterjee 2019), this is an ongoing area of debate. To address this issue best, we need to identify and dissect the host galaxies of FRBs better, through localization of their radio signals.
MUSE-ALMA Haloes XI: gas flows in the circumgalactic medium
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MeerKAT view of the dancing ghosts - peculiar galaxy pair PKS 2130−538 in Abell 3785
ABSTRACT We present MeerKAT L-band (886–1682 MHz) observations of the extended radio structure of the peculiar galaxy pair PKS 2130−538 known as the ‘Dancing Ghosts’. The complex of bending and possibly interacting jets and lobes originate from two active galactic nuclei hosts in the Abell 3785 galaxy cluster, one of which is the brightest cluster galaxy. The radio properties of the PKS 2130−538 – flux density, spectral index, and polarization – are typical for large, bent-tail galaxies.
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