AndreaBozzo/ceres-open-data-index huggingface dataset:
Parkes observations for project P1165 semester 2025APRS_01

We recently discovered two new pulsars J1849+1001 (35.1 ms) and J1839+0542 (57.9 ms) in a FAST pulsar survey at intermediate Galactic latitudes (PT2020_0141). Follow-up timing observations show that they are in circular orbits with massive companions. This suggests that PSR J1849+1001 and J1839+0542 can be classified as the intermediate-mass binary pulsar (IMBP). Their massive companions also make them promising systems to measure "Post-Keplerian" parameters through pulsar timing. These Parkes observations will be combined with regular timing observations with FAST or MeerKAT to measure "Post-Keplerian" parameters and then measure both neutron star and companion masses.

Organization: CSIRO Data Access Portal
Optimising fertilisation kinetics models for broadcast spawning corals in the genus Acropora

This dataset contains information about fine-scale gamete properties of spawning corals on the Great Barrier Reef. This data was collected and used to optimise fertilisation kinetics models for spawning corals. Sperm swimming speed assays were conducted for A. cf. kenti (previously A. “Maggie” tenuis) to gather species-specific metrics for the analysis. 
Sperm samples were examined at 40x magnification with phase contrast using a Zeiss Primostar 3 trinocular compound light microscope with a CMOS 8.3 MP camera attachment. Videos of sperm were taken using the ImageView software (YSCTechnologies 2024) at 60 frames per second (FPS) for 3 seconds. Three videos were taken per slide at three different locations around the slide, and this was repeated five times for each replicate cross. 
Sperm swimming was analysed with a point tracking method using the DLTdv8a app (Hedrick 2008) in Matlab. Initial (vi) and final (vf) velocity parameters were used to calculate the average velocity (vavg) of all motile sperm in each video. Some videos were omitted due to poor quality or lack of visible or motile sperm for long enough durations (&gt;2 sec). A total of 82 total sperm tracks were quantified across 35 videos.

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Parkes observations for project PX500 semester 2025APRS_10

This proposal relates to time purchased by the Chinese Academy of Sciences for Parkes follow-up confirmation and timing of FAST discoveries.  As the observing time has been purchased this proposal (and the related PX501) does not require TAC grading.  The primary reason for submitting a proposal is to ensure an outreach statement and that the proposal is entered into OPAL for the data archive to access. The Chinese team have two time requests. The time scheduled for the first, relating to this proposal, will be allocated in blocks of 24 hours and the data will become available in the data archive with an 18 month embargo period.  The second type of time will be scheduled in shorter blocks and the data archived with a 10 year embargo.

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Parkes observations for project P1364 semester 2025APRS_01

The propagation effects of the ionized interstellar medium (IISM) on pulsars are not well understood, and increase uncertainty on pulsar timing measurements. As high-precision pulsar timing is critical for using pulsars to detect phenomena as varied as gravitational waves and neutron star glitches, it is important to improve our understanding of these propagation effects. One such effect is chromatic dispersion, which contributes to timing noise but has been detected only once. We propose a set of 4 pointings with the Murriyang 64m Parkes Radio Telescope Ultra-Wide bandwidth Low frequency receiver (UWL), totaling 10 hours of telescope time. Our three targets are all strongly polarized pulsars in the Galactic plane, selected to maximize our chances of detecting one or both of the two types of chromatic dispersion. Non-detections will place upper limits on magnetic field strength and electron density in the IISM.

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Parkes observations for project P1171 semester 2025APRS_01

The origin of Fast Radio Bursts (FRBs) is still unclear with a plethora of theoretical models for their origin.
  Several models predict associated multi-wavelength emission, but previous searches for optical, X-ray or
  gamma-ray counterparts of FRBs have not led to any detection. The Galactic magnetar SGR 1935+2154A has
  been observed to simultaneously emit FRB-like bursts and X-ray flares, which suggests that also extragalactic
  FRB sources may exhibit X-ray counterparts. Because of the high cost of X-ray satellites and in face of the
  relatively low FRB detection probability in their small field of view, coordinated radio and X-ray observations are
  logistically very difficult to set up. We propose a new approach using the X-ray satellite XMM-Newton and the
  Parkes/Murriyang radio telescope to put constraints on the theoretical models: We aim to conduct shadowing
  observations with the Parkes telescope to search for new FRBs in fields that are simultaneously covered by
  XMM-Newton. We hereby target regular XMM observations of nearby (low-z) galaxies, to increase our
  detection chances of possibly associated X-ray emission. In case of an FRB detection in the radio band, we will
  have guaranteed simultaneous X-ray coverage and will get detailed information about the associated X-ray
  spectrum and light curve since all XMM-Newton data will become public a year after the observation.

Organization: CSIRO Data Access Portal
Proximal grain composition of 240 globally diverse chickpea lines

The proximal composition (starch, protien, soluble sugars, lipid, insoluble fiber, and moisture) of 240 varieties of chickpea (Cicer arietinum) sourced from the ICRISAT genebank. 
Data is linked to the publication "GWAS of chickpea grain macronutrient and lipidomic profiles from a global diversity panel" Buck et. al. 2025

Organization: CSIRO Data Access Portal
Parkes observations for project PX500 semester 2025APRS_09

This proposal relates to time purchased by the Chinese Academy of Sciences for Parkes follow-up confirmation and timing of FAST discoveries.  As the observing time has been purchased this proposal (and the related PX501) does not require TAC grading.  The primary reason for submitting a proposal is to ensure an outreach statement and that the proposal is entered into OPAL for the data archive to access. The Chinese team have two time requests. The time scheduled for the first, relating to this proposal, will be allocated in blocks of 24 hours and the data will become available in the data archive with an 18 month embargo period.  The second type of time will be scheduled in shorter blocks and the data archived with a 10 year embargo.

Organization: CSIRO Data Access Portal
LBA observations for project V642 semester 2024APRS

With supreme timing stabilities, millisecond pulsars (MSPs) have been used to test gravitational theories, and to collectively probe the stochastic gravitational-wave background (GWB) at the nano-Hz regime. Recent years have seen the major pulsar timing array (PTA) consortia closing in on high-significance detections of the GWB, which marks the dawn of a new GWB era. To deepen our understanding of the sources of the GWB requires steady enhancement of the PTA sensitivity. The best strategy to sustain the enhancement is to continuously add new qualified MSPs to the PTAs. VLBI (very long baseline interferometry) astrometry of MPSs would empower this strategy by refining the pulsar timing model with precise astrometric measurements obtained in a relatively short timeline. In addition, VLBI astrometry of MSPs contributes to MSP-related/based studies in many ways: it can strengthen the tests of gravitational theories, probe the formation channels of millisecond pulsars, refine the Galactic interstellar medium distribution, and even sharpen the constraints on the Galactic dark matter distribution. So far, 24 MSPs have been astrometrically determined with VLBI. As the only southern-hemisphere-based VLBI network, the LBA has only contributed to one astrometric determination of MSPs. We propose to carry out the first LBA astrometric survey of MSPs, which will benefit the aforementioned scientific aspects, and significantly reduce sky-position-related selection effects on statistical studies based on MSP astrometry. This proposal aims at piloting the astrometric survey by observing 28 MSP candidates at 13cm.

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LBA observations for project V653 semester 2024APRS

Roughly 1 in 10 O stars have been found to harbour extremely stable, ordered (usually dipolar) magnetic fields, which are of ~kG strength. The presence of such organized surface magnetic fields can channel and confine the outflowing stellar winds, creating a magnetosphere that can radiate in various wavebands. Several attempts were made to detect radio emissions from magnetic O-type stars at low frequencies. However, no detection was found, which can be explained by the absorption of non-thermal emission in sub-GHz frequencies due to the dense wind of such high mass-loss rate systems. The first exception to this scenario is the detection of sub-GHz radio emission with the upgraded Giant Metrewave Radio Telescope (uGMRT) from a binary O-star system HD 148937. The 325 MHz detection of this target makes it the lowest frequency detection of any magnetic massive star. The observed emission is non-thermal in nature, with radio luminosity much higher than expected. We attribute the possible emission mechanism to be either synchrotron emission from wind-wind collision, or Electron Cyclotron Maser Emission (ECME) from the magnetic primary. Given the extreme and unique nature of the radio emission from this system, we plan to follow up this target and make use of the high resolution of the LBA to pinpoint the emission region and the corresponding mechanism.

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LBA observations for project V646 semester 2024APRS

This proposal aims to measure the parallax of pulsar B1055-52. PSR B1055-52 is particularly important for studying neutron star properties. Bright at radio and gamma-rays, the pulsar is also well detected at near-infrared, optical, UV and X-ray frequencies. In X-rays, we even can see the surface's thermal emission and can investigate the non-uniformity of the temperature distribution over rotation phase. Since PSR B1055-52 is a rare interpulse pulsar, there is an exceptionally good constraint on the angle between the magnetic dipole and rotation axes, allowing to resolve many model degeneracies. The wealth of observational data enable a very detailed investigation of this pulsar and neutron stars in general. However, these investigations cannot be completed without one  essential parameter - the distance. Currently, the possible distance range obtained from the dispersion measure has a span of almost a factor 10 if different Galactic electron density models are considered. At the same time, there are several indicators that PSR B1055-52  is close enough to obtain a parallax-based distance with high accuracy.

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LBA observations for project V651 semester 2024APRS

We propose an LBA pilot phase-referenced observation at 8.4GHz of a pulsar J1638-4713 associated with a bow shock pulsar wind nebula.  The estimated velocity of 1500 km/s for the driving pulsar, makes it potentially one of the fastest-moving pulsars. We propose this study in order to (i) derive a more accurate position for future VLBI epochs, (ii) determine the suitability of the source and phase-reference calibrator for subsequent multi-epoch studies to measure a proper motion, and possibly parallax, for this source and (iii) determine the milli-arcsecond scale structure of the source.

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LBA observations for project V636 semester 2023OCTS

To improve the link accuracy between the bright Gaia-CRF and ICRF, we request four 8-hour epochs using all available LBA antennas for phase-reference observations of five radio stars.
  YY Men is an important star located near the southern celestial pole, so we aim to measure its parallax and proper motion with multiple epochs (three in this semester).
  The other four stars are also distributed in the southern sky, and we aim to measure their proper motions with two epochs (one in this semester).
  Observing these stars will increase the number of available radio stars for CRF link and improve the sky distribution uniformity.

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LBA observations for project V626 semester 2024APRS

ASASSN-14ko is a transient source in the ESO 253-G003 galaxy system, which is in the process of merging. It was discovered by the ASAS-SN survey in 2014, and it periodically flares in the optical every 114 days, with a period that is decreasing (Payne et al. 2021). This variability is likely due to multiple partial tidal disruption events involving a giant star orbiting the supermassive black hole in the northeastern galaxy of ESO 253-G003.
  The ESO 253-G003 system has been detected in radio by historic ASKAP and ATCA observations. The X-ray spectrum, the large gas fraction in the core region, based on the merging galaxy scenario and line diagnostics from MUSE observations, suggests that pTDE-triggered jet launching could explain the observed radio emission. VLBI observations will allow us to resolve the core region of the pTDE hosting AGN.

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LBA observations for project V603 semester 2024APRS

The energetics and central engines of Fast Radio Bursts (FRBs) are still mysterious, and it is unclear whether the subset of repeating FRBs are a function of their host environments or form an entirely different source class. Characteristics of the Persistent Radio Source (PRS) and its relation to FRB provide crucial clues to FRB origin and surrounding environment. We propose multi-epoch sensitive VLBI observations of one of the only two repeating FRBs with confirmed compact PRS counterparts, namely FRB 190520, using the LBA combined with Chinese radio telescopes including FAST. The monitoring VLBI observations can reveal possible variability in location, physical size and flux of both FRB and its PRS, which allow us to distinguish models of FRB origin and offer a clue to their possible evolution.

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LBA observations for project V645 semester 2024APRS

Traditionally searches for techno-signatures have utilised raw voltage data from single-dish radio telescopes or beam-formed data from radio arrays with relatively short baselines. We propose a short LBA observation as a pilot experiment to explore the options for utilising VLBI for SETI searches. Widely separated telescopes are naturally more immune to confusion from RFI sources, and the phase response from any detection can be used to distinguish terrestrial signals from distant emitters (past the moon).

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LBA observations for project V650 semester 2024APRS

We request 8 GHz LBA observations of a nearby radio galaxy hosted by an active and likely unstable lenticular galaxy that may have underwent a minor merger in the past. Based on sub-arcsec resolution VLA observations, we propose to investigate the central 2 kpc region of the galaxy where we detected multi-component radio emission reminiscent of a relativistic jet but severely misaligned with the older large scale radio morphology (~80 deg reorientation). With this proposal we intend to verify if the detected central multi-component radio emission is indeed a relativistic jet as opposed to emission from star formation (or star bursts). This is a detection experiment and a pilot study. If the observations confirm that the radio emission is associated with a freshly launched realigned relativistic jet, a multi-epoch monitoring program will be designed and proposed in future semesters to characterise the emission and establish phenomenon at play causing the realignment.

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LBA observations for project V652 semester 2024APRS

Relativistic outflows from cosmic explosions are some of the most extreme environments in the Universe, providing a natural laboratory to study the physics of jets, radiative transfer theory, and to uncover the nature of the explosions and their progenitors. The outflows from cosmic explosions -- from gamma-ray bursts (GRBs) to core-collapse supernovae (CCSNe), fast blue optical transients (FBOTs), and tidal disruption events (TDEs) -- have primarily been studied through modelling multi-wavelength photometry and spectra. However, such an approach is often limited by degeneracies intrinsic to the models (and limited number of observables). 
  Very Long Baseline Interferometry (VLBI) offers valuable, complementary insight into these systems. The ${\sim}$mas angular resolution achievable with VLBI allows direct measurements (or constraints) on the source size, structure, geometry and evolution (expansion or proper motion), independent of multi-wavelength modelling. This in turn sheds light onto the role relativistic outflows play in these cosmic explosions, revealing insights into the spectrum of ejecta velocities, universality in the physics of relativistic outflow between different systems, and consequentially, the nature of the system progenitors.

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Parkes observations for project P1338 semester 2025APRS_15

Fast radio bursts (FRBs) are millisecond-duration radio bursts of extragalactic origin. Since the discovery of the first FRB in the archival Parkes/Murriyang multibeam data, a broad dichotomy in population has emerged. Some FRBs have been seen to be repeating, while others are not, despite a significant amount of follow-up using different radio telescopes. The repeating FRB 20240114A was recently discovered by CHIME/FRB, which has been seen to have an exceptionally high burst activity. Such extreme burst activity has not been seen in any other source. The repeating FRBs, such as FRB 20240114A, provide an unparalleled window into their circumburst environment due to their repeating nature, which can be used to constrain possible progenitor models and test underlying emission mechanisms. The previous Parkes/Murriyang source follow-up has also revealed intriguing spectro-polarimetric properties, such as frequency-dependent evolution of burst central frequency or chromaticity, a possible activity window, significantly large circular polarisation (CP), and frequency-dependent CP. These properties hold the key towards understanding the circumburst environment of the FRBs, and test possible progenitor models. A large bandwidth instrument with reliable polarimetry has been critical in uncovering these properties. The ultra-wideband low (UWL) receiver on Parkes/Murriyang is ideally suited to explore the source's wideband spectro-temporal and polarimetric behaviour. We propose a campaign to regularly follow up FRB 20240114A to ascertain its long-term evolution of spectro-temporal properties.

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RV Investigator Voyage IN2025_V01 End of Voyage (EOV) Archive

This record describes the End of Voyage (EOV) data archive from the Marine National Facility (MNF) RV Investigator voyage IN2025_V01, titled "Collaborative Australian Postgraduate Sea Training Network (CAPSTAN)." The voyage took place between March 08, 2025 and March 17, 2025 (AEST), departing from Hobart and returning to Hobart.
For further information please refer to the voyage documentation links.
Instruments used and data collected include:
Regular measurements:
Acoustic Doppler Current Profiler (ADCP; 75, 150 KHz), CTD, Disdrometer, Fisheries Echosounder (EK60, EK80), Gravimeter, Fluorometer, Hydrochemistry, Lowered ADCP (LADCP), Radon sensor, Sub-bottom Profiler (SBP120), Weather Radar, pCO2, Video, Argo Floats.
Voyage-specific measurements:
Bongo Net, Deep Towed Camera (DTC), Triaxus
The archive for the IN2025_V01 EOV raw data is curated by the CSIRO National Collections and Marine Infrastructure (NCMI) Information and Data Centre (IDC) in Hobart, with a permanent archive at the CSIRO Data Access Portal (https://data.csiro.au/), providing access to voyage participants and processors of the data collected on the voyage.
All voyage documentation is available electronically to MNF support via the local network. Applications to access voyage documentation by non-CSIRO participants can be made via data-requests-hf@csiro.au All processed data from this voyage are made publicly available through the MNF Data Trawler (in the related links)

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Parkes observations for project P1338 semester 2025APRS_16

Fast radio bursts (FRBs) are millisecond-duration radio bursts of extragalactic origin. Since the discovery of the first FRB in the archival Parkes/Murriyang multibeam data, a broad dichotomy in population has emerged. Some FRBs have been seen to be repeating, while others are not, despite a significant amount of follow-up using different radio telescopes. The repeating FRB 20240114A was recently discovered by CHIME/FRB, which has been seen to have an exceptionally high burst activity. Such extreme burst activity has not been seen in any other source. The repeating FRBs, such as FRB 20240114A, provide an unparalleled window into their circumburst environment due to their repeating nature, which can be used to constrain possible progenitor models and test underlying emission mechanisms. The previous Parkes/Murriyang source follow-up has also revealed intriguing spectro-polarimetric properties, such as frequency-dependent evolution of burst central frequency or chromaticity, a possible activity window, significantly large circular polarisation (CP), and frequency-dependent CP. These properties hold the key towards understanding the circumburst environment of the FRBs, and test possible progenitor models. A large bandwidth instrument with reliable polarimetry has been critical in uncovering these properties. The ultra-wideband low (UWL) receiver on Parkes/Murriyang is ideally suited to explore the source's wideband spectro-temporal and polarimetric behaviour. We propose a campaign to regularly follow up FRB 20240114A to ascertain its long-term evolution of spectro-temporal properties.

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Parkes observations for project P1356 semester 2025APRS_04

Magnetars are neutron stars with exceptionally high magnetic fields. From the 30 known magnetars, only six have had radio emission detected so far. The remaining 24 magnetars are generally only searched for radio emission after an X-ray outburst. This added a strong selection bias to whether magnetars are radio loud or not. From the known six radio loud magnetars, we know that the radio emission changes quickly with time and for the magnetar XTE J1810-197, it has been observed that the radio flux increases strongly without an enhancement in X-ray flux. Thus, it remains unclear whether the radio quiet magnetars are in fact radio quiet and the radio X-ray relation appears to be rather complex.
  In this proposal, we propose a regular monitoring campaign of 4 radio quiet magnetars with bi-weekly observations using the Parkes UWL receiver. For 3 of the sources, we will have accompanying X-ray observations and thus, this will give an unique data set to probe the relation between radio and X-ray independent outbursts. Any detection of radio emission, i.e. single pulses or folded profiles, would be a major discovery and help to constrain the emission mechanisms of magnetars. This will also help to improve the understanding of the emission mechanism of fast radio bursts. However, also a non-detection of radio emission will provide upper limits that serve as a baseline before any future outburst of the observed magnetars as well as allow to constrain the formation process of magnetars in contrast to pulsars.

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