We discovered PSR J1716-2808A (NGC6316A), a highly accelerated binary millisecond pulsar (MSP), in NGC6316. We are currently observing it with Parkes (P1330) to solve for the orbit. At the time of this proposal submission, we have not yet solved the orbit. We have 6 scheduled observations in August 2024, which we expect to provide a good orbital solution to use in the proposed observations for this proposal. The goal of the proposed observations is to conduct a year long timing campaign. This is crucial to break the timing degeneracy that occurs between the pulsar's position and the pulsar's spindown rate. We will be able to use this to connect the pulsar to our previous observations spanning back to 2022. This will also confirm whether the pulsar is a part of the cluster. A secondary advantage of having these observations is that the data can also be used to search for faint pulsars via stack searching and time any new pulsars that are discovered in any subsequent observations.

We propose a timing follow-up project for two newly discovered pulsars, J0915-6635 and J0917-6642, from the MWA-SMART survey. These pulsars were recently discovered from a blind periodic search of an 80-min SMART survey observation, with an localisation precision of 4 arcminutes. Initial flux density estimates suggest they are faint, requiring follow-up with the Parkes UWL receiver for precise timing solutions, flux density measurements, and polarimetric analysis. Initial analysis suggests a flux density 0.2-0.5 mJy for J0915-6635, and 0.1-0.3 mJy for J0917-6642 at 1.4 GHz, assuming a spectral index of -1.6. Observations with the Murriyang's UWL receiver will help enable a faster convergence to the full coherent timing solution and determine their spin and astrometric parameters, as well as further investigate this through measurements of pulsar flux densities and spectral indices. We will also perform a polarimetric analysis across a wide frequency range to better constrain the pulsars' geometries and emission properties.

We propose a timing follow-up project for two newly discovered pulsars, J0915-6635 and J0917-6642, from the MWA-SMART survey. These pulsars were recently discovered from a blind periodic search of an 80-min SMART survey observation, with an localisation precision of 4 arcminutes. Initial flux density estimates suggest they are faint, requiring follow-up with the Parkes UWL receiver for precise timing solutions, flux density measurements, and polarimetric analysis. Initial analysis suggests a flux density 0.2-0.5 mJy for J0915-6635, and 0.1-0.3 mJy for J0917-6642 at 1.4 GHz, assuming a spectral index of -1.6. Observations with the Murriyang's UWL receiver will help enable a faster convergence to the full coherent timing solution and determine their spin and astrometric parameters, as well as further investigate this through measurements of pulsar flux densities and spectral indices. We will also perform a polarimetric analysis across a wide frequency range to better constrain the pulsars' geometries and emission properties.

The Parkes Pulsar Timing Array (PPTA) project has three primary goals: (a) detection of gravitational waves from astronomical sources, (b) establishment of a pulsar timescale, and (c) improvement of our understanding of Solar-system dynamics. We are now in an exciting regime where a signal detected in our (and other data sets) has the form expected for a gravitational wave background. We are therefore now attempting to confirm, or deny, this exciting result. With this proposal we aim to maintain our pre-eminent position in the field. Unlike most observing proposals, this is a continuing proposal for which the observations will continue to improve bounds on ultra-low-frequency gravitational waves until they are finally detected. Continued Parkes observations will remain valuable at least until the first stage of the SKA is able to improve on our sensitivity and observing cadence. Even after the gravitational wave background is detected we will want to continue observations in support of the nascent field of gravitational wave astronomy!

With this proposal, we aim to continue P1032, the rapid measurements of relativistic parameters of southern binary pulsar systems using data from the Parkes Ultra Wideband Low (UWL) receiver. As the MeerTime project at the MeerKAT radio telescope ended in early 2024, observations with the UWL receiver now form the backbone for extending the timing baselines of many pulsars that have been part of this project. Since the source selection in APRS2024 was tailored such that the UWL receiver is the most (versatile and) suited instrument to achieve the proposed scientific goals for the chosen pulsars, we propose to continue these observations. We will use the UWL data to obtain significant orbital coverage and timing baselines on these pulsars and obtain important constraints on orbital and temporal DM variations that will help in identifying the nature of the companion stars. Increasing the number of measured Neutron Star (NS) masses, as well as improving on current constraints has profound implications for NS internal structure and for stellar and binary evolution physics. We request pre-graded status for this project for the next semester.

With this proposal, we aim to continue P1032, the rapid measurements of relativistic parameters of southern binary pulsar systems using data from the Parkes Ultra Wideband Low (UWL) receiver. As the MeerTime project at the MeerKAT radio telescope ended in early 2024, observations with the UWL receiver now form the backbone for extending the timing baselines of many pulsars that have been part of this project. Since the source selection in APRS2024 was tailored such that the UWL receiver is the most (versatile and) suited instrument to achieve the proposed scientific goals for the chosen pulsars, we propose to continue these observations. We will use the UWL data to obtain significant orbital coverage and timing baselines on these pulsars and obtain important constraints on orbital and temporal DM variations that will help in identifying the nature of the companion stars. Increasing the number of measured Neutron Star (NS) masses, as well as improving on current constraints has profound implications for NS internal structure and for stellar and binary evolution physics. We request pre-graded status for this project for the next semester.

With this proposal, we aim to continue P1032, the rapid measurements of relativistic parameters of southern binary pulsar systems using data from the Parkes Ultra Wideband Low (UWL) receiver. As the MeerTime project at the MeerKAT radio telescope ended in early 2024, observations with the UWL receiver now form the backbone for extending the timing baselines of many pulsars that have been part of this project. Since the source selection in APRS2024 was tailored such that the UWL receiver is the most (versatile and) suited instrument to achieve the proposed scientific goals for the chosen pulsars, we propose to continue these observations. We will use the UWL data to obtain significant orbital coverage and timing baselines on these pulsars and obtain important constraints on orbital and temporal DM variations that will help in identifying the nature of the companion stars. Increasing the number of measured Neutron Star (NS) masses, as well as improving on current constraints has profound implications for NS internal structure and for stellar and binary evolution physics. We request pre-graded status for this project for the next semester.

With this proposal, we aim to continue P1032, the rapid measurements of relativistic parameters of southern binary pulsar systems using data from the Parkes Ultra Wideband Low (UWL) receiver. As the MeerTime project at the MeerKAT radio telescope ended in early 2024, observations with the UWL receiver now form the backbone for extending the timing baselines of many pulsars that have been part of this project. Since the source selection in the previous semesters was tailored such that the UWL receiver is the most (versatile and) suited instrument to achieve the proposed scientific goals for the chosen pulsars, we propose to continue these observations. We will use the UWL data to obtain significant orbital coverage and timing baselines on these pulsars and obtain important constraints on orbital and temporal DM variations that will help in identifying the nature of the companion stars. Increasing the number of measured Neutron Star (NS) masses, as well as improving on current constraints has profound implications for NS internal structure and for stellar and binary evolution physics.

With this proposal, we aim to continue P1032, the rapid measurements of relativistic parameters of southern binary pulsar systems using data from the Parkes Ultra Wideband Low (UWL) receiver. As the MeerTime project at the MeerKAT radio telescope ended in early 2024, observations with the UWL receiver now form the backbone for extending the timing baselines of many pulsars that have been part of this project. Since the source selection in the previous semesters was tailored such that the UWL receiver is the most (versatile and) suited instrument to achieve the proposed scientific goals for the chosen pulsars, we propose to continue these observations. We will use the UWL data to obtain significant orbital coverage and timing baselines on these pulsars and obtain important constraints on orbital and temporal DM variations that will help in identifying the nature of the companion stars. Increasing the number of measured Neutron Star (NS) masses, as well as improving on current constraints has profound implications for NS internal structure and for stellar and binary evolution physics.

The Parkes Pulsar Timing Array (PPTA) project has three primary goals: (a) detection of gravitational waves from astronomical sources, (b) establishment of a pulsar timescale, and (c) improvement of our understanding of Solar-system dynamics. We are now in an exciting regime where a signal detected in our (and other data sets) has the form expected for a gravitational wave background. We, along with the international community, are now working hard to either confirm or deny this result, and to determine the astrophysical origin of this signal. With this proposal, we aim to maintain our pre-eminent position in the field. This is a continuing proposal for which observations of millisecond pulsars (MSPs) will continue to improve bounds on ultra-low-frequency gravitational waves until they are detected with confidence. Continued Parkes observations will remain valuable at least until the first stage of the SKA is able to improve on our sensitivity and observing cadence. Even after the gravitational wave background is detected, continued observations will resolve the background origin and individual sources will be identified; advancing the nascent field of gravitational wave astronomy.