We propose a modest program to continue monitoring 4 of the 6 known radio magnetars in order to achieve three primary science goals. The first is to characterise magnetar outbursts over long timescales, for which tracking their rotational, flux density, and polarisation properties provide a clear view of the impulse response of their magnetic fields. Second, understanding the links between magnetars the mysterious fast radio burst phenomenon through the discovery of rare emission and propagation effects, shared spectro-temporal phenomenology, and connections to high-energy (X-ray/gamma-ray) phenomena. Lastly, our continued monitoring has enormous benefit to the wider magnetar community, providing rapid alerts to changes in activity, adding context to unusual behaviour detected by high-enery observations, and a host of supplementary science through the teams extensive collaborative networks. The project and its precursors have been running since 2007 and have contributed to 21 publications since then. We are seeking to convert the project to long-term status, thereby also carrying these investigations into the SKA era.

We propose a modest program to continue monitoring 4 of the 6 known radio magnetars in order to achieve three primary science goals. The first is to characterise magnetar outbursts over long timescales, for which tracking their rotational, flux density, and polarisation properties provide a clear view of the impulse response of their magnetic fields. Second, understanding the links between magnetars the mysterious fast radio burst phenomenon through the discovery of rare emission and propagation effects, shared spectro-temporal phenomenology, and connections to high-energy (X-ray/gamma-ray) phenomena. Lastly, our continued monitoring has enormous benefit to the wider magnetar community, providing rapid alerts to changes in activity, adding context to unusual behaviour detected by high-enery observations, and a host of supplementary science through the teams extensive collaborative networks. The project and its precursors have been running since 2007 and have contributed to 21 publications since then. We are seeking to convert the project to long-term status, thereby also carrying these investigations into the SKA era.

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.

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.

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.

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.

This proposal aims to constrain burst rates and spin down properties of a sample of new Rotating Radio Transients (RRATs) discovered with the ASKAP CRAFT Coherent upgrade (CRACO) system. Over the past 12-months of commissioning, CRACO discovered and precisely localised 15 new RRATs, characterised by their sporadic pulses with dispersion measures (DM) consistent with Galactic sources. We request 22.5h of Parkes time split into three 30min observations spanning 6-months for each target. This can help constrain periods and potentially phase-coherent timing solutions given that we already have arcsec-precision interferometric localisations. Our main science goals are: 1) to measure their burst rates, periods, and spin-down properties; 2) to assess their nulling fraction and intermittency; 3) to measure their polarimetric properties and constrain their emission mechanism; 4) to determine if the CRACO RRATs are fundamentally different from the known RRAT population. Some of these goals can be answered even with the detection of a limited number of pulses.

This proposal aims to constrain burst rates and spin down properties of a sample of new Rotating Radio Transients (RRATs) discovered with the ASKAP CRAFT Coherent upgrade (CRACO) system. Over the past 12-months of commissioning, CRACO discovered and precisely localised 15 new RRATs, characterised by their sporadic pulses with dispersion measures (DM) consistent with Galactic sources. We request 22.5h of Parkes time split into three 30min observations spanning 6-months for each target. This can help constrain periods and potentially phase-coherent timing solutions given that we already have arcsec-precision interferometric localisations. Our main science goals are: 1) to measure their burst rates, periods, and spin-down properties; 2) to assess their nulling fraction and intermittency; 3) to measure their polarimetric properties and constrain their emission mechanism; 4) to determine if the CRACO RRATs are fundamentally different from the known RRAT population. Some of these goals can be answered even with the detection of a limited number of pulses.

This proposal aims to constrain burst rates and spin down properties of a sample of new Rotating Radio Transients (RRATs) discovered with the ASKAP CRAFT Coherent upgrade (CRACO) system. Over the past 12-months of commissioning, CRACO discovered and precisely localised 15 new RRATs, characterised by their sporadic pulses with dispersion measures (DM) consistent with Galactic sources. We request 22.5h of Parkes time split into three 30min observations spanning 6-months for each target. This can help constrain periods and potentially phase-coherent timing solutions given that we already have arcsec-precision interferometric localisations. Our main science goals are: 1) to measure their burst rates, periods, and spin-down properties; 2) to assess their nulling fraction and intermittency; 3) to measure their polarimetric properties and constrain their emission mechanism; 4) to determine if the CRACO RRATs are fundamentally different from the known RRAT population. Some of these goals can be answered even with the detection of a limited number of pulses.

This proposal aims to obtain timing solutions and constrain burst rates and spin down properties of a sample of new rotating radio transients (RRATs) discovered with the ASKAP CRAFT Coherent upgrade (CRACO) system. In the last 6-months of commissioning, CRACO discovered and localised 10 new RRATs, identified by their sporadic pulses with dispersion measures (DM) consistent with Galactic objects. We request 15h of Parkes time split into three 30min observations spanning 6-months for each target. This will allow us to constrain phase-coherent timing solutions given that we already have arcsec-precision interferometric localisations. Our main science goals are: 1) to measure their burst rates, periods, and spin-down properties; 2) to assess their nulling fraction and emission mechanism 3) to determine if the CRACO RRATs are different to the known RRATs population.