ICTS

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talk given as part of workshop

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SPOTLIGHT is a time-domain survey instrument to perform a real-time commensal search for FRBs (Fast Radio Bursts) and Pulsars with a PetaFlop system hosting 60 CDAC’s indigenously developed Rudra servers equipped with 90 A100 GPUs connected to a 2 PB storage over a 100 Gbps Infiniband network. The system executes real-time HPC and AI applications to ensure simultaneous time-domain detection and arc-second imaging localisation of the detected bursts across the GMRT observing band of 300 to 1460 MHz. The 60 Rudra servers are arranged in three sub-clusters implementing the correlator, transient search and imaging analysis. The first cluster, consisting of 16 servers, performs correlation and beamformation forming 2000 beams at 1.3 millisecond time-resolution and sends the 2000 beams to the 24 servers of the second cluster for multi-beam transient detection pipeline to search for FRBs using Machine Learning for classification. The 2000 beams are optimally located well within the half-power beamwidth of the primary beam of a GMRT antenna. Imaging localisation on the detected FRBs and candidate confirmation is done on the 20 servers of the third cluster.

The first stage of the system is equipped to accept Nyquist sampled digitised data of baseband signals of both polarisations of all antennas of GMRT at the rate of 25 GB/s over 32 ten gigabit fibre links to perform correlation and beamformation. The data ingestion to the SPOTLIGHT system is done via UDP packet broadcasting from the GMRT samplers, ensuring piggy-back operation with the GMRT Wide-band Backend. The received digitised data on each server over two ten gigabit fibre links is buffered, time-sliced and shared between the servers on a 100 Gbps network such that each server gets a slice of contiguous time series digitised data of all antennas, on which it performs operations like FFT, Multiplication and Accumulation (MAC) and beamformation using dual A100 GPUs. MAC is designed to give visibilities at 1.3 ms time resolution. The post-correlation beams are formed using the phased addition of the 1.3 ms time resolution visibilities. The post-correlation beams reduce the effect of radio frequency interferences and systematics in the data by eliminating the auto-correlation products (Figure 1). Cleaning the dynamic spectrum and more importantly, the dispersion measure-time image significantly increases the efficiency of the AI classifier. The beam-steering implemented at the post-correlation stage significantly minimizes computational costs. The 2000 beams thus formed are distributed over the servers of the second stage such that each server receives data of ~84 beams. The beam data received is buffered in a shared memory which is accessed by the multi-beam transient detection pipeline for pulsar and FRB searches.

The 1.3 ms time resolution visibilities formed in the first stage are integrated up to 1 second or higher and sent to a dedicated host node for archiving. This visibility data at this reduced time-resolution is used to detect the non-working antennas to remove them from the array and also to perform real-time phase and amplitude calibration of the data. In the first stage, in parallel to performing correlation and beamforming, the digitised Nyquist data is written to a shared memory. Upon detection of a transient event in the second stage, this baseband shared memory is accessed to write the Nyquist sampled voltages to the 2 PB storage over 100 Gbps network. The availability of the full Nyquist samples from the full array covering the dispersion sweep of the FRBs opens up the possibility of probing the underlying emission physics aided with full polarisation information and the propagation effects at an unprecedented sensitivity. In addition to this baseband buffering, in the second stage, the 1.3 ms time resolution visibilities are buffered in another shared memory which is accessed to write these visibilities to the 2 PB storage upon detection of a burst. This facilitates real-time imaging localisation of the FRB at arc-second resolution, enabling the host galaxy association to use the burst as a cosmological tool. The sizes of shared memory for the beam data (~ 2.4 TB) and 1.3 millisecond resolution visibilities (~ 5 TB) in the second stage and the baseband shared memory (~ 4.8 TB at 4-bits per sample) in the first stage are large enough to hold the data on Random Access Memory to accommodate detection of bursts even at high dispersion measure.

The SPOTLIGHT system is being realized in a phased manner. The entire hardware installation was completed by October 2024. Following this, the software pipelines are being tested with an increasing number of beams progressively. The real-time system currently being tested at the GMRT can generate 800 beams, along with all promised data products, using 32 A100 GPUs, achieving 40% of the final specification.

Fast Radio Bursts (FRBs) represent one of modern astronomy's most compelling mysteries. Despite cataloging approximately 800 FRBs, including 65 repeaters, their exact emission mechanisms remain unknown. This knowledge gap persists largely due to limitations in localization accuracy and timing. Current FRB detection systems face a critical tradeoff: wide-field instruments discover numerous FRBs but provide poor localization accuracy, while interferometric arrays offer precise positions but process data with substantial delays—typically a week between detection and localization. This delay severely limits multi-wavelength follow-up observations, particularly for transient repeaters that may remain active only briefly after discovery. SPOTLIGHT (Survey for sPoradic radiO bursTs via a commensaL, multIbeam, GPU-powered HPC at the GMRT) addresses this challenge through an innovative real-time imaging localization pipeline. Operating commensally with GMRT, the system searches for FRBs across 2000 phased array beams using combined HPC and AI techniques. Upon detection, SPOTLIGHT triggers high-time resolution (1.3ms) visibility recording across a 16-node cluster. These visibilities undergo immediate processing: de-dispersion at the candidate dispersion measure, conversion to CASA measurement sets, and imaging for precise localization. The entire process completes within approximately ~2 minutes post detection—dramatically faster than existing systems. The implementation leverages 8 servers with 384 CPUs dedicated to real-time imaging, capable of handling approximately 100 triggers daily. This capability enables immediate multi-wavelength follow-up observations, critical for capturing rapid afterglows and understanding repeater behavior. SPOTLIGHT represents the first operational survey providing real-time FRB localization—a transformative advancement for radio astronomy that maximizes scientific opportunities from each detection.

The latest enhancement to the GMRT’s transient science capability is the SPOTLIGHT project, designed to detect Fast Radio Bursts (FRBs) in real-time. This is achieved by forming 2000 post-correlation (PC) beams across the sky while piggybacking on regular GMRT observations over a frequency range from 300 MHz to 1460 MHz. In addition to real-time FRB detection, SPOTLIGHT includes a quasi-real-time pulsar search using 10% of the full field-of-view. The acquired data will undergo weekly processing using a Fourier Domain Acceleration Search pipeline, aiming to discover new pulsars from SPOTLIGHT observations. In this presentation, I will highlight the development and optimisation of the multi-GPU pulsar search pipeline designed for SPOTLIGHT. Additionally, I will discuss the key scientific goals of the pulsar search component, including the expected pulsar yield and the broader astrophysical implications of this project. Enabling commensal pulsar searches on GMRT, serving as both a science initiative and a technology demonstrator.

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The Murchison Widefield Array (MWA) is a low-frequency interferometer telescope located in the Western Australian outback, operating in the 70 – 300 MHz band, and comprised of 8096 dual-polarisation dipole antennas that are arranged in groups of 16 (tiles), with a maximum baseline out to ~6 km. Even though the array was originally designed and built primarily as an imaging telescope, the eventual development of a voltage capture system (VCS) functionality, whereby unprocessed voltage data can be recorded from all operating tiles opened up opportunities for pulsar and fast transient exploration in the southern skies with this next-generation telescope. Over the past decade, a series of capability enhancements around the VCS and associated software subsystems for post processing (on HPC platforms) has enabled a wide range of pulsar science, provided triggering/shadowing opportunities for GRBs/FRBs, and even facilitated non-astronomical applications involving passive radar or tracking space debris. These efforts have also led to the conception and undertaking of the Southern-sky MWA Rapid Two-metre (SMART) survey – an ambitious project that aims to conduct sensitive searches for pulsars and fast transients in the low-frequency southern skies. With the imminent transition of the array to Phase III by the end of the year, real-time processing and beamforming will replace the data-intensive VCS. I will present an overview of some key technical/science accomplishments in the past years, including new pulsar discoveries flowing on from the SMART project, ongoing efforts to develop a fast-imaging capability (offline processing) to realise large sky surveys for FRBs, and new opportunities now on the horizon for monitoring science in the areas of pulsars and fast transients.

The Bustling Universe Radio Survey Telescope in Taiwan (BURSTT) is a pioneering array designed to detect and precisely localize bright, nearby fast radio bursts (FRBs) in the 300–800 MHz band. Its key features include wide-area coverage of ~10,000 square degrees using multiple beams, along with continuous 24/7 operation. These capabilities significantly enhance the likelihood of detecting nearby FRBs and provide important clues for investigating the repetition rates and potential counterparts of FRBs. The first phase, BURSTT-256 (comprising 256 antennas) is currently fully operational, with a real-time FRB search running around the clock. Daily detections of giant pulses from the Crab pulsar demonstrate the system’s performance, and localization tests with multiple outrigger stations are currently underway. In this presentation, we will report the current status of BURSTT, along with results from our monitoring and localization efforts.

Fast Radio Bursts (FRBs) have emerged as one of the most enigmatic phenomena in modern astrophysics, characterized by their millisecond-duration flashes of extreme luminosity originating from cosmological distances. Despite significant progress in the field, the exact nature and progenitors of FRBs remain elusive. Our group has made substantial advancements in the precise localization of FRBs using Very Long Baseline Interferometry (VLBI), leveraging the unparalleled resolution and sensitivity of the European VLBI Network (EVN). These efforts have enabled us to localize the millisecond-duration bursts to milliarcsecond precision, and directly image the persistent radio sources associated with some FRBs. These findings provided critical insights into their environments and potential progenitors, such as young magnetars, superluminous supernovae, and massive black hole systems. In this talk, I will present the latest results from our VLBI observations within the PRECISE and AstroFlash activities. By combining multi-wavelength data and theoretical modeling, we have been able to differentiate between various formation channels and evolutionary stages of FRB sources. Our findings not only shed light on the physical conditions required to produce these bursts but also pave the way for future research with next-generation facilities. This work represents a significant step forward in understanding the origins and mechanisms of FRBs, contributing to the broader field of astrophysics and cosmology.

Events between 05 Dec 2025 to 13 Dec 2025

24 Jan 2016 : 05 Dec 2025 : 13 Dec 2025 : 05 Feb 2016

RFI mitigation algorithms aim to remove this interference and improve the signal-to-noise ratio of any detectable transient, but with the growing number of techniques, selecting the most appropriate methodology for a given survey can be problematic. Currently, the strategy is decided by the astronomer, which is not scalable for real-time systems planned for next-generation telescopes such as the SKAO telescopes. We have tried to explore the algorithm selection problem by simulating several RFI environments along with pulses injected into a white noise filterbank file, which is then cleaned using each of a number of RFI mitigation algorithms and run through a single pulse search pipeline to analyse the recovery of the injected pulses. We examine the recovery of the known single-pulse parameters with an emphasis on a number of realistic corner cases. In addition to this, look for some solutions to the identified problem as well.

This talk will explore our current understanding of the fast radio burst (FRB) radiation mechanism, highlighting key observational findings and the constraints they place on theoretical models. I will also discuss how FRBs can serve as powerful probes of the reionization era, providing unique insights into the early universe.

Fast radio bursts (FRBs) are brilliant short-duration flashes of radio emission originating at cosmological distances. Vast diversity in the properties of currently known FRBs and the fleeting nature of these events make it difficult to understand their progenitors and emission mechanisms. Some of the 'pulsar-like' properties of FRBs indicate their neutron star origin. Interestingly, the high-time-resolution properties of FRB 20210912A, a highly energetic event detected by the Australian Square Kilometre Array Pathfinder (ASKAP) in the Commensal Real-time ASKAP Fast Transients (CRAFT) survey, revealed remarkable resemblance with a previously reported CRAFT FRB, FRB 20181112A, including similar rest-frame emission timescales and polarization profiles. The observed properties of these two FRBs may be explained by emission from rapidly spinning neutron stars, with rest-frame spin periods of ∼ 1.1 ms — comparable to the shortest known period of a pulsar and close to the shortest possible rotation period of a neutron star. In this talk I will discuss the similarities between these two FRBs and their implications on FRB progenitor models.

Fast Radio Bursts (FRBs) are millisecond-duration, high-energy radio transients of extragalactic origin. FRB 20201124A is a repeating source that has shown significant activity across a broad frequency range. In this presentation, I will present a spectro-temporal analysis of FRB 20201124A using observations from the uGMRT conducted between 8 May and 15 June 2021. Bursts were detected in Band 4 (550–850 MHz) and Band 5 (1060–1460 MHz), with high-frequency activity ceasing after 24 May. On 28 May, multiple bursts were detected in Band 4 but none in Band 5, suggesting possible spectral evolution. Two burst pairs separated by less than 300 ms were identified, consistent with short repetition timescales or potential sub-second periodicity. The waiting time and energy distributions show a bimodal structure, indicating the presence of distinct emission modes. The fluence distribution follows a broken power-law, similar to other known repeating FRBs. These results provide constraints on the spectral and temporal behaviour of FRB 20201124A.

CRACO is the new Commensal Realtime ASKAP Fast Transient COherent upgrade searching in the image domain for FRBs with an expected 5 times higher sensitivity than the incoherent sum survey. During commissioning, CRACO probed a new parameter space of long FRB durations from 14 ms to 110 ms time resolution. We found two slower FRBs at the high end of the search range. The detections demonstrate the presence of a detectable population of not-so-fast radio bursts at timescales of hundreds of milliseconds. The scattering times of ~70 ms and 700 ms at 0.8 GHz are among the highest observed so far. The second FRB also shows scintillation from the Milky Way restricting the scattering screen to be close to the source. These highly scattered events at moderate to low distances (z=0.3247 and 0.04973, respectively) extend the observed scattering timescales to 7 orders of magnitude. This extent together with the placement of one scattering screen in the host galaxy questions the applicability of a proposed scattering-distance relation. The vastly different estimated host dispersion measures of ~120 and ~220 pc/cm3 also question the transferability of the pulsar scattering-DM relationship to FRBs.
 

"FRB 20240114A (R147) is a hyperactive repeating FRB discovered by CHIME/FRB in January 2024. Since its discovery, it has been extensively followed up across the electromagnetic spectrum, including X-ray and optical observations . Several telescopes like FAST, Parkes, Meerkat, etc. have detected hundreds to thousands of bursts from the source. Our uGMRT monitoring campaign (300–1460 MHz) started from 1st February 2024, with our recent study (Kumar et. al. 2024) reporting 60 bursts observed between 300–750 MHz. These bursts exhibit narrow emission bandwidths (~10%) and probe the lower end of the energy distribution. We also observe variations in burst activity, including a coincident burst storm reported by FAST. Preliminary indications suggest possible chromaticity in its burst activity, which, if confirmed, could provide crucial insights into the emission mechanisms of repeating FRBs.
Continued monitoring until March 2025 has yielded in detection of more than 100 additional bursts in Band-4 (550-750 MHz) with uGMRT after entering a quiet phase in August last year. Notably, we recently detected a bright burst in S-band (2–3 GHz) with the VLA on 31st March 2025, following renewed activity reported by the Hyperflash team earlier this year. We have also been observing with VLA across S-band to X-band (2–12 GHz) to study the spectral properties of the potential PRS associated with the FRB source. We will discuss our results, on bursts as well as the PRS, in the context of other recent multi-wavelength observations of FRB 20240114A and its associated candidate PRS, to provide a comprehensive picture of its activity and emission mechanisms."
 

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The mechanism of emission of bright radio flashes from Fast Radio Bursts (FRBs) remains an open question to date. From observations, FRBs are of two types - repeaters and one-off events. Some repeaters have been localised to their host galaxy, thereby shedding some light on the possible progenitors. Of these repeaters, FRB121102, FRB190520B and FRB20240114A stand out as the only events for which persistent radio emission associated with the FRBs has been seen. In this talk, I will describe our follow-up observations of the persistent radio source associated with FRB190520B using both the upgraded Giant Metrewave Radio Telescope and the Jansky Very Large Array and present the results in the context of various models that predict the emission and evolution of the persistent source associated with an FRB.

Fast Radio Bursts (FRBs) are brief yet highly energetic pulses of radio emission, the origin of which remains largely uncertain. FRBs are classified into two categories based on their repetition behavior: repeaters and non-repeaters. Distinct progenitor models have been proposed to account for these differences, with magnetars often associated with repeaters and cataclysmic events with non-repeaters. Therefore, elucidating the differences between these two populations is essential for constraining their underlying origins. However, the difficulty in accurately localizing FRBs has posed a significant challenge in confirming whether their progenitors are indeed distinct. In this study, we estimate the galaxy number density around FRBs listed in the CHIME catalog 1 by utilizing the WISE × PS1 galaxy catalog. Our methodology emphasizes the large-scale galactic environments surrounding FRBs, thereby it is independent of precise localization. This approach enables the inclusion of a significantly larger sample—26 repeaters and 238 non-repeaters—approximately twice the number of currently localized FRBs. If repeaters and non-repeaters originate in distinct galactic environments, it could imply different host and progenitor types. Conversely, similar environments might suggest a common progenitor. Here, we present our findings by comparing the density increments of both repeaters and non-repeater sources. The Kolmogorov-Smirnov (KS) test for the distributions of galaxy number densities around the FRB sources indicates no significant difference between repeaters and non-repeaters with a p-value of 0.405. Our finding suggests that repeaters and non-repeaters could share similar galactic environments and, hence, similar host and progenitor types. In addition to this, we find that the majority of FRBs occur in underdense galactic environments compared to randomly selected regions, exhibiting a mild preference for young stellar populations.

Radio interferometric observations, specially at low frequencies, are often hindered by radio frequency interferences (RFIs), making data processing a time-intensive challenge. With next-generation radio telescopes producing increasingly large datasets, the demand for automated data processing solutions has grown critical. We present GARUDA (Generic AI-based GMRT-tUned Radio Data Analysis pipeline), a novel automated pipeline designed for uGMRT data reduction. Written in Python and utilising modular CASA for calibration, GARUDA includes GNET, our custom Deep Learning based RFI detection model. With only two tunable parameters, GNET ensures flexibility and ease of use across diverse observations and frequency bands. The pipeline handles system issues and performs RFI excision, producing high-quality calibrated data ready for imaging. In this talk, I will present the capabilities of GARUDA, integrated with the LOFAR Transients Pipeline (TraP), for searching Long-Period Transients (LPTs) in GMRT archival data. This dataset spans nearly 20 years and offers adequate time resolution and sensitivity at low radio frequencies -- where LPTs are typically most luminous. We have processed a large set of Galactic plane observations from the GMRT archive and identified several intriguing transient candidates, which will also be highlighted.

The discovery of persistent radio sources (PRSs) associated with three repeating fast radio bursts (FRBs) has provided crucial insight into the local environments of these enigmatic sources. Here, we present deep radio observations of the fields surrounding four active repeating FRBs—FRB 20220912A, FRB 20240114A, FRB 20240619D and FRB 20230607A —using the upgraded Giant Metrewave Radio Telescope (uGMRT) at low radio frequencies and Karl G. Jansky Very Large Array  (VLA) at high frequencies. Towards FRB 20240114A, we report the detection of a compact radio source at 650 MHz with a flux density of 65.6 ± 8.1 μJy/beam. Our spectral index measurements, host galaxy star formation rate, and constraints on the physical size of the source strongly support the interpretation that this is a persistent radio source (PRS) associated with the FRB. We also present preliminary results on the variability of the PRS over a month-long baseline. For FRB 20220912A, while our uGMRT data indicate that the radio emission is likely associated with star formation in the host galaxy, we will also present high-resolution follow-up observations from the VLA across the C, X, Ku, and K bands (5–21 GHz). These reveal a compact radio source at the FRB location nature of which is still unclear. In addition, we will present very recent results from our imaging study of FRB 20230607A, a repeater with an extremely high rotation measure (RM ≈ 12,000 rad/m²), Using uGMRT Band 4 and Band 5. For FRB 20240619D, we place upper limits on radio emission from an associated PRS or from star formation in the host galaxy. The detection of the PRS associated with FRB 20240114A is a valuable addition to the small but growing sample of PRSs associated with FRBs, reinforcing the idea that such sources arise from a magnetoionic medium surrounding the FRB sources.

Giant pulses (GPs) are rare, and extremely energetic bursts of radio emission that can exceed the average pulse energy by factors of 100 or more ( Ershov & Kuzmin 2005). These are intrinsically short timescale phenomena, with individual subpulses having durations as brief as 2 ns (Hankins et al. 2003). Such “nanopulses” exhibit brightness temperatures as high as 1037 K. First revealed in the Crab pulsar (Staelin & Reifenstein 1968), GPs have since been identified in both young and millisecond pulsars (MSPs), typically localized to narrow phase windows and coinciding with high-energy X-ray emission, highlighting their likely origin in regions of strong magnetic field near the light cylinder. However, Giant pulses have been studied in detail in only a handful of MSPs (e.g. PSRs B1937+21 (Cognard et al. 1995), B1821−24 (Romani et al. 2001), and J1823−3021A (Knight et al. 2005))-in part because of the fast pulsar period, large dispersive smearing timescale, and relatively weak signal conspires to make single-pulse observations difficult. Interestingly, GPs have also been observed in slow pulsars lacking strong magnetic fields at the light cylinder, such as PSRs J1752+2359, B1112+50, and B0031−07, suggesting multiple physical channels for GP production. These bursts are often phase-stable and can form short temporal clusters, providing clues about magnetospheric processes and emission geometry. The SPOTLIGHT program—a real-time, commensal survey for pulsars and Fast Radio Bursts (FRBs) using the GMRT—has identified 10s of bright single pulses already within a week of deployment, motivating a systematic statistical study of pulse energy, phase localization, and morphology across both MSPs and normal pulsars. Such efforts allow us to examine correlations with intrinsic pulsar properties like magnetic field strength and spin-down luminosity. We aim to conduct a systematic statistical analysis of bright single pulses across a broader sample of normal pulsars as well as MSPs, focusing on energy distributions, pulse-phase localization, morphology, and variability. This will allow us to characterize the emission physics of these pulses and explore correlations with intrinsic pulsar properties such as spin-down luminosity and magnetic field strength. Notably, a moderate anti-correlation between profile stability and magnetic field strength in MSPs hints that stronger magnetic fields may destabilize pulse shapes, potentially enhancing the occurrence of bright pulses (Ghosh et al. 2025, in preparation). These investigations are especially relevant in the context of recent observations of plasma lensing in systems like PSR B1957+20 (Main et al. 2018), where narrowband amplification and temporal clustering of pulses have drawn parallels with the properties of repeating Fast Radio Bursts (FRBs), such as FRB 121102 (Main et al. 2018). Given the similar spectral and temporal behaviors, studying bright pulses from MSPs may offer a valuable window into the emission mechanisms of FRBs and their propagation through dense, dynamic magneto-ionic environments. Through this effort, we aim to bridge the phenomenology of giant pulses in pulsars with that of coherent bursts from other neutron star populations, including magnetars and FRBs
 

The Square Kilometre Array (SKA) is the most sensitive Radio Telescope to be deployed in the most radio-quiet parts of the world: African and Australian deserts. The first phase of the project, SKA1  will commission up to 197 dish antenna arrays in South Africa and up to 1,31,072 element aperture arrays in Western Australia. Together, these arrays will observe over an extensive frequency range from 50 MHz to about 15 GHz. These arrays will produce very high volume imaging and non-imaging data streams and support exploring a variety of radio astronomy problems. Complex hardware forms part of the digital backend, namely the Tile Processing Module(TPM). We are involved in characterizing and developing firmware features to form multiple beams for the SKA-Low telescope. We also contribute to the accelerated pulsar search associated candidate sifting using High Performance SOC FPGA. In this talk, I will provide an overview of firmware features developed for SKA-LOW beamforming especially for FRB-like transient search point of view, and provide an update on how we plan to test using Gauribidanur Observatory facilities and also present challenges involved in candidate sifting during a search and present our approaches towards solving them.

"Magnetars are highly magnetised neutron stars and are considered leading candidates for explaining Fast Radio Bursts (FRBs), at least a subset of them. Repeating FRBs, in particular, often exhibit band-limited bursts. Intriguingly, similar spectral characteristics have been observed in radio bursts from the Galactic magnetar J1809-1943. If such features are confirmed to be intrinsic to the source and not a result of propagation through the interstellar medium or instrumental effects, they would offer strong support for a direct physical connection between magnetars and repeating FRBs.
In this work, we have developed a pipeline to systematically search for such narrowband bursts. We further characterise the spectral properties of the detected bursts and provide evidence that the observed emission is intrinsic to the source. These findings contribute not only to bridging the gap between magnetars and FRBs, but also to advancing our understanding of magnetar radio emission mechanisms.

The association of quasi-steady persistent radio sources (PRSs) with a few repeating fast radio bursts (FRBs) offers a valuable testbed for examining the magnetar progenitor hypothesis. A widely favored interpretation attributes the PRS emission to synchrotron radiation from highly charged electron-positron pairs in a magnetar wind nebula. Observational probes—including radio imaging, scintillation studies, and equipartition analysis—consistently point to a very compact source size. This compactness strongly disfavors scenarios involving rapid expansion, such as those expected from millisecond magnetars formed in superluminous or ultra-stripped supernovae. In this talk, I will show that the observed PRS properties are naturally explained by a magnetar wind nebula powered by the decay of the internal magnetic field of a magnetar formed in a sub-energetic supernova, with an initial spin period of a few tens of milliseconds. This scenario also leads to clear observational predictions at both ends of the PRS spectrum: a synchrotron self-absorption break near 200 MHz and a cooling break around 150 GHz—features that can be tested with current radio telescopes.

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Now approaching completion, the TRAPUM (TRAnsients and PUlsars with MeerKAT) project has ushered in a new era of pulsar discovery. Over its 5 year campaign, TRAPUM has systematically targeted globular clusters, nearby galaxies and high-energy sources lacking known radio counterparts, yielding hundreds of new pulsars—including a remarkable population of fast-spinning millisecond pulsars (MSPs) as well as slow pulsars. Among these are numerous exotic binaries, such as black widow and redback systems, double neutron star systems as well as a surge of new pulsars in the Magellanic Clouds. A highlight is a candidate neutron star–black hole binary in NGC 1851, potentially probing the elusive LIGO “mass gap.”

These discoveries have been enabled by TRAPUM’s dedicated multibeam beamformer and GPU-based high-time-resolution processing system, technologies that have dramatically expanded MeerKAT’s capability for wide-field, sensitive pulsar searches. This infrastructure has also allowed quasi-real-time data analysis, demonstrating the survey’s potential as a technical and scientific pathfinder for the SKA.

As TRAPUM nears its conclusion, its instrumentation, methodologies, and scientific outcomes highlight the transformative power of interferometric pulsar surveys and provide crucial lessons for the next generation of large-scale radio time-domain projects.

We present results for searches for astrophysical neutrinos from pulsars, magnetars,  and FRBs. We show that the combined Super-Kamiokande and MACRO data show a  2.6 sigma spatial coincidence excess from PSR B1509-58 and then propose  additional tests to ascertain if this excess corresponds to an astrophysical signal . We then present results for searches for TeV energy neutrinos from pulsars,magnetars,  and FRBs using the publicly released  IceCube 10-year point source catalog.

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