2.1 Hardware

ASKAP is located at Inyarrimanha Ilgari Bundara, the CSIRO Murchison Radio-astronomy Observatory (MRO), a site selected for having low levels of radio-frequency interference (RFI). The array comprises 36 12-m antennas. The maximum baseline length of the antennas is 6 km. Each antenna is equipped with a phased array receiving system (PAF; Hay Reference Hay2007), enabling multiple quasi-independent beams to be digitally formed on the sky. This increases the field of view of the telescope by a factor of approximately 30 over an equivalent single-element system.

In this section, we briefly summarise aspects of the ASKAP hardware and signal path relevant to the searches described here. Hotan et al. (Reference Hotan2021) describe the general ASKAP hardware and standard ASKAP imaging system in more detail. A schematic diagram describing the FRB search and localisation systems is found in Fig. 4.

Figure 4. CRAFT/ICS search system. The dashed boxes indicate processesing stages operated within the telescope digital receiving system, antenna beamformers, and the CRAFT server (labelled ‘CRAFT Box’), respectively

Each PAF receiver comprises 188 dipole elements arranged in a chequerboard pattern. The signal from each dipole element is transmitted from the PAF to the MRO control building via radio frequency over fibre systems (Beresford et al. Reference Beresford2017). Observing is undertaken in one of three bands (bands 1,2, and 3, with 1 being the lowest and 3 the highest). Within each band, it is possible to tune the observing frequencies best suited to the science goals. The signal from each element is then digitised and channelised in a digital receiver (Brown et al. Reference Brown2014). The signals are channelised using a polyphase filter into coarse 1 MHz channels oversampled by a factor of 32/27 (Tuthill et al. Reference Tuthill2012).

Digital beamformers then combine signals from the dipoles to form beams on the sky through appropriate weighting of each dipole element (van Veen & Buckley Reference van Veen and Buckley1988; Hampson et al. Reference Hampson2014). In typical survey observations, 36 beams are produced in either square or hexagonal close pack arrangements. The separation between the beams is tailored to the goals of the observations, but varies between $0.75$ and $1.05$ $\deg$ , with beam separation largely guided by spacing of the frequency-dependent primary beam response, resulting in larger beam separation at lower frequencies. The beam weights are determined initially through observations of the Sun. While the weights are invalidated when certain changes to the observing system are made (e.g. changes between observing bands), they can be re-derived using an on-dish calibration solution (Hotan et al. Reference Hotan2021). Up until this point, the data products are common between FRB detection mode and standard ASKAP synthesis-imaging observations.

The beamformers produce two data products used by the CRAFT/ICS systems. The first is total power summed over both polarisations for each coarse channel, integrated over $\approx 1$ ms timescale, at 1 MHz frequency resolution. These signals are broadcast over a network using unicast data protocol, and ingested by the CRAFT server where they are searched (as discussed in the next section). The second set of data products essential to the survey are voltages. Each beamformer contains random access memory that is configured in a series of ring buffers. For the searches presented here, a ring buffer is created for each beam for all of the antennas used in the searches. The voltages can currently be recorded with 1-bit, 4-bit, or 8-bit depth. For all data presented here, we have used 4-bit depth, which enables 3.1 s length voltage buffers. The relatively short buffer length necessitates a low-latency search pipeline (discussed in the next section). When the search pipeline detects a candidate FRB, the pipeline is stopped and the voltage buffers frozen. Voltages for both polarisations from the candidate beam for each antenna are then downloaded to the CRAFT server. Both data products provide a total of 336 MHz of bandwidth, in contrast to the 288 MHz bandwidth available from the standard ASKAP hardware correlator. Observations when the array operates in high-frequency resolution (zoom mode) observing are not compatible with the searches.

2.2 FRB searches

The primary motivation for implementing the ICS search method is the relative ease of computation compared to array-coherent approaches. The searches require only 36 data streams, fewer than those required for the previous fly’s eye searches. Array-coherent approaches require either imaging a large number of pixels for each phased array beam, or forming a similarly large number of tied array beams. The CRAFT server ingests the integrated intensities from each polarisation for each beam. These are summed (after rescaling to ensure each stream had zero mean and the same variance) to create a pseudo total intensity, after synchronising data from each antenna beamformer to ensure temporal alignment.

Despite the MRO having low levels of nearby interference, RFI is present in the searches. The largest sources of interference are satellite interference from global navigation systems in band-2 observations and ionospheric ducting of mobile phone signals (base towers and handsets) in band 1. Data were also affected by interference associated with lightning and electrical storms (even when storms were more than 100 km from the observatory). Real-time RFI flagging is conducted using a number of heuristics. Frequency channels with abnormally high kurtosis are set to zero, while remaining channels are normalised to a mean of zero and unit standard deviation. Impulsive RFI is removed by subtracting the frequency integrated signal at zero dispersion measure (DM). This is applied dynamically – additionally, a hard-coded list of known RFI channels is maintained, and these frequencies are zeroed for all observations. The methods were developed during commissioning of the ICS system (and the previous fly’s eye survey), with the algorithms tuned to reduce the false positive rate. The fraction of data flagged depended on the observing band, and was typically 10–20%. The level of false trigger varied between bands. In the band 1, after flagging there could be cases where there were no false triggers for many days. In band 2, false triggers would occur at a rate of a few per day to one per hour. In the presence of electrical storms, lightning produce false triggers at rate of many per hour. The effectiveness of the mitigation was tested through observations of pulsars. We confirmed that we were detecting the pulses at the expected rate and signal to noise ratio as had been conducted for the fly’s eye survey (James et al. Reference James2019b).

Searches are conducted using the FREDDA code (a Fast Real-time Engine for De-Dispersing Amplitudes, Bannister et al. Reference Bannister, Zackay, Qiu, James and Shannon2019a; Qiu et al. Reference Qiu, Keane, Bannister, James and Shannon2023), which is a graphical processing unit (GPU) implementation of a fast dispersion measure transform (Zackay & Ofek Reference Zackay and Ofek2017). Searches for all beams can be conducted on a single GPU.

The searches produce a stream of raw candidates (time, signal-to-noise ratio, dispersion measure, width) which are broadcast over User Datagram Protocol. A burst (either RFI or a bona-fide FRB) produces candidates over a region of candidate parameter space. A density-based spatial clustering algorithm (Ester et al. Reference Ester, Kriegel, Sander and Xu1996) is used to group raw candidates. This is important as it allows RFI (which typically has the greatest S/N at low DM) to be distinguished from FRBs. Candidates were clustered using based on time (expressed as sample number within the scan), boxcar width, and dispersion measure (expressed as integer DM trial reported by FREDDA). The density based spatial clustering algorithm used parameters $\epsilon=1$ and $n_\mathrm{min}= 1$ in the clustering. To ensure that the real-time clustering algorithm was working properly, raw candidates were also inspected off-line after being clustered using a friends-of-friends algorithm (Huchra & Geller Reference Huchra and Geller1982). The friends of friends algorithm clustered based on DM (measured as integer DM units in FREDDA) and time (measured as samples within a scan). The temporal clustering was normally set to a distance of 32 samples. DM clustering was set to a distance of 20 integer DM units.

The search latency ranges from a few hundred milliseconds to a few seconds. The time resolution of searches varied over the course of the survey, between $860\,\mu$ s and $1.7$ ms, as system performance was optimised. There is a trade-off between the number of antennas that can be ingested and the time resolution. For the majority of the searching, a time resolution of $1.182$ ms was chosen, which allowed the incoherent sum of intensities from $\sim$ 24 antennas to be formed.

2.3 Localisations

When a candidate FRB is detected, the voltage buffers are stopped and the beam-based buffers in which the burst is found are downloaded from the antenna beamformers to the CRAFT server. They are then transferred offsite for further processing. As the searches stop on the first clustered candidate above a fixed signal-to-noise (S/N) ratio this is not necessarily the in which the burst has the most significant detection. In rare cases (e.g. very bright bursts, or bursts equally spaced between multiple beams), the beam downloaded was not the beam in which the FRB had the maximum S/N ratio. Latency in the search pipeline and the short duration of the voltage buffers meant that for some FRBs the voltage buffer was of insufficient length to save the highest frequency emission. This is especially the case for the most dispersed FRBs, for which dispersed emission could extend over most of the voltage buffer. If a candidate is confirmed (through visual inspection of the search data stream), additional observations are conducted for calibration. This included an observation of a bright compact radio galaxy (PKS 1934 $-$ 638 or PKS 0407 $-$ 658) to calibrate the bandpass, and a pulsar (PSR J0834 $-$ 4510, PSR J1644 $-$ 4559, or PSR J2048 $-$ 1616) as a polarisation reference. A detailed description of the calibration, localisation, and astrometric performance is presented in Day et al. (Reference Day2021). An end-to-end pipeline (CELEBI, The CRAFT Effortless Localisation and Enhanced Burst Inspection pipeline) processes voltage data, both to measure burst positions and produce high time resolution spectro-polarimetric data products (discussed in more detail in the next section). It is described in detail in Scott et al. (Reference Scott2023).

2.4 High time resolution spectropolarimetry

Access to the voltage data allows us to study in detail the spectro-temporal-polarimetric properties of the bursts. These studies provide insight into burst emission physics, as well as the effects of propagation through intervening ionised media, for example through the measurement of scatter broadening times and rotation measures. This was done through high time and frequency resolution imaging (Day et al. Reference Day2020) and through high time resolution beamforming (Cho et al. Reference Cho2020; Scott et al. Reference Scott2023). The technique of high time resolution imaging (Day et al. Reference Day2020) did not provide the same time resolution possible through beamforming ( $54\,\mu$ s). It was a natural and (relatively) easily implemented extension of FRB burst localisation pipelines prior to the development of a tied array beamforming pipeline. As the upstream ASKAP digital system implements channelisation through oversampled filterbanks, it is possible to invert the 1 MHz coarse channels of the voltage buffers to produce time series with temporal resolution as high as the Nyquist sampling rate of the digital receiving system ( $1/(336\,\mathrm{MHz}) \approx 3$ ns). Using both methods, polarisation calibration was conducted by using a bright pulsar as a reference source to correct for polarisation leakage. Rotation measures can be inferred using a Bayesian methodology described in Bannister et al. (Reference Bannister2019b).

4.1 Optical and infrared photometry

After obtaining high precision FRB positions, we first searched for FRB host-galaxy candidates. The FRB coordinates were first checked against available imaging archives, photometric and spectroscopic catalogues using tools such as the Data Aggregation Service (DAS) (Miszalski et al. Reference Miszalski, O’Toole, Tocknell, Marnoch and Ryder2022). While some of the lower-DM FRBs had an apparent host galaxy identified in wide-field surveys such as the Sloan Digital Sky Survey (SDSS; Alam et al. Reference Alam2015), the Pan-STARRS 3 $\pi$ survey (PS1; Chambers et al. Reference Chambers2016), or the Dark Energy Camera Legacy survey (DECaLS; Dey et al. Reference Dey2019), the majority of ASKAP-detected FRBs had little or no reliable photometry or spectroscopy available for potential host-galaxy candidates. We therefore obtained our own multi-band photometry to both identify the host galaxies and model the host galaxy properties including total stellar mass and star formation history. Photometric observations of the host galaxies were taken predominantly using the FOcal Reducer and low dispersion Spectrograph (FORS2) instrument on the VLT (Appenzeller & Rupprecht Reference Appenzeller and Rupprecht1992); Gemini Multi Object Spectograph (GMOS-S) on Gemini-South (Hook et al. Reference Hook2004); or the Low Resolution Imaging Spectrometer (LRIS) on Keck (Oke et al. Reference Oke, Crawford and Craine1994). Infrared imaging observations were also undertaken with the HAWK-I (Kissler-Patig et al. Reference Kissler-Patig2008) instrument on the VLT, usually in combination with a ground layer adaptive optics module (GRAAL). Photometric data reduction strategies are described in detail elsewhere (e.g. Heintz et al. Reference Heintz2020; Marnoch et al. Reference Marnoch2023; Glowacki et al. Reference Glowacki2023).

4.2 Host associations

Central to establishing the redshift of an FRB is to identify its host galaxy. Our approach for the well-localised FRBs of the CRAFT/ICS survey has been to implement the Probabilistic Association of Transients to their Hosts (PATH) formalism introduced in Aggarwal et al. (Reference Aggarwal2021). The PATH methodology inputs the localisation region of the FRB and the position and apparent magnitudes of all candidate galaxies within or near that region. The analysis requires prior assumptions on the probability of the host being unobserved in the image, the distribution of host galaxy magnitudes, and the offset angular separations of FRBs from the centre of the galaxy. For galaxy magnitudes, we adopt an uninformative prior that weights galaxies inversely proportional to their number density on the sky. For the separations, Aggarwal et al. (Reference Aggarwal2021) adopted an exponential profile with scale length equal to an angular size metric of the galaxy, specifically the semimajor_sigma parameter of the photutils software package ( $\phi$ ).

We revisit this assumption and suggest an updated formulation for this offset prior. Fig. 6 shows the normalised PDF of the angular offsets $\theta$ relative to $\phi$ for 32 FRBs. This FRB sample was restricted to the ICS sample presented in this manuscript with a secure association (see Section 5.2) and with ${P_{\mathrm{host}}} \unicode{x003E} 0.90$ using the original PATH analysis and priors. We also include the ASKAP-localised CHIME repeating source FRB 20201124A (Fong et al. Reference Fong2021). Approximately half of the sample shows $\theta/\phi \unicode{x003C} 1$ with the remainder exhibiting a tail to $\theta/\phi \approx 5$ .

Figure 6. Comparison of PATH prior distributions (curves) to FRB offsets (histogram) obtained through CRAFT/ICS observations. Here we have restricted to those FRBs with PATH posteriors $P(O|x)$ in excess of 0.9 using the original priors. This corresponds to the grey curve which is an exponential with scale length equal to the half-light radius of the galaxy $\phi$ . We now advocate the prior described by the black curve with scale-length equal to $\phi/2$ .

Overplotted on the observed distribution are the exponential priors for host galaxy offset with scale lengths of $\phi$ and $\phi/2$ . These have been convolved with the reported uncertainties in the FRB localisations. They have also been weighted by a geometrical factor ( $2\pi\theta$ ) which disfavours low offsets.Footnote ^d Clearly, the exponential with scale-length of $\phi$ is disfavoured while the data are reasonably well-described by the smaller scale length ( $\phi/2$ ). We advocate adopting this new prior for future work on FRBs with PATH, and we utilise it throughout the manuscript. It is also possible as the sample continues to increase that one will adopt a different functional form to better describe the distribution.

Reanalysing all of the FRBs presented in Bhandari et al. (Reference Bhandari2020b), we find few changes in the posterior probabilities. Most of them were previously ${P_{\mathrm{host}}} \unicode{x003E} 0.95$ and the values increased towards 1. The only notable changes were significant increases in ${P_{\mathrm{host}}}$ for FRB 20181112A and FRB 20191001A. The former FRB is associated with a $z=0.4755$ which has a $z=0.3674$ galaxy in the foreground (Prochaska et al. Reference Prochaska2019) The latter FRB is associated with a $z=0.2340$ galaxy which is separated by $\approx 5$ ” from a galaxy at a similar redshift ( $z=0.2339$ Bhandari et al. Reference Bhandari2020a). In Tables C1 and C2 in the Appendix we present PATH probabilities for nearby host galaxies for all ASKAP-localised FRBs.

4.3 Optical spectroscopy

We obtained spectroscopic observations of the probable host galaxy candidates that lacked archival data, both to determine the redshift but also to study the global properties of the hosts. These were primarily obtained with FORS2 or X-shooter (Vernet et al. Reference Vernet2011) on the VLT, or LRIS or the Deep Imaging Multi-Object Spectrograph (DEIMOS; Faber et al. Reference Faber, Iye and Moorwood2003) on Keck. Brighter host galaxies were observed with the Goodman Spectrograph on the Southern Astrophysical Research Telescope (SOAR, Clemens, Crain, & Anderson Reference Clemens, Crain, Anderson, Moorwood and Iye2004). Spectroscopic data reduction is described in detail in Glowacki et al. (Reference Glowacki2023), Gordon et al. (Reference Gordon2023), Ryder et al. (Reference Ryder2023), and A. Muller et al. (in prep). Uncertainties in the redshifts derived from spectroscopy are approximately $0.0001$ for X-shooter and $0.0005$ for other instruments.

Integral field unit (IFU) and multi-object spectroscopy enabled more detailed spatially resolved studies of the host galaxies and the mapping of structure foreground to the FRB host through spectroscopic identification and characterisation of galaxies close to the line of sight. We have obtained IFU spectroscopy of some of the FRB hosts with the Multi Unit Spectroscopic Explorer on the VLT (Bacon et al. Reference Bacon, McLean, Ramsay and Takami2010) and with the Keck Cosmic Web Imager (Morrissey et al. Reference Murphy2018). Wider-field spectroscopic study of host galaxy foregrounds was also taken with the Anglo Australian Telescope’s AAOmega and two-degree field (2dF) fibre-fed multi object spectrograph (Smith et al. Reference Smith, Moorwood and Iye2004), in collaboration with the FLIMFLAM project (Lee et al. Reference Lee2022; Khrykin et al. Reference Khrykin2024).

4.4 Radio and high energy follow-up

We also searched for sources spatially coincident with the FRBs and their hosts across the electromagnetic spectrum.

Radio-wavelength follow-up entailed searches for persistent radio sources sometimes associated with (repeating) FRBs, extended radio continuum emission (most likely associated with star formation) and spectral lines (especially targeting the 21-cm Hydrogen hyperfine transition at decimetre wavelengths and carbon monoxide transitions at millimetre wavelengths). Observations at radio wavelengths of the FRB hosts were made with the Atacama Large Millimeter/submillimeter Array (e.g. Chittidi et al. Reference Chittidi2023), Australia Telescope Compact Array (ATCA, e.g. Bhandari et al. Reference Bhandari2022), Jansky Very Large Array (JVLA, e.g. Bhandari et al. Reference Bhandari2023), and MeerKAT (e.g. Glowacki et al. Reference Glowacki2024). Some of these observations (particularly those made with ATCA) were also used for the first FRBs discovered in order to reference radio continuum sources in images produced from the 3-s voltage dumps with the International Celestial Reference Frame. As our understanding of the astrometric precision of the 3-s images improved this was no longer necessary (Day et al. Reference Day2021).

We also searched for X-ray emission from a sample of our hosts using the Chandra X-ray observatory (Eftekhari et al. Reference Eftekhari2023). Such emission could be associated with coincident Active Galactic Nuclei, or Ultra-luminous X-ray sources.

5.1 Previously reported FRBs

We briefly summarise the key properties of the previously published ICS FRBs, including motivation for the observations in which they were found.

FRB 20180924B– The first FRB localised in the ICS survey was reported in Bannister et al. (Reference Bannister2019b). It was discovered in one of the $|b|=50$ Galactic latitude fields used in the previous fly’s eye survey (Shannon et al. Reference Shannon2018) during a dedicated time allocation from the ATNF to secure a FRB localisation. The FRB host galaxy was initially speculated to be either a lenticular or early-type spiral galaxy; however subsequent observation and analysis indicates it to be the latter type from both detailed study of the host galaxy spectral energy distribution (Gordon et al. Reference Gordon2023), and high spatial resolution imaging with HST (Mannings et al. Reference Mannings2021) that showed the presence of spiral arms, with one of the arms coincident with the FRB localisation.

FRB 20181112A– The discovery and localisation was first reported in Prochaska et al. (Reference Prochaska2019). The FRB was discovered in one of the $|b|=50$ Galactic latitude fields used in the previous fly’s eye survey (Shannon et al. Reference Shannon2018).

FRB 20190102C– The discovery and localisation was first reported in Macquart et al. (Reference Macquart2020). The FRB was discovered in the circumpolar R.A. $=22$ h, Decl. $=-80$ field.

FRB 20190608B– The discovery and localisation was first reported in Macquart et al. (Reference Macquart2020). The FRB was found during an attempt to localise FRB 20171019A, an FRB discovered in the fly’s eye survey (Shannon et al. Reference Shannon2018) from which repetitions had been detected with the GBT (Kumar et al. Reference Kumar2019). A high-resolution imaging and kinematic study of the host galaxy by Chittidi et al. (Reference Chittidi2021) showed the FRB to be closely associated with star formation in a spiral arm.

FRB 20190611B– The discovery and localisation was first reported in Macquart et al. (Reference Macquart2020). The FRB was discovered in the circumpolar R.A. $=22$ h, Decl. $=-80$ field. The FRB has the largest DM deficit relative to the Macquart relation of any FRB discovered in the CRAFT/ICS survey. The veracity of the host association has been questioned based on this (Cordes, Ocker, & Chatterjee Reference Cordes, Ocker and Chatterjee2022).

FRB 20190711A– The discovery and localisation was first reported in Macquart et al. (Reference Macquart2020). The FRB was discovered in the circumpolar R.A. $=22$ h, Decl. $=-80$ field. This is the only FRB discovered in the ICS survey that has been observed to repeat in our follow-up observations (Kumar et al. Reference Kumar2021).

FRB 20190714A– The discovery and localisation was reported in Heintz et al. (Reference Heintz2020). Only one of the voltage polarisation data streams was able to be downloaded for the FRB, making polarimetric analysis of the burst properties difficult to undertake.Footnote ^e The FRB was discovered in one of the $b=50$ Galactic latitude fields used in the previous fly’s eye survey (Shannon et al. Reference Shannon2018). A wide-field spectroscopic survey around the FRB 20190714A sight line (Simha et al. Reference Simha2023) shows a clear excess of foreground galaxy halos that contributes $\sim$ 2/3 of the observed extragalactic DM.

FRB 20191001A– The discovery and localisation was reported in Bhandari et al. (Reference Bhandari2020a). The FRB was detected commensally with pilot survey observations for the Evolutionary Map of the Universe (EMU) survey science project (Norris et al. Reference Norris2021). The burst was sufficiently bright to be detected as an image-plane transient in 10-s hardware correlator visibilities.Footnote ^f

FRB 20191228A– The discovery and localisation was reported in Bhandari et al. (Reference Bhandari2022). The FRB originated just 2 arcmin from Fomalhaut ( $\alpha$ PsA), complicating optical identification and redshift determination for the host galaxy. The FRB was discovered commsensally in observations for the DINGO survey (Rhee et al. Reference Rhee2023) targeting the GAMA-23 field.

FRB 20200430A– The discovery and localisation was reported in Heintz et al. (Reference Heintz2020). The FRB was detected commensally in test observations for the first low-frequency epoch of the Rapid ASKAP Continuum Survey (RACS, McConnell et al. Reference McConnell2020).

FRB 20200906A– The discovery and localisation was reported in Bhandari et al. (Reference Bhandari2022). The FRB was detected in observations searching for repetitions from FRB 20171116A, which had been detected in the ASKAP Fly’s Eye Survey (Shannon et al. Reference Shannon2018). It had been selected for follow up because of its relatively large pulse width, which may be correlated with being a repeating FRB (Connor, Miller, & Gardenier Reference Connor, Miller and Gardenier2020; Pleunis et al. Reference Pleunis2021). Only seven antennas were recording CRAFT data during the observation. The search system would select antennas for recording based on the number of antennas that were on-source at the beginning of an observation. Occasionally, antennas would arrive on source ascynchronously, resulting in smaller subsets of antennas being used in the searches and localisation.

FRB 20210117A– The discovery and localisation was reported in Bhandari et al. (Reference Bhandari2023). The FRB was detected commensally with observations for the mid-frequency RACS survey (Duchesne et al. Reference Duchesne2023). The FRB was found to be originating from a dwarf galaxy with a high host excess DM, similar to archetypal repeating sources FRBs 20121102A and 20190520B (Chatterjee et al. Reference Chatterjee2017; Niu et al. Reference Niu2022).

FRB 20210320C– The discovery and localisation were reported in James et al. (Reference James2022b) and Gordon et al. (Reference Gordon2023), respectively. The FRB was discovered in one of the $|b|=50$ Galactic latitude fields used in the previous fly’s eye survey (Shannon et al. Reference Shannon2018).

FRB 20210807D– The discovery and localisation were reported in James et al. (Reference James2022b) and Gordon et al. (Reference Gordon2023), respectively. The FRB was discovered during time-lapse photography of ASKAP being undertaken for a documentary, demonstrating the ability for the survey to be commensal with non-scientific observations. The FRB was wider than the width threshold for voltage download, but was sufficiently bright to be localised in hardware-correlator 10-s visibilities like FRB 20191001A (Bhandari et al. Reference Bhandari2020a).

FRB 20211127I– The discovery and localisation were reported in James et al. (Reference James2022b) and Gordon et al. (Reference Gordon2023), respectively. The FRB was detected commensally in Widefield ASKAP L-band Legacy All-sky Blind Survey (WALLABY) (Koribalski et al. Reference Koribalski2020) pilot survey observations towards the NGC 5044 group, but is not associated with the group. Glowacki et al. (Reference Glowacki2023) present an analysis of the FRB and the commensal detection of HI from the host galaxy.

FRB 20211203C– The discovery and localisation were reported in James et al. (Reference James2022b) and Gordon et al. (Reference Gordon2023), respectively. This FRB was detected commensally in POlarisation Sky Survey of the Universe’s Magnetisation (POSSUM) (Gaensler et al. Reference Gaensler, Landecker, Taylor and POSSUM2010) pilot-survey observations.

FRB 20211212A– The discovery and localisation were reported in James et al. (Reference James2022b) and Gordon et al. (Reference Gordon2023), respectively. The FRB was discovered in one of the $|b|=50$ Galactic latitude fields used in the previous fly’s eye survey (Shannon et al. Reference Shannon2018). This was also the first FRB detected in the ASKAP high band (at a central frequency of $1\,632.5$ MHz)

FRB 20220105A– The discovery and localisation was reported in Gordon et al. (Reference Gordon2023). The FRB was detected commensally with the first epoch of the RACS high band survey.

FRB 20220610A– The discovery and localisation was reported in Ryder et al. (Reference Ryder2023). Subsequent imaging with the Hubble Space Telescope revealed the burst originated from a compact galaxy group at redshift $z=1.016$ (Gordon et al. Reference Gordon2024). The FRB was discovered in observations attempting to identify repetitions from ASKAP-discovered (but poorly localised) FRB 20220501A (discussed further in Section 5.2.2).

FRB 20230718A– The discovery and localisation was reported in Glowacki et al. (Reference Glowacki2024). The host galaxy was identified through 21-cm HI emission using the MeerKAT radio telescope. The FRB was detected commensally with WALLABY survey observations, but the ASKAP hardware correlator data stream had a technical error and the WALLABY spectral line data was unusable. A DECam image of the field is shown in Fig. 1.

FRB 20201124A– In addition to FRBs discovered by CRAFT, we also localised one repeating FRB initially discovered by another facility. The detection and localisation of this repeating FRB source was reported in Fong et al. (Reference Fong2021). The FRB was first detected by CHIME. In April 2021, The CHIME/FRB Collaboration (2021) reported an episode of increased activity from the burst source, which motivated follow up with ASKAP. In total 11 bursts were detected by ASKAP from the source (Kumar et al. Reference Kumar2022). The brightest of these bursts was detected with high significance (S/N > 10) in 20 beams that spanned the phased array feed. As the FRB detection system triggers off the first significant candidate, voltages of the first localised burst from this source were downloaded from a beam adjacent to the primary detection.

5.2 New localised FRBs

We summarise the properties and localisations of a few other FRBs discovered in the ICS searches, though detailed analyses of the bursts and their host galaxies are deferred to subsequent studies.

5.3 Poorly localised FRBs

During the ICS searches we detected a sub sample of FRBs for which we were unable to obtain interferometric positions. This was usually due to the absence of a voltage download. Fortunately, in one case (FRB 20210807D), as noted above, the burst was sufficiently bright to be detected in commensal image-plane 10-s images. This was not possible for other bursts because they were either too faint or the hardware correlator was not recording data (as was the case in the filler observing mode). Nonetheless, the bursts represent detections with the ICS search pipeline so should be considered when modelling the FRB population.

FRB 20200627A was detected in a filler observation in a field targeting the fly’s eye FRB 20180131A (Shannon et al. Reference Shannon2018). The burst width exceeded that for the threshold for downloading voltages.

FRB 20210214A was detected during a pulsar check observation of PSR B0031-07. During pulsar check observations voltage downloading is disabled. While the majority of these were of two pulsars in the Galactic plane, PSR B0833-45 and PSR B1641-45 (being high DM so having more stable flux density in the ASKAP bands as they are less affected by diffractive scintillation), PSR B0031 $-$ 07 was observed when the others were not visible.

FRB 20210809C was detected commensally with time-lapse filming of the array for a documentary, as was the case for FRB 20210807D. As with FRB 2020627A the burst duration was too long to trigger a voltage download. However, the burst was insufficiently bright to be detected in 10-s visibilities.

FRB 20220531A was detected during a bandpass calibration observation for the hardware correlator visibilities. The array switched observing bands without having a voltage calibration observation conducted.Footnote ^g It may potentially be possible to calibrate the data using PKS 1934 $-$ 638 as an off-axis calibrator, but this has not been attempted.

FRB 20230521A was detected during FLASH survey observations. This was the first FRB detected in the lowest frequency band used by ASKAP (the central frequency is set to $832.5$ MHz). The burst width failed to meet the criteria for voltage download. The burst was confirmed in routine inspection of FRB candidates.

FRB 20231006A was detected during a bandpass observation. Only a subset of the voltages for the FRB were downloaded (for a subset of antennas and a single polarisation), as voltage downloads stopped at the end of the short scan. No attempt has been made to further localise this FRB.

6.1 Survey detection rates

Given the commensal nature of a large portion of the survey it is important to assess how detection rates depending on the nature of the underlying observing programmes which observed over a wide range of Galactic latitudes across the entire available ASKAP band.

When assessing the detection rate, it is important to consider the range of central frequencies of the observations. Fig. 7 shows the distribution of survey times per central frequency. Nominally, we classify observations into three categories: 900 MHz ( $\overline{\nu} \unicode{x003C} 1$ GHz), 1.3 GHz (1 GHz $\unicode{x003C}\overline{\nu} \unicode{x003C} 1.5$ GHz), and 1.6 GHz ( $\overline{\nu} \unicode{x003E} 1.5$ GHz), reflecting the three bands used for ASKAP observing. While the Fly’s Eye survey was conducted exclusively at 1.3 GHz, the ICS survey was conducted at a range of frequencies – many of the ASKAP survey projects have chosen to observe at lower frequencies to avoid interference from global navigation system satellites.

Figure 7. Histogram of observation time for ASKAP in ICS mode as a function of central observing frequency.

The cumulative detection rate is plotted against observation hours in Fig. 8. ASKAP ICS observations have detected, on average, one FRB per 414 h, with the rates in each of the three frequency bands being once per 533, 326, and 383 h for 900 MHz, 1.3, and 1.6 GHz respectively. These rates are lower than expected when compared to that found during observations in Fly’s Eye mode (20 FRBs in 1 274.6 days, i.e. one FRB per 1 530 hr; Shannon et al. Reference Shannon2018; James et al. Reference James2019b). The sensitivity in ICS mode is expected to scale as $N_\mathrm{ant}^{1/2}$ with the number of antennas, and hence the rate should vary as $N_\mathrm{ant}^{3/4}$ , assuming a Euclidian distribution of bursts. For $\sim25$ antennas being used simultaneously, this implies a rate of once per 137 h, i.e. 2.5 times higher than the 1.3 GHz ICS rate. The cause of this deficit is so far unexplained.

Figure 8. Cumulative total survey time for ICS observations to the end of 2023 as a function of date, and cumulative time divided according to approximate central frequency (dotted lines). This is compared to cumulative FRB discoveries (solid lines). The vertical dashed lines denote when different versions of FREDDA were used in the analysis.

6.2 Modelling frequency dependence

We model the frequency dependence of the detection rate $R(\nu)$ to be

(1) \begin{eqnarray}R(\nu) & \propto & T(\nu) F(\nu) W(\nu) N_\mathrm{ant}^{3/4} \nu^{\alpha}\,, \end{eqnarray}

where $T(\nu)$ describes the dependence on the observing system, $F(\nu)$ the dependence on the beam shape, $W(\nu)$ on the effective width, and the factor $\nu^\alpha$ represents the intrinsic dependence of the FRB rate on observation frequency with the rate index $\alpha$ . In all cases, we assume a Euclidean dependence of the rate on the detection threshold, that is, $R \propto F_\mathrm{th}^{-3/2}$ (see Section 6.4). The term $T(\nu) \propto T_\mathrm{sys}^{-3/2}$ , reflecting the frequency-dependent system temperature from Hotan et al. (Reference Hotan2021). F is the ‘footprint’ term, calculated as

(2) \begin{eqnarray}F & = & \int B^{3/2} d\Omega,\end{eqnarray}

for the beam values B calculated as the envelope over 36 Gaussian beams (in either a hexagonal ‘closepack 36’ or ‘square 6x6’ configuration, with pitch angles varying from 0.72 $^\circ$ –1.1 $^\circ$ ), full width half maximum of $1.1 \lambda/D$ , (where $\lambda$ is the wavelength of the emission and D in the 12-m antenna diameter) and peak amplitude depending on offset from boresight according to Hotan et al. (Reference Hotan2021), where $\lambda$ is the wavelength. The ‘width factor’, W, is due to the effective width (and hence the threshold: $F_\mathrm{th} \propto W^{1/2}$ ) of FRBs changing with sampling time, FRB intrinsic width, degree of scatter broadening, and dispersion measure smearing; the latter two of which are frequency-dependent. This is calculated using the measured properties of FRBs in the high time resolution sample of (D. R. Scott, et al. in preparation), and the effective width according to Cordes & McLaughlin (Reference Cordes and McLaughlin2003). $N_\mathrm{ant}$ is the number of antennas used in the observation, such that sensitivity scales as $N_\mathrm{ant}^{1/2}$ , and thus rate as $N_\mathrm{ant}^{3/4}$ .

We compare the cumulative integral of Equation (1) against FRB detections during the stable ‘v3’ period in Fig. 9, assuming no intrinsic rate dependence ( $\alpha=0$ ). To account for high-DM FRBs being undetectable in low-frequency observations due to only 4096 DM samples being searched, we remove all FRBs with a DM above 980 pc cm $^{-3}$ . The rates predicted by Equation (1) are re-scaled to have an average of unity, i.e. they convert real hours into weighted hours. The result is that the total number of detected FRBs closely matches the expected number in each frequency band, i.e. we see no evidence for an intrinsic rate dependence.

Figure 9. Weighted exposure (dotted lines; see text) against cumulative FRB detections (solid lines) for the period during which ‘v3’ of our FRB detection algorithm was operating.

Our study of the spectral behaviour of 23 Fly’s Eye FRBs (Macquart et al. Reference Macquart2019) suggested that, on average, spectral fluence $F_{\nu} \propto \nu^{-1.6_{-0.2}^{+0.3}}$ . However, as we note in James et al. (Reference James2022a), biases due to beam shape would revise this to $\alpha=-0.65 \pm 0.3$ should FRBs have extremely narrow bandwidths. Varying $\alpha$ , and comparing the relative to predicted rates between the low and mid bands, produces $\alpha = -0.3_{-1.6}^{+1.4}$ . Thus our observations cannot yet constrain the spectral dependence of FRBs.

The modelling of Equation (1) also predicts that the ASKAP configuration in Fly’s Eye mode was – when excluding the $N_\mathrm{ant}^{3/4}$ factor – 33% more efficient at detecting FRBs than the average ICS observation, and 22% more efficient than ICS 1.3 GHz observations. Allowing for this, the expected rate for ICS 1.3 GHz observations becomes one per 167 h, i.e. the observed rate of once per 326 h is a factor of $\sim2$ below expectation.

6.3 Galactic latitude dependence

During the initial Murriyang surveys that established FRBs as a class of astrophysical transient, there were suggestions of a deficit of FRBs at mid-to-low Galactic latitudes (Petroff et al. Reference Petroff2014), which was speculated to be due to interstellar scintillation (Macquart & Johnston Reference Macquart and Johnston2015). Analysis after further detections did not find evidence for a strong effect (Bhandari et al. Reference Bhandari2018). In Fig. 10 we compare Galactic latitude coverage against the 30 FRB detections for which we have logging data. We find no significant evidence for a latitude-dependent event rate, so discount this as an explanation for the rate deficit.

Figure 10. Cumulative exposure to Galactic latitude b of 12 701.7 h of CRAFT data, against FRB discoveries in Galactic coordinates. The increase in exposure at $|b|$ =50 is the result of the latitude-50 CRAFT filler observations.

6.4 Source counts analysis

The FRBs detected in the fly’s eye survey have been shown to have a S/N distribution consistent with the Euclidean expectation of $N_\mathrm{FRB}\unicode{x003E}\mathrm{S/N} \propto \mathrm{ S/N}^{-3/2}$ (James et al. Reference James, Ekers, Macquart, Bannister and Shannon2019a). Fig. 11 shows this distribution for all ASKAP ICS FRBs, excluding those two discovered during the period when FREDDA returned incorrect S/N values. Using the method of Crawford, Jauncey, & Murdoch (Reference Crawford, Jauncey and Murdoch1970) to estimate the power-law index $\alpha$ for all FRBs produces $\alpha = -1.50 \pm 0.27$ , which becomes $-1.46 \pm 0.27$ when correcting for the expected bias. This suggests that if the source counts distribution does indeed flatten, as predicted by Macquart & Ekers (2018a) and potentially observed in Murriyang (James et al. Reference James, Ekers, Macquart, Bannister and Shannon2019a) and MeerKAT(Jankowski et al. Reference Jankowski2023) data, this occurs below the detection threshold of CRAFT ICS observations.

Figure 11. Source counts for ASKAP/ICS FRBs. We show the counts using ‘all’ frequencies, and splitting source counts into ‘low’, ‘medium’, and ‘high’ ranges. The two FRBs detected during the period when the search algorithm returned incorrect S/N values have been excluded. Also shown is the best-fit value of the power-law slope $\alpha$ in each case, and the p-value of a KS-test against $\alpha = -3/2$ .

The observed source counts distribution is also a good diagnostic tool for biases in the search pipeline: human vetting, RFI mitigation algorithms, or both, may reject candidates that are close to the nominal detection threshold, or well above it (Macquart & Ekers 2018b). We have performed Kolmogorov-Smirnov tests (Kolmogorov Reference Kolmogorov1933; Smirnov Reference Smirnov1948) for consistency with a pure $\alpha = -1.50$ power-law on ICS FRBs, with p-values quoted in Fig. 11, and find no strong statistical evidence for a deviation. The same conclusion is reached when dividing the sample into FRBs detected in low, medium, and high frequency ranges.

There is some evidence however for a reduced number of FRBs in the $S/N \le 14$ regime, and a deficit of FRBs with very high S/N, but this is not conclusive. Fitting to all FRBs with S/N>14 increases the expected total number of FRBs by a factor of 1.40, that is, a lack of S/N $\unicode{x003C}14$ FRBs cannot explain the deficit found in Section 6.1. Equivalently, scaling up the observed ICS rate at 1.3 GHz by 1.4 to one FRB per 250 days, and comparing this rate to the fly’s eye rate, implies a source-counts slope of $\alpha = -1.1$ . Yet fitting to Fig. 11 for S/N $\unicode{x003E}14$ produces $\alpha = -2.2 \pm 0.5$ . In other words, a change in source-counts slope would also require our detection pipeline to miss high-S/N FRBs, or otherwise reduce the S/N of those detected.

6.5 Non-linearities in detection

Analysis of the source-counts slope using S/N assumes a linear relation between FRB fluence and S/N (James et al. Reference James, Ekers, Macquart, Bannister and Shannon2019a). There are several possible causes of non-linearities in our detection system, which could feasibly reduce the S/N of high-S/N events, which we consider below.

The FREDDA detection algorithm normalises channelised power according to the mean and standard deviation of each ‘block’ of 256 samples, approximately 300 ms in duration. However, this normalisation is applied to data in a subsequent block, which means that a bright FRB cannot influence its own S/N estimates. Similarly, a check on the kurtosis of each channel to remove RFI is also applied to subsequent blocks. The only possible effect then would be for an extremely bright FRB to exceed the 8-bit dynamic range of the ICS data at detection. The RMS of each time–frequency scintle is typically set to 16 digital units (d.u.), meaning that the peak S/N of a narrow FRB, with 128 d.u. of power in all 336 frequency channels, would be of 144, above which the system response must be less-than-linear. FRBs will always be DM-smeared in time, which increases the S/N threshold beyond which the system becomes non-linear; while scintillation and narrow effective bandwidths will decrease the threshold, due to individual scintles exceeding 128 d.u. We estimate scintillated, low-DM FRBs to suffer non-linear effects for S/N $\unicode{x003E}102 \, (\Delta \nu /336\,\mathrm{MHz})$ , where $\Delta \nu$ is the FRB bandwidth. However, such FRBs will only have their S/N reduced; they will not be missed, and could be readily identified in offline analysis. We have not detected any such FRBs yet in our sample.

We also observe that ASKAP beams typically overlap near the half-power points. Hence, any FRB with very high S/N, even if vetoed by some unforeseen part of the system, would be detected by adjacent beams, similarly to one burst from FRB 20201124A (Kumar et al. Reference Kumar2022).

The final possible cause of detection biases we consider is in the anti-RFI candidate vetting script that parses raw candidates, and determines whether or not to trigger the system. This has been developed by using ASKAP FRBs detected in Fly’s Eye mode (Shannon et al. Reference Shannon2018), and in theory could introduce a S/N-dependent bias. However, no such bias was observed during tests. Therefore, if the observed deviations (at moderate significance) from a pure power-law in S/N are real, we cannot explain their origin with known systematic effects.

6.6 Elevation dependence

The effect of RFI on FRB detection rates is expected to be elevation-dependent, as RFI sources – particularly those on the horizon – move in and out of ASKAP’s sensitivity pattern. Fig. 12 plots the elevation dependence of FRB rates against the total exposure (approximated by the boresight elevation at scan start) for which we have records. We find no evidence for an elevation-dependence to the FRB detection rate.

Figure 12. Cumulative exposure as a function of local elevation angle (calculated at the beginning of each scan), compared to the elevation angles at which ICS FRBs have been detected, over the period October 2019–December 2023 for which we have records. The exposure and rates are also shown divided into the three frequency ranges described in Section 6.1.

6.7 Assessing fly’s eye localisation

The capability to localise FRBs to arcsecond positions also enables us to examine the localisation and fluence measurements presented in the fly’s eye surveys. For the fly’s eye surveys, we leveraged the multiple-beam detections to improve on FRB localisation and to better determine FRB fluence. The algorithm, described in Bannister et al. (Reference Bannister2017), used the relative signal-to-noise ratios of detections in multiple beams to determine the location of the burst position on the focal plane. The algorithm marginalised over uncertainties in beam shape, gain, and position when determining burst position and brightness, and uncertainties on the parameters. It utilised Bayesian inference, and the maximum a-posteriori parameters and their uncertainties were derived from posterior samples calculated from a nested sampling algorithm (Feroz, Hobson, & Bridges Reference Feroz, Hobson and Bridges2009).

We assess the position performance using a $\chi^2$ test:

(3) \begin{equation}\hat{\chi}^2 = \boldsymbol{\Delta} r \boldsymbol{C}^{-1} \boldsymbol{\Delta} \boldsymbol{r}^T,\end{equation}

where $\boldsymbol{\Delta} \boldsymbol{r} = [ \Delta \alpha \, \Delta \delta ]$ is the vector difference between the interferometric and multi-beam positions and $\boldsymbol{C}$ is a covariance matrix parameterising the uncertainty in the multi-beam position. We assume the position uncertainty as determined using the multi-beam method to be a bivariate Gaussian, parameterised by the variance in right ascension and declination, and their covariance. These were calculated directly from the posterior samples. We do not account for uncertainty in the interferometrically derived position as it is typically a factor of $\gtrsim 200$ smaller than that of the multi-beam-derived position. In Fig. 13, we show the cumulative distribution function of the $\hat{\chi^2}$ values, and compare to the expected $\chi^2$ distribution with two degrees of freedom. We find modest disagreement between the measurements and the expected distribution, with a Kolmogorov Smirnov test reporting a probability of $p=0.04$ that the distributions agree. This can be attributed to a few outlying burst localisations ( $\hat{\chi}^2 \unicode{x003E} 10$ ). FRB 20240201A was found to originate in a null of the primary beam. The beam model used in the multi-beam localisation method assumes a Gaussian beam so does not include nulls or side lobes. FRB 20210320C originated from an outer edge beam, which is also significantly non-Gaussian. The origin of the large disagreement between the interferometric and multi-beam positions observed for FRB 20230902A is unclear; however it was the only FRB localised at the lowest standard ASKAP central observing frequency (832 MHz). It is likely that at the lowest frequencies the ASKAP beams deviate greatest from Gaussian shape. We find that if we increase the size of the uncertainties by $10 \%$ (which would reduce the $\chi^2$ by a factor of approximately 20%), the reported probability from the K-S test would increase to $0.3$ .

Figure 13. Cumulative distribution function of multi-beam positions goodness of fit. The dashed line shows the expected $\chi^2$ distribution if the model was well specified.

6.8 Burst positions within beams

Fig. 14 shows the relative position of the FRB positions relative to the primary beam for the FRBs for which we obtained interferometric localisation. We have assumed a beam of full width at half power (FWHP) following $1.1 \lambda/D$ (McConnell et al. Reference McConnell2016). The number of bursts increases radially, matching the relative area which scales with the square of radial distance. It then decreases at larger radius. The inner beams are spaced at distances typically smaller than the FWHP. There is a population of bursts localised well outside the half power point of the primary beam. These bursts were predominantly discovered in the outer beams of the PAF. Future image-plane ASKAP detection systems (discussed below) have a more limited field of view, so are potentially not sensitive to these side-lobe detections.

Figure 14. Distribution of FRB localisations relative to beam centre.

6.9 Burst modulation

Many of the ASKAP FRBs show spectral modulation: intensity variations in frequency that could either be diffractive scintillation or intrinsic to the emission mechanism. This was identified in the fly’s eye survey(Shannon et al. Reference Shannon2018). We investigated if there is any correlation between modulation and dispersion measure using the FRBs in the search data stream. We choose to investigate modulation and dispersion measure to consider both the fly’s eye and ICS FRBs. We calculate the spectral modulation index to be

(4) \begin{equation}m_I = \frac{\sigma_\mathrm{FRB}^2 - \sigma_n^2}{\sigma_n^2},\end{equation}

where $\sigma_\mathrm{FRB}^2$ is the variance on pulse and $\sigma_n^2$ is the variance of (thermal) noise measured in a segment of data of equal temporal duration close to the FRB. We estimate the uncertainty on $m_I$ using bootstrap (Efron Reference Efron1979). For each FRB, we resample (with replacement) the spectrum and re-calculate $m_I$ on each of the realisations. We use the standard deviation of these resampled modulation indices as the uncertainty.

Figure 15 shows the modulation indices that we have calculated. While FRBs with DM $\lesssim 500\,$ pc cm $^{-3}$ show a variety of spectral modulation, those with DM $\unicode{x003E} 800\,$ pc cm $^{-3}$ show little spectral modulation. Spectra of two FRBs with high modulation and two FRBs with high DM are shown in Fig. 16. It is possible that spectral modulation is being quenched at higher DM. If scintillation in the Milky Way is causing the spectral modulation, quenching would occur if the bursts are spatially resolved by Milky Way scattering screens, i.e. had been scatter broadened by a second screen. As there is a correlation between dispersion measure and distance (Macquart et al. Reference Macquart2020), this would suggest the extra-Galactic scattering scr Studies of a larger sample of bursts in higher spectral and time resolution (such as using data products derived from the CELEBI pipeline) are required to assess this effect. Study of bursts produced by the CELEBI pipeline also benefit from the array-coherennt improvement in signal to noise ratio. This could be complemented with bursts from CHIME/FRB, DSA-110 (Sharma et al. Reference Sharma2024), or MeerKAT (Jankowski et al. Reference Jankowski2023). The latter two would allow for comparison of large FRB samples detected at comparable central frequencies.

Figure 15. FRB modulation indices $m_I$ for ICS and fly’s eye FRBs. The most dispersed FRBs show an absence of spectral modulation.

Figure 16. Pulse averaged spectrum of high and low DM FRBs. The spectrum is shown as a black solid line. An off pulse spectrum is shown offset in grey. The dashed horizontal lines show zero fluence. FRB 2020610A (DM $343.8$ pc cm $^{-3}$ ) has the highest modulation index of the FRBs in our sample. FRB20180924B (DM $362.4$ pc cm $^{-3}$ ) also has high modulation. FRBs 20220610 (DM $1458.1$ pc cm $^{-3}$ ) and FRB20210407E (DM $1785.3$ pc cm $^{-3}$ ) have the largest DM of the ICS FRB.

7.1 FRB host galaxies

By virtue of delivering the largest sample of localised FRBs in its era, the CRAFT/ICS survey has provided a great opportunity to understand the demography of FRB host galaxies and the attribution of FRBs to potential progenitor populations. Figs. 1–3 show images of the sub sample of our FRB host galaxies observed primarily with the Very Large Telescope (VLT), arranged in increasing redshift. Updated photometry for a sub sample of FRBs observed with the VLT is presented in Table C3. A plot showing the multi-band photometry as a function of redshift for this sub sample is shown in Fig. 18.

Over the course of the survey, we undertook a series of studies investigating the properties of FRB hosts. Bhandari et al. (Reference Bhandari2020b) and Heintz et al. (Reference Heintz2020) conducted the first demographic studies of FRB host galaxies, finding them to be largely late-type star forming galaxies. Bhandari et al. (Reference Bhandari2022) extended the analysis to include a larger sample of FRBs and compared the properties of the hosts of apparently one-off FRBs with those of repeating sources. The sample size was insufficient to distinguish any difference between the repeating and non-repeating sources. Based on the Kolmogorov Smirnov tests reported in Bhandari et al. (Reference Bhandari2022) (which for many had $P_\mathrm{KS} \approx 0.25$ ), which included a sample of 10 apparently one-off FRBs and 6 repeating FRBs, the expected sample size needed to be approximately a factor of approximately two larger for each sub-population to reach 95% confidence and a factor of approximately four larger in each to reach $99.9\%$ confidence assuming the distributions had identical distributions.

Gordon et al. (Reference Gordon2023) undertook detailed modelling of host galaxy spectral energy distributions to assess the star formation histories of nearly all our FRB hosts identified prior to the beginning of 2022. From these studies it is now clear that the host galaxies of one-off bursts are markedly different from that of the first repeating FRB 20121102A, which was found to originate in a metal-poor dwarf galaxy (Tendulkar et al. Reference Tendulkar2017).

The high angular resolution afforded by ASKAP-detected FRBs can exceed that easily obtained on the ground with natural seeing, warranting further follow up with the Hubble Space Telescope (HST). In Mannings et al. (Reference Mannings2021) we presented the analysis of seven ASKAP localised FRBs (and one localised by the European VLBI Network), and showed that most of the bursts were located near spiral arm features in their hosts. This implies that many FRB sources are associated with active star formation and young stellar populations. This was only possible because of the combination of the high precision ASKAP positions and the high resolution HST images. Woodland et al. (Reference Woodland2024) used laser guide star adaptive optics with the Gemini South telescope to undertake a similar assessment of a further five ASKAP FRB host galaxies. This provides support for the origin of FRB emission from young neutron stars, with the notable exception of the repeating CHIME FRB source 20200120E which has been localised to a globular cluster in the halo of M81 (Kirsten et al. Reference Kirsten2022).

Very few of the host galaxies showed continuum radio emission. No unresolved persistent radio emission has been identified coincident with any of the bursts discovered by ASKAP (e.g. Bannister et al. Reference Bannister2019b; Bhandari et al. Reference Bhandari2020b) despite sensitive observations. However only one of the FRBs in the sample (FRB 20190711A) has been found to repeat, and originated at a redshift of $z=0.521$ . Diffuse emission attributed to star formation was observed for two host galaxies. Hydrogen and carbon-monoxide line emission was also detected for the host galaxies of three FRBs (FRBs 20230718A and 20180924B, Glowacki et al. Reference Glowacki2023; Chittidi et al. Reference Chittidi2023; Glowacki et al. Reference Glowacki2024).

7.2 Burst-emission physics

Access to the voltage buffers allowed us for the first time to study ASKAP-detected FRBs both at time resolutions much shorter than 1 ms, and with full polarisation. This enabled improved insight into burst emission physics and the properties of intervening material along the line of sight. Cho et al. (Reference Cho2020) demonstrated the power of using the voltage buffers to form a tied-array beam time series at the position of the bursts. What appeared at low time resolution to be a single pulse in FRB 20181112A was in fact four distinct bursts, with each showing different pulse morphologies and polarimetric properties. Day et al. (Reference Day2020) used high time resolution imaging on a larger sample of ASKAP bursts, uncovering a diversity of polarimetric properties and morphologies. While some bursts were obviously scatter-broadened, many had multiple components with varying levels of linear and circular polarisation, including variations in both across pulses. This was in contrast to previous studies of repeating FRB sources which in general showed high degrees of linear polarisation, constant linear polarisation position angles, and less evidence for circular polarisation.

Figure 18. VLT photometry of ASKAP/ICS fast radio burst host galaxies.

The spectropolarimetry enabled searches for conventional and generalised Faraday rotation (Bera et al. Reference Bera2024), and spectral depolarisation. The searches showed that most of the detected FRBs had low rotation measures (RMs) $\ll 10^2$ rad m $^{-2}$ (Mannings et al. Reference Mannings2023), in contrast to the first repeating FRB which has a high RM (Michilli et al. Reference Michilli2018). Similarly, constraints on spectral depolarisation suggest that the scattering media foreground to the ASKAP FRB sample are less magnetoionically active compared to that of repeating FRB sources (Uttarkar et al. Reference Uttarkar2024; Ryder et al. Reference Ryder2023).

7.3 FRB repetitions

One of the fundamental (but potentially unproveable) questions about FRBs is whether they all (eventually) repeat. This uncertainty stems from the observational limitations and the stochastic nature observed in the repetition rates across the FRB population. In self-conducted follow up within the fly’s eye survey, which spanned thousands of hours, none of the FRBs were found to repeat (Shannon et al. Reference Shannon2018). Initial studies of the first repeating FRB 20121102A suggested a steeper luminosity function, highlighting the importance of using more sensitive radio telescopes for such investigations (Law et al. Reference Law2017; Connor & Petroff Reference Connor and Petroff2018).

The presence of repetitions excludes cataclysmic progenitor models for producing some FRB emission. The large volumetric rate of repeating FRBs is also inconsistent with cataclysmic progenitor models (Ravi Reference Ravi2019).

Throughout the ICS survey, we have conducted an extensive monitoring programme to search for repeat bursts from detected FRBs. This has been executed using some of the world largest single-dish radio telescopes, providing unprecedented time resolution ( $\sim$ 20–80 s) and frequency coverage (as large as $\sim$ 3 GHz bandwidth). Follow-up campaigns were conducted with the 110-m Robert C. Byrd Green Bank Telescope (GBT) using the L-band and the 800 MHz receivers (Prestage et al. Reference Prestage2015), and the Murriyang telescope using the 20-cm multi-beam (Staveley-Smith et al. Reference Staveley-Smith1996) and the ultra wide-bandwidth low (UWL) receiving systems (Hobbs et al. Reference Hobbs2020). The GBT allowed us to monitor FRB sources in the northern sky (Decl. > $-46^\circ$ ) with higher sensitivity than Murriyang. The Murriyang telescope, equipped with the UWL receiver, offered unparalleled frequency coverage from 704 to 4032 MHz, unique among the existing facilities. Additionally, we searched for repetitions using the Five hundred meter Aperture Spherical radio Telescope (FAST) for the source FRB 20171019A. It is pertinent to note that the majority of the ICS-detected FRBs are at southern declinations, not visible from FAST. Searches for repetitions were also undertaken with ASKAP through filler observations. These included repeated observations of the latitude-50 fields, targeted monitoring of FRB sources known to repeat, and specific targeting of ASKAP-detected FRBs exhibiting properties similar to known repeaters, notably the ‘sad-trombone’ pulse morphology (Hessels et al. Reference Hessels2019).

In this monitoring programme, we collected a total of 1 070 h of high-resolution data using the GBT and Murriyang. We monitored 42 FRB sources, with an average observation time of 25 h per source. This included 26 FRBs detected in the Fly’s Eye Survey and 15 sources detected in the ICS survey (up to March 2021). We also included the prolific repeater FRB 20201124A in our monitoring campaign to study its polarisation properties. The bulk of our follow-up time, totalling 568 h, was spent with the Parkes/UWL. We followed a standard search methodology, as described in Kumar et al. (Reference Kumar2021).

Our efforts yielded several notable findings. We detected faint repetitions from one of the brightest FRBs found in the fly’s eye survey, FRB 20171019A, using the GBT (Kumar et al. Reference Kumar2019). Additionally, we discovered an extremely narrow-band repeat burst from FRB 20190711A, with a spectral occupancy of only 2% (Kumar et al. Reference Kumar2021). Furthermore, using the ASKAP/ICS and the Parkes/UWL, we observed multiple bursts from FRB 20201124A during a period of heightened activity, which included significant circularly polarised emission in one of the bursts, a phenomenon not previously observed in repeating FRBs (Kumar et al. Reference Kumar2022).

Among the 41 ASKAP-detected sources we monitored, only two showed definitive evidence of repetition. The remaining sources did not display any clear signs of repeat activity during our follow-up observations, suggesting either longer inactivity periods or that their repeat bursts are too faint to be detected with the current generation of radio telescopes.

We have also used the lack of repetition observed in ASKAP FRB searches and follow up to show that the number density of very strong repeaters must be less than 27 Gpc $^{-3}$ with 95% confidence (James Reference James2019), and in follow-up observations to limit their repetition rates (James et al. Reference James2020b). In particular, we have shown that if the likely nearest FRB detected in CRAFT observations (FRB 20171020, detected in Fly’s Eye mode; Mahony et al. Reference Mahony2018) does repeat, its repetition rate must be less than 0.011 bursts per day above $10^{39}$ erg (Lee-Waddell et al. Reference Lee-Waddell2023). We have also used these measurements, under the assumption that all FRBs do repeat, to derive an FRB rate distribution $\mathrm{d}N_\mathrm{frb}/\mathrm{d}R \propto R^{-\gamma_r}$ with $\gamma_r \unicode{x003C} -1.94$ (James et al. Reference James2020a). This has been shown by James (Reference James2023) to be consistent with observations of both repeating and apparently one-off FRBs by the CHIME/FRB Collaboration (CHIME/FRB Collaboration: Amiri et al. 2021).

7.4 Population modelling

The distribution of FRB DMs, redshifts, and luminosities is a function of three factors: the properties of the FRB population (e.g. the intrinsic FRB luminosity function, source evolution, and DM contribution of host galaxies); cosmological parameters such as the Hubble Constant $H_0$ and the baryonic content $\Omega_b$ ; and properties of the detecting instrument, in particular its total sensitivity, beamshape, and DM-dependent biases (Macquart & Ekers Reference Macquart and Ekers2018a; Macquart & Ekers Reference Macquart and Ekers2018b; Connor Reference Connor2019). Due to ICS FRBs having accurate measurements of all three properties, they have been used in a number of ways to constrain both cosmological and FRB population parameters.

A statistical relationship between FRB DM and luminosity was first established by Shannon et al. (Reference Shannon2018) using FRBs detected by Murriyang and ASKAP in fly’s eye mode, and further modelled by Arcus et al. (Reference Arcus, Macquart, Sammons, James and Ekers2021). The zDM code has subsequently been developed by the CRAFT and F4 Collaborations to model the redshift, DM, and fluence distribution of FRBs (James et al. Reference James2022a), as well as cosmological parameters (see Section 7.5). Using primarily ICS FRBs, it has found evidence for source evolution consistent with the star formation rate, a burst fluence ( $\sim$ luminosity) distribution consistent with a power-law with differential slope $\mathrm dN_\mathrm{ FRB}/\mathrm dF \propto F^\gamma$ with $\gamma = -0.95_{-0.15}^{+0.18}$ (James et al. Reference James2022b), and a characteristic maximum FRB energy of $10^{41.7 \pm 0.2}$ erg, assuming a 1 GHz emission bandwidth (Ryder et al. Reference Ryder2023).

These studies have also prompted investigations into possible biases in FREDDA, with Qiu et al. (Reference Qiu, Keane, Bannister, James and Shannon2023) and Hoffmann et al. (Reference Hoffmann2024) identifying deviations from the DM-dependent sensitivity predicted by Cordes & McLaughlin (Reference Cordes and McLaughlin2003). When excluding FRB 20191128A from parameter estimation analysis (due to the aforementioned version 2 of FREDDA which detected it reporting incorrect values) however, these deviations result in a very small systematic error on parameter estimates, for example, of 0.2 km s $^{-1}$ Mpc $^{-1}$ for $H_0$ , which is small compared to the statistical errors in the current FRB sample.

7.5 Intergalactic and circumgalactic media

As a large sample of FRBs began to be amassed, it became clear that the burst dispersion measure is correlated with redshift. We first identified this trend by comparing high-fluence FRBs detected in fly’s eye mode with lower-fluence FRBs detected by Murriyang (Shannon et al. Reference Shannon2018). This provided, for the first time, the opportunity to measure the baryon density $\Omega_b$ in the nearby low-redshift ( $z\unicode{x003C}0.5$ ) Universe. While $\Omega_b$ is well-measured at high redshift from Big Bang nucleosynthesis, at low redshift nearly 50% of the baryons were undetected in optical and X-ray searches, but thought to reside in the diffuse IGM. The use of extragalactic radio bursts to detect this gas had been suggested as far back as 1965 (Haddock & Sciama Reference Haddock and Sciama1965; Ginzburg Reference Ginzburg1973), and quantitative predictions based on $\Lambda$ CDM cosmology in the context of gamma-ray bursts had been made (Ioka Reference Ioka2003; Inoue Reference Inoue2004). However, it was the late Jean-Pierre Macquart who had most strongly espoused using ASKAP to detect FRBs and find these missing baryons as early as 2008, leading to CRAFT being formalised as an ASKAP survey science project in 2009 (Macquart et al. Reference Macquart2010).

With a sample of just seven FRBs, we were able to measure the entirety of the baryon content of the Universe (Macquart et al. Reference Macquart2020) and resolve the missing baryon problem. The relation between FRB dispersion measure and redshift is now referred to as the ‘Macquart Relation’ in honour of Jean-Pierre Macquart’s key contribution. The technique was extended, first to estimate the Hubble constant ( $73^{+12}_{-8}$ km s $^{-1}$ Mpc $^{-1}$ ; James et al. Reference James2022b), and then to assess fluctuations in the Macquart relation about its mean, which is related to feedback processes (Baptista et al. Reference Baptista2023).

Our discoveries have also enabled us to uniquely probe circumgalactic media, the similarly diffuse media in galaxy haloes that is difficult to study, but which plays an important role in galaxy formation and evolution. The second FRB we localised (FRB 20181112A) was observed to pass through the halo of an intervening galaxy (Prochaska et al. Reference Prochaska2019). Using the resultant limits on pulse broadening and Faraday rotation, we constrained the turbulence and magnetisation in this galaxy halo. Simha et al. (Reference Simha2020) investigated in detail the foreground galaxies towards FRB 20190608B, and Simha et al. (Reference Simha2021) undertook a similar analysis towards FRB 20180924B. We have also been working with the FLIMFLAM collaboration (Lee et al. Reference Lee2022) to detect galaxy halos along the sightlines to FRBs, with first results on ASKAP FRBs presented in Khrykin et al. (Reference Khrykin2024) and Huang et al. (Reference Huang2024).

Fig. 19 shows the Macquart relation for the FRBs detected in the ICS survey. The dispersion measure of the FRBs has been corrected for the Milky Way contribution using a model for the Milky Way disk (Cordes & Lazio Reference Cordes and Lazio2002), a Milky Way halo contribution assumed to be 50 pc cm $^{-3}$ , and a host galaxy contribution of 50 pc cm $^{-3}$ . This is compared to expectations (median, and 90% range, and mean) for $p(\mathrm{DM}_\mathrm{cosmic}|z)$ using the model of Macquart et al. (Reference Macquart2020) with $H_0 = 70$ km s $^{-1}$ Mpc $^{-1}$ and fluctuation parameter $F=0.32$ . Our FRBs fluctuate significantly about the expectation value $\langle \mathrm{DM_\mathrm{cosmic}} \rangle$ given by the relation. Two FRBs lie significantly below the minimum expectation, which we take as evidence of very small host contributions, under-fluctuations in Milky Way contributions, or a combination of the two. In the future it might be possible to use host galaxy or host environment properties to ascertain if DM excesses are local to the burst and tune FRB studies for studies of extragalactic matter. Several FRBs lie significantly above the relation, notably FRB 20210117A, the excess DM of which is attributable to the local environment of the FRB (Bhandari et al. Reference Bhandari2023; Simha et al. Reference Simha2023). For a given observed DM, measured redshifts vary by at least a factor of two, which cautions against relying on the redshift inferred by the Macquart relation for modelling purposes. We note that all well-localised ICS FRBs with $\mathrm{DM}_\mathrm{cosmic}\unicode{x003C} 1\,000$ pc cm $^{-3}$ have firm host galaxy identifications, while at larger DMs, host galaxy identification becomes redshift-dependent (e.g. FRB 20210912A; Marnoch et al. Reference Marnoch2023). This introduces potential biases when using high-DM data which must be accounted for in population models (James et al. Reference James2022b; Jahns-Schindler et al. Reference Jahns-Schindler, Spitler, Walker and Baugh2023).

Figure 19. The Macquart relation (solid blue line) compared to the z–DM distribution of CRAFT/ICS FRBs (blue crosses). The shading shows the probability density of the DM for the cosmic web $\mathrm{DM}_\mathrm{cosmic}$ , for which the median DM, and the range encompassing 90% of the probability, is also given.