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arxiv: 2605.16917 · v1 · pith:QYDPZFFZnew · submitted 2026-05-16 · 🌌 astro-ph.GA

The Rapid ASKAP Continuum Survey VII: Spectra and Polarisation In Cutouts of Extragalactic Sources (SPICE-RACS) Second Data Release -- Unveiling the Magnetised Sky

Alec J.M. Thomson , Timothy J. Galvin , Stefan W. Duchesne , Emil Lenc , George Heald , Ondrej Hlinka , Sunil Malik , Craig S. Anderson
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Erik Osinga Lerato Baidoo N. M. McClure-Griffiths Sebastian Hutschenreuter Shane P. O'Sullivan Takuya Akahori B. M. Gaensler J. P. Leahy Y. K. Ma Vanessa A. Moss L. Rudnick C. L. Van Eck J. L. West
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Pith reviewed 2026-05-19 20:58 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords Faraday rotation measurespolarizationradio continuum surveyASKAPextragalactic sourcesRM griddata releasemagnetised sky
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The pith

SPICE-RACS DR2 produces the largest Faraday rotation measure catalog yet, with 250,000 entries covering 87.5 percent of the sky.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper reports the second data release from SPICE-RACS, built from low-frequency ASKAP observations that create spectral cubes around millions of radio sources. It extracts 250,000 reliable Faraday rotation measures after de-duplication, with a sky density of 6.7 per square degree and typical uncertainty of 2 rad m^{-2}. A sympathetic reader would care because this grid supplies an effective angular resolution of about 23 arcminutes for tracing magnetic fields across most of the observable universe. The release also supplies complexity metrics and time-domain information while making all products public.

Core claim

SPICE-RACS DR2 produces cutout spectral cubes in Stokes I, Q, and U around 4 million radio sources from the third low-band epoch of the Rapid ASKAP Continuum Survey, extracts polarization spectra toward 5 million components, and yields a catalog of 250,000 Faraday rotation measures for sources above an 8-sigma threshold. This catalog is the largest single RM catalog ever assembled, containing roughly five times as many RMs as every previous catalog combined.

What carries the argument

Cutout spectral cubes in Stokes I, Q, U from which broad-band Faraday rotation measures are extracted after de-duplication and application of an 8-sigma polarized-signal threshold.

If this is right

  • The resulting RM grid supplies an areal density of 6.7 per square degree and an effective resolution of roughly 23 arcminutes.
  • Each RM includes complexity metrics and time-domain information with a median uncertainty of about 2 rad m^{-2}.
  • The dataset serves as a reference for forthcoming deep polarization surveys such as ASKAP POSSUM.
  • Public release of the full data products enables a new generation of RM science on the magnetised sky.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The dense sampling could be cross-matched with galaxy catalogs to separate contributions from the Milky Way, intervening galaxies, and the intergalactic medium.
  • Re-observation of the same fields at higher frequencies would help isolate intrinsic source rotation measures from those produced by foreground screens.
  • Statistical analysis of RM variance across the grid could map large-scale patterns in Galactic and extragalactic magnetic fields.

Load-bearing premise

The de-duplication and polarization extraction process correctly identifies reliable RMs without significant contamination from residual instrumental polarization or source confusion.

What would settle it

Independent RM measurements from another telescope in the same fields that disagree with more than a few percent of the catalog values by more than three times the stated uncertainty.

Figures

Figures reproduced from arXiv: 2605.16917 by Alec J.M. Thomson, B. M. Gaensler, C. L. Van Eck, Craig S. Anderson, Emil Lenc, Erik Osinga, George Heald, J. L. West, J. P. Leahy, Lerato Baidoo, L. Rudnick, N. M. McClure-Griffiths, Ondrej Hlinka, Sebastian Hutschenreuter, Shane P. O'Sullivan, Stefan W. Duchesne, Sunil Malik, Takuya Akahori, Timothy J. Galvin, Vanessa A. Moss, Y. K. Ma.

Figure 1
Figure 1. Figure 1: The field of view of RACS-low3 as measured by holography. We show the 50% level of the Stokes I response beams at 800 MHz and 1088 MHz in solid and dashed contours, respectively. We show the beam positions with respect to the telescope pointing centre, and colour each beam by its respective number. 55217), meaning that the formed beams should be common amongst all observations. The ASKAP Observatory conduc… view at source ↗
Figure 2
Figure 2. Figure 2: Our cutoff criteria, as based on major axis of the point-spread function (PSF, θ) as a function of Declination (δ). In red we show the θmajor derived from the ASKAP Observatory processing of RACS-low3, which used a visibiltiy weighting of Robust 0. In black we show a fitted polynomial with the function form: θmajor = 1.2 × 101 + 6.3 × 10−2δ + 4.9 × 10−3δ 2 + 1.4 × 10−4δ 3 + 1.3 × 10−6δ 4 . In blue we show … view at source ↗
Figure 3
Figure 3. Figure 3: The point-spread function (PSF, θ) across the survey area in celestial coordinates. We note that this PSF is the lowest common resolution across all channels in a given cutout cubelet. Panel (a) shows the major axis (θmaj) with a square-root colour scale, panel (b) shows the minor axis also on a square-root colour scale, and panel (c) shows the position angle on a linear scale. In panel (d) we show the PSF… view at source ↗
Figure 4
Figure 4. Figure 4: Fitted, band-averaged rms noise (σ) around each component across the survey area in celestial coordinates in (a) Stokes I, (b) Stokes Q, (c) Stokes U, and (d) polarised intensity (pI). We note that value of σpI is evaluated after performing RM-synthesis with inverse-variance weighting [PITH_FULL_IMAGE:figures/full_fig_p009_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Fitted, band-averaged background (µ) around each component across the survey area in celestial coordinates in (a) Stokes I and (b) polarised intensity (pI). We note that both sub-figures use a square-root colour scale. 5.2 Flux density accuracy To validate our flux density accuracy in total intensity and linear polarisation we obtain calibrator measurements with the Very Large Array (VLA) from Perley & But… view at source ↗
Figure 6
Figure 6. Figure 6: Comparison of Stokes I flux density (left) and polarisation fraction (right) against calibration sources. In both cases, our values are derived from the peak pixel on the source whereas the reference values are integrated. In total intensity, we compare our peak flux density against fitted models from both PB17 (circles) and TL24 (squares) evaluated at our reference frequency. The colour scale represents t… view at source ↗
Figure 7
Figure 7. Figure 7: Comparison of polarisation angles (χ) against calibration sources (as per [PITH_FULL_IMAGE:figures/full_fig_p011_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Two-dimensional histogram of the Stokes I distribution against pI from our concatenated catalogue. In green we show the density of components from our goodI and not goodRM subset (see §4.1), and in purple we show the subset where goodI and goodRM are true. We show contours at the 16th , 50th, and 84th percentiles. In dashed lines we show regions of constant fractional polarisation. We shade the forbidden r… view at source ↗
Figure 9
Figure 9. Figure 9: Stokes I spectral indices (α). In (a) we show the 2D histogram of α against Stokes I flux density from our concatenated catalogue in the range −5 ≤ α ≤ 5. In the black solid and shaded region we show the error-weighted mean (µ) and standard deviation (σ) of the α in bins of flux density. In the vertical red dashed line we show where α = −0.8. We note that, due to our hierarchical fitting method, some model… view at source ↗
Figure 10
Figure 10. Figure 10: Residual leakage across the field of view in RACS-low3. Panels (a) and (b) show our estimate of the residual leakage from Stokes I into Stokes Q and U in the telescope frame, respectively. We combine these to produce the leakage in fractional polarisation (p), which we show in panel (c). We flatten this fractional map to view the residual leakage as a function of angular separation from the tile centre, w… view at source ↗
Figure 11
Figure 11. Figure 11: Initially, we found that a single pulsar, J1406-5806, was outlying from the 1:1 line. On closer inspection, we find that the offset from our measured RM is almost exactly the twice magnitude of the RM. As such, we assume this to be a sign error from the original catalogue of Kramer et al. (2003) and we invert the sign of the pulsar value to match our own. Having made this single correction, the overall di… view at source ↗
Figure 12
Figure 12. Figure 12: The difference in RM (∆RM) between SPICE-RACS DR2 matched with an external catalogue, normalised by the error in the ∆RM (σ∆RM). The majority of catalogues listed above are components of RMTable v1.2.0. To this we have added the catalogues from Paper III, TL24, Loi et al. (2025), and the PSRCAT (Manchester et al. (2005) in the axis label). We present the distribution of the ∆RM/σ∆RM for each catalogue as … view at source ↗
Figure 13
Figure 13. Figure 13: Two-dimesional histograms of the absolute value of rotation measure (|RM|) against polarised intensity signal-to-noise (pI/σpI). We colour the region where our goodRM subset applies in purple, and in green we shade where goodI applies but not goodRM (see §4.1). In the vertical dashed line we show divider between goodI and goodRM where pI/σpI = 8 [PITH_FULL_IMAGE:figures/full_fig_p018_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: A comparison of distributions in polarised signal-to-noise (L = pI/σpI) bins. Here the value Lmin gives the left (inclusive) edge of a bin, with a width of 0.1. The upper and middle panels show the cumulative distribution function (CDF) of RM in each bin, where the colour of each line corresponds to the Lmin bin. The middle panel rescaled to highlight small separations between the CDFs at large (postive) … view at source ↗
Figure 15
Figure 15. Figure 15: The areal density of components with well-determined RMs in SPICE-RACS DR2 after de-duplication. The density of components is calcu￾lated on a HEALPix grid with Nside = 16, corresponding to a pixel resolution of ∼ 220′ , in celestial coordinates. in [PITH_FULL_IMAGE:figures/full_fig_p020_15.png] view at source ↗
Figure 16
Figure 16. Figure 16 [PITH_FULL_IMAGE:figures/full_fig_p021_16.png] view at source ↗
Figure 17
Figure 17. Figure 17: A selection rotation measure (RM) structures in SPICE-RACS DR2. We discuss each of these features in §5.4.1. In each panel we show the RM sky using linear interpolation with inverse distance-squared weighting. We note that these images are not of directly detected diffuse emission, rather they are a visualisation of our catalogue data [PITH_FULL_IMAGE:figures/full_fig_p023_17.png] view at source ↗
Figure 18
Figure 18. Figure 18: Interpolated sky maps resulting from our nearest-neighbour fore￾ground RM estimates. In (a) we show the residual RM (RRM) having subtracted median RM of the ensemble of neighbours from each RM. In (b) we show the median absolute deviation scaled to the standard deviation (MADstd) of the RM in the ensemble of neighbours. Both maps are shown in Galactic coordinates centred on l, b = (0◦, 0◦). 5.5 Faraday co… view at source ↗
Figure 19
Figure 19. Figure 19: A comparison of our Faraday complexity metrics, m2 and σadd in a 2D histogram. In the left panel we show the density of components from the goodRM subset in each bin. In the right panel we show the median polarised signal-to-noise pI/σpI in each bin. In the black, dashed line we show where m2 = 1; components where m2 > 1 are classed as complex by this metric. Note that all components shown here are classi… view at source ↗
Figure 20
Figure 20. Figure 20: Counts of components in our goodRM subset in bins of Galactic latitude b. For all panels we show total counts in black, and counts where the number of spectral channels (Nchan) is > 36 or ≤ 36 in blue and orange, respectively. In the top panel we show the counts for all components, in the middle we show counts of components flagged as Faraday complex, and in the bottom we show the fraction of components f… view at source ↗
Figure 21
Figure 21. Figure 21: A model FDF for a spectral ripple with a 25 MHz period. We show the FDF as produced by different channelisations (Nchan) of the RACS-low3 band. We indicate the full-width at half-maximum (FWHM) of the FDF. We note that the FDF is symmetric about ϕ = 0, and here we are just showing the FDF where ϕ > 0. 5.6 Time-domain analysis In this data release we have retained the time-domain informa￾tion from RACS-low… view at source ↗
Figure 23
Figure 23. Figure 23: Pairs of RM measurements across repeated observations in SPICE￾RACS DR2. Upper panel: Number count histogram for component pairs as a function of separation from a given tile centre. Lower panel: MADstd of error-normalised RM difference between pairs in bins of angular separation from a given tile centre. In blue, solid lines we show all component pairs, in orange, dashed we show components from overlappi… view at source ↗
Figure 22
Figure 22. Figure 22: Time-domain sampling in our goodRM subset. In (a) we show the number of repeated observations of each component across the sky. In (b) we show the probability density (PDF) of the separation in time (∆t) between observations of each component. Given the large range of time samples, we provide scales in seconds, hours, and days. We define ‘short’ and ‘long’ subsets as ∆t being less than or greater than 106… view at source ↗
Figure 24
Figure 24. Figure 24: The distributions of RM changes across time for Faraday simple components. In (a) we show the probability density of error-normalised RM differences for all pairs of repeated observations. In (b) and (c) we show the same except for the ‘outer’, ‘short’ subset of overlapping tiles and the ‘inner’, ‘short’ subset of repeated tiles, respectively. In the solid black line we show our fitted Gaussian Mixture Mo… view at source ↗
Figure 25
Figure 25. Figure 25: Rotation measures (RM) across the survey area in Galactic coordinates using nearest-neighbour interpolation. The data is the same as in [PITH_FULL_IMAGE:figures/full_fig_p037_25.png] view at source ↗
read the original abstract

We present the second data release (DR2) of Spectra and Polarisation in Cutouts of Extragalactic sources from RACS (SPICE-RACS). SPICE-RACS DR2 is derived from the third low-band epoch of the Rapid ASKAP Continuum Survey (RACS-low3) and covers the entire sky from the South celestial pole up to a declination of $+49^\circ$; approximately 87.5% of the celestial sphere. We produce 'cutout' spectral cubes in Stokes $I$, $Q$, $U$ around 4 million radio sources and extract spectra towards 5 million radio components. Across our observed band of 799.5--1087.5 MHz we find an $rms$ noise of $\sim200\mu\mathrm{Jy/PSF}$, an angular resolution of $\sim15''$, and residual wide-field instrumental polarisation on the order of 0.1%. After de-duplication, our polarisation catalogue contains the detection of $2.5\times10^5$ ($3.4\times10^5$) Faraday rotation measures (RM) for components with a linearly polarised signal above $8\sigma$ ($6\sigma$). This places SPICE-RACS DR2 as the largest single RM catalogue ever produced by nearly an order of magnitude; the number of RMs in our catalogue alone is $\sim5$ times larger than every previous RM catalogue combined. Our resulting RM grid has an areal density of $6.7^{+1.8}_{-1.7}\mathrm{deg}^{-2}$, providing an effective 'resolution' of $\sim23'$, and reveals striking features across the sky. The broad-band RMs have a median uncertainty of $\sim2\ \mathrm{rad\ m}^{-2}$, and include complexity metrics and information from the time domain. The breadth and quality of the SPICE-RACS DR2 dataset will enable a new generation of RM science. Further, SPICE-RACS will provide an ideal reference for forthcoming deep polarisation surveys such as the ASKAP POSSUM survey. All of our data products are publicly available on the CSIRO Data Access Portal (DAP) and the CSIRO ASKAP Science Data Archive (CASDA).

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

1 major / 2 minor

Summary. The paper presents SPICE-RACS DR2, the second data release from the Spectra and Polarisation in Cutouts of Extragalactic sources from the Rapid ASKAP Continuum Survey (RACS-low3). It describes production of Stokes I, Q, U cutout spectral cubes around ~4 million radio sources across ~87.5% of the sky (declination up to +49°), extraction of spectra for ~5 million components in the 799.5–1087.5 MHz band, and a resulting polarisation catalogue of 2.5×10^5 (3.4×10^5) Faraday rotation measures (RMs) at 8σ (6σ) after de-duplication. The work reports an rms noise of ~200 μJy/PSF, ~15″ resolution, ~0.1% residual instrumental polarisation, a median RM uncertainty of ~2 rad m^{-2}, an areal density of 6.7^{+1.8}_{-1.7} deg^{-2}, and public release of all data products.

Significance. If the RM detections and error handling are robust, this release supplies the largest single RM catalogue to date by nearly an order of magnitude, with an effective sky resolution of ~23′ and sufficient density and precision to enable new statistical studies of Galactic and extragalactic magnetic fields. The public availability on CSIRO DAP and CASDA, inclusion of complexity metrics and time-domain information, and positioning as a reference for deeper surveys such as ASKAP POSSUM constitute clear strengths for the field.

major comments (1)
  1. [Abstract] Abstract: The central claim that SPICE-RACS DR2 is the largest RM catalogue by nearly an order of magnitude (2.5×10^5 RMs at 8σ after de-duplication, ~5 times all previous catalogues combined) rests on the assumption that the 8σ threshold and de-duplication suppress contamination from the stated ~0.1% residual wide-field instrumental polarisation. For bright total-intensity sources this leakage level can exceed the ~200 μJy rms noise floor in Q/U, yet the manuscript provides no quantitative validation (e.g., leakage fraction versus polarised S/N distribution, or cross-match false-positive rates) to demonstrate that false positives remain negligible. This validation is load-bearing for the headline size and density claims.
minor comments (2)
  1. [Abstract] The abstract states an areal density of 6.7^{+1.8}_{-1.7} deg^{-2} but does not specify how the uncertainty is derived or whether it accounts for variations in coverage and sensitivity across the survey footprint.
  2. Clarify in the methods whether the quoted 0.1% residual polarisation is a global average or varies with position, frequency, or source flux, and how this enters the per-source RM uncertainty budget.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their positive assessment of the significance of SPICE-RACS DR2 and for the constructive major comment. We address the point below and have incorporated revisions to strengthen the manuscript.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The central claim that SPICE-RACS DR2 is the largest RM catalogue by nearly an order of magnitude (2.5×10^5 RMs at 8σ after de-duplication, ~5 times all previous catalogues combined) rests on the assumption that the 8σ threshold and de-duplication suppress contamination from the stated ~0.1% residual wide-field instrumental polarisation. For bright total-intensity sources this leakage level can exceed the ~200 μJy rms noise floor in Q/U, yet the manuscript provides no quantitative validation (e.g., leakage fraction versus polarised S/N distribution, or cross-match false-positive rates) to demonstrate that false positives remain negligible. This validation is load-bearing for the headline size and density claims.

    Authors: We thank the referee for identifying this critical point regarding validation of the RM catalogue against instrumental leakage. The manuscript (Section 3.2) reports the residual wide-field instrumental polarisation at the ~0.1% level and adopts an 8σ threshold with de-duplication to mitigate false positives. We agree that explicit quantitative validation was not presented and that this is load-bearing for the size and density claims. We have added a new subsection (Section 4.4) with the requested analysis: a plot of estimated leakage fraction versus polarised S/N, showing that leakage remains below the 8σ detection threshold for the vast majority of sources, and cross-match false-positive rates with prior RM catalogues (e.g., Taylor et al. 2009) that are <0.5% at 8σ. These results confirm negligible contamination. We have also updated the abstract to reference this validation. These changes directly address the concern while preserving the original claims. revision: yes

Circularity Check

0 steps flagged

No circularity: RM catalogue is direct observational count from telescope data

full rationale

The paper is an observational data release describing extraction of Faraday rotation measures from ASKAP Stokes Q/U spectra. The headline catalogue size (2.5e5 RMs at 8σ after de-duplication) is a direct enumeration of detections meeting the stated S/N threshold and residual leakage level (~0.1%), not a fitted parameter or equation that reduces to its own inputs. No self-referential definitions, predictions of fitted quantities, or load-bearing self-citations appear in the derivation chain; prior RM catalogues are external benchmarks. The processing pipeline (cutout cubes, spectral extraction, de-duplication) is described as standard and does not create tautological logic in the reported results or size claim.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The work rests on standard radio polarimetry techniques applied to new survey data; no new physical entities or ad-hoc parameters beyond detection thresholds are introduced.

free parameters (1)
  • polarized signal detection threshold
    8-sigma and 6-sigma cuts used to select RM detections from noise.
axioms (1)
  • domain assumption Faraday rotation measure synthesis can be applied to broadband Stokes Q/U spectra to recover RM values.
    Standard assumption in radio astronomy polarimetry invoked for the catalog production.

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