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REVIEW 3 major objections 4 minor 88 references

The SARAO MeerKAT Galactic Plane Survey filamentary source catalogue

T0 review · 3 major / 4 minor · reviewed 2026-08-11 · deepseek-v4-flash

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Pith's one-line read The paper claims that 77 of 130 isolated radio filaments in the MeerKAT Galactic Plane Survey are likely non-thermal, making them the first such filaments found outside the Galactic Centre.

desk verdict Useful catalogue, but the 'first NRFs outside the GC' claim rests on an uncalibrated by-eye MIR proxy and needs spectral-index confirmation. read the letter →

arxiv 2412.07852 v1 pith:LCJEBXAK submitted 2024-12-10 astro-ph.GA

Gwenllian M. Williams , Mark A. Thompson , Mubela Mutale , Andrew J. Rigby , Cristobal Bordiu , Simone Riggi , Michael Bietenholz , Loren D. Anderson
show 6 more authors
Fernando Camilo Sharmila Goedhart Sarah E. Jaffa Willice O. Obonyo Corrado Trigilio Grazia Umana
This is my paper · ORCID
classification astro-ph.GA
keywords radiofilamentsnon-thermalGalacticplaneMeerKATSMGPSmid-infraredclassificationsynchrotronemissioninterstellarmedium
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

The paper argues that the Milky Way's plane contains a population of isolated, narrow radio filaments that are likely non-thermal, based on a catalogue of 933 filaments extracted from the MeerKAT 1.3 GHz Galactic Plane Survey. Of these, 130 are isolated from known structures such as supernova remnants and HII regions, and 77 of those lack spatially coincident 8.3-micron mid-infrared emission, the paper's proxy for non-thermal (synchrotron) emission. If correct, these are the first non-thermal radio filaments found outside the Galactic Centre, undercutting models that tie filament formation to the unique cosmic-ray and magnetic-field environment of the Galactic Centre. The paper also compares the plane filaments to filaments re-extracted from the Galactic Centre mosaic, finding the latter are narrower and shorter, and that the plane filaments' position angles are uniformly distributed, suggesting they do not trace the large-scale Galactic magnetic field.

What carries the argument

The central mechanism is a semi-automated filament extraction pipeline applied to the SMGPS moment-zero tiles: a median-filter high-pass step removes emission on scales larger than 2 arcminutes, then 3-sigma thresholding creates source masks, which are filtered by the J2 < 0 elongation-moment criterion and a mask aspect ratio of at least 4, with final manual artefact removal. The surviving masks are skeletonised into one-pixel spines, from which length, width, position angle and flux are measured. Non-thermal classification then uses the proxy that absence of spatially coincident 8.3-micron mid-infrared emission indicates synchrotron emission, while thermal radio filaments are bright in the mid-infrared. The same pipeline is applied to the Galactic Centre mosaic to obtain a consistent comparison sample.

What would settle it

A multi-frequency radio observation of a sample of the 77 candidate non-thermal filaments that measures flat or positive spectral indices (indicating thermal free-free emission), or the detection of bright, spatially coincident mid-infrared emission at higher resolution than 20 arcseconds, would falsify the non-thermal classification for those filaments.

Watch

Extended reading notes

Core claim

The paper's central claim is that 77 of the 130 isolated filaments are excellent candidates for non-thermal radio filaments, the first such population identified outside the Galactic Centre. The claim rests on a by-eye classification using 8.3-micron mid-infrared images: filaments with no bright coincident infrared emission are judged likely non-thermal, while those with such emission are likely thermal. Since spectral indices could not be measured from the survey data, the classification is explicitly provisional. The paper further shows that the candidate plane filaments are angularly longer and wider than the Galactic Centre filaments, but have comparable flux densities, and that their position angles on the sky are consistent with a uniform distribution, unlike the perpendicular-to-plane alignment of the longest Galactic Centre filaments. These morphological differences are interpreted as possibly due to distance, or to the more extreme environment of the Galactic Centre.

Load-bearing premise

The load-bearing premise is that the absence of spatially coincident 8.3-micron mid-infrared emission reliably identifies non-thermal radio emission, even though the paper cannot measure spectral indices and line-of-sight infrared contamination could misclassify filaments.

Editorial extensions

If this is right

  • If the 77 candidate non-thermal filaments are confirmed by spectral-index measurements, they would constitute the first population of non-thermal radio filaments in the Galactic Plane, showing that filament formation does not require the Galactic Centre's unique environment.
  • The uniformly distributed position angles of the plane filaments imply that the local magnetic field orientation they trace does not follow the large-scale spiral Galactic field, adding a new constraint on disc magnetic-field structure.
  • If the plane filaments are closer than the Galactic Centre population, the similar flux densities imply the Galactic Centre filaments are intrinsically more luminous and host a more energetic cosmic-ray electron population.
  • The catalogue of 933 filaments, split into 803 non-isolated and 130 isolated sources with measured positions, lengths, widths and fluxes, provides a homogeneous sample for targeted follow-up of individual filaments and their possible cosmic-ray sources.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • A direct test of the classification would be to measure radio spectral indices by combining the SMGPS 1.3 GHz data with higher-frequency images (e.g., 3 or 5 GHz); synchrotron emission typically shows a negative spectral index, whereas the tentative thermal sources would show flat or positive indices.
  • If higher-resolution 8-micron imaging reveals faint mid-infrared counterparts along the lines of sight of the 77 candidates, the true non-thermal fraction among the isolated filaments could be lower than the paper's 59 percent, since line-of-sight confusion would have hidden some thermal sources.
  • The uniform position-angle distribution, if it persists in a larger sample, suggests that synchrotron filaments in the disc may be shaped by local turbulence or shock compression rather than by the global spiral magnetic field; polarimetric observations could test whether the field is disordered at filament scales.
  • Without distance measurements, the morphological comparison between plane and Galactic Centre filaments remains ambiguous; future parallax or association studies that place the plane filaments at known distances would determine whether the differences are intrinsic or purely geometric.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 4 minor

Summary. This paper presents a catalogue of 933 filamentary structures extracted from the SARAO MeerKAT 1.3 GHz Galactic Plane Survey (SMGPS), of which 130 are classified as isolated from extended radio structures. Using by-eye coincidence with MSX 8.3 μm mid-infrared emission, the authors classify 77 of the 130 isolated filaments as candidate non-thermal radio filaments (NRFs) and claim these are the first such objects found outside the Galactic Centre. The paper also applies the same extraction pipeline to the MeerKAT Galactic Centre mosaic and compares the two populations, finding that GC filaments are shorter and narrower, have a brighter tail in mean spine brightness, and show a more anisotropic position-angle distribution. The catalogue itself, including spine masks, is made publicly available.

Significance. If the classification is reliable, the catalogue would provide the first evidence for an isolated NRF population outside the Galactic Centre, directly challenging models that require the unique GC environment for NRF formation. The catalogue and the morphological comparison are valuable resources for follow-up spectral-index and polarisation studies, and the paper is transparent about its main limitations, including a robustness check in Section 5.2.5 that repeats the GC comparison without relying on the MIR classification. The data availability statement provides public access to the catalogues and spine masks, which supports reproducibility. However, the headline claim depends on a proxy that is not quantitatively calibrated, and the GC comparison is affected by several methodological asymmetries.

major comments (3)
  1. [§5.1] The classification of 77/130 isolated filaments as 'likely to be non-thermal' rests entirely on the by-eye absence of spatially coincident MSX 8.3 μm emission, with no quantitative threshold for 'bright' MIR emission, no repeatability test, and no validation against objects with known spectral indices. The manuscript itself states in §5.1 that 'without distance information in the MIR nor the radio we can only speculate on the coincidence of the MIR emission', and in §5.2.5 that 'widespread MIR emission ... may result in a large number of filaments being misidentified as candidate thermal filaments due to line-of-sight confusion'. Because the headline claim that these are the first NRFs outside the GC depends on this proxy, the abstract's 'likely to be non-thermal' overstates the evidence. I request either a quantitative MIR analysis (e.g., measured 8.3 μm brightness at the spines compared with a control sample, or cross-validation with known HII regions and SNRs) or a softening of the language to 'IR-dark candidates', plus a discussion of why the MSX 20″ resolution, comparable to the median filament FWHM, does not compromise the classification.
  2. [§5.2, Fig. 11] The GC comparison is made with a different synthesised beam (4″ versus 8″), a different physical area cutoff (20 beams corresponds to a factor-four smaller physical area for the GC), a different median-filter scale in units of beam (30 versus 15 beams), and a different detection threshold (3σ of a 40 μJy/beam rms, i.e., ~120 μJy/beam, versus the fixed 20 μJy/beam used for SMGPS). These asymmetries are not quantified, so the conclusions that GC filaments are shorter and narrower, and that the GC flux distribution has a brighter tail, may be biased by resolution and selection effects. The authors mention the beam difference but do not test its impact. I recommend convolving the GC mosaic to the SMGPS 8″ beam and re-running the extraction, and/or applying a matching physical size threshold, to demonstrate the robustness of the morphological comparison.
  3. [Abstract; §5.2.2] The statement 'The SMGPS filaments have flux densities similar to those of the GC' is not supported by the analysis, which compares the mean flux along the spine in units of mJy/beam (a surface-brightness measure), not integrated flux densities. The catalogue does not include integrated flux densities, and the conclusion about a more energetic cosmic-ray population in the GC (Section 5.2.2) depends on the luminosity interpretation. Please either compute integrated flux densities for the filaments (e.g., by summing over the source masks or the spine neighbourhood) or revise the abstract and interpretation to refer to mean spine brightness, not flux density.
minor comments (4)
  1. [§3.1] The description of the intensity threshold is internally inconsistent: the text first states that a mask is created 'above 3× the rms background brightness', then reports an rms of 10–15 μJy/beam, but the adopted threshold is given as σ = 20 μJy/beam, which is not 3σ for the stated rms range. Please clarify the actual threshold used for the SMGPS extraction.
  2. [Abstract; §4.2.2] The abstract states that the filament position angles are 'uniformly distributed', but the K-S analysis in Section 4.2.2 only shows that the isolated-filament PA distribution is consistent with uniform (the p-value distribution peaks near 0.22 and extends below 0.05), while the non-isolated sample is inconclusive. Please phrase the claim as 'consistent with a uniform distribution' rather than asserting uniformity.
  3. [Throughout] There are numerous typographical and formatting issues, including the character '□' appearing in place of expected symbols (e.g., in Figure 1 axis labels and elsewhere), the axis label 'pos.galactic.lon' in Figure 1, the header 'MNRAS000, 1–17 (2023)' not updated to the current year, and inconsistent citation formatting for companion papers (e.g., 'Mutale et al., in preparation' versus 'to be submitted'). A careful proofreading pass is needed.
  4. [§5.2.3] The interpretation that the uniform PA distribution implies the local magnetic field traced by SMGPS filaments does not follow the large-scale Galactic field assumes that radio filaments are aligned with the magnetic field. This assumption is not established for the SMGPS sample and should be stated explicitly as a working hypothesis rather than an inference.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the catalogue construction and thermal/non-thermal classification rest on external data and an explicitly stated proxy, not on fitting or predicting the paper's own inputs.

full rationale

The central derivation chain is: extract filaments from SMGPS moment-zero tiles via high-pass filtering, thresholding, and morphological cuts; separate isolated vs. non-isolated filaments by cross-matching to the SMGPS extended source catalogue; classify isolated filaments as candidate thermal or non-thermal by by-eye coincidence with MSX 8.3 micron emission; and compare the candidate NRFs to Galactic Centre filaments extracted with the same pipeline. None of these steps fits a parameter to a subset and then predicts a closely related quantity. The 77/130 split is an observational classification, not a fitted prediction. The MIR proxy is an external assumption whose limitations are explicitly acknowledged in Sections 5.1 and 5.2.5, e.g. 'without distance information in the MIR nor the radio we can only speculate on the coincidence of the MIR emission to the filaments' and 'the classification of these filaments as thermal or non-thermal may be affected by line-of-sight confusion'. Acknowledging that the proxy can misclassify objects is a correctness risk, not circularity. The GC comparison sample is extracted from an independent published mosaic (Heywood et al. 2022) using the same code, so the reported morphological differences are not imposed by construction. The only same-team dependencies (Bordiu et al., under review; Mutale et al., in prep) are companion data products used as inputs, not as validations of this paper's claims; they are independently falsifiable and are not derived from the filament catalogue itself. No circular step is exhibited, so the score is 0.

Assumptions & free parameters 6 free parameters · 4 assumptions · 0 invented entities

The central NRF claim depends on hand-chosen extraction thresholds, an indirect MIR proxy for thermal/non-thermal nature, and the assumption that identical-looking extraction on two different surveys yields comparable populations. No new physical entities are introduced.

free parameters (6)
  • Median filter window size = 15 beam widths (2 arcmin)
    Chosen by eye as best enhancing filamentary features; defines what is removed as diffuse emission and therefore what structures remain (Section 3.1).
  • Intensity threshold (SMGPS) = 3 sigma = 20 uJy/beam
    Chosen after testing as a compromise between tiles of different noise; sets the detection limit for all filament masks (Section 3.1).
  • Minimum mask area = 20 synthesised beam areas
    Judged by eye to remove artefacts and small sources; affects which filaments enter the catalogue (Section 3.1).
  • Mask aspect ratio cut = >= 4
    Adopted from star formation filament definitions; selects elongated structures (Section 3.1).
  • Straightening polynomial order = n = 10
    From testing, best results; affects transverse profile and width measurements (Section 4.2.1).
  • Intensity threshold (GC mosaic) = 3 sigma = 40 uJy/beam
    Measured in emission-free regions of the GC mosaic; used with the same morphological cuts but a different beam size, which may bias the comparison (Section 5.2).
assumptions (4)
  • domain assumption Absence of bright 8.3 micron MSX emission is a reliable signpost of non-thermal radio emission.
    Invoked in Section 5.1 for classification; paper concedes line-of-sight confusion and no spectral index verification.
  • domain assumption Hand-chosen extraction thresholds and manual refinement do not bias the comparison between SMGPS and GC filament populations.
    Section 3.1 and 5.2; the same method is applied to both, but thresholds and beams differ and visual inspection is subjective.
  • domain assumption Filament position angles trace the local magnetic field direction.
    Section 5.2.3; used to infer that the local field does not follow the large-scale Galactic field.
  • domain assumption Mean spine flux densities are not systematically biased by the negative bowl artifacts from high-pass filtering.
    Section 5.1 describes negative bowls that steepen spectra, but flux comparisons with the GC still use the filtered images.

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Cite this review

Pith. "Pith review of The SARAO MeerKAT Galactic Plane Survey filamentary source catalogue." pith.science (2026). https://pith.science/paper/LCJEBXAK

@misc{pith2026241207852,
  author       = {Pith},
  title        = {Pith review of: The SARAO MeerKAT Galactic Plane Survey filamentary source catalogue},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/LCJEBXAK}},
  note         = {Machine review of arXiv:2412.07852}
}
read the original abstract

We present a catalogue of filamentary structures identified in the SARAO (South African Radio Astronomy Observatory) MeerKAT 1.3 GHz Galactic Plane Survey (SMGPS). We extract 933 filaments across the survey area, 803 of which (~86%) are associated with extended radio structures (e.g. supernova remnants and HII regions), whilst 130 (~14%) are largely isolated. We classify filaments as thermal or non-thermal via their associated mid-infrared emission and find 77/130 (~59%) of the isolated sources are likely to be non-thermal, and are therefore excellent candidates for the first isolated, non-thermal radio filaments observed outside of the Galactic Centre (GC). Comparing the morphological properties of these non-thermal candidates to the non-thermal filaments observed towards the GC we find the GC filaments are on the whole angularly narrower and shorter than those across the SMGPS, potentially an effect of distance. The SMGPS filaments have flux densities similar to those of the GC, however the distribution of the latter extends to higher flux densities. If the SMGPS filaments were closer than the GC population, it would imply a more energetic population of cosmic ray electrons in the GC. We find the filament position angles in the SMGPS are uniformly distributed, implying that the local magnetic field traced by the filaments does not follow the large-scale Galactic field. Finally, although we have clearly shown that filaments are not unique to the GC, the GC nevertheless has the highest density of filaments in the Milky Way.

Figures

Figures reproduced from arXiv: 2412.07852 by the authors.

Figure 1
Figure 1. (a) SMGPS 1.3 GHz moment zero continuum towards a filamen￾tous region in the G342.5+0.0 tile (341◦ < 𝑙 < 344◦ , −1.56◦ < 𝑏 < 1.56◦ ). (b) The same region as shown in (a), but following the high-pass filter tech￾nique (see Section 3) for removal of diffuse emission on scales larger than 2 arcminutes. 2 OBSERVATIONS The SARAO MeerKAT 1.3 GHz Galactic Plane Survey (SMGPS; Goedhart et al. 2024) carried out a survey of a… view at source ↗
Figure 2
Figure 2. Positions of all identified filaments across the survey area, with their major axes marked by coloured markers (these major axes are referred to as “spines” from Section 4 onwards). Marked in blue and orange are filaments classed as isolated and non-isolated respectively (see Section 3.2). Grey shaded regions indicate areas not covered by the survey (see Section 2), and the horizontal grey dashed line marks a Galact… view at source ↗
Figure 2
Figure 2. (cont.) Caption as on previous page. The dashed black box marks the region presented in the SMGPS overview paper (Goedhart et al. 2024). The shift in latitude for panels with 𝑙 < 300◦ marks the shift in the SMGPS coverage to account for the Galactic warp. MNRAS 000, 1–17 (2023) [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figures from the paper (13 more)
Figure 3
Figure 3. Figure 3: SMGPS 1.3 GHz moment zero continuum (unfiltered) towards examples of identified filaments. Filaments found within extended structures are plotted in orange (i.e. non-isolated), whilst those found to be isolated are plotted in blue. Dashed black box/circles represent th…
Figure 4
Figure 4. Figure 4: Distribution of (a) Galactic longitude, and (b) Galactic latitude, of non-isolated filaments (orange), and isolated filaments (blue). The distri￾bution is shown both as a histogram (coloured bins, left y-axis), and as a cumulative probability (solid coloured lines, rig…
Figure 5
Figure 5. Figure 5: (a) High-pass filtered 1.3 GHz continuum image of an isolated filament shown in [PITH_FULL_IMAGE:figures/full_fig_p008_5.png]
Figure 6
Figure 6. Figure 6: Normalised histograms of (a) the filament lengths in arcminutes, (b) the fitted FWHMs in arcseconds, and (c) the length-to-width ratios, of non-isolated filaments (orange) and isolated filaments (blue). The corresponding cumulative distributions are shown in panels (d)…
Figure 7
Figure 7. Figure 7: (a) Normalised histogram of position angle (PA, in degrees) of non-isolated filaments in orange, and isolated filaments in blue. (b) Cumulative distribution function (CDF) of the PAs of non-isolated filaments. Plotted in grey are 1000 realisations of randomly drawn uni…
Figure 8
Figure 8. Figure 8: Normalised histograms of (a) the filament lengths in arcminutes, (b) the fitted FWHMs in arcseconds, (c) the length-to-width ratios, and (d) position angles, of isolated filaments. Those in red have coincident MSX 8.3𝜇m infrared emission, whilst those in blue do not. B…
Figure 9
Figure 9. Figure 9: Distribution of (a) Galactic longitude, and (b) Galactic latitude, of the isolated SMGPS filaments expressed as a histogram (coloured bins, left y-axis), and as a cumulative distribution function (CDF; solid coloured lines, right y-axis). Red corresponds to filaments t…
Figure 10
Figure 10. Figure 10: MeerKAT 1.28 GHz total-intensity mosaic of the Galactic Centre (Heywood et al. 2022). Overlaid in green are the one-pixel wide spines of filaments extracted using the same method as applied to the SMGPS in this work (detailed in §3.1). Three named NRF regions that are…
Figure 11
Figure 11. Figure 11: Normalised histograms of (a) the filament lengths in arcminutes, (b) the fitted FWHMs in arcseconds, (c) the length-to-width ratios (i.e. the ratio of the length to the fitted FWHM), and (d) the mean flux along the source spines in mJy beam−1 , of the candidate non-th…
Figure 12
Figure 12. Figure 12: (a) Normalised histogram of position angle (PA, in degrees) of of isolated, candidate non-thermal SMGPS sources in blue, and IR-dark GC filaments in green. (b) Cumulative distribution function (CDF) of the PAs of IR-dark GC filaments. Plotted in grey are 1000 realisat…
Figure 13
Figure 13. Figure 13: Distribution of filament position angle (PA) against length for (a) the IR-dark Galactic Centre filaments, and (b) the IR-dark SMGPS filaments (see §5.1). The vertical grey dashed line marks PA= 0 ◦ . large scale magnetic field oriented parallel to the Galactic Plane …
Figure 14
Figure 14. Figure 14: Distribution of (a) Galactic longitude, and (b) Galactic latitude, of the candidate non-thermal SMGPS filaments (blue), and the IR-dark GC filaments (green). The distribution is shown both as a histogram (coloured bins, left y-axis), and as a cumulative probability (s…
Figure 15
Figure 15. Figure 15: Normalised histograms of (a) the filament lengths in arcminutes, (b) the fitted FWHMs in arcseconds, (c) the length-to-width ratios (i.e. the ratio of the length to the fitted FWHM), (d) the mean flux along the source spines in mJy beam−1 , and (e) position angles, of…

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Works this paper leans on

88 extracted references · 15 canonical work pages

  1. [1]

    write newline

    " write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.state := if if FUNCTION not #0 #1 if FUNCTION and 'skip pop #0 if FUNCTION or pop #1...

  2. [2]

    D., et al., 2017, @doi [ ] 10.1051/0004-6361/201731019 , https://ui.adsabs.harvard.edu/abs/2017A&A...605A..58A 605, A58

    Anderson L. D., et al., 2017, @doi [ ] 10.1051/0004-6361/201731019 , https://ui.adsabs.harvard.edu/abs/2017A&A...605A..58A 605, A58

    doi:10.1051/0004-6361/201731019 2017

  3. [3]

    D., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2409.16607 , https://ui.adsabs.harvard.edu/abs/2024arXiv240916607A p

    Anderson L. D., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2409.16607 , https://ui.adsabs.harvard.edu/abs/2024arXiv240916607A p. arXiv:2409.16607

    arXiv doi:10.48550/arxiv.2409.16607 2024

  4. [4]

    I., Pudritz R

    Andr \'e P., Di Francesco J., Ward-Thompson D., Inutsuka S. I., Pudritz R. E., Pineda J. E., 2014, in Beuther H., Klessen R. S., Dullemond C. P., Henning T., eds, Protostars and Planets VI. p. 27 ( @eprint arXiv 1312.6232 ), @doi 10.2458/azu\_uapress\_9780816531240-ch002

    arXiv 2014

  5. [5]

    Arzoumanian D., et al., 2019, @doi [ ] 10.1051/0004-6361/201832725 , https://ui.adsabs.harvard.edu/abs/2019A&A...621A..42A 621, A42

    doi:10.1051/0004-6361/201832725 2019

  6. [6]

    Astropy Collaboration et al., 2013, @doi [ ] 10.1051/0004-6361/201322068 , https://ui.adsabs.harvard.edu/abs/2013A&A...558A..33A 558, A33

    doi:10.1051/0004-6361/201322068 2013

  7. [7]

    V., Lyutikov M., 2019, @doi [ ] 10.1093/mnrasl/slz124 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.489L..28B 489, L28

    Barkov M. V., Lyutikov M., 2019, @doi [ ] 10.1093/mnrasl/slz124 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.489L..28B 489, L28

    doi:10.1093/mnrasl/slz124 2019

  8. [8]

    Bianchi S., et al., 2017, @doi [ ] 10.1051/0004-6361/201629013 , https://ui.adsabs.harvard.edu/abs/2017A&A...597A.130B 597, A130

    doi:10.1051/0004-6361/201629013 2017

Show all 88 references
  1. [9]

    O., et al., 2024, @doi [ ] 10.3847/1538-4357/ad12b9 , https://ui.adsabs.harvard.edu/abs/2024ApJ...963..130B 963, 130

    Butterfield N. O., et al., 2024, @doi [ ] 10.3847/1538-4357/ad12b9 , https://ui.adsabs.harvard.edu/abs/2024ApJ...963..130B 963, 130

    2024 doi

  2. [10]

    M., Amato E., Petrov A

    Bykov A. M., Amato E., Petrov A. E., Krassilchtchikov A. M., Levenfish K. P., 2017, @doi [ ] 10.1007/s11214-017-0371-7 , https://ui.adsabs.harvard.edu/abs/2017SSRv..207..235B 207, 235

    2017 doi

  3. [11]

    T., Davidson J

    Chuss D. T., Davidson J. A., Dotson J. L., Dowell C. D., Hildebrand R. H., Novak G., Vaillancourt J. E., 2003, @doi [ ] 10.1086/379538 , https://ui.adsabs.harvard.edu/abs/2003ApJ...599.1116C 599, 1116

    2003 doi

  4. [12]

    E., Hensley B

    Clark S. E., Hensley B. S., 2019, @doi [ ] 10.3847/1538-4357/ab5803 , https://ui.adsabs.harvard.edu/abs/2019ApJ...887..136C 887, 136

    2019 doi

  5. [13]

    D., Williams G

    Clarke S. D., Williams G. M., Ib \'a \ n ez-Mej \' a J. C., Walch S., 2019, @doi [ ] 10.1093/mnras/stz248 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.484.4024C 484, 4024

    2019 doi

  6. [14]

    D., Williams G

    Clarke S. D., Williams G. M., Walch S., 2020, @doi [ ] 10.1093/mnras/staa2298 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.497.4390C 497, 4390

    2020 doi

  7. [15]

    J., 2001, @doi [ ] 10.1046/j.1365-8711.2001.04421.x , https://ui.adsabs.harvard.edu/abs/2001MNRAS.325..531C 325, 531

    Cohen M., Green A. J., 2001, @doi [ ] 10.1046/j.1365-8711.2001.04421.x , https://ui.adsabs.harvard.edu/abs/2001MNRAS.325..531C 325, 531

    2001

  8. [16]

    R., Nixon C

    Coughlin E. R., Nixon C. J., Ginsburg A., 2021, @doi [ ] 10.1093/mnras/staa3771 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.501.1868C 501, 1868

    2021 doi

  9. [17]

    M., Jones D

    Crocker R. M., Jones D. I., Melia F., Ott J., Protheroe R. J., 2010, @doi [ ] 10.1038/nature08635 , https://ui.adsabs.harvard.edu/abs/2010Natur.463...65C 463, 65

    2010 doi

  10. [18]

    M., Hartmann D., Thaddeus P., 2001, @doi [ ] 10.1086/318388 , https://ui.adsabs.harvard.edu/abs/2001ApJ...547..792D 547, 792

    Dame T. M., Hartmann D., Thaddeus P., 2001, @doi [ ] 10.1086/318388 , https://ui.adsabs.harvard.edu/abs/2001ApJ...547..792D 547, 792

    2001 doi

  11. [19]

    Ferri \`e re K., 2009, @doi [ ] 10.1051/0004-6361/200912617 , https://ui.adsabs.harvard.edu/abs/2009A&A...505.1183F 505, 1183

    2009 doi

  12. [20]

    Goedhart S., et al., 2024, @doi [ ] 10.1093/mnras/stae1166 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.531..649G 531, 649

    2024 doi

  13. [21]

    Gravity Collaboration et al., 2019, @doi [ ] 10.1051/0004-6361/201935656 , https://ui.adsabs.harvard.edu/abs/2019A&A...625L..10G 625, L10

    2019 doi

  14. [22]

    D., Cram L

    Gray A. D., Cram L. E., Ekers R. D., Goss W. M., 1991, @doi [ ] 10.1038/353237a0 , https://ui.adsabs.harvard.edu/abs/1991Natur.353..237G 353, 237

    1991 doi

  15. [23]

    A., 2014, @doi [Bulletin of the Astronomical Society of India] 10.48550/arXiv.1409.0637 , https://ui.adsabs.harvard.edu/abs/2014BASI...42...47G 42, 47

    Green D. A., 2014, @doi [Bulletin of the Astronomical Society of India] 10.48550/arXiv.1409.0637 , https://ui.adsabs.harvard.edu/abs/2014BASI...42...47G 42, 47

    2014 doi arXiv

  16. [24]

    Guan Y., et al., 2021, @doi [ ] 10.3847/1538-4357/ac133f , https://ui.adsabs.harvard.edu/abs/2021ApJ...920....6G 920, 6

    2021 doi

  17. [25]

    Han J.-L., Wielebinski R., 2002, @doi [ ] 10.1088/1009-9271/2/4/293 , https://ui.adsabs.harvard.edu/abs/2002ChJAA...2..293H 2, 293

    2002 doi

  18. [26]

    R., et al., 2020, @doi [ ] 10.1038/s41586-020-2649-2 , https://ui.adsabs.harvard.edu/abs/2020Natur.585..357H 585, 357

    Harris C. R., et al., 2020, @doi [ ] 10.1038/s41586-020-2649-2 , https://ui.adsabs.harvard.edu/abs/2020Natur.585..357H 585, 357

    2020 doi

  19. [27]

    Heywood I., et al., 2019, @doi [ ] 10.1038/s41586-019-1532-5 , https://ui.adsabs.harvard.edu/abs/2019Natur.573..235H 573, 235

    2019 doi

  20. [28]

    Heywood I., et al., 2022, @doi [ ] 10.3847/1538-4357/ac449a , https://ui.adsabs.harvard.edu/abs/2022ApJ...925..165H 925, 165

    2022 doi

  21. [29]

    G., Han J

    Hou L. G., Han J. L., 2014, @doi [ ] 10.1051/0004-6361/201424039 , https://ui.adsabs.harvard.edu/abs/2014A&A...569A.125H 569, A125

    2014 doi

  22. [30]

    D., 2007, @doi [Computing in Science and Engineering] 10.1109/MCSE.2007.55 , https://ui.adsabs.harvard.edu/abs/2007CSE.....9...90H 9, 90

    Hunter J. D., 2007, @doi [Computing in Science and Engineering] 10.1109/MCSE.2007.55 , https://ui.adsabs.harvard.edu/abs/2007CSE.....9...90H 9, 90

    2007 doi

  23. [31]

    Hurley-Walker N., et al., 2019, @doi [ ] 10.1017/pasa.2019.33 , https://ui.adsabs.harvard.edu/abs/2019PASA...36...48H 36, e048

    2019 doi

  24. [32]

    Indriolo N., et al., 2015, @doi [ ] 10.1088/0004-637X/800/1/40 , https://ui.adsabs.harvard.edu/abs/2015ApJ...800...40I 800, 40

    2015 doi

  25. [33]

    Jackson T., Werner M., Gautier T. N. I., 2003, @doi [ ] 10.1086/378671 , https://ui.adsabs.harvard.edu/abs/2003ApJS..149..365J 149, 365

    2003 doi

  26. [34]

    E., Whitworth A

    Jaffa S. E., Whitworth A. P., Clarke S. D., Howard A. D. P., 2018, @doi [ ] 10.1093/mnras/sty696 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.477.1940J 477, 1940

    2018 doi

  27. [35]

    Kalberla P. M. W., Kerp J., Haud U., Winkel B., Ben Bekhti N., Fl \"o er L., Lenz D., 2016, @doi [ ] 10.3847/0004-637X/821/2/117 , https://ui.adsabs.harvard.edu/abs/2016ApJ...821..117K 821, 117

    2016 doi

  28. [36]

    Kalberla P. M. W., Kerp J., Haud U., 2020, @doi [ ] 10.1051/0004-6361/202037602 , https://ui.adsabs.harvard.edu/abs/2020A&A...639A..26K 639, A26

    2020 doi

  29. [37]

    Kansabanik D., et al., 2024, @doi [ ] 10.3847/1538-4357/ad0b7f , https://ui.adsabs.harvard.edu/abs/2024ApJ...961...96K 961, 96

    2024 doi

  30. [38]

    Knowles K., et al., 2022, @doi [ ] 10.1051/0004-6361/202141488 , https://ui.adsabs.harvard.edu/abs/2022A&A...657A..56K 657, A56

    2022 doi

  31. [39]

    W., Rosolowsky E

    Koch E. W., Rosolowsky E. W., 2015, @doi [ ] 10.1093/mnras/stv1521 , http://adsabs.harvard.edu/abs/2015MNRAS.452.3435K 452, 3435

    2015 doi

  32. [40]

    C., Anantharamaiah K

    Lang C. C., Anantharamaiah K. R., Kassim N. E., Lazio T. J. W., 1999a, @doi [ ] 10.1086/312180 , https://ui.adsabs.harvard.edu/abs/1999ApJ...521L..41L 521, L41

    doi

  33. [41]

    C., Morris M., Echevarria L., 1999b, @doi [ ] 10.1086/308012 , https://ui.adsabs.harvard.edu/abs/1999ApJ...526..727L 526, 727

    Lang C. C., Morris M., Echevarria L., 1999b, @doi [ ] 10.1086/308012 , https://ui.adsabs.harvard.edu/abs/1999ApJ...526..727L 526, 727

    doi

  34. [42]

    J., Yusef-Zadeh F., Cotton W

    Law C. J., Yusef-Zadeh F., Cotton W. D., 2008, @doi [ ] 10.1086/588218 , https://ui.adsabs.harvard.edu/abs/2008ApJS..177..515L 177, 515

    2008 doi

  35. [43]

    Lee T., Kashyap R., Chu C., 1994, @doi [CVGIP: Graphical Models and Image Processing] https://doi.org/10.1006/cgip.1994.1042 , 56, 462

    1994

  36. [44]

    S., Leurini S., Csengeri T., Wyrowski F., Menten K

    Li G.-X., Urquhart J. S., Leurini S., Csengeri T., Wyrowski F., Menten K. M., Schuller F., 2016, @doi [ ] 10.1051/0004-6361/201527468 , https://ui.adsabs.harvard.edu/abs/2016A&A...591A...5L 591, A5

    2016 doi

  37. [45]

    J., et al., 1984, @doi [ ] 10.1086/184213 , https://ui.adsabs.harvard.edu/abs/1984ApJ...278L..19L 278, L19

    Low F. J., et al., 1984, @doi [ ] 10.1086/184213 , https://ui.adsabs.harvard.edu/abs/1984ApJ...278L..19L 278, L19

    1984 doi

  38. [46]

    Mangilli A., et al., 2019, @doi [ ] 10.1051/0004-6361/201935072 , https://ui.adsabs.harvard.edu/abs/2019A&A...630A..74M 630, A74

    2019 doi

  39. [47]

    Mattern M., et al., 2018, @doi [ ] 10.1051/0004-6361/201833406 , https://ui.adsabs.harvard.edu/abs/2018A&A...619A.166M 619, A166

    2018 doi

  40. [48]

    pp 56 -- 61, @doi 10.25080/Majora-92bf1922-00a

    McKinney W., 2010, in S t\'efan van der W alt & J arrod M illman ed., P roceedings of the 9th P ython in S cience C onference. pp 56 -- 61, @doi 10.25080/Majora-92bf1922-00a

    2010 doi

  41. [49]

    MeerKAT Collaboration 2018, Monthly Notes of the Astronomical Society of South Africa, https://ui.adsabs.harvard.edu/abs/2018MNSSA..77..102. 77, 102

    2018

  42. [50]

    A., et al., 2010, @doi [ ] 10.1051/0004-6361/201014678 , https://ui.adsabs.harvard.edu/abs/2010A&A...518L.104M 518, L104

    Miville-Desch \^e nes M. A., et al., 2010, @doi [ ] 10.1051/0004-6361/201014678 , https://ui.adsabs.harvard.edu/abs/2010A&A...518L.104M 518, L104

    2010 doi

  43. [51]

    Molinari S., et al., 2016, @doi [ ] 10.1051/0004-6361/201526380 , https://ui.adsabs.harvard.edu/abs/2016A&A...591A.149M 591, A149

    2016 doi

  44. [52]

    C., Muno M

    Morris M., 2006, in Sch \"o del R., Bower G. C., Muno M. P., Nayakshin S., Ott T., eds, Journal of Physics Conference Series Vol. 54, Journal of Physics Conference Series. IOP, pp 1--9, @doi 10.1088/1742-6596/54/1/001

    2006 doi

  45. [53]

    Morris M., Serabyn E., 1996, @doi [ ] 10.1146/annurev.astro.34.1.645 , https://ui.adsabs.harvard.edu/abs/1996ARA&A..34..645M 34, 645

    1996 doi

  46. [54]

    R., Zhao J.-H., Goss W

    Morris M. R., Zhao J.-H., Goss W. M., 2017, @doi [ ] 10.3847/2041-8213/aa9985 , https://ui.adsabs.harvard.edu/abs/2017ApJ...850L..23M 850, L23

    2017 doi

  47. [55]

    Nishiyama S., et al., 2010, @doi [ ] 10.1088/2041-8205/722/1/L23 , https://ui.adsabs.harvard.edu/abs/2010ApJ...722L..23N 722, L23

    2010 doi

  48. [56]

    M., Lang C

    Par \'e D. M., Lang C. C., Morris M. R., 2022, @doi [ ] 10.3847/1538-4357/aca40a , https://ui.adsabs.harvard.edu/abs/2022ApJ...941..123P 941, 123

    2022 doi

  49. [57]

    O., Chuss D

    Par \'e D., Butterfield N. O., Chuss D. T., Guerra J. A., Iuliano J. I., Karpovich K., Morris M. R., Wollack E. J., 2024, @doi [ ] 10.3847/1538-4357/ad4462 , https://ui.adsabs.harvard.edu/abs/2024ApJ...969..150P 969, 150

    2024 doi

  50. [58]

    D., Egan M

    Price S. D., Egan M. P., Carey S. J., Mizuno D. R., Kuchar T. A., 2001, @doi [ ] 10.1086/320404 , https://ui.adsabs.harvard.edu/abs/2001AJ....121.2819P 121, 2819

    2001 doi

  51. [59]

    E., Henning T., Tackenberg J., Beuther H., Johnston K

    Ragan S. E., Henning T., Tackenberg J., Beuther H., Johnston K. G., Kainulainen J., Linz H., 2014, @doi [ ] 10.1051/0004-6361/201423401 , https://ui.adsabs.harvard.edu/abs/2014A&A...568A..73R 568, A73

    2014 doi

  52. [60]

    Ramatsoku M., et al., 2020, @doi [ ] 10.1051/0004-6361/202037800 , https://ui.adsabs.harvard.edu/abs/2020A&A...636L...1R 636, L1

    2020 doi

  53. [61]

    J., et al., 2019, @doi [ ] 10.3847/1538-4357/ab4a11 , https://ui.adsabs.harvard.edu/abs/2019ApJ...885..131R 885, 131

    Reid M. J., et al., 2019, @doi [ ] 10.3847/1538-4357/ab4a11 , https://ui.adsabs.harvard.edu/abs/2019ApJ...885..131R 885, 131

    2019 doi

  54. [62]

    J., et al., 2019, @doi [ ] 10.1051/0004-6361/201935236 , https://ui.adsabs.harvard.edu/abs/2019A&A...632A..58R 632, A58

    Rigby A. J., et al., 2019, @doi [ ] 10.1051/0004-6361/201935236 , https://ui.adsabs.harvard.edu/abs/2019A&A...632A..58R 632, A58

    2019 doi

  55. [63]

    M., Heyer M., Johnson A., Rathborne J., Shah R., Simon R., 2009, @doi [ ] 10.1088/0004-637X/699/2/1153 , https://ui.adsabs.harvard.edu/abs/2009ApJ...699.1153R 699, 1153

    Roman-Duval J., Jackson J. M., Heyer M., Johnson A., Rathborne J., Shah R., Simon R., 2009, @doi [ ] 10.1088/0004-637X/699/2/1153 , https://ui.adsabs.harvard.edu/abs/2009ApJ...699.1153R 699, 1153

    2009 doi

  56. [64]

    M., Heyer M., Rathborne J., Simon R., 2010, @doi [ ] 10.1088/0004-637X/723/1/492 , https://ui.adsabs.harvard.edu/abs/2010ApJ...723..492R 723, 492

    Roman-Duval J., Jackson J. M., Heyer M., Rathborne J., Simon R., 2010, @doi [ ] 10.1088/0004-637X/723/1/492 , https://ui.adsabs.harvard.edu/abs/2010ApJ...723..492R 723, 492

    2010 doi

  57. [65]

    Rosner R., Bodo G., 1996, @doi [ ] 10.1086/310286 , https://ui.adsabs.harvard.edu/abs/1996ApJ...470L..49R 470, L49

    1996 doi

  58. [66]

    Schisano E., et al., 2020, @doi [ ] 10.1093/mnras/stz3466 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.492.5420S 492, 5420

    2020 doi

  59. [67]

    G., 1979, @doi [ ] 10.1086/190609 , https://ui.adsabs.harvard.edu/abs/1979ApJS...41...87S 41, 87

    Schneider S., Elmegreen B. G., 1979, @doi [ ] 10.1086/190609 , https://ui.adsabs.harvard.edu/abs/1979ApJS...41...87S 41, 87

    1979 doi

  60. [68]

    D., et al., 2020, @doi [ ] 10.1051/0004-6361/202038882 , https://ui.adsabs.harvard.edu/abs/2020A&A...642A.163S 642, A163

    Soler J. D., et al., 2020, @doi [ ] 10.1051/0004-6361/202038882 , https://ui.adsabs.harvard.edu/abs/2020A&A...642A.163S 642, A163

    2020 doi

  61. [69]

    Thomas T., Pfrommer C., En lin T., 2020, @doi [ ] 10.3847/2041-8213/ab7237 , https://ui.adsabs.harvard.edu/abs/2020ApJ...890L..18T 890, L18

    2020 doi

  62. [70]

    M., Greene C

    Thyng K. M., Greene C. A., Hetland R. D., Zimmerle H. M., DiMarco S. F., 2016, @doi [Oceanography] 10.5670/oceanog.2016.66 , 29, 3

    2016 doi

  63. [71]

    Tsuboi M., Inoue M., Handa T., Tabara H., Kato T., Sofue Y., Kaifu N., 1986, @doi [ ] 10.1086/114215 , https://ui.adsabs.harvard.edu/abs/1986AJ.....92..818T 92, 818

    1986 doi

  64. [72]

    der Tak van van der Tak F. F. S., Belloche A., Schilke P., G \"u sten R., Philipp S., Comito C., Bergman P., Nyman L. A ., 2006, @doi [ ] 10.1051/0004-6361:20065289 , https://ui.adsabs.harvard.edu/abs/2006A&A...454L..99V 454, L99

    2006 doi

  65. [73]

    der Walt Van van der Walt S., et al., 2014, @doi [PeerJ] 10.7717/peerj.453 , https://ui.adsabs.harvard.edu/abs/2014PeerJ...2..453V 2, e453

    2014 doi

  66. [74]

    L., Schmelz J

    Verschuur G. L., Schmelz J. T., Asgari-Targhi M., 2018, @doi [ ] 10.3847/1538-4357/aae4df , https://ui.adsabs.harvard.edu/abs/2018ApJ...867..139V 867, 139

    2018 doi

  67. [75]

    Virtanen P., et al., 2020, @doi [Nature Methods] https://doi.org/10.1038/s41592-019-0686-2 , https://rdcu.be/b08Wh 17, 261

    2020 doi

  68. [76]

    Whiteoak J. B. Z., Green A. J., 1996, , https://ui.adsabs.harvard.edu/abs/1996A&AS..118..329W 118, 329

    1996

  69. [77]

    Yusef-Zadeh F., Wardle M., 2019, @doi [ ] 10.1093/mnrasl/slz134 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.490L...1Y 490, L1

    2019 doi

  70. [78]

    Yusef-Zadeh F., Morris M., Chance D., 1984, @doi [ ] 10.1038/310557a0 , https://ui.adsabs.harvard.edu/abs/1984Natur.310..557Y 310, 557

    1984 doi

  71. [79]

    Yusef-Zadeh F., Wardle M., Parastaran P., 1997, @doi [ ] 10.1086/310484 , https://ui.adsabs.harvard.edu/abs/1997ApJ...475L.119Y 475, L119

    1997 doi

  72. [80]

    W., Cotton W., 2004, @doi [ ] 10.1086/425257 , https://ui.adsabs.harvard.edu/abs/2004ApJS..155..421Y 155, 421

    Yusef-Zadeh F., Hewitt J. W., Cotton W., 2004, @doi [ ] 10.1086/425257 , https://ui.adsabs.harvard.edu/abs/2004ApJS..155..421Y 155, 421

    2004 doi

  73. [81]

    G., Wardle M., Boldyrev S., Heywood I., Cotton W., Camilo F., 2022a, @doi [ ] 10.1093/mnras/stac1696 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.515.3059Y 515, 3059

    Yusef-Zadeh F., Arendt R. G., Wardle M., Boldyrev S., Heywood I., Cotton W., Camilo F., 2022a, @doi [ ] 10.1093/mnras/stac1696 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.515.3059Y 515, 3059

    doi

  74. [82]

    G., Wardle M., Heywood I., Cotton W., 2022b, @doi [ ] 10.1093/mnras/stac2415 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.517..294Y 517, 294

    Yusef-Zadeh F., Arendt R. G., Wardle M., Heywood I., Cotton W., 2022b, @doi [ ] 10.1093/mnras/stac2415 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.517..294Y 517, 294

    doi

  75. [83]

    G., Wardle M., Heywood I., Cotton W., Camilo F., 2022c, @doi [ ] 10.3847/2041-8213/ac4802 , https://ui.adsabs.harvard.edu/abs/2022ApJ...925L..18Y 925, L18

    Yusef-Zadeh F., Arendt R. G., Wardle M., Heywood I., Cotton W., Camilo F., 2022c, @doi [ ] 10.3847/2041-8213/ac4802 , https://ui.adsabs.harvard.edu/abs/2022ApJ...925L..18Y 925, L18

    doi

  76. [84]

    G., Wardle M., 2022d, @doi [ ] 10.3847/2041-8213/ac982a , https://ui.adsabs.harvard.edu/abs/2022ApJ...939L..21Y 939, L21

    Yusef-Zadeh F., Arendt R. G., Wardle M., 2022d, @doi [ ] 10.3847/2041-8213/ac982a , https://ui.adsabs.harvard.edu/abs/2022ApJ...939L..21Y 939, L21

    doi

  77. [85]

    G., Wardle M., Heywood I., 2023, @doi [ ] 10.3847/2041-8213/acd54b , https://ui.adsabs.harvard.edu/abs/2023ApJ...949L..31Y 949, L31

    Yusef-Zadeh F., Arendt R. G., Wardle M., Heywood I., 2023, @doi [ ] 10.3847/2041-8213/acd54b , https://ui.adsabs.harvard.edu/abs/2023ApJ...949L..31Y 949, L31

    2023 doi

  78. [86]

    H.-H., 2018, @doi [ ] 10.3847/1538-4357/aad3b5 , https://ui.adsabs.harvard.edu/abs/2018ApJ...864..152Z 864, 152

    Zucker C., Chen H. H.-H., 2018, @doi [ ] 10.3847/1538-4357/aad3b5 , https://ui.adsabs.harvard.edu/abs/2018ApJ...864..152Z 864, 152

    2018 doi

  79. [87]

    Zucker C., Battersby C., Goodman A., 2018, @doi [ ] 10.3847/1538-4357/aacc66 , https://ui.adsabs.harvard.edu/abs/2018ApJ...864..153Z 864, 153

    2018 doi

  80. [88]

    G., 2017, @doi [Physics of Plasmas] 10.1063/1.4984017 , https://ui.adsabs.harvard.edu/abs/2017PhPl...24e5402Z 24, 055402

    Zweibel E. G., 2017, @doi [Physics of Plasmas] 10.1063/1.4984017 , https://ui.adsabs.harvard.edu/abs/2017PhPl...24e5402Z 24, 055402

    2017 doi

Pith tools

Reviewed August 11, 2026 · model on record in the stance chip above.