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Star formation at different stages of ram-pressure stripping as observed through far-ultraviolet imaging of 13 GASP galaxies

T0 review · 3 major / 6 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read In 13 ram-pressure-stripped galaxies, far-ultraviolet and H-alpha light coincide in star-forming knots, showing that young stars power bright tails, while H-alpha without UV points to other heating.

desk verdict Useful FUV sample paper whose most interesting JO147 claim rests on an untested zero-dust assumption. read the letter →

arxiv 2505.15066 v2 pith:MIBL5SXI submitted 2025-05-21 astro-ph.GA

Koshy George , B. M. Poggianti , B. Vulcani , M. Gullieuszik , J. Postma , Jacopo Fritz , P. Côté , Yara L. Jaffe
show 7 more authors
A. Moretti Alessandro Ignesti Giorgia Peluso Neven Tomićić A. Subramaniam S. K. Ghosh S.N. Tandon
This is my paper · ORCID
classification astro-ph.GA
keywords ram-pressurestrippingstarformationfar-ultravioletimagingH-alphaemissionjellyfishgalaxiesgalaxyclustersdisctruncationthermalconduction
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

Using far-ultraviolet (FUV) images of 13 galaxies caught in the act of ram-pressure stripping, this study asks where star formation actually occurs in the stripped tails and discs, and whether H-alpha light in the tails always means young stars. The paper finds that in seven strong and extreme stripping cases, clumpy FUV and H-alpha knots coincide, so photoionization by young massive stars (ages under about 10 Myr) powers both emissions. In six other galaxies the tails show H-alpha with little or no FUV, and the paper argues that these unresolved H-alpha tails are likely produced by something other than star formation, such as thermal conduction from the hot intracluster medium. Two galaxies with truncated discs confine their FUV to the galaxy centers, which the paper reads as direct evidence of outside-in quenching after the outer gas was stripped.

What carries the argument

The load-bearing tool is paired FUV and H-alpha imaging of the same galaxies, analyzed as flux in knot-like segments. Segments are defined by running segmentation photometry on the H-alpha images, then measuring FUV flux in the same areas; FUV-only segmentation is done as a cross-check. Emission-line diagnostic (BPT) maps from integral-field spectroscopy classify each region as star-forming, composite, LINER, or AGN, and the paper checks that FUV-bright regions match the star-forming class. The age logic rests on the different lifetimes of the stars that produce each band: FUV emits from stars younger than roughly 200 Myr, H-alpha only from ionizing OB stars younger than roughly 10 Myr, so the FUV/H-alpha ratio per segment sorts regions into recent star formation (both bands), older star formation (FUV only), and non-stellar ionization (H-alpha only). A phase-space diagram of cluster radius versus line-of-sight velocity places the galaxies' stripping stages into infall histories.

What would settle it

Take deep FUV imaging of JO147's tail that reaches below the FUV flux expected from its measured H-alpha flux, and measure dust attenuation in the tail (for example with a Balmer-decrement map or infrared emission). If FUV knots appear once extinction is accounted for, the claim that unresolved tail H-alpha comes from processes other than star formation would be falsified.

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Extended reading notes

Core claim

The central claim is that direct far-ultraviolet imaging separates true ongoing star formation from other sources of ionized-gas emission in ram-pressure-stripped galaxies. FUV traces stellar photospheres with lifetimes under about 200 Myr, while H-$\alpha$ traces photoionization by OB stars younger than about 10 Myr; where the two coincide in the same knot-like segments, recent star formation is the cause. Across 500 segments detected in both bands (330 in discs, 170 in tails), the paper measures a tight relation $\log_{10}\mathrm{H\alpha_{fd}} = (1.12\pm0.03)\,\log_{10}\mathrm{FUV_{fd}} + (3.45\pm0.62)$, with tail-only segments showing a steeper slope ($0.81\pm0.06$). In JO147 and five other galaxies, unresolved H-$\alpha$ tail emission has no FUV counterpart even where the expected FUV flux lies above the detection limit, so the paper concludes those tails are not powered by young stars but by processes such as thermal conduction of the hot intracluster medium. In two truncated-disc galaxies (JO36 and JO23), FUV emission is confined to a smaller central region than the H-$\alpha$, interpreted as outside-in quenching after a cluster crossing.

Load-bearing premise

The H-alpha-only tails are interpreted as non-star-forming because no FUV is seen there, and this assumes that dust extinction and older stellar populations do not suppress the FUV below detection in those tail regions, since no attenuation correction is applied.

Editorial extensions

If this is right

  • Seven strong and extreme stripping galaxies host clumpy FUV-bright knots in their tails, meaning star formation is genuinely occurring outside the disc in the stripped gas, with ages under about 10 Myr.
  • Unresolved H-alpha tails without FUV, seen in JO147 and five other galaxies, are likely heated by mechanisms other than star formation, most plausibly thermal conduction at the interface with the hot intracluster medium.
  • In truncated-disc galaxies, FUV emission covers a smaller area than H-alpha, providing direct evidence that star formation shuts down from the outside in as stripping progresses.
  • The empirical FUV-H-alpha flux-density relation lets observers estimate one tracer from the other in ram-pressure-stripped galaxies, as long as star formation has occurred within the last 10 Myr.
  • Phase-space positions indicate strong and extreme strippers are likely recent infalls, while truncated-disc galaxies have probably completed a cluster crossing.

Reading between the lines

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

  • Beyond the paper, H-alpha-only tails could be used as a spatial map of where the hot intracluster medium is physically interacting with stripped cold gas, since thermal conduction would be strongest at that boundary.
  • Beyond the paper, the sharp FUV-versus-H-alpha truncation in discs could serve as a clock for when stripping removed the outer gas: H-alpha fades after about 10 Myr while FUV persists to about 200 Myr, so comparing the two edge locations dates the event.
  • Beyond the paper, the steeper FUV-H-alpha slope in tail segments compared to disc segments suggests stripped-tail star formation may have a different recent history or initial-mass-function sampling; resolved stellar populations in one or two bright tail knots could test this directly.
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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 / 6 minor

Summary. Using UVIT FUV imaging and MUSE Hα maps for 13 GASP ram-pressure-stripped galaxies, the paper identifies Hα- and FUV-selected segments in the discs and tails, derives empirical FUV–Hα flux-density relations, and compares the FUV/Hα morphology with BPT emission-line classifications. It reports that seven strong and extreme strippers show clumpy tail star formation with good FUV–Hα correspondence, six show minimal tail FUV with unresolved Hα, and two have truncated discs. The most novel claim is that JO147's unresolved Hα tail is not powered by young stars: applying a tail-specific FUV–Hα relation predicts FUV flux densities above the UVIT detection limit, so the non-detection is argued to reflect thermal conduction or another non-star-formation process. The paper also places the sample in a cluster phase-space diagram and interprets the results as outside-in quenching for truncated-disc galaxies.

Significance. If the main conclusions hold, this is a valuable observational contribution: it significantly expands the sample of GASP galaxies with matched FUV/Hα segment photometry, provides a quantitative FUV–Hα relation for stripped tails, and offers a concrete, falsifiable test of whether unresolved Hα tails can be powered by processes other than star formation. The paper is explicit about its segmentation method, detection limits, and the lack of attenuation correction, and the descriptive morphological comparisons are supported by the presented maps. The JO147 inference, however, rests on two unverified premises—negligible dust attenuation and the extrapolation of a relation fitted to segments detected in both bands—so the paper's headline novelty depends on analysis that is not yet fully demonstrated. The FUV–Hα correspondence for the seven strong and extreme strippers is a solid descriptive result that is not affected by these concerns.

major comments (3)
  1. [§3.2.3, Eq. (1), Table 3] The predicted FUV flux densities for JO147 (3×10−20 and 7.6×10−22 erg s−1 cm−2 Å−1 kpc−2) are obtained by inverting the tail relation from Table 3, which is calibrated only on segments detected in both Hα and FUV. The 29 Hα-only tail segments in JO147 are by construction below the FUV detection limit and are not represented in the calibration sample, so this is an extrapolation. In addition, the relation is fitted to the same 13 galaxies, including four JO147 tail segments with both Hα and FUV detections; the influence of those segments is not quantified. The paper does not propagate the slope/intercept uncertainties or the intrinsic scatter into the predicted FUV values. Please quote the predictions with their uncertainties, report the scatter of the relation, and consider testing the prediction with the existing MUSE Balmer-decrement data rather than relying on the relation alone.
  2. [§3.2.3, Appendix A.0.8] The inference that JO147's missing FUV is not due to extinction relies on the assertion that diffuse Hα morphology implies significant dust is unlikely, but this is not demonstrated. JO147 is viewed at inclination 81.6° (Appendix A.0.8), and the paper's own cited median A_V = 0.5 mag for GASP tail clumps would attenuate FUV by roughly 1–2 mag (a factor of roughly 2–6 for typical extinction curves), comparable to or larger than the factor-of-3 difference between the shallowest and deepest limiting fluxes shown in Fig. 2. Under A_V ≈ 0.5, the highest predicted FUV flux density falls close to or below the detection threshold, making the non-detection consistent with dust-obscured recent star formation. The authors should use the MUSE Balmer decrement in the JO147 tail to measure, or place upper limits on, E(B−V) rather than assuming it is negligible.
  3. [§3.1, Table 3, Summary] The reported best-fit relation changes slope from 1.12 ± 0.03 for all Hα-selected segments to 0.83 ± 0.06 for all FUV-selected segments, and the tail slope (0.81) is shallower than the disc slope (1.06) in both selections. This large sensitivity to the detection image is not discussed, so Eq. (1) is not established as a unique 'global relation'. Moreover, the text and the Summary state that the correlation becomes steeper for tail segments, which is contradicted by Table 3, where the tail slope is the shallowest. Please clarify the selection effects, report the intrinsic scatter, justify the choice of regression direction for prediction, and correct the contradiction between the text and Table 3.
minor comments (6)
  1. [Abstract, Introduction] Please fix typographical errors such as 'Hαimaging' in the Abstract and 'clues to the, star formation nature' in the Introduction.
  2. [Fig. 2, Eq. (1)] The axis labels and units in Fig. 2 are difficult to read (missing superscripts and nonstandard spacing), and the variables in Eq. (1) are not formally defined; please state explicitly that Hα_fd and FUV_fd are in erg s−1 cm−2 Å−1 kpc−2.
  3. [Table 2] The column headers in Table 2 are cryptic (for example, NHαHαdisc and NFUV Hαtail); consider splitting into two tables or adding a clear legend explaining each column.
  4. [§2.1] The software package is referred to as 'SW ARP'; the correct name is SWarp.
  5. [§3.2.3] When stating that 29 Hα-only tail segments exist for JO147, please refer explicitly to Table 2 (33 Hα-tail segments minus 4 with FUV detections) to make the arithmetic transparent.
  6. [Appendix A] The appendix subsection numbering (A.0.1, A.0.2, etc.) is nonstandard; use A.1, A.2, ... for consistency with journal style.

Circularity Check

0 steps flagged · score 2.0 of 10

No significant circularity: FUV–Hα comparison is direct; the JO147 expected-FUV estimate is a calibrated extrapolation, not a fitted input renamed as prediction.

full rationale

The paper's central observational claims—that FUV and Hα flux densities correlate in detected segments, that seven galaxies show FUV in their tails, and that six show little or no tail FUV—are direct measurements compared at fixed segmentation apertures. No derived quantity is defined in terms of the conclusion it supports, and no equation reduces to its input by construction. The JO147 argument uses Eq. 1 to estimate the FUV flux expected from the Hα-only tail segments. Eq. 1 is an empirical regression on the 500 segments with both FUV and Hα detections, while the 29 Hα-only JO147 segments used for the prediction are not in the fit, so the predicted FUV is an extrapolation rather than a statistically forced reproduction of the fitted data. The inference that the missing FUV implies non-star-formation mechanisms therefore rests on the stated assumptions that the calibration applies to the diffuse tail gas and that dust attenuation is negligible—assumptions the paper explicitly acknowledges (Sec. 3.2.3 and Sec. 4: 'we have assumed they are negligible when comparing Hα with FUV flux along these tails'). That is a robustness limitation, not a circular reduction. Self-citations to GASP data products (Poggianti et al. 2025 for JTypes, Poggianti et al. 2019b for median A_V) are used as observational inputs and caveats, not as proofs of the paper's conclusions, so they do not make the derivation circular. Overall, the analysis is self-contained against the imaging data; the JO147 conclusion is conditional on an unverified extrapolation, but the derivation chain does not collapse into its own inputs.

Assumptions & free parameters 4 free parameters · 5 assumptions · 0 invented entities

The paper's central quantitative objects are direct measurements. The fitted FUV-H-alpha relation (Eq.1 and Table 3) is the main added free parameter, used for the JO147 extrapolation. No new physical entities are introduced. The main domain assumptions are standard stellar-population diagnostics and the unpublished JType classification from the same collaboration.

free parameters (4)
  • FUV-Halpha flux density relation slope (Eq.1, all segments) = 1.12 +/- 0.03
    Linear regression fit to segment flux densities of 13 galaxies; presented as a predictive relation.
  • FUV-Halpha flux density relation intercept (Eq.1, all segments) = 3.45 +/- 0.62
    Intercept of the same empirical fit.
  • Tail-specific slope (Table 3) = 0.81 +/- 0.06
    Used to predict expected FUV for JO147 H-alpha-only tail segments.
  • Tail-specific intercept (Table 3) = -3.10 +/- 1.34
    Used with the tail slope for the JO147 expectation.
assumptions (5)
  • domain assumption H-alpha traces star formation younger than about 10 Myr and FUV traces stars younger than about 200 Myr, so the FUV-H-alpha ratio separates these age regimes.
    Section 2.1 and 3.1. Standard interpretation adopted from Kennicutt and Evans 2012, but stochasticity and IMF variations are acknowledged.
  • domain assumption MUSE continuum isophotes delineate the galaxy main body from the tail.
    Section 2.1 and Gullieuszik et al. 2020; projection effects can misclassify tail segments as disc, noted in the text.
  • ad hoc to paper Dust attenuation is negligible when comparing FUV and H-alpha along stripped tails.
    Section 4: 'we have assumed they are negligible when comparing Halpha with FUV flux along these tails'; no extinction correction is applied, though median A_V=0.5 mag for star-forming clumps is cited.
  • domain assumption The JType classification of Poggianti et al. 2025 (submitted) correctly orders stripping stages.
    Section 2.1; the sample is divided into strong, extreme, and truncated based on this unpublished scheme.
  • domain assumption Unresolved H-alpha without FUV, when expected FUV is above the detection limit, can be attributed to non-star-formation processes such as thermal conduction.
    Sections 3.2.3 and 4; this is the interpretive framework for JO147 and the six low-FUV galaxies.

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Cite this review

Pith. "Pith review of Star formation at different stages of ram-pressure stripping as observed through far-ultraviolet imaging of 13 GASP galaxies." pith.science (2026). https://pith.science/paper/MIBL5SXI

@misc{pith2026250515066,
  author       = {Pith},
  title        = {Pith review of: Star formation at different stages of ram-pressure stripping as observed through far-ultraviolet imaging of 13 GASP galaxies},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/MIBL5SXI}},
  note         = {Machine review of arXiv:2505.15066}
}
abstract

Galaxies undergoing ram-pressure stripping develop gaseous tails that can extend several kiloparsecs outside the galaxy disc. We used far-ultraviolet and H$\alpha$ imaging from the GASP survey to investigate how different stages of stripping affect star formation properties in the tail and disc of 13 galaxies undergoing stripping. These galaxies have different stripping strengths, as identified from the MUSE integral field spectroscopy. The star-forming knots in the disc and tails show a good correspondence between the measured FUV and H$\alpha$ flux. This is especially true for strong and extreme cases of stripping, which have developed extended ionized gaseous tails featuring clumpy structures. The mechanism behind the H$\alpha$ emission on the tails of these regions, which correlates well with FUV emission, is photoionization caused by young massive stars. The optical emission line ratio maps enable us to understand the emission mechanism, which can be attributed to star formation, LINER activity, or a combination of both phenomena and AGN. The star-forming regions in the emission line maps correspond well to the areas with significant FUV flux in these galaxies. Six galaxies exhibit minimal star formation in their tails, with two cases star formation is limited to the central regions and their discs are truncated. In galaxies with truncated discs, star formation is confined to a smaller region on the disc, as indicated by the FUV flux, compared to H$\alpha$. Galaxies with strong stripping are undergoing recent star formation and are likely recent infalls. Galaxies with truncated discs confine star formation to the center, likely because they have completed a cluster crossing that depleted most of their outer gaseous disc. Galaxies with minimal FUV flux along their tails exhibit unresolved H$\alpha$ emission which may be attributed to processes other than star formation.

Figures

Figures reproduced from arXiv: 2505.15066 by the authors.

Figure 1
Figure 1. Segmentation map for galaxies created from ProFound run over FUV images. The ratio of FUV and H [PITH_FULL_IMAGE:figures/full_fig_p006_1.png] view at source ↗
Figure 2
Figure 2. Far-ultraviolet flux density of the segments detected for [PITH_FULL_IMAGE:figures/full_fig_p007_2.png] view at source ↗
Figure 3
Figure 3. Colour composite image of galaxies created by combining the FUV image from UVIT with optical B,V imaging from the [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figures from the paper (2 more)
Figure 4
Figure 4. Figure 4: Far-ultraviolet, Hα flux image, and emission line diagnostic map of galaxies. The Hα flux contours in white colour are overlaid over FUV and Hα images. The green line defines the galaxy’s main body. Regions covered due to emission from LINER, composite (AGN+SF) and sta…
Figure 5
Figure 5. Figure 5: Phase space diagram for 11 jellyfish galaxies is shown [PITH_FULL_IMAGE:figures/full_fig_p009_5.png]

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. The MUSE view of ram pressure stripped galaxies in clusters: the GASP sample

    astro-ph.GA 2025-05 conditional novelty 6.0 of 10

    89% of optically selected ram-pressure stripping candidates in 39 clusters are confirmed with MUSE integral-field spectroscopy, and a ring of [OI] emission is found at galaxy disk edges.

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    " write newline "" before.all 'output.state := FUNCTION n.dashify 't := "" t empty not t #1 #1 substring "-" = t #1 #2 substring "--" = not "--" * t #2 global.max substring 't := t #1 #1 substring "-" = "-" * t #2 global.max substring 't := while if t #1 #1 substring * t #2 gl...

Pith tools

Reviewed August 7, 2026 · model on record in the stance chip above.