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REVIEW 2 major objections 6 minor 89 references

The central spectra of massive star-forming galaxies

T0 review · 2 major / 6 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read Most very massive star-forming galaxies are LINERs

desk verdict A careful measurement of a genuinely new population-level LINER fraction, but the headline 79-83% rests on a 47% spectral sub-sample whose representativeness is not checked on the classification axis. read the letter →

arxiv 2506.08474 v1 pith:4YNGV35U submitted 2025-06-10 astro-ph.GA

Jaimie R. Sheil , Michael J. I .Brown , Virginia A. Kilborn , Michelle E. Cluver , Thomas Jarrett This is my paper
classification astro-ph.GA
keywords LINERgalaxiesmassivestar-formingBPTdiagramemission-lineclassificationsuperspiralgalaxybimodalitynuclearspectraWISEphotometry
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 asks whether the rare galaxies that are both very massive and still forming stars have unusual nuclear spectra. Using archival optical spectra for 59 of 126 nearby galaxies with stellar masses above $10^{11}$.3 solar masses and star formation rates above 1 solar mass per year, the authors measure the standard diagnostic emission lines and classify each nucleus. They find 79±6% of the galaxies with spectra are LINERs by the [NII]/H-$\alpha$ ratio alone, and 83±6% of the 35 galaxies with all four lines measured are LINERs on a BPT diagram, compared with roughly 30% for the general massive-galaxy population. The paper argues this over-abundance connects LINER emission to the presence of gas that also fuels star formation.

What carries the argument

The carrier of the argument is the BPT emission-line diagnostic diagram, using the ratios [NII] λ6583 / Hα and [OIII] λ5008 / Hβ with the Kauffmann et al. criteria ([NII]/Hα > 0.6 and [OIII]/Hβ < 3 for LINERs). Classification by the single ratio [NII]/Hα is used when the blue lines are too noisy. Before measuring fluxes, the spectra are continuum-subtracted using an 11 Gyr, Z=0.008 Bruzual & Charlot simple stellar population model, because under-subtracting Hα absorption inflates the LINER fraction. The machinery also includes a signal-to-noise threshold of 3 per line and simultaneous multi-Gaussian fitting of Hα with the two [NII] lines.

What would settle it

Obtain homogeneous nuclear spectra for all 126 galaxies in the parent sample (or a randomly selected subset) and re-measure the LINER fraction; if the 67 galaxies currently missing spectra are mostly non-LINERs, the 79-83% figure would fall toward the ~30% baseline. Alternatively, spatially resolved IFU observations showing that the LINER emission is decoupled from the star-forming gas would weaken the proposed link.

Watch

Extended reading notes

Core claim

The paper's central claim is that very massive star-forming galaxies in the local universe are predominantly LINERs (low-ionisation nuclear emission-line regions). A sample of 126 galaxies with $10^{11}$.3 <= M_stellar <= $10^{11}$.7 Msun, SFR between 1 and 13 Msun/yr, and distances under 100 Mpc was drawn from the 2MRS-Bright WXSC catalogue; 59 have archival spectra, and after subtracting stellar continuum models and fitting Gaussians, emission-line ratios were used to classify the nuclei. Using the Kauffmann et al. criterion [NII]6583/H-$\alpha$ > 0.6, 79±6% (46 galaxies) are LINERs, and among the 35 galaxies with all four lines measured, 83±6% (29) fall in the LINER region of the BPT diagram. The same measurement on the higher-redshift Ogle et al. super-spiral sample gives 64% LINERs, well above the ~30% baseline for massive galaxies. The authors conclude that LINER emission in massive galaxies may be linked to the gas that fuels star formation.

Load-bearing premise

The central claim assumes that the 59 galaxies with archival spectra are representative of the full 126-galaxy sample in nuclear emission, even though spectra come from surveys with different selection functions, one of which was partly designed to find active nuclei.

Editorial extensions

If this is right

  • If the central claim holds, most very massive galaxies that still form stars have LINER-type nuclei, so LINERs are the rule rather than the exception in this rare population.
  • The ~30% LINER fraction in the general massive-galaxy population cannot be explained by mass alone; active star formation or the gas associated with it must be a major factor.
  • The local sample and the higher-redshift Ogle et al. super-spiral sample both show high LINER fractions, indicating the connection persists over at least 1-3 Gyr of cosmic time.
  • Future IFU spectroscopy of these galaxies can test whether the LINER ionisation traces star-forming gas or a central low-luminosity AGN.
  • The near-absence of passive nuclei (at most ~9%) implies that gas supply, not morphological type, is the key condition for LINER emission in massive galaxies.

Reading between the lines

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

  • If spectra availability is biased toward active nuclei—for instance, the Ho et al. sample was partly selected for nuclear activity—the true population fraction could be lower than 79-83%; measuring the 67 galaxies without archival spectra would settle this.
  • A natural extension is to map the spatial distribution of LINER emission with integral-field units; if LINER emission is co-located with star-forming regions, it would support ionisation by evolved stars or shocks rather than a central AGN.
  • The selection of galaxies above 10^11.3 Msun with SFR > 1 Msun/yr may effectively select a particular gas reservoir state; analogous samples at lower mass could test whether the LINER link is specific to the most massive galaxies.
  • If the connection is causal, LINER classification could serve as a cheap proxy for the presence of cool gas in massive galaxies when other gas tracers are unavailable.
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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

2 major / 6 minor

Summary. The paper selects 126 very massive (M* >= 10^11.3 Msun) star-forming (SFR > 1 Msun/yr) galaxies within 100 Mpc from the 2MRS-Bright WXSC catalogue, and obtains archival optical spectra for 59 of them (47%). After subtracting a fixed Bruzual & Charlot (2003) stellar population model and fitting Gaussians to [NII], Halpha, Hbeta, and [OIII], the authors classify galaxies using the Kauffmann et al. (2003b) BPT criterion ([NII]/Halpha > 0.6, [OIII]/Hbeta < 3). They report that 83 +/- 6% of the 35 galaxies with complete BPT measurements and 79 +/- 6% of the 59 galaxies with spectra are LINERs, compared with ~30% in the general massive galaxy population, and they find 64% LINERs in a re-analysis of the Ogle et al. (2019) super-spiral sample. The paper interprets the high LINER fraction as evidence that LINER emission in massive galaxies is linked to the presence of gas fuelling star formation.

Significance. If the population-level inference is valid, the paper demonstrates a strong, systematic connection between ongoing star formation and low-ionization nuclear emission in very massive galaxies, with implications for our understanding of LINERs and AGN activity in this mass regime. The manuscript has several strengths: the sample selection is clearly defined, the spectral reduction and classification pipeline is described in detail, continuum-subtraction sensitivity tests are presented, the authors re-analyse a comparison sample with the same code, and the full data table is promised as supplementary material. The main weakness is the treatment of the selection function of the archival spectra, which is the load-bearing assumption for extending the measured LINER fraction from the spectral sub-sample to the full parent sample.

major comments (2)
  1. [§3, §4] The manuscript's central quantitative claim, that the vast majority of massive star-forming galaxies are LINERs, rests on extrapolating from 59 galaxies with archival spectra (47% of the parent sample) and 35 galaxies with complete BPT measurements (28%) to the full 126-galaxy sample. The paper correctly notes that the spectral sub-sample is representative in mass, SFR, redshift, and morphology, but these axes do not guarantee representativeness in the property that matters for the headline: the nuclear emission-line classification. Six of the 59 spectra originate from Ho et al. (1995), a survey the paper itself describes as 'designed to gather spectra for bright, local galaxies that were thought to host AGNs' (§3), i.e., selected on the very property being counted. If the 67 missing galaxies are preferentially star-forming (with [NII]/Halpha < 0.6) or passive (with no measurable lines), the population fraction could be substantially lower than 79-83%. I request either a quantitative sensitivity analysis (e.g., showing how the inferred population fraction changes under different assumptions about the missing galaxies) or a reframing of the headline claim as a measurement on the spectral sub-sample, with the selection caveat stated prominently.
  2. [§3.1, §4] The 17 galaxies classified as LINERs using [NII]/Halpha alone, without a detected (or with an upper-limit) Halpha or [OIII]/Hbeta, are not explicitly shown to be inconsistent with Seyfert classification. The Kauffmann criterion [NII]/Halpha > 0.6 places a galaxy above the Kewley et al. (2006) separator, but the separation between LINERs and Seyferts requires [OIII]/Hbeta < 3, which is unavailable for these 17. The Discussion asserts that these galaxies are 'genuinely LINERs' based on narrow line widths and two literature classifications, but narrow line widths do not exclude Seyfert 2 galaxies. Please provide a quantitative estimate of the possible Seyfert contamination (e.g., using the observed 1/35 Seyfert fraction in the BPT sub-sample as a prior) or explicitly treat the ratio-only classification as a separate statistic with this caveat.
minor comments (6)
  1. [Abstract] The phrase '83 +/- 6% of our galaxies, with sufficient signal-to-noise to measure all 4 emission lines' is ambiguous; please state the denominator explicitly (35 of the 126-galaxy sample) to avoid the impression that the fraction applies to the full sample.
  2. [§2] The selection criteria are stated as '1 < SFR <= 13 Msun/yr', but Mrk 1239 is retained with SFR12um = 37 Msun/yr; please state explicitly in Section 2 that this is an exception justified by suspected AGN contamination, and check the sensitivity of the results to its inclusion.
  3. [§3] The sentence 'as such we expect the results from the sub-sample to be true for the whole sample as well' would be more rigorous if supported by a formal two-sample test (e.g., a KS test on mass, SFR, redshift, morphology) or explicitly marked as an assumption.
  4. [§5] There is a typo: 'it’s the strong, central radio source' should be 'its the strong, central radio source'.
  5. [§5] The text contains an unclosed bracket: 'NII]λ6583' should be '[NII]λ6583'.
  6. [Figure 7] The BPT diagram would be clearer if the LINER and Seyfert regions were labelled directly on the figure, rather than only in the caption.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the LINER fraction is measured from archival spectra with fixed literature cuts, and the sample-selection calibrations from the authors' prior work do not encode the spectral classification.

full rationale

The derivation chain is self-contained with respect to the headline claim. The 126-galaxy parent sample is selected using WISE-based stellar mass and star-formation-rate calibrations from Cluver et al. (2014, 2017) and the 2MRS-Bright WXSC catalogue (Jarrett et al., 2019/in prep); these calibrations are independent photometric relations and do not contain any information about line ratios or LINER status. The spectral classification is performed on archival SDSS, 6dFGS, 2MRS FAST, and Ho et al. (1995) spectra, with continuum subtraction and Gaussian fitting described in Section 3.1, and LINER classification is assigned using fixed external literature cuts: [NII]lambda6583/Halpha > 0.6 from Kauffmann et al. (2003b) and the Kewley et al. (2006) and Schawinski et al. (2007) BPT boundaries. The reported 83 +/- 6% and 79 +/- 6% LINER fractions are simple proportions of measured classifications, not fitted parameters, and no quantity used to define the sample is defined in terms of the LINER classification. The authors' self-citations to Cluver et al. and Jarrett et al. are used for mass, SFR, and morphological data, not for the spectral classification, so they are not load-bearing for the central result. The concern that the 59-galaxy spectral subsample may be unrepresentative because Ho et al. (1995) was activity-selected is a selection-bias or statistical-inference issue, not circularity: it does not make the measured fraction equivalent to an input by construction. The comparison to Ogle et al. (2019) provides an external, independent check. No step in the paper reduces to its own input, and no self-citation chain forces the conclusion.

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

The paper introduces no new entities. Its central fraction depends on three borrowed or assumed ingredients: WISE mass and SFR calibrations, a fixed old-population continuum model, and the representativeness of the 59-galaxy spectral subsample. These are enumerated above; none is a new mechanism, particle, or conserved quantity.

free parameters (4)
  • W1-W2 stellar mass-to-light calibration (Cluver et al. 2014) = log(M/L) = -2.54(W1-W2) - 0.17
    Borrowed from prior work and used to define the M*>10^11.3 Msun selection; a systematic offset changes which galaxies enter the sample.
  • 12 micron SFR calibration (Cluver et al. 2017) = log SFR = 0.889 log L12 - 7.76
    Borrowed from prior work and used to require SFR > 1 Msun/yr; if AGN-heated dust inflates L12, the sample is biased toward active nuclei.
  • BC03 simple stellar population model age and metallicity = age = 11 Gyr, Z = 0.008
    Chosen by hand to represent old bulges; directly sets H-alpha absorption in-fill and therefore the [NII]/H-alpha ratios used for LINER classification.
  • Signal-to-noise threshold for emission-line measurement = S/N > 3 (MAD-based)
    Determines which galaxies enter the BPT subsample; a different threshold changes the subsample and the 83% figure.
assumptions (5)
  • domain assumption WISE W1-W2 colours of the sample are not significantly contaminated by AGN hot dust, so WISE mass and SFR estimates are not inflated.
    Invoked in Section 2 and Figure 3; justifies excluding AGN contamination except for Mrk 1239.
  • domain assumption A single 11 Gyr, Z=0.008 Bruzual and Charlot SSP is an adequate stellar continuum model for all 59 spectra after scaling and tilt correction.
    Section 3.1; determines H-alpha in-fill and hence line ratios; the authors tested other ages and metallicities.
  • domain assumption The Kauffmann, Kewley, and Schawinski BPT criteria separate star-forming galaxies, LINERs, and Seyferts as claimed.
    Section 3 and Figure 2; the classification labels depend on these literature diagnostics being valid for this mass and SFR regime.
  • domain assumption The 59 galaxies with archival spectra are representative of the 126-galaxy sample in the property being measured, nuclear emission.
    Section 3; checked for mass, SFR, redshift, and morphology, but not for spectral class, and Ho et al. spectra are partly selected for activity.
  • domain assumption The three-Gaussian [NII]/H-alpha fit with fixed 2.95 ratio and common width recovers true line fluxes in low-resolution heterogeneous spectra.
    Section 3.1; if the fixed line-ratio prior is wrong, measured [NII]/H-alpha values are biased.

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Pith. "Pith review of The central spectra of massive star-forming galaxies." pith.science (2026). https://pith.science/paper/4YNGV35U

@misc{pith2026250608474,
  author       = {Pith},
  title        = {Pith review of: The central spectra of massive star-forming galaxies},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/4YNGV35U}},
  note         = {Machine review of arXiv:2506.08474}
}
abstract

We have examined the nuclear spectra of very massive star-forming galaxies at $z \sim 0$ to understand how they differ from other galaxies with comparable masses, which are typically passive. We selected a sample of 126 nearby massive star-forming galaxies ($<100~{\rm Mpc}$, $10^{11.3}~\rm{M_\odot} \leq M_{\rm stellar} \leq 10^{11.7}~\rm{M_\odot}$, $1 ~{\rm M_\odot~yr^{-1}}< {\rm SFR} <13 ~{\rm M_\odot~yr^{-1}}$) from the 2MRS-Bright WXSC catalogue. LEDA morphologies indicate at least 63\% of our galaxies are spirals, while visual inspection of Dark Energy Survey images reveals 75\% of our galaxies to be spirals with the remainder being lenticular. Of our sample 59 have archival nuclear spectra, which we have modelled and subsequently measured emission lines ([NII]$\rm{\lambda 6583}$, H$\alpha\rm{\lambda 6563}$, [OIII]$\rm{\lambda 5008}$, and H$\beta\rm{\lambda 4863}$), classifying galaxies as star-forming, LINERS, or AGNs. Using a BPT diagram we find $83 \pm 6$ \% of our galaxies, with sufficient signal-to-noise to measure all 4 emission lines, to be LINERs. Using the [NII]$\rm{\lambda 6583}$/H$\alpha\rm{\lambda 6563}$ emission line ratio alone we find that $79 \pm 6$ \% of the galaxies (46 galaxies) with archival spectra are LINERs, whereas just $\sim 30\%$ of the overall massive galaxy population are LINERs (Belfiore et al. 2016). Our sample can be considered a local analogue of the Ogle et al. (2016, 2019) sample of $z \sim 0.22$ massive star-forming galaxies in terms of selection criteria, and we find 64\% of their galaxies are LINERs using SDSS spectra. The high frequency of LINER emission in these massive star-forming galaxies indicates that LINER emission in massive galaxies may be linked to the presence of gas that fuels star formation.

Figures

Figures reproduced from arXiv: 2506.08474 by the authors.

Figure 1
Figure 1. The SDSS spectrum of the super spiral 2MASX J07404205+4332412, which was identified by Ogle et al. (2016, 2019). The redshifted Hαλ6563 and [NII]λ6583 are evident and are comparable in strength, which identifies this galaxy as a LINER. provide insights into quenching, and is a motivation for this work. The Ogle et al. (2016, 2019) super spiral galaxies have higher star formation rates (SFR), ranging from 1−30 M⊙ yr−… view at source ↗
Figure 2
Figure 2. Our BPT diagram of 6dF galaxies along with com￾monly used galaxy classification criteria from the literature (Bald￾win et al., 1981). The green line from Kewley et al. (2006) sep￾arates star-forming galaxies from Seyferts and LINERs, while the black dotted line from Schawinski et al. (2007) separates Seyferts and LINERs. The Kauffmann criteria shows alternative cuts to classify galaxies with and the emission line ra… view at source ↗
Figure 3
Figure 3. The WISE colour-colour diagram for all 2MRS-Bright galaxies (grey) and for our local, massive, star-forming sample of galaxies (coloured). Our sample lies in the spiral region of the W1-W2 against W2-W3 plot, which reflects that these galaxies have some star-formation present, as we selected for. We do not have an AGN locus for this plot currently as it is part of the ongoing work by Jarrett et al. in prep. There is… view at source ↗
Figures from the paper (9 more)
Figure 4
Figure 4. Figure 4: As there is no infrared excess in Figure 3 [PITH_FULL_IMAGE:figures/full_fig_p005_4.png]
Figure 4
Figure 4. Figure 4: The sample for this paper consists of 126 galaxies with Mstellar ≥ 1011.3 M⊙, SFR > 1 M⊙ yr−1 , and distance < 100 Mpc (red), selected from the 2MRS-Bright < 100 Mpc sample (purple). The region the sample space populates against the wider selection of galaxies can be s…
Figure 5
Figure 5. Figure 5: An example of the corrections and fits applied to archival spectra of galaxies in our local sample. The top panel, shows the original spectra in red, at wavelengths surrounding the redshifted emission lines Hαλ6563 and [NII]λ6583. The Bruzual & Charlot (2003) model is …
Figure 6
Figure 6. Figure 6: The corrections and fits applied to archival spectra for Hβλ4863 and [OIII]λ5008 emission lines. The top panel, shows the original spectra in green, the scaled Bruzual & Charlot (2003) is shown in black and the subtracted spectra is shown in purple. The corrected spect…
Figure 8
Figure 8. Figure 8: Our sample of galaxies against the wider galaxy popu￾lation with our local sample divided into those with and without spectra and then further into those with that are LINERs. The LINERs clearly make up the majority of those galaxies with spec￾tra. The SFMS by Whitaker…
Figure 9
Figure 9. Figure 9: shows the histogram of the emission line ra￾tios broken down by the origin of the spectra. This reveals that the classification of LINER or star-forming is not strongly dependent on the source of the spec￾tra. It also shows that the sample as a whole has very high valu…
Figure 10
Figure 10. Figure 10: The available Dark Energy Survey (DES) images of galaxies in our sample with LEDA morphologies sourced by Jarrett et al, in prep. As can be seen these galaxies are largely disc galaxies with spiral structure and do not show signs of major mergers. The galaxy in the fi…
Figure 11
Figure 11. Figure 11: A representative selection of the heterogeneous spectra from our sample of LINERs, comprised primarily of spectra from 6dFGS (Jones et al., 2006; Jones et al., 2009), as well as additional spectra from SDSS (Alam et al., 2015), 2MRS Fast Survey (Huchra et al., 2012) a…
Figure 12
Figure 12. Figure 12: A representative selection of the stellar population subtracted spectra from our sample of LINERs, comprised primarily of spectra from 6dFGS (Jones et al., 2006; Jones et al., 2009), as well as additional spectra from SDSS (Alam et al., 2015), 2MRS Fast Survey (Huchra…

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    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.stat...

Pith tools

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