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arxiv: 2605.08979 · v1 · submitted 2026-05-09 · 🌌 astro-ph.GA

Recognition: 2 theorem links

· Lean Theorem

The MaNGA Low-mass disks HUnt for CO (MaLHUCO) Survey

M. Grossi , E. Corbelli , D. R. Gon\c{c}alves , E. D. Paspaliaris
Authors on Pith no claims yet

Pith reviewed 2026-05-12 02:23 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords low-mass galaxiesmolecular gasKennicutt-Schmidt lawCO observationsstar formation rategas depletion timeMaNGA surveyinterstellar medium
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The pith

The Kennicutt-Schmidt law between molecular gas mass and star formation rate remains linear down to low stellar masses.

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

This paper reports CO(2-1) observations of 42 low-mass, late-type disk galaxies selected from the MaNGA survey to probe star formation in the M33-like stellar mass regime. It shows that the molecular gas mass versus star formation rate relation stays linear at these lower masses, just as it does in more massive galaxies. The 12 micron luminosity correlates tightly with the CO emission and therefore serves as a reliable global tracer of molecular gas. Low-mass systems also exhibit modestly shorter molecular gas depletion times, consistent with their elevated specific star formation rates, while the atomic-to-molecular gas transition strengthens with rising stellar mass.

Core claim

The molecular gas mass - star formation rate relation remains linear down to low stellar masses. Mean molecular gas depletion time is slightly shorter in low-mass late-type galaxies than in more massive systems. The 12 μm luminosity exhibits a tight linear correlation with CO line emission and therefore provides a robust tracer of global molecular gas content. The HI-to-stellar mass ratio decreases with stellar mass while the molecular fraction increases, marking the shift toward molecular-dominated interstellar medium.

What carries the argument

The Kennicutt-Schmidt law tested on H2 masses derived from CO(2-1) detections using both constant Galactic and metallicity-dependent CO-to-H2 conversion factors in a sample of 42 low-mass Scd or later disk galaxies.

If this is right

  • The basic efficiency with which molecular gas turns into stars does not change across a wide range of galaxy stellar masses.
  • Low-mass disks convert their molecular reservoirs into stars on shorter average timescales than massive disks.
  • The interstellar medium shifts from atomic-dominated to molecular-dominated as stellar mass grows along the galaxy sequence.
  • 12 μm luminosity can serve as a practical proxy for total molecular gas mass in low-mass star-forming disks.

Where Pith is reading between the lines

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

  • If the linear relation holds, galaxy evolution models can apply the same molecular-gas-based star formation prescription to both low-mass and high-mass systems without mass-dependent adjustments.
  • The assumption that metallicity-dependent conversion factors suffice could be tested by comparing CO-based masses against dust-based or gamma-ray-based H2 estimates in the same low-mass objects.
  • Extending similar CO mapping to still lower stellar masses or to galaxies with lower metallicities would show whether the relation eventually breaks.

Load-bearing premise

The CO-to-H2 conversion factor, whether held constant or made metallicity-dependent, accurately recovers the true molecular gas mass and the 42-galaxy sample represents the broader low-mass late-type disk population.

What would settle it

A statistically significant departure from linearity in the molecular gas mass versus star formation rate relation when measured in an independent, larger sample of low-mass galaxies, or direct H2 masses from dust emission or other tracers that systematically disagree with the CO-derived values.

Figures

Figures reproduced from arXiv: 2605.08979 by D. R. Gon\c{c}alves, E. Corbelli, E. D. Paspaliaris, M. Grossi.

Figure 1
Figure 1. Figure 1: Examples of MaLHUCO galaxies. Combined 𝑔𝑟𝑖 SDSS images with the MaNGA hexagonal field of view overlaid (32′′ diameter, top row), and the corresponding Hα emission with the JCMT beam at 230 GHz overlaid (20′′ diameter, bottom row). et al. 2014). Stellar masses were taken from C. Maraston et al. (2013) for SDSS DR84 (𝑀SED ∗ ). We considered only galaxies with SFR as traced by Hα line, SFRHα, around or larger… view at source ↗
Figure 3
Figure 3. Figure 3: Central emission line ratios [O iii]/Hβ versus [N ii]/Hα of the MaLHUCO sample. Galaxies below the dashed line from G. Kauffmann et al. (2003) are unlikely to host an AGN. Targets are color-coded by their oxygen abundance. Galaxy 43-47 is not included in this plot because its properties are not available in the MaNGA database. the xCOLDGASS and ALLSMOG surveys. In this case, the difference between the two … view at source ↗
Figure 2
Figure 2. Figure 2: Comparison between different stellar mass estimates for the MaLHUCO (red squares) and MASCOT (blue circles) samples. 𝑀P3D ∗ are compared with stellar masses from the MPA-JHU catalog (top) and from C. Maraston et al. (2013, bottom). The solid line indi￾cates to the one-to-one relation, while the green shaded region marks a ± 0.5 dex dispersion. The dashed horizontal line at log(𝑀∗/M⊙) = 9.7 highlights the t… view at source ↗
Figure 4
Figure 4. Figure 4: Distribution of CO detections (filled histogram) and non-detections (open histrogram) as a function of 𝑀∗, sSFR, oxygen abundance at 1 𝑅𝑒, 𝑀HI/𝑀∗, stellar surface density at 1 𝑅𝑒, Σ∗,𝑒, visual attenuation, 𝐴 BD V , 12 µm luminosity, 𝐿12, and bar parameter. relation between 𝐿CO and 𝐿12 will be discussed in more detail later. Bars drive gas inflows toward galaxy centers, triggering and fueling star formation… view at source ↗
Figure 5
Figure 5. Figure 5: Top: Relation between SFRP3D SSP and 𝑀P3D ∗ for MaNGA-late (crosses), MASCOT (circles) and MaLHUCO galaxies (squares: CO detections; downward-pointing triangles: CO non-detections). The solid line shows the ODR fit to the MaNGA-late sample. The dashed line corresponds to the main sequence at 𝑧 = 0 (F. Belfiore et al. 2018). Bottom: The specific SFR (sSFR=SFRP3D SSP /𝑀P3D ∗ as a function of 𝑀P3D ∗ . Symbols… view at source ↗
Figure 6
Figure 6. Figure 6: 𝐿CO versus 𝐿12 (top panel) and 𝐿CO versus 𝐿22 (bottom panel) for MaLHUCO (squares: detections; downward-pointing tri￾angles: non-detections) and MASCOT (circles) samples. In both panels, the green lines show fitted relations inferred using Bayesian methods for MALHUCO targets only. The red lines indicate the ODR best fit to MASCOT and MALHUCO CO-detected galaxies. Data have been color-coded by sSFR (left p… view at source ↗
Figure 7
Figure 7. Figure 7: The molecular gas main sequence (𝑀H2 vs. 𝑀∗). The top panel shows the relation for 𝑀MW H2 , while the bottom panel displays the relation for 𝑀A17 H2 . In both panels, the red line corresponds to the ODR fit to the MaLHUCO+MASCOT sample, the magenta line is the ODR fit to the MaLHUCO galaxies with a CO detection (squares), the green line highlights the Bayesian fit to all MaLHUCO galaxies (squares and downw… view at source ↗
Figure 8
Figure 8. Figure 8: Left: The global KS relation for the MaLHUCO (squares: detections; left-pointing triangles: non-detections) and MASCOT (circles) sample. The dashed purple line is the result of the ODR fit to the CO detections of the full sample (MaLHUCO+MASCOT). The red solid line shows the fit for the MaLHUCO CO-detected galaxies only. The parameters of the two best-fit relations are given in [PITH_FULL_IMAGE:figures/fu… view at source ↗
Figure 9
Figure 9. Figure 9: Top: 𝜏H2 as a function of the stellar mass for both MASCOT (circles) and MaLHUCO (squares: detections; down￾ward-pointing triangles: non-detections) samples. Binned values (diamonds) are calculated as medians in stellar-mass intervals of 0.5 dex and restricted to detected galaxies with log(𝑀P3D ∗ /M⊙) > 9. The star marks the location of M33. Bottom: correlation between 𝜏𝐻2 and sSFR for MASCOT and MALHUCO s… view at source ↗
Figure 10
Figure 10. Figure 10: Left: 𝑀H2 /𝑀P3D ∗ as a function of 𝑀P3D ∗ for MaLHUCO and MASCOT galaxies, color-coded by the offset from the main sequence, log Δ(MS). Right: 𝑀HI/𝑀P3D ∗ as a function of 𝑀P3D ∗ for MANGA-late, MaLHUCO, and MASCOT galaxies with detections in the Hi-MaNGA catalog. Targets from the last two samples are color-coded by specific molecular mass (𝑀H2 /𝑀∗). Symbols are the same as in the previous figures. 1.50 1.… view at source ↗
Figure 11
Figure 11. Figure 11: 𝑀H2 /𝑀gas versus 𝑀HI/MP3D ∗ for MASCOT and MaL￾HUCO galaxies with detections in the Hi-MaNGA catalog . Symbols are the same as in the previous figures. The parameters of the best-fit relation (dashed line) are given in [PITH_FULL_IMAGE:figures/full_fig_p017_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: 𝑀H2 of MASCOT and MaLHUCO samples as a function of the attenuation from the Balmer decrement and from SSP models, shown in the left and right panel, respectively. Data have been color-coded by the oxygen abundance. Symbols are the same as in the previous figures. MH2 M* Mbar * MHI O/H 0.0 0.1 0.2 0.3 0.4 0.5 0.6 Relative Importance [PITH_FULL_IMAGE:figures/full_fig_p018_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Relative importance of galaxy parameters derived from the RF regression used to predict the global SFR in the combined MASCOT and MaLHUCO sample. A. Saintonge & B. Catinella 2022; B. Hagedorn et al. 2024), especially for MS galaxies. However, some authors also re￾port no statistically significant correlations between these two parameters (A. Boselli et al. 2014; G. Accurso et al. 2017). The absence of a r… view at source ↗
Figure 14
Figure 14. Figure 14: Left: SDSS 𝑔𝑟𝑖 image of a MaLHUCO galaxy, with the hexagonal MaNGA field of view and the FWHM of the JCMT beam at 230 GHz overlaid in magenta and red, respectively. Right: the corresponding observed 12CO(J=2-1) spectrum. Detected signals are highlighted in yellow, while marginal detections, not included in our analysis are shown in light blue. The vertical red line indicates V𝑜 𝑝𝑡 for each target. This la… view at source ↗
Figure 14
Figure 14. Figure 14: continued [PITH_FULL_IMAGE:figures/full_fig_p024_14.png] view at source ↗
Figure 14
Figure 14. Figure 14: continued [PITH_FULL_IMAGE:figures/full_fig_p025_14.png] view at source ↗
Figure 14
Figure 14. Figure 14: continued [PITH_FULL_IMAGE:figures/full_fig_p026_14.png] view at source ↗
read the original abstract

We present James Clerk Maxwell Telescope (JCMT) observations of the $^{12}$CO(J = 2-1) emission of 42 low-mass, star-forming disk galaxies of morphological type Scd or later from the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey. The sample, which probes the M33-like stellar-mass regime, is complemented with metallicities, star formation rates, and \hi\ masses used to investigate the star formation process and to test scaling relations involving molecular gas mass in low-mass systems. We detect CO emission in 55% of the sample and derive H$_2$ masses using both a constant Galactic and a metallicity-dependent CO-to-H$_2$ conversion factor. The 12 $\mu$m luminosity, which includes polycyclic aromatic hydrocarbon features, exhibits a tight linear correlation with the CO line emission, making it a robust tracer of global molecular gas content. The molecular gas mass - star formation rate relation, i.e. the Kennicutt-Schmidt law, is the most fundamental one and it is found to remain linear down to low stellar masses. We also find that the mean molecular gas depletion time is slightly shorter in low-mass late-type galaxies than in more massive systems, consistent with their higher specific star formation rates. Finally, while the specific molecular gas mass ($M_{\rm H_2}/M_*$) shows no significant dependence on stellar mass and a large intrinsic scatter, the HI-to-stellar mass ratio ($M_{\rm HI}/M_*$) decreases with increasing stellar mass and molecular fraction ($M_{\rm H_2}/M_{\rm gas}$), highlighting the progressive transition from atomic- to molecular-dominated interstellar medium along the galaxy population.

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

2 major / 2 minor

Summary. The manuscript reports JCMT CO(2-1) observations of 42 low-mass (M33-like), late-type (Scd or later) MaNGA disk galaxies. CO is detected in 55% of the sample. Molecular gas masses are derived using both a constant Galactic X_CO and a metallicity-dependent conversion factor. The authors find that the global Kennicutt-Schmidt relation (M_H2 versus SFR) remains linear at low stellar masses, that 12 μm luminosity correlates tightly with CO emission, that molecular depletion times are slightly shorter than in higher-mass systems, and that M_H2/M_* shows no strong stellar-mass trend while M_HI/M_* decreases with mass.

Significance. If the derived M_H2 values are unbiased, the work supplies rare CO data in the low-mass regime and supports a mass-independent star-formation efficiency down to M_* ~ 10^9 M_⊙. The MaNGA ancillary metallicities and SFRs allow direct testing of scaling relations that are otherwise poorly constrained below the typical CO survey limits. The 12 μm–CO correlation offers a potentially useful ancillary tracer.

major comments (2)
  1. [Abstract and H2 mass derivation section] Abstract and the section deriving H2 masses: the central claim that the Kennicutt-Schmidt relation remains linear rests on M_H2 values obtained with both a constant Galactic X_CO and a metallicity-dependent prescription. No quantitative test is shown of how the choice of conversion factor (or its extrapolation to the lowest metallicities in the sample) alters the fitted slope or the treatment of the 45% upper limits. A systematic mass-dependent bias in the adopted X_CO would move the observed relation toward unity even if the true relation is not linear.
  2. [Depletion time results paragraph] The paragraph reporting the mean molecular depletion time: the statement that depletion times are slightly shorter in low-mass late-type galaxies than in more massive systems is derived directly from the same M_H2 values. Without an independent cross-check (dust continuum, [C I], or virial masses) in the M33-like metallicity range, the result inherits the same conversion-factor uncertainty that affects the linearity claim.
minor comments (2)
  1. [Sample selection paragraph] The sample selection from the parent MaNGA catalog (exact stellar-mass and morphological cuts, completeness corrections) should be stated more explicitly so that readers can assess representativeness of the 42-galaxy subset.
  2. [Figure captions] Figure captions and text should consistently label which panels or points use the constant versus metallicity-dependent X_CO so that the two cases can be compared directly.

Simulated Author's Rebuttal

2 responses · 1 unresolved

We thank the referee for their careful and constructive review of our manuscript. The comments raise important points about the robustness of our conclusions to the choice of CO-to-H2 conversion factor. We address each major comment below and outline the revisions we will make.

read point-by-point responses

  1. Referee: [Abstract and H2 mass derivation section] Abstract and the section deriving H2 masses: the central claim that the Kennicutt-Schmidt relation remains linear rests on M_H2 values obtained with both a constant Galactic X_CO and a metallicity-dependent prescription. No quantitative test is shown of how the choice of conversion factor (or its extrapolation to the lowest metallicities in the sample) alters the fitted slope or the treatment of the 45% upper limits. A systematic mass-dependent bias in the adopted X_CO would move the observed relation toward unity even if the true relation is not linear.

    Authors: We agree that a quantitative assessment of the impact of X_CO choice on the fitted slope and upper-limit treatment is needed. In the revised manuscript we will add a new subsection and accompanying figure that directly compares the Kennicutt-Schmidt relation obtained with the constant Galactic X_CO versus the metallicity-dependent prescription. This will include linear fits performed with and without the 45% upper limits (using appropriate censored-data methods) and will quantify the change in slope and scatter. We will also discuss the range of metallicities in the sample and the extrapolation of the metallicity-dependent factor, showing that any residual mass-dependent bias is unlikely to be large enough to force linearity given the observed consistency with the independent 12 μm tracer. revision: yes

  2. Referee: [Depletion time results paragraph] The paragraph reporting the mean molecular depletion time: the statement that depletion times are slightly shorter in low-mass late-type galaxies than in more massive systems is derived directly from the same M_H2 values. Without an independent cross-check (dust continuum, [C I], or virial masses) in the M33-like metallicity range, the result inherits the same conversion-factor uncertainty that affects the linearity claim.

    Authors: We acknowledge that the reported depletion times rely on the same M_H2 estimates and therefore carry the same X_CO uncertainties. Independent cross-checks (dust continuum, [C I], or virial masses) are not available for this specific low-mass sample. In the revision we will expand the relevant paragraph and discussion section to explicitly state this limitation, compare our depletion times to literature values obtained with alternative methods where possible, and note that the shorter times remain consistent with the higher specific star-formation rates measured for these galaxies. We will also add a brief sensitivity test showing how the mean depletion time changes when the two X_CO prescriptions are used. revision: partial

standing simulated objections not resolved
  • Independent cross-checks of M_H2 (via dust continuum, [C I], or virial masses) do not exist for this sample in the M33-like metallicity regime, preventing a direct empirical validation of the adopted conversion factors.

Circularity Check

0 steps flagged

No circularity: purely observational survey reporting empirical correlations from new data.

full rationale

The paper reports JCMT CO(2-1) observations of 42 MaNGA low-mass disks, derives M_H2 via standard (constant or metallicity-dependent) X_CO prescriptions, and presents direct empirical relations including the linearity of the global M_H2-SFR (Kennicutt-Schmidt) relation down to low stellar mass. No first-principles derivations, fitted parameters renamed as predictions, self-citations used as load-bearing uniqueness theorems, or ansatzes smuggled via prior work appear in the chain. All scaling relations are measured outcomes, not tautological reductions of the inputs. The 55% detection rate and handling of upper limits are standard observational choices, not circular by construction.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

Claims depend on the accuracy of the CO-to-H2 conversion factor (treated as a free parameter with two variants) and standard domain assumptions for deriving gas masses and star-formation rates from line and continuum data.

free parameters (1)
  • CO-to-H2 conversion factor
    Both a constant Galactic value and a metallicity-dependent version are applied to derive H2 masses; the choice directly affects reported gas masses and depletion times.
axioms (2)
  • domain assumption Standard assumptions for converting observed CO(2-1) integrated intensity to molecular hydrogen column density
    Invoked when deriving H2 masses from the JCMT data.
  • domain assumption MaNGA-derived metallicities, SFRs, and HI masses are accurate and directly comparable to the new CO measurements
    Used to test scaling relations and gas fractions.

pith-pipeline@v0.9.0 · 5642 in / 1632 out tokens · 82220 ms · 2026-05-12T02:23:08.423779+00:00 · methodology

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