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The EDGE-CALIFA Survey: An integral field unit-based integrated molecular gas database for galaxy evolution studies in the Local Universe

T0 review · 3 major / 5 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read Quenched galaxies do not just run out of molecular gas; their central regions also lose the ability to turn the gas they still have into stars, by about two orders of magnitude.

desk verdict iEDGE is a valuable public database, but the headline inside-out quenching claim rests on censored CO data and an internal magnitude inconsistency. read the letter →

arxiv 2507.06375 v1 pith:ZLET2E3Y submitted 2025-07-08 astro-ph.GA astro-ph.COastro-ph.IM

D. Colombo , V. Kalinova , Z. Bazzi , S. F. Sanchez , A. D. Bolatto , T. Wong , V. Villanueva , N. Mudivarthi
show 9 more authors
E. Rosolowsky A. Wei{ss} K. D. French A. Leroy J. Barrera-Ballesteros Y. Garay-Solis F. Bigiel A. Tripathi B. Rodriguez
This is my paper · ORCID
classification astro-ph.GAastro-ph.COastro-ph.IM
keywords galaxyevolutionmoleculargasCOemissionstarformationefficiencyquenchingintegralfieldspectroscopyCALIFAsurveystar-formingmainsequence
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

This paper builds iEDGE, a homogenised database of integrated molecular-gas, star-formation, and stellar-mass measurements for 643 local galaxies from the CALIFA survey, combining optical integral-field data with CO observations from three telescopes. The authors use the database to test how galaxies shut down star formation as they move from the star-forming main sequence, through the green valley, and into the retired sequence. They find that the three classic scaling relations (SFR–$M_*$, SFR–$M_{\rm mol}$, $M_{\rm mol}$–$M_*$) are bimodal, cleanly separating star-forming spirals from passive early-type galaxies. The central result concerns the inner regions: while the molecular gas fraction $f_{\rm mol}$ stays roughly constant from galaxy centres to discs, the star formation efficiency SFE in the cores of passive galaxies (those more than about 1.5 dex below the main sequence) is almost two orders of magnitude lower than the global value. This indicates that inside-out quenching requires not only low molecular gas fractions but also a strongly suppressed ability to turn molecular gas into stars in galactic centres.

What carries the argument

The carrying object is the iEDGE database itself, organised around a beam-versus-global split in every quantity. Beam quantities are measured within the 26.3-arcsec APEX beam; global quantities cover the full CALIFA footprint, roughly two effective radii. Three homogenisation techniques make the heterogeneous data comparable: tapering the CALIFA maps with a two-dimensional Gaussian to match the APEX beam, smoothing CARMA and ACA datacubes to APEX spatial and spectral resolution, and an aperture correction for the APEX single-pointing data, $\log L^{\rm APEX,G}_{\rm CO(2-1)} = 0.08 + 1.02 \log L^{\rm APEX,B}_{\rm CO(2-1)}$. That correction converts beam CO luminosities to global values by assuming that WISE W3 12-$\mu$m luminosity measured in the same beam traces the CO flux lying outside the beam, and it is what produces the global quantities whose contrast with beam values defines the central SFE result.

What would settle it

Map the full CO(2-1) extent of a sample of passive E/S0 galaxies more than 1.5 dex below the star-forming main sequence with total-power or interferometric observations, and compare the directly measured global CO luminosities with the APEX aperture-corrected values; agreement around the expected factor of 1.7 would confirm the central SFE suppression, while a systematic offset would show it is an artifact of the correction.

Watch

Extended reading notes

Core claim

On the paper's own terms, the discovery is that passive early-type galaxies quench from the inside out through two channels working together. Using beam quantities (measured within the 26.3-arcsec APEX beam, roughly the inner one effective radius) and global quantities (integrated over the full galaxy), the paper shows that $f_{\rm mol}=M_{\rm mol}/M_*$ is spatially flat: beam and global molecular gas fractions scatter around the 1:1 relation across all morphological types. Star formation efficiency, SFE $=$ SFR/$M_{\rm mol}$, behaves differently. In spiral, star-forming galaxies the beam and global SFEs agree, but in E/S0 galaxies more than about 1.5–2 dex below the star-forming main sequence, the inner SFE is roughly 10–100 times lower than the global value, producing a flattened SFE$_{\rm global}$–SFE$_{\rm beam}$ relation. The paper interprets this as a direct manifestation of inside-out quenching: removing molecular gas is not enough; galactic centres must also lose the capacity to form stars from the gas they retain. The authors add the caution that the global APEX quantities depend on an aperture correction, so the significance of the bending should be interpreted with care.

Load-bearing premise

The headline result depends on the assumption that the 12-micron light from a galaxy's central beam region faithfully predicts the carbon-monoxide emission outside the beam for every galaxy type, including the passive early-type galaxies that drive the finding.

Editorial extensions

If this is right

  • If the central claim is right, quenching models must include a mechanism that suppresses star formation efficiency by about two orders of magnitude in the centres of passive early-type galaxies, not only a mechanism that removes or heats molecular gas.
  • The bimodality of the SFR–$M_*$, SFR–$M_{\rm mol}$, and $M_{\rm mol}$–$M_*$ relations means an integrated molecular-gas measurement alone can tell whether a galaxy belongs to the star-forming or retired population.
  • Galaxies between about 1.5 and 2 dex below the main sequence mark the switch point where the inner SFE drops relative to the global value even though the molecular gas fraction remains spatially flat.
  • Because $f_{\rm mol}$ is flat while SFE is not, future resolved surveys must measure both quantities simultaneously; a single global measurement cannot reveal which channel is quenching a galaxy.
  • The many CO non-detections among passive galaxies imply that the gas-removal channel may be even stronger than the measured molecular gas fractions indicate, since those values are upper limits.

Reading between the lines

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

  • A testable extension: apply the same beam-versus-global decomposition to resolved CO maps of green-valley galaxies with $\Delta_{\rm SFMS}$ between −1.5 and −2 to determine whether the central SFE drop precedes or follows the drop in molecular gas fraction; the integrated sample cannot cleanly separate those two stages.
  • A validation experiment: add total-power CO(2-1) maps for the passive APEX-only targets in iEDGE; the existing overlap galaxies already test the aperture correction, but the passive population is exactly the one with no direct global-CO check.
  • If the central SFE suppression is physical, numerical simulations of galaxy formation that reproduce quenching through gas depletion alone may need an additional stabilisation or feedback term that acts preferentially in high-stellar-density centres.
  • The flatness of $f_{\rm mol}$ centre-to-disc in passive galaxies hints that the residual molecular gas is not arranged in star-forming complexes; resolved CO observations could test whether it is diffuse or dynamically stabilised.
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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 / 5 minor

Summary. This paper presents iEDGE, an integrated database of stellar, nebular, and molecular gas properties for 643 CALIFA galaxies, combining CALIFA IFU optical data with CARMA CO(1-0), ACA CO(2-1), and APEX CO(2-1) observations. The authors homogenize beam and global quantities via tapering, smoothing, and a WISE W3-based aperture correction (Eq. 4), and use the database to examine the SFR-M*, SFR-Mmol, and Mmol-M* relations. The headline result is that for early-type/passive galaxies below Delta_SFMS of about -1.5, the star formation efficiency in the inner regions is suppressed relative to the global SFE, while the molecular gas fraction remains roughly constant; the authors interpret this as evidence that inside-out quenching requires not only low f_mol but also strongly reduced SFE in galaxy centers. The paper also provides a public data release and a series of cross-telescope consistency checks.

Significance. If the central result holds, it would strengthen the case that quenching in galaxy centers is not solely due to gas depletion. The database itself is a substantial community resource: it is large, covers a broad range of SFR, stellar mass, and morphology, and the homogenization, tapering, and aperture-correction procedure is clearly described and benchmarked against overlapping observations. The paper ships a public Zenodo release and includes transparent flags for upper limits. These are genuine strengths. However, the central claim is not yet established because the treatment of censored CO non-detections and the internal inconsistency in the claimed magnitude are load-bearing and currently under-supported. I find no fundamental circularity in the analysis: the database measurements come from external observations, and the key calibrations are not defined in terms of the target result.

major comments (3)
  1. [Abstract; Section 4.5; Fig. 9 caption; Section 5] The paper states the central result with inconsistent magnitudes. The abstract says the inner-region SFE of passive galaxies is 'almost two orders of magnitude lower' than the global value; Section 5 repeats '~2 dex' for Delta_SFMS < -1.5; Section 4.5 says the inner regions form stars at a rate 'roughly 10 times lower', and the Fig. 9 caption says '~1 dex lower'. Because the size of this offset is the paper's headline and the basis for the inside-out-quenching interpretation, the authors must adopt a single, well-defined measurement (for example, the median of log(SFE_G) - log(SFE_B) over a specified Delta_SFMS and morphology selection) and use it consistently throughout.
  2. [Section 4.5; Fig. 9] The apparent suppression of central SFE in passive galaxies is not separated from the treatment of CO non-detections. In the low-SFE tail, which the authors state is 'dominated by non-detections', M_mol_B is a 3-sigma upper limit, so SFE_B = SFR_B / M_mol_B is a lower limit rather than a measurement. Plotting these limits as points in the SFE_G versus SFE_B plane systematically displaces the passive-galaxy population toward low SFE_B and can create the reported offset even if the true central efficiencies are comparable to the global values. The central claim requires a survival-analysis or Bayesian upper-limit treatment, or at minimum a version of Fig. 9 restricted to S/N > 3 detections, before it can be taken as evidence for reduced central SFE. The caveat in the text is not sufficient because the abstract and conclusions do not carry this qualification.
  3. [Eq. 4; Section 3.1.3; Section 4.1] The aperture correction used to estimate APEX global CO luminosities is calibrated on the WISE W3 relation and benchmarked against ACA and CARMA samples that are predominantly star-forming, late-type galaxies. No direct global CO validation exists for the passive early-type population that dominates the offset claim. Because SFE_G in Fig. 9 is computed with M_mol_G derived from Eq. 4, a systematic error in the aperture correction for quiescent objects could change the magnitude or even the direction of the apparent offset. The authors should either provide independent global CO constraints for a subsample of passive E/S0 galaxies (for example, wide-beam single-dish measurements) or demonstrate that the Fig. 9 result is robust to plausible alternative aperture corrections, including the directly measured ACA and CARMA global-to-beam ratios.
minor comments (5)
  1. [Section 5; Section 2.4; Section 3.1.1] Section 5 states that beam measurements cover 'within 23.6 arc-seconds, or the APEX beam at 230 GHz', but the APEX beam FWHM is 26.3 arcsec in Section 2.4 and Section 3.1.1; 23.6 arcsec is the FWHM of the tapering Gaussian, not the APEX beam. Please correct this inconsistency.
  2. [Eq. 14; References] Equation 14 cites 'den Brok et al. (in prep.)' for the R21-Sigma_SFR relation, but no such work appears in the reference list (den Brok et al. 2021 and 2023 are listed). This calibration is central to the molecular gas mass scale and must be citable and reproducible.
  3. [Fig. 9] The figure uses transparent diamonds to indicate upper limits, but these limits are still plotted as point symbols in the SFE_B panel. Showing them as downward arrows or otherwise visibly different symbols would make the censorship status clearer and reduce the risk of readers misinterpreting lower limits as detections.
  4. [Table C.1] The column name 'Observatory_Type_k2jypb' appears to be a garbled or placeholder name for a Jy/beam per K conversion factor; please rename it to something descriptive such as 'Observatory_Type_Jy_per_K'.
  5. [Section 4.3.1] The sentence 'We used ACA data instead of APEX data in case the latter showed better S/N compared to the former' is ambiguous about which dataset is preferred in the consolidated sample; please rephrase to state explicitly the selection rule.

Circularity Check

1 steps flagged · score 6.0 of 10

The passive-galaxy 'gas is not scarce' argument is partly built into the WISE-based aperture correction; the SFE offset itself is not forced, but the f_mol constancy used to interpret it reduces to the fitted mapping.

  1. fitted input called prediction [Section 3.1.3, Eq. (4); applied in Section 4.5 and Fig. 9 caption]
    "Finally, by combining the beam APEX CO(2-1)-WISE W3 12µm relationship, and the global-to-beam WISE W3 12µm relationship, we aperture-corrected the beam APEX CO(2-1) luminosities to infer the global APEX CO(2-1) luminosities. This gives log(L_APEX,G_CO(2-1)) = 0.08 + 1.02 log(L_APEX,B_CO(2-1)). ... While fmol does not appear to vary across the galaxy discs, the SFE in the centre of the retired early-type galaxies in particular is ∼ 1 dex lower compared to the SFE across the entire galaxies."

    For APEX galaxies (the main population driving the passive SFE trend), the 'global' CO luminosity is not an independent measurement: it is defined by the fitted aperture relation Eq. (4) from the beam luminosity. Therefore f_mol,G/f_mol,B = (M*,B/M*,G)(αCO,G/αCO,B)10^{0.08}L_B^{0.02} ≈ (M*,B/M*,G)×1.2. The calibration was anchored to WISE W3 12µm, which in passive early-type galaxies is dominated by old stellar light, so the correction effectively assumes CO follows the stellar 12µm distribution. The paper's statement that fmol 'does not appear to vary across the galaxy discs' is thus a consequence of this fitted mapping and the stellar-mass profile, not evidence that gas is not scarce in the centres.

full rationale

The paper's headline SFE result is not, by itself, circular: for APEX galaxies SFE_G/SFE_B is essentially (SFR_G/SFR_B)×(M_mol_B/M_mol_G), and M_mol_B/M_mol_G is set by Eq. 4 (≈0.7–0.8), so the 1–2 dex offset is dominated by the independently measured CALIFA SFR ratio. The circularity is in the companion claim that molecular gas is not scarce in the centres. Because the 'global' CO luminosity for APEX objects is generated by Eq. 4, which was calibrated on WISE W3 12µm, and because 12µm in passive early-types traces the old stellar population, the resulting f_mol,G/f_mol,B ≈ (M*,B/M*,G)×1.2 is forced to lie near unity whenever the stellar-mass profile is similar to the 12µm profile. The paper then uses this constructed constancy to argue that quenching is due to reduced SFE rather than gas availability. This is a fitted input being presented as an observed radial gas distribution. The rest of the derivation chain is self-contained: tapering and smoothing are described in place; αCO and R21 come from external calibrations (Bolatto+13; den Brok+ in prep) with appendices exploring systematics; CARMA/ACA global CO is measured, not fitted; no uniqueness theorem is imported from the authors. The paper's own caution that the SFE tail is dominated by non-detections and that the bend may be influenced by the aperture correction is an honest limitation, but it does not remove the constructed nature of the f_mol constancy for the APEX-dominated passive sample.

Assumptions & free parameters 6 free parameters · 7 assumptions · 0 invented entities

The central measurement chain depends on several fitted or adopted calibration parameters: an aperture correction derived from WISE 12um, an unpublished R21 relation, a literature alpha_CO prescription, and a mass-metallicity relation. No new physical entities are postulated; iEDGE is a data product.

free parameters (6)
  • APEX aperture correction coefficients (Eq. 4) = slope m = 1.02, intercept b = 0.08
    Fitted in Section 3.1.3 using linmix to WISE W3 beam/global 12um and APEX beam CO(2-1)-to-12um relations; applied to all 454 APEX galaxies to convert beam CO to global CO, directly entering SFE_G and the central SFE contrast.
  • R21-Sigma_SFR relation coefficients (Eq. 14) = slope 0.12, intercept 0.06
    Adopted from den Brok et al. (in prep.) to convert CO(2-1) to CO(1-0) for APEX and ACA; this sets Mmol for a large fraction of the sample.
  • alpha_CO(1-0) model parameters = 2.9 norm, 0.4 metallicity exponent, gamma=0.5, 100 Msun/pc2 threshold
    Adopted from Bolatto et al. (2013) Eq. 13; scales every molecular gas mass and therefore f_mol and SFE.
  • Mass-metallicity relation coefficients (Sanchez et al. 2017) = 8.73 + 0.01 (x-3.50) exp(-(x-3.50))
    Used in Eq. 12 to assign metallicities to pixels without emission lines; these metallicities drive alpha_CO through Eq. 13.
  • Universal metallicity gradient = -0.1 dex/Re
    Assumed to build radial metallicity maps in non-star-forming regions, directly affecting alpha_CO in passive galaxy centers.
  • Fiducial line width for CO upper limits = W50 = 300 km/s
    Section 3.2.1: adopted as the fiducial full width for non-detected galaxies when computing flux upper limits; affects the low-SFE tail populated by non-detections.
assumptions (7)
  • domain assumption CO(1-0) luminosity traces molecular gas mass through the Bolatto et al. (2013) conversion factor and its metallicity and surface-density dependence (Eq. 13).
    Used in Section 3.2.2, Eq. 13, to convert all CO luminosities to Mmol; the parameters are adopted from prior literature and not tested here.
  • domain assumption WISE W3 12um luminosity can stand in for CO(2-1) emission to extrapolate single-beam APEX CO fluxes to global galaxy fluxes (Eq. 4).
    Section 3.1.3: assumes the APEX beam CO-to-12um relation and the WISE global-to-beam relation are valid for all galaxy types, including passive early-type galaxies for which no direct ACA/CARMA global CO validation exists.
  • domain assumption Gas-phase metallicity in non-star-forming regions is recovered from the mass-metallicity relation plus a universal -0.1 dex/Re gradient.
    Section 3.2.2, after Eqs. 11-12: needed to compute alpha_CO in regions without HII-region emission lines, including quenched centers, which directly affects Mmol and f_mol.
  • domain assumption The CO(2-1)/CO(1-0) ratio R21 is determined by the star formation rate surface density through Eq. 14.
    Section 3.2.2, Eq. 14: used to convert CO(2-1) luminosities from APEX and ACA to CO(1-0) equivalent for Eq. 8; the calibration is unpublished at the time of submission.
  • domain assumption Total mass surface density can be approximated by stellar mass surface density in the alpha_CO model.
    Section 3.2.2: the paper sets Sigma_total approximately equal to Sigma_star because gas is about ten times lower, avoiding iterative solution of Eq. 13.
  • domain assumption SFR calibration from Halpha with Balmer-decrement extinction (Kennicutt 1998, Cardelli et al. 1989) is valid for spaxels passing the WHalpha >= 6 A and BPT masks.
    Section 3.2.2, Eqs. 9-10: underlying all SFR_G and SFR_B values, hence SFE; masks exclude AGN and old-star ionized regions.
  • domain assumption CALIFA maps extending to about 2 Re are sufficient to represent global galaxy quantities.
    Section 2.1 and Section 3.1: global SFR and stellar mass are computed by summing over the full CALIFA maps, and the CO global values are matched to this footprint.

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Pith. "Pith review of The EDGE-CALIFA Survey: An integral field unit-based integrated molecular gas database for galaxy evolution studies in the Local Universe." pith.science (2026). https://pith.science/paper/ZLET2E3Y

@misc{pith2026250706375,
  author       = {Pith},
  title        = {Pith review of: The EDGE-CALIFA Survey: An integral field unit-based integrated molecular gas database for galaxy evolution studies in the Local Universe},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/ZLET2E3Y}},
  note         = {Machine review of arXiv:2507.06375}
}
abstract

Studying galaxy evolution requires knowledge not only of the stellar properties, but also of the interstellar medium (in particular the molecular phase) out of which stars form, using a statistically significant and unbiased sample of galaxies. To this end, we introduce here the integrated Extragalactic Database for Galaxy Evolution (iEDGE), a collection of integrated stellar and nebular emission lines, and molecular gas properties from 643 galaxies in the local Universe. These galaxies are drawn from the CALIFA datasets, and are followed up in CO lines by the APEX, CARMA, and ACA telescopes. As this database is assembled from data coming from a heterogeneous set of telescopes (including IFU optical data and single-dish and interferometric CO data), we adopted a series of techniques (tapering, spatial and spectral smoothing, and aperture correction) to homogenise the data. Due to the application of these techniques, the database contains measurements from the inner regions of the galaxies and for the full galaxy extent. We used the database to study the fundamental star formation relationships between star formation rate (SFR), stellar mass ($M_*$), and molecular gas mass ($M_{\rm mol}$) across galaxies with different morphologies. We observed that the diagrams defined by these quantities are bi-modal, with early-type passive objects well separated from spiral star-forming galaxies. Additionally, while the molecular gas fraction ($f_{\rm mol}=M_{\rm mol}/M_*$) decreases homogeneously across these two types of galaxies, the star formation efficiency (SFE=SFR/$M_{\rm mol}$) in the inner regions of passive galaxies is almost two orders of magnitude lower compared to the global values. This indicates that inside-out quenching requires not only low $f_{\rm mol}$, but also strongly reduced SFE in the galactic centres.

Figures

Figures reproduced from arXiv: 2507.06375 by the authors.

Figure 1
Figure 1. Aperture correction for APEX observation-related tests and measurements. Upper left: Global versus beam luminosities calculated for WISE W3 (12 µm; green), ACA (red), and CARMA (blue) detected galaxies. The dotted lines indicate the 2:1, 5:1, and 10:1 loci, respectively. Upper middle: CO(2-1) luminosities from APEX measurements (L B CO) vs WISE W3 (12 µm) luminosities (L B 12µm ) calculated within the APEX beam. The… view at source ↗
Figure 2
Figure 2. Number of galaxies within the iEDGE observed by the different telescopes represented as a Venn diagram. Objects solely observed by APEX eventually constitute 64% of the final database, and CARMA data add up to 22% of the database. The rest of the targets have been observed by multiple telescopes. the W50 distributions calculated for APEX, ACA, and CARMA￾detected galaxies. The parameter ϵCO is used to provide an up￾p… view at source ↗
Figure 3
Figure 3. Comparison between beam-wise (top panels) and global luminosities (bottom panels) from ACA and APEX (left panels) and from CARMA and APEX (right panels). The blue circles indicate galaxies detected (with S/N > 3) from both telescopes, yellow arrows indicate galaxies detected only by ACA or CARMA, the green arrows indicate galaxies detected only by APEX, and the red crosses show galaxies not detected by both telescop… view at source ↗
Figures from the paper (6 more)
Figure 4
Figure 4. Figure 4: Detection distance bias shown as the beam S/N vs the distance to the galaxies, for APEX- (red), CARMA- (yellow), CARMA (D+E)- (green empty), ACA- (blue) observed galaxies. The black dashed line indicates a S/N=3 that marks the separation between detections and non-dete…
Figure 5
Figure 5. Figure 5: SFR-M∗ diagrams defined by the different samples considered in this paper (left panel): full CALIFA (cyan hexagons), and galaxies observed in CO lines by APEX (red circles), CARMA (yellow diamonds), CARMA (D+E galaxies only, empty green diamonds), ACA (blue squares). I…
Figure 6
Figure 6. Figure 6: Histograms across samples (full CALIFA, cyan bars; galaxies in the full iEDGE sample, black empty bars; CO detected galaxies in the iEDGE, red bars) related (from left to right) to M∗, SFR, specific SFR (sSFR=SFR/M∗), and logarithmic distance from the SF main sequence …
Figure 7
Figure 7. Figure 7: Distributions of the inferred CO(2-1)-to-CO(1-0) ratio (R21, left) and CO(1-0)-to-H2 conversion factors (αCO(1−0), right). These quantities are derived using IFU maps from models described in equations 13 and 14 (for αCO(1−0) and R21, respectively). Histograms show med…
Figure 8
Figure 8. Figure 8: Star formation scaling relations studied here colour-coded by the median equivalent width of Hα (WHα, upper row) and morphology (lower row), from left to right SFR-M∗, SFR-Mmol, and Mmol − M∗. In the left panel, the elements follow [PITH_FULL_IMAGE:figures/full_fig_p0…
Figure 9
Figure 9. Figure 9: Relationships between global and beam quantities, namely star formation efficiency, SFE, left column, and molecular gas fraction fmol, right column, colour-coded by the distance from the SFMS (∆SFMS, top row), morphology (middle row), and the different samples included…

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