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The Close AGN Reference Survey (CARS): A comparison between sub-mm and optical AGN diagnostic diagrams

T0 review · 2 major / 5 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read The paper claims that three nearby AGN follow the dense-gas/star-formation scaling relation despite the AGN, and that the sub-mm and optical classification diagrams agree in the one case where both could be completed.

desk verdict Honest small-sample ALMA study with new dense-gas detections in five CARS AGN; the central interpretation is speculative but the paper explicitly says so. read the letter →

arxiv 2507.01549 v1 pith:JKR7IEDL submitted 2025-07-02 astro-ph.GA

Jacob S. Elford , Timothy A. Davis , Ilaria Ruffa , Stefi A. Baum , Francoise Combes , Massimo Gaspari , Rebecca McElroy , Christopher P. O'Dea
show 4 more authors
Osase Omoruyi Mainak Singha Grant R. Tremblay Nico Winkel
This is my paper
classification astro-ph.GA
keywords activegalacticnucleidensemoleculargasHCNHCO+sub-mmdiagramBPTGao-SolomonrelationAGNdiagnostics
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 tests whether a luminous AGN leaves a measurable imprint on the dense molecular gas that traces star formation, using ALMA observations of HCN(4-3), HCO+(4-3) and CS(7-6) in five nearby Type-1 AGN from the CARS survey. It finds that in the three galaxies where the dense-gas lines are detected, the infrared and HCN luminosities follow the Gao-Solomon relation, so whatever effect the AGN has on these lines is not enough to break the global scaling. It then compares the sub-mm HCN diagnostic diagram against the classic optical BPT classification built from MUSE data: in the one source where all three sub-mm lines are detected, both diagrams agree, and in the other two the available lower limits do not rule out agreement. The paper reads this as evidence that AGN can excite both the warm ionised gas and the dense molecular gas at the same time, and that strong star formation can still dominate both phases even close to an AGN.

What carries the argument

The argument runs on three tools. The Gao-Solomon relation, in the $L_{\rm IR}$-$L_{\rm HCN(4-3)}$ and $L_{\rm IR}$-$L_{\rm HCO^+(4-3)}$ forms calibrated by Tan et al. (2018), is the scaling relation the AGN are tested against. The sub-mm HCN diagram of Izumi et al. (2016a) uses the HCN(4-3)/HCO+(4-3) and HCN(4-3)/CS(7-6) line-intensity ratios to separate AGN- from starburst-dominated dense gas. The optical BPT diagram, with the Kauffmann, Kewley and Schawinski demarcation lines, classifies the warm ionised gas in the same nuclear regions, isolated within one ALMA beam. The comparison between the two classification schemes, and the t-test residuals against the scaling relation, carry the central claim.

What would settle it

Detect CS(7-6) in HE0433-1028, the source the BPT classifies as AGN-dominated, and measure HCN(4-3)/CS(7-6); if the ratio exceeds about 8 the source moves into the AGN region and the claimed agreement for the fully measurable set fails, or observe these galaxies at <200 pc resolution and check whether the sub-mm ratios climb to AGN levels while the optical classification stays AGN-dominated, which would show the reported agreement is a beam-dilution artefact.

Watch

Extended reading notes

Core claim

The paper reports ALMA band-7 detections of HCN(4-3) and HCO+(4-3) in three of five CARS Type-1 AGN and a stacked CS(7-6) detection in one. It claims that, despite the potential impact of the AGN on line fluxes, these sources follow the Gao-Solomon $L_{\rm IR}$-$L_{\rm HCN}$ relation within the scatter of the Tan et al. (2018) calibration, with one-sample t-tests giving p=0.32 for HCN and p=0.51 for HCO+. It further claims that in the only source with all three lines measured (HE1108-2813), the sub-mm HCN diagram and the optical BPT diagram agree, both classifying the excitation as star-formation-driven, while in the two remaining sources the lower limits are consistent with either conclusion. The authors interpret this as evidence that AGN can excite both the warm ionised medium and dense molecular clouds simultaneously, possibly through X-ray, cosmic-ray or shock heating, while strong star formation can still dominate both phases.

Load-bearing premise

The comparison assumes that the ALMA beam (373-633 pc) covers the region where AGN influence on dense gas would appear, even though higher-resolution work places enhanced HCN excitation within r<200 pc, so the large beams may dilute any AGN-excited component and push the sources into the starburst part of the sub-mm diagram.

Editorial extensions

If this is right

  • The $L_{\rm IR}$-$L_{\rm HCN}$ and $L_{\rm IR}$-$L_{\rm HCO^+}$ scaling relations survive in these AGN hosts at the current resolution, so they remain usable as dense-gas-to-star-formation calibrators even when a luminous AGN is present.
  • In the one source with all three lines measured (HE1108-2813), the sub-mm HCN and optical BPT diagrams agree on star-formation-driven excitation, showing the two diagnostics can be cross-checked on identical nuclear scales.
  • Non-detections of CS(7-6) are the main limitation: in the other two sources only HCN/CS lower limits are available, so their sub-mm classification is not settled.
  • If AGN enrich HCN as suggested for other systems, the enrichment is not large enough in these three sources to shift them off the global scaling relations in log-log space.
  • The results are consistent with AGN exciting both warm ionised and dense molecular gas through X-ray, cosmic-ray or shock heating, while strong star formation still dominates both phases when present.

Reading between the lines

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

  • If the beam-dilution reading is right, the apparent sub-mm/optical agreement is a resolution effect, not a physical statement about AGN: at <200 pc resolution, HCN(4-3)/CS(7-6) and HCN(4-3)/HCO+(4-3) should rise toward the AGN region while the BPT stays AGN-dominated, and a targeted high-resolution ALMA follow-up of these three sources would test this directly.
  • HE0433-1028, BPT-classified as AGN-dominated, sits on a HCN/CS lower limit; if CS(7-6) is detected and the ratio exceeds about 8, the two diagrams would agree in the AGN sense, which would strengthen the paper's conclusion that optical and sub-mm classifications agree.
  • The implied simultaneous excitation of warm ionised and dense molecular gas favours volume-filling mechanisms such as X-ray or cosmic-ray heating and turbulence over pure photoelectric heating in photodissociation regions; mapping shock- or cosmic-ray-sensitive tracers like [Fe II] or H2 at the same nuclear scales would provide a cross-check.
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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 / 5 minor

Summary. The paper presents new ALMA Band 7 observations of HCN(4-3), HCO+(4-3), and CS(7-6) for five Type-1 AGN from the CARS survey, together with MUSE-based BPT classifications. The authors detect dense gas in three of five targets, find that these three follow the Tan et al. (2018) L_IR-L_HCN relation (with p-values 0.32 and 0.51 from a one-sample t-test), and place the three sources on the Izumi et al. (2016a) sub-mm HCN diagram, where all fall in the starburst region. For the one source with all three lines detected (HE1108-2813), the sub-mm classification agrees with the composite/star-forming BPT classification. The paper concludes that AGN may contribute to the excitation of both warm ionised and dense molecular gas, but explicitly labels this interpretation as speculative and notes the small sample size.

Significance. The paper provides new, useful ALMA observations of dense gas tracers in nearby AGN and a transparent comparison of optical and sub-mm diagnostics. Its strengths include a careful stacking analysis, explicit treatment of upper limits, and an honest discussion of limitations, including beam-dilution effects. The sample size is very small (three detections, one with a complete sub-mm measurement), but the paper is appropriately cautious in its language and does not overstate the statistical support. If the results hold, they suggest that on large scales AGN do not produce a measurable enhancement of dense-gas excitation, and that the sub-mm HCN diagram can be consistent with optical BPT classifications, providing a useful pilot result for future surveys.

major comments (2)
  1. [Abstract and Section 5] The abstract's concluding claim that 'AGN can contribute to the excitation of both the low density gas in the warm ionised medium and the high density gas in molecular clouds simultaneously' is not directly tested by the sub-mm data because the ALMA beams (373-633 pc; Section 2.1.2) are much larger than the r<200 pc region where AGN-enhanced HCN excitation has been found (Viti et al. 2014). Although Section 5 explicitly acknowledges this beam-dilution issue, the abstract presents the interpretation without this caveat. Please add a sentence to the abstract stating that the sub-mm/optical agreement is based on one source with complete detections and that the current resolution cannot rule out a compact AGN-excited component.
  2. [Abstract and Section 4.2.2] The statement 'Where it was possible to complete the analysis we find general agreement between optical and sub-mm classified gas excitation mechanisms' is based on a single galaxy, HE1108-2813, which has all three sub-mm lines detected. For HE0433-1028 and HE1029-1831, only lower limits on HCN/CS are available and the sub-mm diagram cannot discriminate between AGN and starburst excitation. The paper should explicitly say that the agreement is established for one source only, rather than 'general agreement' that could be read as applying to the sample as a whole.
minor comments (5)
  1. [Section 2.1] There is a typo: 'calibrated using the the Common Astronomy Software Applications' should read 'calibrated using the Common Astronomy Software Applications'.
  2. [Table 1] In the table notes, the galaxy names 'HE0433-1831' and 'HE1108-1813' are misspelled and should be 'HE0433-1028' and 'HE1108-2813'.
  3. [Figure 8 caption] The caption is confusing: it states the CARS targets are 'plotted in green and red, as labelled by the colour bar', but the colour bar represents BPT classification, not a green/red dichotomy. Please clarify how points are colour-coded.
  4. [Section 3.2] The improvement in signal-to-noise from ∼3.7 to ∼4.1 after stacking is modest; please specify the S/N of each detection before and after stacking to help the reader assess the benefit of the stacking procedure.
  5. [Throughout] The paper uses 'sub-mm HCN diagram' and 'submm-HCN diagram' inconsistently; please use a single spelling.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the paper compares new ALMA and MUSE measurements to fixed external calibrations and fits no parameter that would force the reported agreement.

full rationale

The paper's derivation chain is self-contained against external benchmarks. For the Gao-Solomon test, the authors use SFRs from Smirnova-Pinchukova et al. (2022), convert them to L_IR using the Kennicutt (1998) relation (Eq. 2), and compare the resulting L_IR values to the externally calibrated Tan et al. (2018) relations (Eqs. 3 and 4). No parameter of the Tan et al. relation is fitted to the CARS data; the one-sample t-test only checks residuals against a fixed relation. For the diagnostic comparison, the BPT demarcation lines are taken from Kauffmann et al. (2003), Kewley et al. (2001), and Schawinski et al. (2007), while the sub-mm HCN regions are taken from Izumi et al. (2016a). The sources are independently classified in the optical and sub-mm diagrams, and the single fully constrained source (HE1108-2813) is placed on the basis of directly measured line ratios. CS non-detections are explicitly treated as upper limits and not converted into detections. The self-citations present (CARS survey papers, Smirnova-Pinchukova et al. 2022, and the Stackarator tool by Davis et al. submitted) provide data or software but do not supply the numerical relations being tested. The beam-dilution caveat raised by a skeptical reader is a legitimate physical-interpretation concern, and the paper itself states that 'the interpretation is speculative'; it is not a logical circularity because no equation reduces the claimed result to an assumed input. No circular step can be exhibited.

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

No free parameters are introduced by this paper; all scaling relation constants are taken from prior literature (Kennicutt 1998, Tan et al. 2018). No invented entities are proposed. The central assumptions are that the SFR-based infrared luminosity is not AGN-contaminated, that external calibrations transfer to type-1 AGN hosts, that the MUSE fluxes are true narrow-line fluxes, and that the ALMA beams do not dilute the AGN-excited dense gas. The last assumption is explicitly discussed by the authors.

assumptions (4)
  • domain assumption The infrared luminosities derived from SFRs via Eq. (2) trace star formation and are not dominated by AGN-heated dust.
    Section 4.1: L_IR is obtained by inverting SFR ~ 2e-10 L_IR from Smirnova-Pinchukova et al. (2022). If AGN-heated dust contributes substantially, the apparent Gao-Solomon agreement would be inflated.
  • domain assumption The Tan et al. (2018) Gao-Solomon calibration, built on starburst, LIRG and ULIRG samples, transfers directly to type-1 AGN hosts.
    Section 4.1, Eqs. 3 and 4: the residual test measures consistency with this external relation, so a sample-specific offset would change the conclusion.
  • domain assumption The MUSE Halpha, Hbeta, [OIII] and [NII] fluxes used for BPT diagrams are narrow-line fluxes suitable for diagnostic ratios in Type-1 AGN.
    Section 2.2: the paper uses extracted MUSE line fluxes from CARS (Husemann et al. 2022) without stating whether broad-line components are excluded; broad Balmer contamination would make BPT classifications unreliable.
  • domain assumption The sub-mm HCN diagram boundary regions from Izumi et al. (2016a) are valid at the resolution and abundances of the CARS targets.
    Section 4.2.2 and Figure 8: classification of sources assumes the literature radiative-transfer-based boundaries apply at beams of 373 to 633 pc.

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Cite this review

Pith. "Pith review of The Close AGN Reference Survey (CARS): A comparison between sub-mm and optical AGN diagnostic diagrams." pith.science (2026). https://pith.science/paper/JKR7IEDL

@misc{pith2026250701549,
  author       = {Pith},
  title        = {Pith review of: The Close AGN Reference Survey (CARS): A comparison between sub-mm and optical AGN diagnostic diagrams},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/JKR7IEDL}},
  note         = {Machine review of arXiv:2507.01549}
}
abstract

The $L_{\rm IR}-L_{\rm HCN}$ relation suggests that there is a tight connection between dense gas and star formation. We use data from the Close AGN Reference Survey (CARS) to investigate the dense gas - star formation relation in AGN hosting galaxies, and the use of dense gas as an active galactic nuclei (AGN) diagnostic. Our sample contains five Type-1 (unobscured) AGN that were observed with the Atacama Large Millimeter/submillimeter Array (ALMA) with the aim to detect HCN(4-3), HCO$^+$(4-3) and CS(7-6). We detect the dense gas emission required for this analysis in 3 of the 5 targets. We find that despite the potential impact from the AGN on the line fluxes of these sources, they still follow the $L_{\rm IR}-L_{\rm HCN}$ relation. We then go on to test claims that the HCN/HCO+ and HCN/CS line ratios can be used as a tool to classify AGN in the sub-mm HCN diagram. We produce the classic ionised emission-line ratio diagnostics (the so-called BPT diagrams), using available CARS data from the Multi Unit Spectroscopic Explorer (MUSE). We then compare the BPT classification with the sub-mm classification made using the dense gas tracers. Where it was possible to complete the analysis we find general agreement between optical and sub-mm classified gas excitation mechanisms. This suggests that AGN can contribute to the excitation of both the low density gas in the warm ionised medium and the high density gas in molecular clouds simultaneously, perhaps through X-ray, cosmic ray or shock heating mechanisms.

Figures

Figures reproduced from arXiv: 2507.01549 by the authors.

Figure 1
Figure 1. Data products of the 12CO(1-0) ALMA observations of HE0433-1028. The moment 0 (integrated intensity), moment 1 (mean line-of-sight velocity) and moment 2 (mean line-of-sight velocity dispersion) maps are shown in the top-left, top-middle and top-right panels, respectively. The position-velocity diagram (PVD) is shown in the bottom-left and the integrated spectrum in the bottom-right panels. The synthesised beam is s… view at source ↗
Figure 2
Figure 2. As in [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Stacked spectra of the HCN (4-3) line in HE0433-1028 (left), HE1029-1831 (middle) and HE1108-2813 (right). The orange lines shows the best-fitting Gaussian profiles. MNRAS 000, 1–12 (2025) [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figures from the paper (5 more)
Figure 4
Figure 4. Figure 4: Stacked spectra of the HCO+ (4-3) line in HE0433-1028 (left), HE1029-1831 (middle) and HE1108-2813 (right). The orange lines shows the best-fitting Gaussian profiles [PITH_FULL_IMAGE:figures/full_fig_p006_4.png]
Figure 5
Figure 5. Figure 5: Stacked spectra of the CS (7-6) line in HE1108-2813. The orange line shows the best-fitting Gaussian profile [PITH_FULL_IMAGE:figures/full_fig_p006_5.png]
Figure 6
Figure 6. Figure 6: Relation between the HCN(4-3) (left) and HCO+ (4-3) (right) luminosity and the IR luminosity from star formation. We additionally plot the points and relation from Tan et al. (2018). using the Stackarator tool 3 of Davis et al. (submitted). This rou￾tine allows to stac…
Figure 7
Figure 7. Figure 7: All pixels BPT diagrams of HE0433-1028 (top), HE1029-1831 (middle) and HE1108-2813 (bottom). The lighter regions are areas with a higher density of points. The red points show the results obtained for the nuclear regions of each object, assumed to be within one ALMA be…
Figure 8
Figure 8. Figure 8: Submm-HCN diagnostic diagram. The three CARS targets for which this analysis has been carried out are plotted in green and red, as labelled by the colour bar on the right (and based on their BPT classification). We also plot on the background the data from Izumi et al.…

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