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JWST MIRI/MRS observations of hot molecular gas in an AGN host galaxy at Cosmic Noon

T0 review · 4 major / 5 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read This paper reports the first detection of hot molecular gas in the z~2.2 X-ray AGN cid_346 via the H2 1-0 S(1) ro-vibrational line at 2.12 $\mu$m, with a hot-to-cold molecular mass ratio of roughly $10^{-5}$--$10^{-6}$.

desk verdict First plausible MIRI/MRS detection of hot H2 at z~2.2, with a robust qualitative conclusion but a mass estimate that depends on a single-LTE assumption the data can't yet test. read the letter →

arxiv 2507.05354 v1 pith:XZU4UN34 submitted 2025-07-07 astro-ph.GA astro-ph.HE

D. Kakkad , V. Mainieri , Takumi S. Tanaka , John D. Silverman , D. Law , Rogemar A. Riffel , C. Circosta , E. Bertola
show 22 more authors
M. Bianchin M. Bischetti G. Calistro Rivera S. Carniani C. Cicone G. Cresci T. Costa C. M. Harrison I. Lamperti B. Kalita Anton M. Koekemoer A. Marconi M. Perna E. Piconcelli A. Puglisi Gabriele S. Ilha G. Tozzi G. Vietri C. Vignali S. Ward G. Zamorani L. Zappacosta
This is my paper
classification astro-ph.GAastro-ph.HE
keywords hotmoleculargasH2ro-vibrationaltransitionsAGNfeedbackcosmicnoonJWSTMIRI/MRSmassCO(3-2)galaxymergers
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 JWST MIRI/MRS spectra of the X-ray AGN cid_346 at $z\sim2.2$, the paper reports the first detection of hot molecular gas at Cosmic Noon through the H2 1-0 S(1) ro-vibrational transition at rest-frame 2.12 $\mu$m, along with the 1-0 S(0) line. From the two lines it derives an excitation temperature of roughly 1100 K and a hot molecular gas mass of a few times $10^5$ solar masses, which is $10^5$--$10^6$ times smaller than the cold molecular gas mass measured from CO(3-2). The authors argue that cold gas still dominates the molecular budget at Cosmic Noon and that the hot-to-cold ratio is similar to values seen in low-redshift galaxies, so the AGN's energy is not converting a significant share of the cold reservoir into a hot molecular phase. This matters because the leading picture of AGN feedback is that the black hole removes or heats the gas that would otherwise form stars, and the hot molecular phase is the earliest stage of that heating.

What carries the argument

The central object is the H2 ro-vibrational transition, a line in which the hydrogen molecule changes both its vibration and rotation state; the 1-0 S(1) line at 2.1218 $\mu$m is the standard tracer of molecular gas at roughly 1000--3000 K. The argument is carried by two constructed quantities: an excitation temperature from the Boltzmann-like Equation (1) applied to the S(1)/S(0) flux ratio, and a hot gas mass from Equation (2), which converts the 2.12 $\mu$m flux into mass using the LTE population fraction $f(v=1,J=3)$ and the laboratory transition probability. A third diagnostic, the 2.2477/2.1218 flux ratio, distinguishes thermal excitation from ultraviolet fluorescence and yields an upper limit of 0.3 in this source, pointing to thermal (X-ray or shock) heating.

What would settle it

A deeper MIRI/MRS spectrum of cid_346 that measures the H2 2.2477 $\mu$m line and finds a ratio to 2.1218 $\mu$m above about 0.3 would show fluorescent excitation, invalidating the single-temperature LTE interpretation of the 1100 K temperature and the hot gas mass.

Watch

Extended reading notes

Core claim

In cid_346, a luminous Type-1 AGN at $z=2.219$ with an ionised outflow and a large CO-based cold gas reservoir, the MIRI/MRS spectrum shows 1-0 S(1) and 1-0 S(0) at $4\sigma$ significance, with a flux ratio $2.2\pm0.7$. The paper interprets this ratio, via a Boltzmann excitation argument, as a hot molecular gas temperature of $1100^{+465}_{-245}$ K, and translates the 2.12 $\mu$m flux into a hot gas mass of about $8\times10^5$ solar masses in the whole cid_346 system. Compared with the ALMA CO(3-2) cold gas mass ($\sim10^{11}$ solar masses), the hot phase is five to six orders of magnitude less massive, and the hot gas is extended to roughly 16 kpc in the same south-east direction as the ionised outflow and the re-identified extended CO emission. The paper concludes that hot H2 is a minor phase locally tracing gas that may be invisible to CO, not a major part of the molecular mass budget at Cosmic Noon.

Load-bearing premise

The load-bearing assumption is that the detected H2 lines come from gas in local thermodynamic equilibrium at a single temperature, so the population fraction in the mass formula is the LTE value; fluorescent excitation or a wide temperature mix would shift the derived temperature and hot gas mass, though not the conclusion that cold gas dominates.

Editorial extensions

If this is right

  • At Cosmic Noon, the cold molecular phase carries nearly all the molecular gas mass, so AGN heating to $\sim1000$ K does not substantially reduce the CO-based reservoir in this system.
  • The hot-to-cold molecular gas ratio in cid_346 is close to low-redshift LIRG values, tentatively indicating no strong redshift evolution in this ratio up to $z\sim2$.
  • H2 ro-vibrational lines can reveal hot molecular gas on kiloparsec scales where CO emission may be weak or absent, adding a complementary tracer to ALMA-style CO surveys.
  • If the AGN's feedback removes cold gas in this galaxy, the removal is not through a large hot molecular phase; the mechanism must act on the cold phase directly or on other gas phases.

Reading between the lines

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

  • An obvious test is to check whether more radio-loud sources at Cosmic Noon show larger hot-to-cold ratios; the radio-jet heating suggested for C1 makes cid_346 a possible low-jet-power case.
  • Because the extended H2 lies near two NIRCam-detected satellites, part of the hot gas could trace merger-shocked gas rather than AGN-driven outflow; separating those requires mapping gas kinematics and excitation on sub-kiloparsec scales.
  • If a statistical MRS+ALMA sample at $z\sim2$ reproduces this ratio, it would strengthen the case that the hot-to-cold ratio is set by galaxy-scale properties or AGN luminosity rather than by redshift.
  • The single-temperature LTE assumption could hide a warmer, lower-mass component; adding the 2.2477 $\mu$m line and higher rotational H2 lines would test whether the hot gas has a multi-temperature distribution.
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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

4 major / 5 minor

Summary. The paper reports JWST MIRI/MRS observations of the z=2.219 X-ray AGN cid_346, claiming the first detection of hot molecular gas at Cosmic Noon via the H2 1-0 S(1) 2.12 micron ro-vibrational line, together with a tentative 1-0 S(0) detection. From the two line fluxes the authors derive an excitation temperature of 1100(+465,-245) K and, using the 1-0 S(1) flux, a hot molecular gas mass of about 8e5 solar masses (central source plus two extended clumps C1 and C2). This is compared with the CO(3-2)-based cold molecular gas mass, yielding a hot-to-cold mass ratio of ~1e-5 to 1e-6. The paper also presents extended H2 and CO emission to the SE, two NIRCam-detected satellite galaxies, and argues that the hot gas is likely excited by X-ray heating or radio jets, with cold gas still dominating the molecular budget at Cosmic Noon.

Significance. If the detection and derived parameters hold, this is a valuable first step in extending hot molecular gas studies from the local universe to Cosmic Noon, and it demonstrates the capability of MIRI/MRS to access rest-frame near-infrared H2 transitions at z~2. The data reduction is careful: the authors use dedicated background exposures, Monte Carlo error estimation, and comparisons with object-free MRS regions, and they place the line ratio in context with low-redshift AGN samples. The qualitative conclusion that cold molecular gas dominates the mass budget is robust to large systematic errors in the hot gas mass, since even an order-of-magnitude error leaves the ratio at ~1e-4 or below. However, the reported numerical values of T_exc and M_H2 rest on assumptions that are only partially tested, and the headline total mass includes a sub-3-sigma component; the manuscript needs to quantify and caveat these points before the quantitative claims can be accepted.

major comments (4)
  1. [Abstract, Section 4.2, Table 1] The total hot molecular gas mass quoted in the abstract and Section 6 (~8e5 solar masses) includes the C1 clump, which is a 2.4-sigma detection (flux 2.5 +/- 0.6 x 10^-18 erg/s/cm^2 in Table 1). Including a sub-3-sigma component in a headline number without an explicit caveat is not supportable; the central-only mass is 5.0(+7.0,-3.5)e5 solar masses, so the total is inflated by the marginal C1 detection. Please either report the central-only mass as the primary value, or clearly label the total as tentative and give the mass with and without C1.
  2. [Section 4.1, Eqs. 1 and 2] The excitation temperature and hot gas mass are derived under the assumption of a single LTE population (Eq. 1 states 'assuming the H2 is in equilibrium', and Eq. 2 uses the LTE population fraction f(v=1,J=3)). With only two detected lines this assumption cannot be verified, and the 2-1 S(1)/1-0 S(1) upper limit of <0.3 reported in Section 5 falls between the thermal expectation (~0.1) and the fluorescent expectation (~0.5), so a substantial non-thermal contribution is not excluded. Please quantify the systematic effect on T_exc and M_H2 (for example, by recomputing f(v=1,J=3) under a two-component or fluorescent model), or explicitly reframe the temperature and mass as conditional on the LTE assumption.
  3. [Table 1, Section 4.1] The measured FWHM of the 1-0 S(1) line is 458 +/- 60 km/s while that of the 1-0 S(0) line is 130 +/- 20 km/s, a factor of ~3.5 difference. Both lines are attributed to the same thermal gas and used together in Eq. 1, but the paper does not discuss this inconsistency. If the S(1) profile contains an additional broad component or is otherwise contaminated, the S(1)/S(0) ratio and the derived temperature and mass are not physically meaningful. Please address this explicitly, either by testing for a second component or by explaining why the widths can differ for lines from the same rovibrational population.
  4. [Section 4.2, Figure 7] The extended cold molecular gas detection in the re-analyzed ALMA data is at ~3-sigma significance, and the C1 H2 clump is at 2.4-sigma. The abstract's statement that 'hot and cold molecular gas [are detected] out to distances >10 kpc' leans on these marginal detections. Please report how many independent spatial apertures or spectral channels were searched, state whether any trial-factor correction was applied, and clearly separate robust detections from tentative ones in the summary.
minor comments (5)
  1. [Abstract vs Section 4.3] The companion offsets are quoted as ~0.4 and ~0.9 arcsec in the abstract but as ~0.8 and ~1.4 arcsec in Section 4.3 and Figure 10; these should be reconciled.
  2. [Figure 5 caption vs Section 4.2] The caption says C1 and C2 are ~0.8 and ~1.5 arcsec from cid_346, while the text says ~1.0 and ~2.0 arcsec; please make the distances consistent.
  3. [Section 5] The derivation of the H2 2.2477/2.1218 upper limit of 0.3 is not described; please state the aperture, spectral window, and noise prescription used to compute this limit.
  4. [Section 1] There is a typo in the sentence 'the hot molecular gas phase at traced by the ro-vibrational transitions' - 'at' should be 'as'.
  5. [Section 5, Maloney et al. estimate] The X-ray heating estimate is presented as 'likely' accounting for most of the observed flux, but the quoted expected range spans an order of magnitude (1e-18 to 1e-17 erg/s/cm^2); please clarify whether this is a rough consistency check or a quantitative inference, and propagate the uncertainty.

Circularity Check

0 steps flagged · score 1.0 of 10

No significant circularity; the hot gas temperature and mass are standard conversions from measured H2 line fluxes using external atomic data, with only minor non-load-bearing self-citations.

full rationale

The derivation chain is self-contained. T_exc is obtained from the measured 1-0 S(1)/1-0 S(0) flux ratio via the standard Boltzmann excitation equation (Eq. 1), and the hot H2 mass is obtained from the measured 1-0 S(1) flux, luminosity distance, and the LTE population fraction f(v=1,J=3) evaluated at that T_exc (Eq. 2). Both equations use external atomic data (Turner et al. 1977; Wolniewicz et al. 1998; Roueff et al. 2019) and literature prescriptions (Storchi-Bergmann et al. 2009; Riffel et al. 2023), not parameters fitted to cid_346. The thermal-excitation interpretation uses an independent 2-1 S(1)/1-0 S(1) upper limit and a Maloney et al. (1996) X-ray heating model as an external consistency check. The cold gas mass used for the hot-to-cold ratio is taken from Circosta et al. (2021) and Bertola et al. (2024); although these have overlapping authors, they are based on independent ALMA CO(3-2) observations, and the paper also re-analyses the archival ALMA data directly, so the citation is not circular evidence. The main caveats (single-LTE assumption, 2-1 S(1)/1-0 S(1) upper limit lying between thermal and fluorescent expectations, and discrepant line widths) are robustness limitations rather than circularity: the quantities are not defined in terms of each other. The score of 1 reflects minor self-citations in target characterization that are not load-bearing, not circular derivation.

Assumptions & free parameters 1 free parameters · 4 assumptions · 0 invented entities

The central H2 mass estimate rests on an LTE assumption for the level populations, on externally adopted CO conversion factors for the cold-gas comparison, and on the same-redshift assumption for the two NIRCam companions. One hand-chosen quantity, the extraction aperture radius, directly scales all reported fluxes and masses. No invented entities are introduced.

free parameters (1)
  • Spectral extraction aperture radii = 0.4 arcsec (central cid_346); 0.25 arcsec (C1 and C2)
    Fluxes and derived masses scale with the chosen aperture. Section 4.1 uses a 0.4 arcsec circular aperture for the nucleus, and Section 4.2 states that the 0.25 arcsec apertures for C1 and C2 were manually chosen to roughly match the extent of the emission.
assumptions (4)
  • domain assumption The H2 gas is optically thin and in LTE at a single excitation temperature, so Eq. 1 and the LTE population fraction f(v=1,J=3) in Eq. 2 are valid.
    Section 4.1 derives T_exc = 1100 K from two lines using Eq. 1, with the phrase 'assuming the H2 is in equilibrium'. The only fluorescent-versus-thermal diagnostic is an upper limit on H2 2.2477/2.1218 < 0.3 in Section 5.
  • domain assumption Cold molecular gas masses from CO(3-2) can be derived using local-universe conversion factors r31 = 0.59 and alpha_CO = 3.6.
    Used in Section 2 and Section 4.2; these factors come from prior literature and are not measured for cid_346. They set the denominator in the hot-to-cold gas mass ratio.
  • domain assumption The two NIRCam components Sa and Sb are at the same redshift as cid_346.
    Section 4.3 explicitly says 'we assume that Sa and Sb are at the same redshift as cid_346' before SED fitting; no spectroscopic redshift for the companions is presented.
  • domain assumption Object-free MRS regions are free of H2 emission and represent the residual instrumental response and fringing.
    Section 4.1 uses three object-free regions to confirm the line detections; if MRS fringing residuals vary spatially, the signal-to-noise estimates for faint extended lines could be affected.

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Cite this review

Pith. "Pith review of JWST MIRI/MRS observations of hot molecular gas in an AGN host galaxy at Cosmic Noon." pith.science (2026). https://pith.science/paper/XZU4UN34

@misc{pith2026250705354,
  author       = {Pith},
  title        = {Pith review of: JWST MIRI/MRS observations of hot molecular gas in an AGN host galaxy at Cosmic Noon},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/XZU4UN34}},
  note         = {Machine review of arXiv:2507.05354}
}
abstract

Active Galactic Nuclei (AGN) are believed to play a central role in quenching star formation by removing or destroying molecular gas from host galaxies via radiation-pressure driven outflows and/or radio jets. Some studies of cold molecular gas in galaxies at Cosmic Noon ($z\sim2$) show that AGN have less cold gas ($<$100 K) compared to mass-matched star-forming galaxies. However, cold gas could also be shock-heated to warmer phases, detectable via H$_{2}$ transitions in the rest-frame near- and mid-infrared spectra. The Medium Resolution Spectrograph (MRS) of the Mid-infrared Instrument (MIRI) aboard JWST has opened a unique window to observe these emission lines in galaxies at Cosmic Noon. We present the first detection of hot molecular gas in cid_346, an X-ray AGN at $z\sim2.2$, via the H$_{2}$ ro-vibrational transition at 2.12 $\mu$m. We measure a hot molecular gas mass of $\sim 8.0 \times 10^{5}$ M$_{\odot}$, which is $\sim 10^{5}-10^{6}$ times lower than the cold molecular gas mass. cid_346 is located in an environment with extended gas structures and satellite galaxies. This is supported by detection of hot and cold molecular gas out to distances $>$10 kpc in MIRI/MRS and ALMA data, respectively and ancillary NIRCam imaging that reveals two satellite galaxies at distances of $\sim$0.4 arcsec (3.3 kpc) and $\sim$0.9 arcsec (7.4 kpc) from the AGN. Our results tentatively indicate that while the CO(3-2)-based cold gas phase dominates the molecular gas mass at Cosmic Noon, H$_{2}$ ro-vibrational transitions are effective in tracing hot molecular gas locally in regions that may lack CO emission.

Figures

Figures reproduced from arXiv: 2507.05354 by the authors.

Figure 1
Figure 1. Top left panel shows the location of cid_346, at the top end of the star forming main sequence (at 𝑧 ∼ 2). The solid line shows the main sequence relation from Schreiber et al. (2015) with 0.3 dex error margins shown as dashed lines. The red and blue data points show the z∼2 AGN and star forming galaxies, respectively (e.g., Tacconi et al. 2018; Boogaard et al. 2020; Birkin et al. 2021; Bertola et al. 2024). The top… view at source ↗
Figure 2
Figure 2. The top panels show the [O iii] flux map (left) and the integrated spectrum covering the entire region of the [O iii] emission (right). The [O iii] is extended towards the SE of the AGN location (marked by black star) and its spectrum shows a prominent blue-wing, indicative of ionised outflows. The bottom panelsshow the ALMA CO(3-2) flux map (left) and the corresponding integrated spectrum (right). Further details a… view at source ↗
Figure 3
Figure 3. 1-0 S(1) and 1-0 S(0) detections in the central AGN, cid_346. The blue curve shows the data extracted from the MRS cubes, the red curve shows the single Gaussian models to the emission lines, along with local continuum, and the yellow shaded region shows the spectral window containing ∼95% (±2𝜎) of the emission line flux. The black dashed line shows the expected location of each line, based on the redshift of cid_34… view at source ↗
Figures from the paper (5 more)
Figure 4
Figure 4. Figure 4: 1-0 S(1) to 1-0 S(0) line ratio in cid_346 (yellow star) and low￾redshift Seyfert galaxies (blue circles) as a function of the bolometric lumi￾nosity. The error bars represent 1𝜎 uncertainties in the respective line ratios. Both studies consist of measurements from typ…
Figure 6
Figure 6. Figure 6: 1-0 S(1) detections in extended regions: the left panel shows spec￾trum from C1 and the right panel shows spectrum from C2 (see [PITH_FULL_IMAGE:figures/full_fig_p008_6.png]
Figure 7
Figure 7. Figure 7: The left panel shows a diffuse extended CO(3-2) emission towards the SE of cid_346 at (0,0) arcsec. The red contours show the CO emission at levels 3𝜎, 4𝜎 and 5𝜎. The spectrum extracted from the yellow circle, covering the extended CO emission, is shown in the right pa…
Figure 10
Figure 10. Figure 10: The background image in the left panel shows the ground-based [O iii] flux map from SINFONI observations (Kakkad et al. 2020), the middle panel shows the extended CO(3-2) channel map from ALMA observations from [PITH_FULL_IMAGE:figures/full_fig_p010_10.png]
Figure 11
Figure 11. Figure 11: Background image shows the 2.12 𝜇m flux map with 6.2 GHz radio contours from VLA A-array (Ilha et al.). erg s−1 cm−2 , for a ∼0.4 arcsec aperture, the same as the one used to extract the MRS spectrum from the central source in cid_346. Com￾paring this emergent flux wi…

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Pith tools

Reviewed August 6, 2026 · model on record in the stance chip above.