arxiv: 2604.18671 · v1 · submitted 2026-04-20 · 🌌 astro-ph.GA · astro-ph.HE

Recognition: unknown

GOALS-JWST: Resolved multi-phase molecular gas in IRAS 20551-4250 using JWST and ALMA

A. S. Evans, C. M. Lofaro, C. Ricci, D. Kakkad, D. Sanders, G. C. Privon, H. Inami, J. Kader, K. L. Larson, L. Armus, L. Barcos-Mu\~noz, L. Lenkic, M. Bianchin, M. Malkan, M. Sanchez-Garcia, N. Torres-Alba, P. N. Appleton, P. van der Werf, S. T. Linden, T. Bohn, T. B\"oker, T. Diaz Santos, T. S.-Y. Lai, V. Buiten, V. Charmandaris, V. U, Y. Song

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Pith reviewed 2026-05-10 04:09 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.HE

keywords ULIRGmolecular gasoutflowsJWSTALMAstar formationgalaxy mergerfeedback

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The pith

Molecular gas in IRAS 20551-4250 is dominated by cold CO with no outflows detected, leaving star formation unquenched by the observed ionised gas feedback.

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

The paper maps the warm and cold molecular gas phases across the central region of the nearby ULIRG IRAS 20551-4250 with JWST mid-infrared spectroscopy and ALMA CO data. Warm H2 shows excitation temperatures and spatial distribution consistent with heating by UV light from stars, while the cold molecular component traced by CO supplies more than 95 percent of the total gas mass and follows the disturbed kinematics of a late-stage merger. No molecular outflows appear in either phase, even though optical data show weak ionised gas outflows with low mass rates. The combined results indicate that current feedback has not removed the molecular reservoir or halted star formation.

Core claim

The molecular gas composition in IRAS20551-4250 is consistent with ongoing star formation in the host galaxy, with warm H2 rotational lines revealing tidal tails and UV-dominated heating, the CO-based cold component accounting for the vast majority of the mass, and velocity fields showing non-rotational motions matching the merger, while ionised outflows remain too weak to expel the molecular gas.

What carries the argument

Spatially resolved JWST/MIRI-MRS maps of warm H2 rotational transitions combined with ALMA CO imaging to trace excitation, mass distribution, and kinematics across multiple gas phases.

Load-bearing premise

The mid-infrared line ratios and excitation diagrams correctly attribute the warm gas heating to UV radiation from stars rather than shocks or AGN, and standard CO-to-H2 conversion factors apply uniformly across the observed region.

What would settle it

Detection of molecular outflows in CO or H2 with mass outflow rates comparable to or exceeding the star formation rate would show that feedback is expelling gas after all.

Figures

Figures reproduced from arXiv: 2604.18671 by A. S. Evans, C. M. Lofaro, C. Ricci, D. Kakkad, D. Sanders, G. C. Privon, H. Inami, J. Kader, K. L. Larson, L. Armus, L. Barcos-Mu\~noz, L. Lenkic, M. Bianchin, M. Malkan, M. Sanchez-Garcia, N. Torres-Alba, P. N. Appleton, P. van der Werf, S. T. Linden, T. Bohn, T. B\"oker, T. Diaz Santos, T. S.-Y. Lai, V. Buiten, V. Charmandaris, V. U, Y. Song.

**Figure 1.** Figure 1: The top panels show images from HST/ACS F814W (top left), JWST/NIRCam F277W (top middle) and JWST/MIRI F770W (top right) covering the full range of spatial scales of IR20551. The horizontal bar in all the top panels show the 10 kpc physical scale. The overlaid white circle, red rectangle, orange rectangle and blue rectangle in the top left image shows the ALMA, MIRI, NIRCam and MUSE coverage regions. The b… view at source ↗

**Figure 2.** Figure 2: Top left panel shows the median MRS image of IR20551 in Channel-3. The red and blue circles show the aperture of extraction for nuclear (R = 0.5 arcsec) and integrated spectra (R = 1.5 arcsec), respectively. The top right panel shows the full MRS spectra from all four channels from the nuclear (red) and integrated (blue) apertures. The nuclear aperture is offset by an arbitrary factor for better visualisat… view at source ↗

**Figure 3.** Figure 3: The nuclear (left) and integrated (right) MRS spectra of IR20551, with the total continuum model and PAH emission line fits from CAFE overlaid. The individual components from AGN, starburst, hot, warm and cold dust etc are not shown due to high degree of degeneracy between these different components. The CAFE model reproduces the overall mid-infrared continuum well, along with the PAH emission and silicate… view at source ↗

**Figure 4.** Figure 4: Rotational hydrogen lines (S(1) – S(8)) from the nuclear (solid red) and integrated (solid blue) spectra and respective single Gaussian fits (dashed lines). The rotational transitions do not show any asymmetry and are reproduced using a single Gaussian function, suggesting that there is no evidence for fast moving warm molecular gas associated with an outflow. S(6) line is affected by an absorption feature… view at source ↗

**Figure 5.** Figure 5: Maps showing the variation in the centroid (left panels), width (FWHM, middle panels) and flux (right panel) of the H2 rotational transitions, S(2) (top panels) and S(7) (bottom panels) as examples. The maps showcase the presence of two tidal tails in the central region of IR20551 - one towards the NE and other towards the SE. S(7), a higher excitation line, is covered in the lower channels of MRS, which h… view at source ↗

**Figure 6.** Figure 6: The grey curve in the top panel shows the extracted CO(2-1) spectra from the ALMA data cube (radius of aperture, R = 1.5 arcsec) and the blue curve overlaid shows the total multi-Gaussian model. The dashed red curves show the individual Gaussians. The vertical line shows the expected location of CO(2-1) line based on the redshift of IR20551. The bottom panel shows the residuals from the fit. The 𝑤80 parame… view at source ↗

**Figure 7.** Figure 7: CO(2-1) maps of IR20551: 𝑣50 which is equivalent of a centroid map is shown in the left panel, the middle panel shows the 𝑤80 map (equivalent of a FWHM map) and the right panel shows the flux map. Non-parametric measurements are shown here due to the double Gaussian fitting in CO(2-1) lines. The black star in the centre of the images mark the putative AGN location. The centroid, width and morphology mirror… view at source ↗

**Figure 8.** Figure 8: Top left panel shows the median MUSE image of IR20551 and the red circle shows the aperture of optical spectral extraction (R = 1.5 arcsec), similar to the aperture radii used for MRS integrated and ALMA CO(2-1) data. Top middle and right panels show the extracted MUSE spectra with emission line model fits, zoomed in on H𝛽, [O iii]𝜆𝜆4959, 5007 (middle panel), H𝛼 and [N ii]𝜆𝜆6549, 6585 (right panel). The ba… view at source ↗

**Figure 9.** Figure 9: Left panel shows the [O iii] 𝑣50 map and the right panel shows the [O iii] 𝑤80 map from two-Gaussian fits to VLT/MUSE data described in Sect. 3.3. The colour coding on the left panel shows [O iii] 𝑣50 values, ranging from -75 (blue) to 75 (red) km s−1 and the colour coding on the right panel shows [O iii] 𝑤80 values, ranging from ∼150 (blue) to ∼600 km s−1 . Neither maps show ordered motions, suggesting th… view at source ↗

**Figure 10.** Figure 10: Top panels: The left panel shows the [N ii]/H𝛼 map of IR20551 within the central 10 × 10 arcsec2 region and the right panel shows the corresponding [N ii]-BPT diagram ([O iii]5007/H𝛽 versus [N ii]6549/H𝛼). The colour coding shows the [N ii]6549/H𝛼 ratio, ranging from 0.35 (Dark Blue) to 0.9 (Red). The dashed line in the right panel indicates the line ratios for the most extreme (high-ionization) starburst… view at source ↗

**Figure 11.** Figure 11: Mid-infrared AGN diagnostics: Left panel: Flux ratio [Ne v]14.3/[Ne ii]12.8 versus PAH 6.2 𝜇m equivalent width. Red squares show AGNs (from Wu et al. 2009; Tommasin et al. 2010), blue diamonds show ULIRGs (Armus et al. 2007) and green circles show the location of starburst galaxies (Bernard-Salas et al. 2009). The location of IR20551 spectra from the two apertures, R = 0.5 arcsec and 1.5 arcsec, are shown… view at source ↗

**Figure 12.** Figure 12: Normalised [O iii]𝜆5007, H2 S(2), and CO(2–1) line profiles plotted on the same wavelength scale. The [O iii] line exhibits the largest velocity dispersion with 𝑤 [OIII] 80 ∼ 790 km s−1 . While the CO(2–1) profile shows mild asymmetry (see also [PITH_FULL_IMAGE:figures/full_fig_p012_12.png] view at source ↗

**Figure 13.** Figure 13: Top panels: Temperatures derived from the nuclear (top left) and integrated (top right) spectra. The nuclear spectrum is extracted from a 0.5 arcsec circular aperture, while the integrated spectrum is taken from a 1.5 arcsec aperture, both centred on the AGN. The plots illustrate a two-temperature model for the H2 transitions: a warm component at ≈500 K, modelled using the S(1)–S(3) lines, and a hot compo… view at source ↗

**Figure 14.** Figure 14: Top panel: The map in this plot shows the CO(2-1) flux distribution, same as the right panel in [PITH_FULL_IMAGE:figures/full_fig_p014_14.png] view at source ↗

**Figure 15.** Figure 15: are taken from Petric et al. (2018), based on a sub-sample of the parent GOALS galaxies from where IR20551 was selected. In Petric et al. (2018), warm gas masses are derived from integrated measurements of high-resolution Spitzer/IRS spectra, using the same methodology adopted in this paper. The cold molecular gas masses are drawn from integrated CARMA CO(1–0) observations Alatalo et al. (2024), who assum… view at source ↗

read the original abstract

Studying the content and distribution of molecular gas provides key insights into how feedback from Active Galactic Nuclei (AGN) and star formation influences galaxy evolution, since molecular gas is the primary fuel for star formation. Ultra-Luminous Infrared Galaxies (ULIRGs) are ideal candidates to study how AGN and/or starbursts affect the interstellar medium due to their intense AGN and star forming activity. We present spatially-resolved multi-phase molecular gas study of IRAS20551-4250, a nearby ($z=0.0429$) ULIRG, using JWST/MIRI-MRS and ALMA. Mid-infrared diagnostics do not rule out the presence of AGN in IRAS20551-4250. [OIII]$\lambda$5007 in VLT/MUSE data reveal ionised gas outflows with $w_{80}^{\rm [OIII]} \sim 790$ km s$^{-1}$ and $\dot{M}_{\rm out}^{\rm[OIII]}<0.01$ M$_{\odot}$ yr$^{-1}$. No outflows are observed in either molecular phases. JWST/MIRI-MRS data reveal several rotational transitions of warm H$_{2}$ (T$\sim500-1400$ K) within the central $\sim4\times4$ kpc$^{2}$ region. Excitation temperature maps suggest that the warm H$_{2}$ is primarily heated by UV radiation from the central source. The CO-based cold molecular component dominates the molecular gas mass, accounting for $>$95% of the total molecular gas mass. Warm H$_{2}$ maps show two tidal tails and the velocity centroid maps show disturbed, non-rotational motions and a systematic gradient across the field-of-view, similar to that of ALMA CO-based cold molecular gas and consistent with a late-stage merger. Together, our analysis indicate that the molecular gas composition in IRAS20551-4250 is consistent with ongoing star formation in the host galaxy and the outflows observed in ionised gas phase appear insufficient to expel the molecular gas or quench ongoing star formation.

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.

Desk Editor's Note private letter to a colleague

This paper gives a useful resolved view of warm and cold molecular gas in one ULIRG but the UV-heating claim needs tighter checks against shocks.

read the letter

The core result is straightforward: JWST/MIRI-MRS maps of several H2 rotational lines combined with ALMA CO show that the cold molecular component makes up more than 95% of the gas mass within the central 4 kpc, the warm H2 has excitation temperatures of 500-1400 K, and neither phase shows outflows while the ionised gas does at a very low rate. The kinematics are disturbed and match between phases, consistent with a late-stage merger and ongoing star formation rather than strong quenching. That combination of datasets on this specific object is new and the maps are presented clearly enough to be usable by others. The tidal features and velocity gradients are shown directly from the data, which is the kind of concrete observational anchor that helps when testing feedback models. The main soft spot is the heating attribution. The excitation diagrams are used to argue for UV radiation from the central source, but the system has non-rotational motions and is a merger, so shocks are a plausible alternative that can produce similar temperatures. The abstract does not describe quantitative comparisons to shock grids or chi-squared tests against PDR models, so the conclusion that the gas is consistent with star formation rests partly on that assumption. The ionised outflow upper limit is interesting but its value depends on the exact conversion and geometry choices in the MUSE analysis. This is the sort of paper that belongs in a reading group for people who work on ULIRG ISM and multi-phase outflows. The data products are solid enough that a referee should see it, even if the heating discussion needs more explicit model testing. I would send it to peer review.

Referee Report

3 major / 3 minor

Summary. The manuscript presents a spatially-resolved study of multi-phase molecular gas in the ULIRG IRAS 20551-4250 at z=0.0429 using JWST/MIRI-MRS for warm H2 rotational lines, ALMA for cold CO, and VLT/MUSE for ionized gas. Key findings include warm H2 temperatures of 500-1400 K within the central 4 kpc, excitation maps suggesting UV heating from the central source, cold molecular gas comprising over 95% of the total molecular mass, disturbed non-rotational kinematics consistent with a late-stage merger, no detected molecular outflows, and an ionized outflow with w80 ~790 km/s and mass rate <0.01 Msun/yr. The authors conclude that the molecular gas is consistent with ongoing star formation and that the observed outflows are insufficient to quench it.

Significance. If the attribution of H2 heating to UV radiation holds, this study offers important resolved insights into the multi-phase ISM in merging ULIRGs, demonstrating the persistence of a dominant cold molecular reservoir alongside limited ionized outflows, with implications for feedback and quenching models in galaxy evolution.

major comments (3)

[H2 excitation analysis] In the analysis of the H2 rotational lines and excitation temperature maps: the claim that warm H2 (T~500-1400 K) is primarily heated by UV radiation from the central source rests on excitation diagrams without a quantitative comparison (e.g., chi-squared or evidence ratios) to shock-heating models such as C-shocks. This is load-bearing for the central conclusion that the gas composition is consistent with ongoing star formation, especially given the late-stage merger kinematics and tidal features where mechanical heating is plausible.
[Outflow analysis] In the outflow rate derivation: the upper limit on the ionized outflow rate (<0.01 M_sun/yr) is reported without a full error budget or explicit discussion of assumptions on geometry, filling factor, and electron density used to convert the [OIII] w80 measurement. This directly affects the robustness of the claim that outflows are insufficient to expel the molecular gas or quench star formation.
[Molecular gas mass estimation] In the molecular gas mass budget: the statement that the CO-based cold component accounts for >95% of the total molecular gas mass assumes standard CO-to-H2 conversion factors without addressing potential spatial variations or merger-induced changes in the central 4 kpc region, which could impact the reported mass fractions and multi-phase composition.

minor comments (3)

The abstract states that mid-infrared diagnostics do not rule out AGN but does not list the specific diagnostics or line ratios used; this should be expanded in the main text for clarity.
[Figure captions] Figure captions for the excitation temperature and velocity maps lack explicit mention of beam sizes, resolution, or contour levels, hindering assessment of the spatial scales of features such as the tidal tails.
Minor notation inconsistencies appear in outflow rate symbols (e.g., dot{M} vs Mdot) and temperature units across sections; standardize for readability.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their thorough and constructive review of our manuscript. We address each major comment in detail below, providing clarifications and committing to revisions that enhance the robustness of our analysis while preserving the core conclusions regarding the multi-phase gas in IRAS 20551-4250.

read point-by-point responses

Referee: [H2 excitation analysis] In the analysis of the H2 rotational lines and excitation temperature maps: the claim that warm H2 (T~500-1400 K) is primarily heated by UV radiation from the central source rests on excitation diagrams without a quantitative comparison (e.g., chi-squared or evidence ratios) to shock-heating models such as C-shocks. This is load-bearing for the central conclusion that the gas composition is consistent with ongoing star formation, especially given the late-stage merger kinematics and tidal features where mechanical heating is plausible.

Authors: We appreciate the referee's emphasis on strengthening the heating mechanism attribution. Our excitation diagrams, derived from multiple H2 rotational transitions observed with JWST/MIRI-MRS, yield temperatures (500-1400 K) that align with expectations for UV-heated gas in photodissociation regions associated with star formation, and the spatial distribution correlates with the central source rather than extended tidal features. However, we acknowledge that a quantitative model comparison would better rule out contributions from C-shocks in the merger environment. In the revised manuscript, we will add a dedicated paragraph (or subsection) performing a simple comparison of observed line ratios to literature C-shock predictions (e.g., from models like those in Flower & Pineau des Forêts), including a qualitative assessment of fit quality. This will support our UV-heating interpretation while noting that the lack of molecular outflows reduces the likelihood of widespread shock heating. The main conclusion on ongoing star formation remains unchanged. revision: partial
Referee: [Outflow analysis] In the outflow rate derivation: the upper limit on the ionized outflow rate (<0.01 M_sun/yr) is reported without a full error budget or explicit discussion of assumptions on geometry, filling factor, and electron density used to convert the [OIII] w80 measurement. This directly affects the robustness of the claim that outflows are insufficient to expel the molecular gas or quench star formation.

Authors: We agree that expanding the outflow analysis will improve transparency and robustness. The current upper limit is derived from the [OIII] w80 ~790 km/s and luminosity using standard conversion methods, but we will revise the manuscript to include: a complete error budget propagating uncertainties from w80, line luminosity, and distance; explicit assumptions on outflow geometry (biconical with opening angle informed by MUSE morphology); a conservative filling factor of 0.01-0.1 with literature justification; and electron density (assumed 100-1000 cm^{-3}, with notes on [SII]-based estimates where available). Even under varied assumptions, the rate remains <0.01-0.1 M_sun/yr, reinforcing that ionized outflows are insufficient to quench the dominant molecular reservoir. This addition will directly address the concern. revision: yes
Referee: [Molecular gas mass estimation] In the molecular gas mass budget: the statement that the CO-based cold component accounts for >95% of the total molecular gas mass assumes standard CO-to-H2 conversion factors without addressing potential spatial variations or merger-induced changes in the central 4 kpc region, which could impact the reported mass fractions and multi-phase composition.

Authors: We thank the referee for noting this assumption. We adopted the standard Galactic X_CO for the ALMA CO(1-0) mass estimate, as is common for such studies, yielding the >95% cold fraction when combined with the independently derived warm H2 mass from JWST lines. In the revision, we will add a paragraph discussing merger/ULIRG-specific X_CO variations (typically factors of 0.2-1 times Galactic in central regions per literature), including a sensitivity test showing the cold fraction under reduced X_CO (e.g., by factors of 2-5). Even in the most conservative case, cold gas remains the dominant component (>85%), and the multi-phase conclusion is unaffected. We will also clarify that warm H2 mass is not reliant on X_CO. revision: partial

Circularity Check

0 steps flagged

No circularity: purely observational data analysis

full rationale

The manuscript reports direct JWST/MIRI-MRS and ALMA observations of line fluxes, constructs excitation temperature maps from measured rotational transitions of H2, applies standard CO-to-H2 conversion factors, and compares observed kinematics and mass budgets to expectations for ongoing star formation. No derivation reduces to a fitted parameter renamed as a prediction, no self-citation chain supports a load-bearing uniqueness claim, and no ansatz is smuggled in. Conclusions are interpretive summaries of the data products rather than tautological restatements of inputs.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

Based on abstract only; standard astrophysical assumptions for molecular excitation and mass conversion are invoked but not enumerated in detail.

axioms (2)

domain assumption Local thermodynamic equilibrium (LTE) for deriving excitation temperatures from H2 rotational lines
Required to produce the T~500-1400 K maps from MIRI-MRS data.
domain assumption Standard CO-to-H2 conversion factor applies across the observed region
Used to conclude that cold CO accounts for >95% of molecular gas mass.

pith-pipeline@v0.9.0 · 5843 in / 1331 out tokens · 34479 ms · 2026-05-10T04:09:52.231769+00:00 · methodology

discussion (0)

Reference graph

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