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JOYS: The [D/H] abundance derived from protostellar outflows across the Galactic disk measured with JWST

T0 review · 4 major / 4 minor · reviewed 2026-08-10 · deepseek-v4-flash

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Pith's one-line read JWST observations of protostellar outflows show gas-phase deuterium varying by a factor of four and running 2–4 times below predicted total D/H, suggesting much of the Galaxy's deuterium is locked in carbonaceous dust.

desk verdict New JWST/MIRI HD census with a load-bearing aperture-filling problem that its own maps contradict. read the letter →

arxiv 2501.02085 v1 pith:LKXK5O6S submitted 2025-01-03 astro-ph.GA astro-ph.SR

L. Francis , E. F. van Dishoeck , A. Caratti o Garatti , M. L. van Gelder , C. Gieser , H. Beuther , T.P. Ray L. Tychoniec , P. Nazari S. Reyes P. J. Kavanagh
show 3 more authors
P. Klaassen M. Güdel T. Henning
This is my paper · ORCID
classification astro-ph.GAastro-ph.SR
keywords astrochemistrystars:formationGalaxy:abundancesISM:jetsandoutflowsinfrared:ISMdeuteriumabundanceprotostellarJWSTMIRI/MRS
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 reports JWST mid-infrared measurements of the gas-phase deuterium-to-hydrogen ratio in protostellar outflows, obtained from H$_2$ and HD rotational lines observed with MIRI/MRS toward ten young stellar objects at Galactocentric radii from 4 to 11 kpc. Its central finding is that gas-phase [D/H] varies by up to a factor of four even among low-mass sources formed from gas expected to share nearly the same total deuterium abundance, and that detected values and useful upper limits mostly sit at or below about $1.0\times10^{-5}$, a factor of 2–4 below the total [D/H] inferred from local ultraviolet absorption lines and predicted by Galactic chemical evolution models. The authors conclude that these observations do not trace the total deuterium reservoir, and propose that a substantial part of the Galaxy's deuterium is locked up in carbonaceous dust grains, released only where shocks destroy the grains. A sympathetic reader would care because the result turns protostellar outflows into a new test bed for deuterium depletion and, with modelling, a possible probe of Galactic chemical evolution.

What carries the argument

The analysis rests on rotation diagrams built from the rotational lines H$_2$ S(1)–S(8) and HD R(4)–R(9) detected with the JWST MIRI/MRS medium-resolution spectrometer. For optically thin, LTE gas, plotting $\ln(N_u/g_u)$ against $E_u/k$ gives the column density from the intercept and the excitation temperature from the slope, and the ratio $N_{\rm HD}/(2N_{\rm H_2})$ yields [D/H]. The H$_2$ diagrams are fitted with a warm plus hot component and an ortho-to-para ratio correction, the same extinction correction derived from the H$_2$ S(1)–S(4) lines is applied to HD, and the LTE [D/H] is multiplied by 2.45 to account for non-LTE excitation and for chemical conversion of HD to atomic D, following the cited Orion outflow analysis. The fixed 1-arcsecond extraction aperture is assumed to be equally filled by H$_2$ and HD, so the ratio is taken to be independent of source size.

What would settle it

Re-extract the spectra with apertures matched to the HD-bright knots instead of a fixed 1-arcsecond aperture and check whether [D/H] climbs toward the local-disk value; if it does, the low values are a filling-factor artefact rather than dust depletion. Alternatively, observe a supernova remnant with MIRI/MRS and test whether complete grain destruction raises gas-phase [D/H] to the level predicted by Galactic chemical evolution models.

Watch

Extended reading notes

Core claim

On the paper's own terms, the discovery is that gas-phase [D/H] derived from HD and H$_2$ rotation diagrams in protostellar outflows is systematically low and variable: detected values run from about $0.12\times10^{-5}$ to $2.27\times10^{-5}$ after the standard correction, with a factor-of-four spread among low-mass sources that cannot be explained by astration, and most measurements fall a factor of 2–4 below the total [D/H] expected from Galactic chemical evolution. HD emission is concentrated in the same high-velocity jet knots and bow shocks as high-excitation H$_2$, [S I], and [Fe I] lines, and in the HH 211 outflow the inner-jet positions with higher gas-phase iron also show higher [D/H]; this spatial pattern is the paper's tentative evidence that deuterium sequestered in dust returns to the gas when shocks destroy grains. The paper concludes that rotational-line observations of outflows are sensitive only to gas-phase deuterium, not the total reservoir, and that significant depletion onto carbonaceous dust is the plausible explanation.

Load-bearing premise

The load-bearing premise is that H$_2$ and HD emission fill the same 1-arcsecond extraction aperture to the same degree, so their column-density ratio is unaffected by source size; if HD is actually more compact than H$_2$, the derived [D/H] is systematically low and the scatter between positions could be partly artificial.

Editorial extensions

If this is right

  • Most gas-phase [D/H] values from this paper and earlier molecular-line work sit at or below $1.0\times10^{-5}$, so any observationally grounded estimate of total deuterium in the disk must budget for deuterium hidden in dust.
  • Because the spatial pattern in HH 211 ties higher [D/H] to positions with higher gas-phase iron, stronger shocks that destroy more dust should show systematically higher gas-phase [D/H] than quiescent outflow gas.
  • The detection at 11 kpc and the constraining upper limits in the inner Galaxy mean that, once depletion is modelled, JWST can sample [D/H] across the Galactic disk rather than only in the local neighbourhood.
  • The 2.45 correction for non-LTE excitation and chemical conversion is applied to every value; without it the discrepancy with Galactic chemical evolution models would be even larger.

Reading between the lines

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

  • An untested consequence of the shared-solid-angle assumption is that any difference in how fully H$_2$ and HD fill the aperture translates directly into an offset in [D/H]; re-extracting on apertures matched to the HD knots would test whether part of the factor-of-four scatter is spatial resolution rather than dust depletion.
  • If deuterium depletion onto carbonaceous grains is real, the low [D/H] values from ultraviolet H I/D I and D I/O I absorption may reflect the same grain reservoir, which would change the reading of the local-disk abundance debate.
  • A clean extension would be MIRI/MRS observations of a supernova remnant, where complete grain destruction should push gas-phase [D/H] up toward the Galactic chemical evolution prediction; the paper notes an earlier HD detection in such a remnant.
  • The strong correlation between HD R(6) line flux and high-excitation H$_2$ and [S I] suggests that HD could serve as a tracer of dust-destructive shocks, making deeper [D/H] maps a way to map dust processing across an outflow.
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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 / 4 minor

Summary. The paper uses JWST/MIRI MRS observations of ten protostellar outflows (five low-mass, five high-mass) to measure gas-phase [D/H] from mid-IR H2 and HD rotational lines. It extracts 1"-radius aperture spectra, builds integrated line maps, fits two-temperature H2 rotation diagrams and single-temperature HD rotation diagrams, applies extinction and ortho-to-para corrections, and multiplies the derived LTE [D/H] by a correction factor for non-LTE excitation and chemical conversion taken from Bertoldi et al. 1999. The key results are that [D/H] varies by up to a factor ~4 among the low-mass sources and that most measured values are ~(0.1-1.8) x 10^-5, i.e. a factor 2-4 below Galactic chemical evolution predictions and below local UV absorption values. The authors interpret the scatter and low values as evidence for deuterium depletion onto carbonaceous dust grains, possibly with release in shocks, and report tentative support from enhanced [D/H] where gas-phase Fe is enhanced in HH 211.

Significance. The observational material is valuable: this is one of the first JWST studies to map HD emission in protostellar outflows across Galactocentric radii of 4-11 kpc, and the paper provides full tabulated line fluxes and rotation-diagram fit parameters that will be useful to the community. If the derived [D/H] values are robust, the conclusion that molecular-line measurements trace gas-phase rather than total deuterium would be an important constraint for Galactic chemical evolution studies and for the deuterium-depletion debate. The strengths of the paper include a diverse sample, careful Gaussian line fitting, and explicit handling of extinction and ortho-to-para corrections. However, the central quantitative claims rest on the assumptions that H2 and HD fill the same aperture and that the warm H2 component is the correct denominator for the HD column; neither assumption is established by the data as presented, and the manuscript contains an internal contradiction in the HH 211 trend that is used to support the depletion interpretation.

major comments (4)
  1. [§3.3] The aperture-filling assumption is load-bearing. The text states that 'the assumed emission solid angle is the same for both H2 and HD and thus there is no impact on any column density ratios or the derived [D/H]'. This is only true if H2 and HD have the same spatial extent. The integrated-line maps (Figs. 1, 2, C.1-C.8) show HD concentrated in bright knots and bow shocks, while H2 emission is extended over the outflow cavities. For a compact HD source with true solid angle Ω_HD < Ω_ap, converting the measured flux to intensity as F/Ω_ap underestimates I_HD, and hence N_HD, by a position-dependent factor Ω_HD/Ω_ap, while the more extended H2 suffers less dilution. The resulting [D/H] is therefore systematically low by a source- and position-dependent factor, which can produce both the factor-of-4 scatter and the low absolute values without any real variation in gas-phase D/H. This issue must be addressed, for example by measuring the emitting solid angles of HD and H2 separately, by restricting the analysis to a common compact region, or by propagating the beam-dilution ratio as a correlated systematic uncertainty on every [D/H] value.
  2. [§3.4 and Fig. 6] The use of the warm H2 column as the denominator is not justified for the gas traced by HD. [D/H] is computed as 0.5 N_HD/N_warm, where N_warm corresponds to the 400-900 K H2 component determined from S(1)-S(4). However, the flux correlations in Fig. 6 show that HD R(6) is most strongly correlated with the high-excitation H2 S(7) line (ρ=0.98) and less with S(1) (ρ=0.79), indicating that the HD emission traces the compact hot component rather than the extended warm component. If the HD-bearing gas is not well mixed with the warm gas used in the denominator, the derived ratio is not a measure of D/H in a single gas parcel and will vary with the local temperature structure. Please derive [D/H] also using the hot H2 component or otherwise demonstrate that the warm H2 column is the appropriate reservoir for the HD traced by the observed R(4)-R(6) transitions.
  3. [§4, §4.1, and Table 2] The HH 211 trend used to support the dust-depletion interpretation appears to be contradicted by the tabulated values. The text states that in HH 211 [D/H] is 'robustly lower in the bow-shock positions (apertures 1-3) than the jet positions (apertures 4-6)', and later that the data are consistent with an 'increased [D/H] in the inner jet (apertures 4-6) relative to the bow-shocks (apertures 1-3)'. Table 2 lists detected values of [D/H] = (1.30±0.49, 1.74±0.14, 1.78±0.47) x 10^-5 for apertures 1-3, while apertures 4-6 are upper limits that are mostly lower. This is the opposite trend to the one stated in the text and abstract. Please verify the aperture classification and either correct the text/abstract or explain how the stated trend is obtained.
  4. [§3.4, Table 2, and Fig. 5] The correction factor for non-LTE excitation and chemical conversion is both internally inconsistent and applied without a propagated uncertainty. The text says the LTE [D/H] estimates are multiplied by a factor of 2.45, whereas the Table 2 caption and Fig. 5 caption state a factor of 2.54. More substantively, the factor is imported from Bertoldi et al. (1999) for the Orion OMC-1 outflow, where the exact value depends on shock density, temperature, and dissociation fraction. Applying a single factor to all sources and positions sets the absolute scale for the claim that the observed [D/H] is a factor of 2-4 below GCE predictions. The expected spread of the correction factor should be propagated into the [D/H] uncertainties, or at least a plausible range should be quoted alongside the central values.
minor comments (4)
  1. [Summary bullet, §6] The bullet states that HD column densities are '∼ 105 orders magnitude smaller' than H2; this should read 'five orders of magnitude'.
  2. [Abstract and Introduction] The phrase 'polycyclic aromatic hydrocarbons' is misspelled as 'polcyclic aromatic hydrocarbons' in the Introduction; please correct the typo.
  3. [Throughout] There are several instances of broken spacing such as 'e ffect' and 'V oort' that should be corrected in the final typeset version.
  4. [Fig. 5 and Table 2] The correction factor is quoted as 2.45 in the main text and 2.54 in the table and figure captions; the inconsistency should be resolved in revision.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the [D/H] values are measured from independent H2 and HD rotation-diagram fits, with external correction factors and external benchmarks.

full rationale

The paper's derivation chain is self-contained in the sense required by the circularity audit: [D/H] is defined as (1/2) N_HD/N_H2, where N_HD and N_H2 come from separate LTE rotation-diagram fits to HD R(4)-R(9) and H2 S(1)-S(8) line fluxes. No parameter is fitted to the derived [D/H] itself, and no equation reduces the conclusion to its inputs by construction. The 2.45 correction factor for non-LTE excitation and chemical conversion of HD is imported from Bertoldi et al. (1999), an independent external study, not fitted to the present data; the paper explicitly notes the factor's sensitivity to shock conditions and treats it as a systematic correction. The aperture-filling assumption in Sect. 3.3 ('we assume that the H2 or HD emission fills the aperture' and 'the assumed emission solid angle is the same for both H2 and HD') makes the solid angle cancel in the column-density ratio, which is a modeling assumption that can bias the absolute ratio if violated, but this is a systematic observational uncertainty, not a circular step: the claimed factor-of-4 scatter is a measurement outcome, not a quantity defined to equal the fit. Comparisons with Galactic chemical evolution models, UV absorption-line values, and previous ISO measurements are external benchmarks rather than inputs to the derivation. Self-citations to JOYS data-reduction papers and previous target papers are data provenance and do not carry the load-bearing argument. The paper's own caveats about depletion, shock conditions, and the need for further modeling are acknowledged limitations, not circularity. Therefore the circularity score is 0.

Assumptions & free parameters 9 free parameters · 5 assumptions · 0 invented entities

The paper introduces no new entities. It relies on a set of fitted line excitation parameters, one adopted Orion-based correction factor, and several domain assumptions about LTE, molecular fraction, source filling, and the correspondence between HD and warm H2 emission. The equal-filling assumption is the most fragile because the paper's own maps contradict it.

free parameters (9)
  • AK extinction = 1.1 to 9.3 mag
    Fitted to H2 S(1) to S(4) intensities to correct line fluxes for extinction; uncertainty propagated into D/H.
  • H2 warm component column density N_warm = 1.0e19 to 3.8e21 cm^-2
    Two-temperature LTE fit to H2 rotation diagram; used as denominator in D/H.
  • H2 warm temperature = 395 to 900 K
    LTE temperature of the warm component from the two-temperature fit.
  • H2 hot component column density N_hot = 1.5e16 to 3.5e19 cm^-2
    Second LTE component added to account for high-J H2 lines.
  • H2 hot temperature = 1160 to 3000 K, often at fit limit
    LTE temperature of the hot component; poorly constrained in several apertures.
  • ortho-to-para ratio OPR = 1.02 to 3.00
    Additional parameter in H2 rotation diagram fits to correct odd-J suppression.
  • HD column density = 5.1e14 to 3.8e15 cm^-2 for detections
    Single-temperature LTE fit to HD rotation diagram; upper limits derived for non-detections.
  • HD temperature = 472 to 1694 K
    Single-temperature LTE fit to HD lines; values are intermediate between warm and hot H2 components.
  • correction factor for non-LTE and chemical conversion = 2.45 (text) / 2.54 (Table 2 and Fig. 5)
    Adopted from Bertoldi et al. 1999 and applied to all LTE D/H values; no uncertainty is propagated, and the paper uses two different values for the same factor.
assumptions (5)
  • domain assumption LTE and optically thin line emission for H2 and HD
    Section 3.3 assumes LTE and optically thin emission for the rotation diagram analysis; non-LTE corrections are borrowed from Bertoldi et al. 1999 but are applied globally.
  • domain assumption H2 and HD emission fill the extraction aperture equally
    Section 3.3 states this assumption and claims it has no impact on column density ratios, but the integrated maps show HD concentrated in knots while H2 is more extended.
  • domain assumption Outflow gas is fully molecular except for a small atomic jet core
    Section 3.4 uses this to set [D/H] = 0.5 * N_HD / N_H2.
  • domain assumption The Orion OMC-1 correction factor applies to all sources and shock conditions
    Section 3.4 applies a single factor of 2.45 or 2.54 to all LTE D/H values; the authors note it is approximately constant, but source-by-source variation is not modeled.
  • domain assumption HD rotational lines trace the same gas as the warm H2 component
    Section 3.3 and 3.4 compare HD column density to the warm H2 column density, although HD excitation temperatures are intermediate between the warm and hot H2 components.

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Cite this review

Pith. "Pith review of JOYS: The [D/H] abundance derived from protostellar outflows across the Galactic disk measured with JWST." pith.science (2026). https://pith.science/paper/LKXK5O6S

@misc{pith2026250102085,
  author       = {Pith},
  title        = {Pith review of: JOYS: The [D/H] abundance derived from protostellar outflows across the Galactic disk measured with JWST},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/LKXK5O6S}},
  note         = {Machine review of arXiv:2501.02085}
}
abstract

The total deuterium abundance [D/H] in the universe is set by just two processes: the creation of deuterium in Big Bang Nucleosynthesis at an abundance of [D/H]$=2.58\pm0.13\times10^{-5}$, and its destruction within stellar interiors. Measurements of the total [D/H] abundance can potentially provide a probe of Galactic chemical evolution, however, most measurements of [D/H] are only sensitive to the gas-phase deuterium, and the amount of deuterium sequestered in carbonaceous dust grains is debated. With the launch of JWST, it is now possible to measure the gas-phase [D/H] at unprecedented sensitivity and distances through observation of mid-IR lines of H$_2$ and HD. We employ data from the JWST Observations of Young protoStars (JOYS) program to measure the gas-phase [D/H] abundance with a rotation diagram analysis towards 5 nearby low-mass and 5 distant high-mass protostellar outflows. The gas-phase [D/H] varies between low-mass sources by up to a factor of $\sim4$, despite these sources likely having formed in a region of the Galactic disk that would be expected to have nearly constant total [D/H]. Most measurements of gas-phase [D/H] from our work or previous studies produce [D/H] $\lesssim 1.0\times10^{-5}$, a factor of $2-4$ lower than found from local UV absorption lines and as expected from Galactic chemical evolution models. The variations in [D/H] between our low-mass sources and the low [D/H] with respect to Galactic chemical evolution models suggest that our observations are not sensitive to the total [D/H]. Significant depletion of deuterium onto carbonaceous dust grains is a possible explanation, and tentative evidence of enhanced [D/H] towards shock positions with higher gas-phase Fe abundance is seen in the HH 211 outflow. Deeper observations of HD and H$_2$ in shocked environments and modelling of dust-grain destruction are warranted to test for the effects of depletion.

Figures

Figures reproduced from arXiv: 2501.02085 by the authors.

Figure 1
Figure 1. Integrated line intensity maps for HH 211 of various lines and the continuum at 17 µm shown with a logarithmic stretch. The maps have been smoothed to a common resolution of 1′′, shown by the white circle in the bottom-left. Apertures used for spectral extraction are shown by the green circles. An index for each aperture is provided in the top-left panel. The coordinates of the aperture centers can be found in Table… view at source ↗
Figure 2
Figure 2. Same as [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Spectral line fits for H2 (top two rows), HD (rows 3 and 4) , and the [S I], [Fe I], and [Fe II] atomic lines (rows 4 and 5) for HH 211 aperture 8. The line flux (shaded blue region) is determined by the simultaneous fit of a Gaussian profile and a first order polynomial to represent the continuum. the rest-frame wavelength of each spectral line is shown by a dashed grey line, and non-detections are shown without a … view at source ↗
Figures from the paper (4 more)
Figure 4
Figure 4. Figure 4: Rotational diagrams for the detected H2 (top row) and HD (bottom row) transitions in IRAS 23385+6053 aperture 1 and HH 211 aperture 8. Corrections for extinction and an ortho-to-para ratio < 3 have been applied (see text and App. F). the lowest column density upper lim…
Figure 5
Figure 5. Figure 5: Comparison of [D/H] abundance ( [PITH_FULL_IMAGE:figures/full_fig_p010_5.png]
Figure 6
Figure 6. Figure 6: Correlations between the extinction corrected flux of the HD R(6) line measured in all apertures for our sample with the extinction corrected flux of various atomic and H2 lines. The line flux is related to the line intensity by a constant factor of the aperture solid …
Figure 7
Figure 7. Figure 7: [D/H] as a function of Galactocentric radius based on our HD and H2 rotational line measurements within JOYS (squares), other rotational line values from ISO (circles) (Wright et al. 1999; Bertoldi et al. 1999), and local Galactic disk values from UV absorption lines (…

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Pith tools

Reviewed August 10, 2026 · model on record in the stance chip above.