REVIEW 2 major objections 4 minor 61 references
Measuring metal sulfides in interstellar dust with PRIMA
T0 review · 2 major / 4 minor · reviewed 2026-08-05 · deepseek-v4-flash
Pith's one-line read The paper argues that PRIMA's FIRESS far-infrared spectrometer can detect the solid-state absorption bands of MgS and FeS in interstellar dust at 20–50 μm, potentially identifying the main reservoir of depleted sulfur.
desk verdict A useful, honest feasibility study for PRIMA metal-sulfide dust observations; the core math holds, but the MgS abundance derivation is wrong and the lack of error propagation makes the headline thresholds optimistic. read the letter →
The pith
A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.
The reading
What carries the argument
The central machinery is a one-hour absorption experiment built from synthesized dust opacity profiles. Opacities for pure and astrosilicate-mixed FeS and Mg_xFe1-xS are generated with the optool software using laboratory optical constants, smoothed to the expected R > 85 resolving power of FIRESS, and converted to optical depth through assumed mass column densities of FeS and MgS. The narrow FeS bands between 30 and 50 μm are the clean diagnostic: they survive mixing with astrosilicates nearly unchanged, so their detection robustly signals FeS dust, while the broad MgS band near 30 μm remains visible and falls within FIRESS's full 24–235 μm coverage.
What would settle it
Point PRIMA/FIRESS at a ~3 Jy low-mass protostar such as BHR 71 for one hour in low-resolution mode. The model predicts a ~30 mJy MgS absorption dip at 30 μm and a ~3 mJy FeS band series between 30 and 50 μm. If neither appears at 5σ, the assumed 50% FeS / 5% MgS sulfur fractions are too high.
Extended reading notes
Core claim
The paper's central claim is that PRIMA's FIRESS far-infrared spectrometer in low-resolution mode (R > 85) can detect the solid-state absorption bands of MgS and FeS at 20–50 μm against bright embedded sources. With 50% of cosmic sulfur in FeS and 5% in MgS, and an assumed hydrogen column density of 10^23 cm^-2, the predicted optical depths are about 0.01 at the MgS 30 μm peak and 10^-3 for the weakest FeS band. Against the 3 Jy continuum of the BHR 71 low-mass protostar, this translates to S/N ≈ 940 for the MgS band and S/N ≈ 90 for the FeS bands in one hour of integration. Generalized to arbitrary background brightness, a 5σ detection of the MgS band needs a source brighter than about 20 m
Load-bearing premise
The predicted band strengths rest on assuming that 50% of cosmic sulfur is locked in FeS dust and 5% in MgS dust along the observed lines of sight; if real clouds hold less sulfur in these minerals, the same one-hour observations would not reach S/N 5.
Editorial extensions
If this is right
- PRIMA will be able to measure solid-phase FeS and MgS column densities directly from one-hour absorption observations of bright young stellar objects, rather than relying on ice upper limits.
- The narrow FeS bands between 30 and 50 μm are robust against astrosilicate mixing, so their detection is a clean signature of FeS dust regardless of the assumed grain mixture.
- The MgS 30 μm band lies outside JWST's wavelength coverage, so PRIMA opens a practical far-infrared window for this carrier.
- Targeting sources across different extinction regimes would let astronomers map where sulfur locks into refractory sulfides, directly testing the sulfur depletion problem.
- Sulfur allotropes such as S8 are predicted to be undetectable with PRIMA (over 500 hours for 5σ), leaving metal sulfides as the most observable refractory sulfur reservoir.
Reading between the lines
- Because the predicted S/N scales linearly with the assumed sulfide mass fraction, the first nondetections with PRIMA would immediately bound the FeS fraction downward—even null results would constrain the sulfur reservoir.
- The same absorption technique could be applied to other far-infrared dust carriers by swapping the assumed opacities, turning PRIMA's low-resolution mode into a general interstellar mineralogy probe.
- If MgS and FeS are detected at the predicted levels, it would strengthen the case that gas-phase MgS and NaS seen toward the Galactic Center come from sputtered grain cores rather than gas-phase formation alone.
- The ~200 mJy threshold for FeS means only the brightest embedded protostars are accessible in one hour; fainter sources would require longer integrations, which could bias early results toward high-column, high-density lines of sight.
Signed reviews
Editorial analysis
A structured set of objections, weighed in public.
Referee Report
Summary. The paper assesses whether PRIMA's FIRESS low-resolution mode (R>85, 24–235 μm) can detect the solid-state absorption bands of FeS and MgS in interstellar dust toward bright low-mass protostars. Using laboratory optical constants and the optool package, the authors synthesize opacity profiles of FeS, Mg0.9Fe0.1S, and Mg0.1Fe0.9S, with and without 1:1 astrosilicate mixtures, smooth them to FIRESS resolution, and convert them to optical depths for adopted sulfide abundances and N(H)=10^23 cm^-2. For the BHR 71 YSO (3 Jy at 30 μm), they predict S/N~940 for the 30 μm MgS band and S/N~90 for the FeS bands in 1 h, and generalize to 5σ thresholds of ~20 mJy (MgS) and ~200 mJy (FeS) for 1 h. The paper concludes that PRIMA can constrain the main refractory reservoir of interstellar sulfur.
Significance. If the abundance assumptions hold, this is a valuable and timely feasibility study. It correctly identifies that FIRESS's low-resolution mode spectrally resolves the key FeS/MgS bands, that the 30 μm MgS band is inaccessible to JWST, and that PRIMA offers orders-of-magnitude better sensitivity than ISO at these wavelengths. The calculations are forward, reproducible, and based on publicly available opacity tools and databases, and the paper explicitly quantifies the impact of astrosilicate mixing. The main result—a one-hour absorption experiment against bright YSOs—would directly bear on the sulfur depletion problem and the sulfur budget of planet-forming material. However, the central detectability thresholds inherit large, unquantified uncertainty from the assumed sulfide fractions and hydrogen column, and one abundance derivation is arithmetically incomplete as stated.
major comments (2)
- [§2, MgS abundance paragraph] The derivation of the MgS abundance is not supported as written. The text states that 6.6×10^-7 is 'derived from the gas-phase abundance of MgS ... and a typical depletion factor of 100.' A gas-phase abundance of a few ×10^-13 times 100 gives ~10^-11, not 6.6×10^-7. The quoted value is simply 5% of the adopted S/H=1.32×10^-5. If the intended calculation is (gas-phase abundance / S/H2) × depletion factor, that normalization must be stated explicitly; otherwise the paper's claim that 6.6×10^-7 is a lower limit anchored to the G+0.693 detection is not reproducible. This matters because the MgS S/N and the 20 mJy threshold in Fig. 5 scale linearly with this abundance.
- [§2–§3 and Fig. 5] The detectability thresholds are quoted without any error budget. The FeS abundance is fixed at 50% of cosmic sulfur with a cited literature range of 30–90%, and N(H)=10^23 cm^-2 is assumed without discussion of typical variations toward low-mass protostars. The 5σ threshold for FeS scales directly with the product f(FeS)×N(H). Combining the lower ends f(FeS)=0.3 and N(H)=3×10^22 cm^-2 lowers the optical depth by a factor of ~5.6 and raises the threshold from ~200 mJy to ~1.1 Jy. The BHR 71 example (3 Jy) would still be detected, but the abstract's 'sources brighter than 200 mJy' claim is not robust. Please provide a range of thresholds under the stated literature range and a plausible N(H) range, or explicitly qualify the central claim.
minor comments (4)
- [§3, MgS intensity calculation] The text writes 'τMgS=-0.01' and uses Iabs = Icont×(1 - e^{τMgS}). For an absorption feature τ is positive and the formula should be 1 - e^{-τ}; the final numerical result is the same, but the sign convention is confusing and should be corrected for consistency with the definition τ=ln(F0/F) given two paragraphs earlier.
- [Abstract and §2] The abstract says 'sources brighter than 200 mJy' for both MgS and FeS, but the body gives 20 mJy for the MgS band. This is technically correct if the goal is to detect both bands simultaneously, but it may mislead readers interested only in MgS. Rephrase for clarity.
- [Typos] Minor language errors: 'Infared' (Introduction), 'fearures' (§2), 'Unnion' (§7), 'revieved' (author biography). A careful proofread is needed.
- [References [46] and [58]] Both are listed as 'FIRESS, JATIS (2005)' with different author names; at least one entry appears incomplete or misattributed. Please provide full bibliographic details.
Circularity Check
No significant circularity: predictions are forward calculations; self-citations are motivational, not load-bearing.
full rationale
The paper's derivation chain is a forward sensitivity estimate: synthesized dust opacities from external laboratory data (optool, JPDOC; refs [53-55]) are multiplied by assumed mass column densities (50% of cosmic S in FeS, 5% in MgS, N(H)=1e23 cm^-2) to obtain optical depths; those optical depths are converted to absorption intensities against the BHR 71 SED and divided by the quoted FIRESS 5-sigma sensitivity (0.16 mJy in 1 h). No parameter is fitted to the predicted S/N, no equation defines an input in terms of the predicted output, and no uniqueness/ansatz is imported from the authors' prior work to force the result. The self-citations ([40] for gas-phase MgS/NaS, [12] for sulfur depletion, [60] for the BHR 71 SED) are motivation or external templates; the MgS abundance of 6.6e-7 is an assumption, not a fitted value. The paper does contain a numerically inconsistent derivation for that abundance: Section 2 states the value 'is derived from the gas-phase abundance of MgS estimated toward the Galactic Center ... and a typical depletion factor of 100,' but few x 10^-13 times 100 is ~10^-11, not 6.6e-7. This is a correctness/support weakness in a load-bearing input, not a circular reduction: the abundance is not defined in terms of the predicted absorption-band S/N. The 200 mJy/1 h FeS threshold scales linearly with the assumed FeS fraction and N(H), but that is ordinary sensitivity to assumptions, not circularity. Accordingly the circularity score is low.
Assumptions & free parameters
free parameters (4)
- Fraction of sulfur locked in FeS =
0.5 (50%)
- Fraction of sulfur locked in MgS =
0.05 (5%)
- Hydrogen column density N(H) =
10^23 cm^-2
- FeS/MgS to astrosilicate mixing ratio =
1:1 by mass
assumptions (5)
- domain assumption Laboratory optical constants for FeS (Henning & Stognienko 1996) and Mg_xFe_1-xS (Begemann et al. 1994) accurately represent interstellar sulfide dust
- domain assumption MgS and FeS exist as dust in the ISM in sufficient abundance
- domain assumption MRN grain size distribution (a^-3.5, 0.1-1 μm) applies to the absorbing grains
- domain assumption The YSO BHR71 SED model and its 3 Jy continuum at 30 μm are representative of low-mass protostars
- standard math Radiative transfer relation τ = ln(F0/F) describes absorption
Cite this review
Pith. "Pith review of Measuring metal sulfides in interstellar dust with PRIMA." pith.science (2026). https://pith.science/paper/NEPQ5S2R
@misc{pith2026250902067,
author = {Pith},
title = {Pith review of: Measuring metal sulfides in interstellar dust with PRIMA},
year = {2026},
howpublished = {\url{https://pith.science/paper/NEPQ5S2R}},
note = {Machine review of arXiv:2509.02067}
}
abstract
Sulfur is known to undergo severe depletion when moving from diffuse clouds to the denser regimes of the interstellar medium in molecular clouds. The form in which sulfur gets depleted onto dust grains, however, remains a mystery. One possibility is that sulfur gets locked in interstellar dust in the form of sulfide minerals. Recently, metal sulfides such as NaS and MgS have been detected in a shocked molecular cloud in the Galactic Center, suggesting that these molecules could represent an important reservoir of sulfur in dust grains. In this contribution, we discuss the prospect of observing metal sulfides such as MgS and FeS in absorption experiments carried out with the FIRESS instrument onboard PRIMA using its low resolution observing mode. Our estimates show that the molecular bands of MgS and FeS found between 20 and 50 ${\mu}$m could be detected in absorption with S/N ${\geq}$ 5 for sources brighter than 200 mJy in just 1 h of observing time against low-mass protostellar objects. This science case, therefore, has the potential to unveil the main reservoir of sulfur in interstellar dust, constraining in what form sulfur is incorporated into minor bodies of our solar system.
Reference graph
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Reviewed August 5, 2026 · model on record in the stance chip above.
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