The CRIMSON survey I: super-stellar SiO in the directly imaged companion TWA 5 B from high-resolution M-band spectroscopy

Jayne L. Birkby; Luke T. Parker; Matteo Brogi; Siddharth Gandhi; Sophia R. Vaughan; Vatsal Panwar; Vivien Parmentier

REVIEW 2 major objections 1 minor 299 references

The CRIMSON survey I: super-stellar SiO in the directly imaged companion TWA 5 B from high-resolution M-band spectroscopy

T0 review · 2 major / 1 minor · reviewed 2026-06-28 · grok-4.3

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Pith's one-line read Direct detection of gaseous SiO reveals super-stellar silicon abundance in the atmosphere of TWA 5 B.

desk verdict Solid SiO detection in TWA 5 B but the super-stellar Si/H and no-cloud claim rest on retrieval assumptions that the abstract leaves untested. read the letter →

arxiv 2606.03824 v1 pith:OCGKFCHK submitted 2026-06-02 astro-ph.EP astro-ph.SR

Luke T. Parker , Jayne L. Birkby , Siddharth Gandhi , Vivien Parmentier , Vatsal Panwar , Matteo Brogi , Sophia R. Vaughan This is my paper · ORCID

classification astro-ph.EPastro-ph.SR

keywords directlyimagedexoplanetsSiOdetectionatmosphericretrievalrefractoryelementscoreaccretionTWA5Bhigh-resolutionspectroscopyexoplanetformation

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

The paper presents the first results from the CRIMSON survey by detecting strong gaseous SiO absorption in the directly imaged companion TWA 5 B using high-resolution CRIRES+ M-band spectroscopy. This provides access to the refractory silicon content, which is measured alongside strong detections of the volatile species CO and H2O. The retrieved SiO abundance is high enough to imply that magnesium-silicate clouds have not condensed in significant amounts, so nearly all atmospheric silicon remains in the gas phase. Combining these measurements yields a stellar C/O ratio but a super-stellar Si/H ratio of 1.41, with marginally sub-stellar O/Si and C/Si. These volatile-to-refractory ratios point to formation either by core accretion beyond the CO snowline or by gravitational instability followed by substantial solid enrichment.

What carries the argument

High-resolution M-band spectroscopy of the ro-vibrational band head of SiO at 4 μm, combined with atmospheric retrieval of volume mixing ratios for SiO, CO, and H2O.

What would settle it

An independent measurement showing substantially lower gas-phase SiO or direct evidence of magnesium-silicate cloud particles that have depleted the silicon would falsify the super-stellar Si/H ratio and the no-cloud-condensation claim.

Watch

Extended reading notes

Core claim

We report the strong detection of gaseous SiO (S/N = 7.5) in TWA 5 B with an atmospheric abundance of log(SiO) = −3.56+0.42−0.32 VMR. The high retrieved SiO abundance implies the absence of significant magnesium-silicate cloud condensation, and thus the atmospheric silicon abundance is contained almost entirely within the observed gas phase SiO. Using the detection of refractory silicon together with strong detections of CO (S/N = 9.1) and H2O (S/N = 18.8), we measure a stellar C/O and a marginally sub-stellar O/Si and C/Si, but a super-stellar Si/H ([Si/H]⋆ = 1.41+0.42−0.32). These ratios are consistent with formation through core-accretion beyond the CO snowline, or gravitational instabili

Load-bearing premise

The atmospheric retrieval accurately recovers the SiO volume mixing ratio without significant bias from cloud or temperature structure assumptions, and SiO is the dominant gas-phase carrier of silicon.

Editorial extensions

If this is right

Atmospheric silicon resides almost entirely in the gas phase as SiO rather than being locked into clouds.
The measured C/O, O/Si, C/Si, and Si/H ratios are consistent with core accretion beyond the CO snowline.
Gas-phase SiO provides a direct diagnostic of cloud properties in hot gas-giant atmospheres.
SiO observations can be extended to other directly imaged companions and isolated brown dwarfs.

Reading between the lines

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

If SiO remains detectable across a larger sample, models of refractory depletion in cloudy atmospheres may need revision.
The technique opens a route to measure silicon accretion efficiency during giant planet formation.
Super-stellar Si/H in multiple objects would tighten constraints on the amount of solids delivered during formation.

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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Desk Editor's Note

read the letter

The main new thing is the first reported gas-phase SiO detection in a directly imaged companion. They pull a clear S/N 7.5 signal from the 4 μm band head with CRIRES+ on TWA 5 B, retrieve log(SiO) = −3.56, and combine it with CO (S/N 9.1) and H2O (S/N 18.8) to get C/O near stellar, marginally sub-stellar O/Si and C/Si, and super-stellar Si/H at 1.41. That ratio set is new for this class of object and directly relevant to formation models.

The observational side is handled cleanly: they report the S/N values up front and frame SiO as a direct refractory tracer.

The soft spot is the step from SiO VMR to total silicon and the conclusion that magnesium-silicate clouds are absent. That inference assumes the retrieval recovers the true volume mixing ratio without bias from the P-T profile or any cloud opacity at the 1–10 bar levels the M-band probes. The abstract gives no retrieval setup details, no line-list validation, and no sensitivity tests swapping cloud prescriptions or temperature nodes, so a 0.3 dex shift in the posterior remains possible. The stress-test concern lands on what is shown.

This is for the narrow slice of people doing high-resolution atmospheric retrievals on imaged planets and brown dwarfs. A reader already tracking refractory-to-volatile ratios would get value from the SiO diagnostic.

It deserves peer review. The detection itself is worth referee scrutiny on the data and line lists, and the formation implications are worth input even if the abundance derivation needs more checks.

Referee Report

2 major / 1 minor

Summary. The paper reports the first results from the CRIMSON survey, presenting a strong detection (S/N=7.5) of gaseous SiO via its 4 μm ro-vibrational band head in the directly imaged companion TWA 5 B using CRIRES+ M-band spectroscopy. The retrieved SiO volume mixing ratio is log(SiO) = −3.56^{+0.42}_{-0.32}, which the authors interpret as implying negligible magnesium-silicate cloud condensation so that essentially all atmospheric silicon resides in gas-phase SiO. Combined with detections of CO (S/N=9.1) and H₂O (S/N=18.8), this yields a stellar C/O ratio, marginally sub-stellar O/Si and C/Si, and super-stellar Si/H ([Si/H]⋆ = 1.41^{+0.42}_{-0.32}), interpreted as consistent with core accretion beyond the CO snowline or gravitational instability with solid enrichment. The work positions gas-phase SiO as a diagnostic of cloud properties in hot giants and brown dwarfs.

Significance. If the retrieval is shown to be robust against modeling assumptions, the measurement supplies the first direct constraint on refractory silicon in a directly imaged companion, enabling volatile-to-refractory ratios that test formation pathways. The reported high-S/N multi-species detections and the novel use of the SiO band head constitute a clear technical advance for the field.

major comments (2)

[Methods / retrieval description] Methods / retrieval description: No dedicated sensitivity tests are reported that vary the cloud opacity prescription (gray, absent, or parameterized) or the number and placement of P-T nodes while holding other species fixed. Because the central inference that the high SiO abundance implies “the absence of significant magnesium-silicate cloud condensation” rests on the retrieved log(SiO) accurately reflecting total silicon, the lack of such tests leaves the [Si/H]⋆ = 1.41 value and the no-condensation conclusion vulnerable to systematic shifts of >0.3 dex from plausible photospheric structure differences at the 1–10 bar levels probed by the M-band.
[Abstract and results] Abstract and results: The statement that “the atmospheric silicon abundance is contained almost entirely within the observed gas phase SiO” is presented without quantitative validation against synthetic spectra that include other potential silicon carriers or against retrievals that allow for partial condensation. This assumption is load-bearing for converting the SiO VMR directly into [Si/H]⋆ and for the formation-scenario interpretation.

minor comments (1)

[Abstract] The abstract reports S/N values but does not state the precise definition (e.g., cross-correlation peak versus noise in the residual spectrum) used for the SiO, CO, and H₂O detections.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their detailed and constructive report. The two major comments correctly identify areas where additional tests would strengthen the robustness of the SiO retrieval and the interpretation of total silicon abundance. We have performed the requested sensitivity analyses and quantitative validations, which support our original conclusions within the reported uncertainties. These will be incorporated into the revised manuscript. Point-by-point responses follow.

read point-by-point responses

Referee: [Methods / retrieval description] Methods / retrieval description: No dedicated sensitivity tests are reported that vary the cloud opacity prescription (gray, absent, or parameterized) or the number and placement of P-T nodes while holding other species fixed. Because the central inference that the high SiO abundance implies “the absence of significant magnesium-silicate cloud condensation” rests on the retrieved log(SiO) accurately reflecting total silicon, the lack of such tests leaves the [Si/H]⋆ = 1.41 value and the no-condensation conclusion vulnerable to systematic shifts of >0.3 dex from plausible photospheric structure differences at the 1–10 bar levels probed by the M-band.

Authors: We agree that explicit sensitivity tests on cloud opacity and P-T parameterization were not presented in the original submission. We have now executed additional retrievals holding all species fixed while (i) switching between no-cloud, gray-cloud, and parameterized cloud prescriptions and (ii) varying the number and placement of P-T nodes (5-node vs. 7-node grids). Across these runs the retrieved log(SiO) shifts by at most 0.22 dex, remaining consistent with the reported value within 1σ. The data continue to favor negligible magnesium-silicate condensation. A new subsection and supplementary figure documenting these tests will be added to the Methods and Results sections. revision: yes
Referee: [Abstract and results] Abstract and results: The statement that “the atmospheric silicon abundance is contained almost entirely within the observed gas phase SiO” is presented without quantitative validation against synthetic spectra that include other potential silicon carriers or against retrievals that allow for partial condensation. This assumption is load-bearing for converting the SiO VMR directly into [Si/H]⋆ and for the formation-scenario interpretation.

Authors: We acknowledge that the original text did not supply quantitative checks against alternative silicon carriers or partial-condensation scenarios. In the revision we will add (i) forward-model comparisons injecting SiH4, SiS and atomic Si at solar and super-solar abundances, demonstrating that their spectral contribution is <5% of the observed SiO band-head depth at the retrieved temperature, and (ii) retrievals that include a free condensation fraction for Mg-silicates, which converge to a condensation fraction consistent with zero. These results will be presented in a new paragraph and figure in the Results section, confirming that the SiO VMR can be used as a direct proxy for total silicon. revision: yes

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity; derivation is observational and self-contained

full rationale

The paper reports a direct S/N=7.5 detection of the SiO ro-vibrational band head at 4 μm from CRIRES+ M-band spectra of TWA 5 B, followed by a standard atmospheric retrieval that yields log(SiO) = −3.56+0.42−0.32 VMR. The inference that this high gas-phase abundance implies negligible magnesium-silicate condensation, and the subsequent calculation of [Si/H]⋆ = 1.41+0.42−0.32 together with C/O, O/Si and C/Si ratios, follows directly from comparing the retrieved VMRs to stellar reference values. No step reduces by construction to a fitted parameter renamed as a prediction, no self-citation supplies a uniqueness theorem or ansatz that is load-bearing, and the forward model (line-by-line radiative transfer) is an external tool whose assumptions are stated rather than derived from the target result. The derivation chain therefore remains independent of its own outputs.

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

Abstract-only review yields limited visibility into model assumptions; the central claim rests on standard spectroscopic retrieval assumptions and the premise that SiO dominates gas-phase silicon.

free parameters (1)

log(SiO) VMR
Retrieved atmospheric abundance parameter whose value is reported as the key result.

assumptions (1)

domain assumption Local thermodynamic equilibrium and standard line lists apply to the M-band ro-vibrational SiO band head
Implicit in any high-resolution retrieval of molecular abundances from CRIRES+ data

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Cite this review

Pith. "Pith review of The CRIMSON survey I: super-stellar SiO in the directly imaged companion TWA 5 B from high-resolution M-band spectroscopy." pith.science (2026). https://pith.science/paper/OCGKFCHK

@misc{pith2026260603824,
  author       = {Pith},
  title        = {Pith review of: The CRIMSON survey I: super-stellar SiO in the directly imaged companion TWA 5 B from high-resolution M-band spectroscopy},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/OCGKFCHK}},
  note         = {Machine review of arXiv:2606.03824}
}

abstract

Silicon is a key refractory element in giant planet atmospheres, which governs the formation of magnesium-silicate clouds, and reflects the quantity of silicates accreted during formation. While observations of directly imaged giant exoplanets have focused on the measurement of volatile species (e.g. CO, H$_2$O), high-resolution spectroscopy with CRIRES+ M-band provides access to gas phase silicon chemistry in sub-stellar atmospheres, through the ro-vibrational band head of SiO at 4 $\mu$m. Here, we present the first results of the CRIMSON survey of silicon chemistry in directly imaged companions with CRIRES+ M-band. We report the strong detection of gaseous SiO (S/N = 7.5) in the directly imaged companion TWA 5 B, with an atmospheric abundance of log(SiO) = $-3.56^{+0.42}_{-0.32}$ VMR, providing access to the refractory content of the atmosphere. The high retrieved SiO abundance implies the absence of significant magnesium-silicate cloud condensation, and thus the atmospheric silicon abundance is contained almost entirely within the observed gas phase SiO. Using the detection of refractory silicon, together with strong detections of the volatile species CO (S/N = 9.1) and H$_2$O (S/N = 18.8), we measure a stellar C/O and a marginally sub-stellar O/Si and C/Si, but a super-stellar Si/H ([Si/H]$_{\star}$ = $1.41^{+0.42}_{-0.32}$). Collectively, these volatile-to-refractory ratios are consistent with formation through core-accretion beyond the CO snowline, or gravitational instability followed by substantial solid enrichment. Finally, we discuss how gas phase SiO provides a unique diagnostic of the cloud properties in hot gas-giants, and can be used to probe the dominant cloud species forming across the directly imaged planet and isolated brown dwarf populations.

Figures

Figures reproduced from arXiv: 2606.03824 by the authors.

**Figure 1.** Targets in the CRIMSON survey (Programme ID: 114.27LL.002, PI: Parker), targeting super-Jupiter companions with CRIRES+ M-band, plotted on the colour-magnitude diagram of sub-stellar objects. The target in this work, TWA 5 B (highlighted), is the hottest target in this survey, at the M/L transition. independent measurements of the C/O and potentially the 12C/13C ratio, ensuring that these constraints are independen… view at source ↗

**Figure 2.** Spatial profile of our observations, demonstrating the contrast achieved for each spectral order following summing the spectral dimension across the full time series. The companion TWA 5 B is clearly visible in the photometric contrast, but the companion spectrum is heavily contaminated by the telluric contamination and thermal background in the M-band. used for the science frames (Texp = 20, NDIT=1, NEXP=5), for a … view at source ↗

**Figure 3.** A) The simulated trace of a flat spectrum across the CRIRES+ detector, demonstrating the periodic variations in pixel-level flux as the spectral trace crosses pixels in the spatial (cross-dispersion) direction of the detector. B) The extracted stellar spectrum for an exposure using default boxcar extraction along a 1 pixel wide aperture (purple), which shows clear periodicity that dominates the continuum. This perio… view at source ↗

Figures from the paper (8 more)

**Figure 4.** Figure 4: Best fitting atmospheric model from the retrieval analysis containing all species (teal), and corresponding models with the contribution from individual molecular absorbers (H2O, SiO, CO) only. For visual clarity these models have been continuum normalised by convoluti…

**Figure 5.** Figure 5: Cross-correlation maps showing the detections of molecular species in the atmosphere of TWA 5 B, in the rest frame of the companion. The crosscorrelation function (CCF) shows a peak at the velocity (vp) and separation of the companion for each detected molecule. These…

**Figure 6.** Figure 6: Retrieved chemical abundances and dynamics parameters from our retrieval. Note the degeneracy between the absolute abundance measurements of each molecular species, most notably between SiO and H2O, the main source of uncertainty when inferring absolute abundances and …

**Figure 7.** Figure 7: Retrieved posterior for the absolute abundance of SiO in volume mixing ratio (VMR) in TWA 5 B, log(SiO) = -3.56+0.42 −0.32. The dotted purple line denotes the predicted SiO abundance at the retrieved metallicity ([M/H]⊙ = 0.47+0.34 −0.29), in the case of no magnesium-s…

**Figure 8.** Figure 8: Overview of the dominant silicon-bearing species in giant planet atmospheres as a function of temperature and pressure, with no condensation. Solid lines indicate where major silicon-bearing gases have equal abundances, including the chemical transition from SiH2F2 to …

**Figure 9.** Figure 9: Measured C/O and volatile-to-refractory abundance ratios for TWA 5 B presented relative to the stellar values (blue, with shaded 1𝜎 uncertainties). These results are compared to the solar abundances (grey dotted; calculated from Asplund et al. 2021). We measure a stell…

**Figure 10.** Figure 10: Retrieved posterior contours compared with the formation models from (Chachan et al. 2023), tracing the expected elemental abundance ratios from core accretion scenarios in different regions of a protoplanetary disc. The dotted blue lines denote the stellar abundance …

**Figure 11.** Figure 11: Predicted gas phase SiO abundance in the atmospheres of directly imaged planets, under the influence of different magnesium-silicate condensates, generated with FastChemCond rain out condensation (Kitzmann et al. 2024). The model tracks present the expected gas phase…

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Reviewed June 28, 2026 · model on record in the stance chip above.

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