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arxiv: 2606.03824 · v1 · pith:OCGKFCHKnew · submitted 2026-06-02 · 🌌 astro-ph.EP · astro-ph.SR

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

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

Pith reviewed 2026-06-28 08:03 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.SR
keywords directly imaged exoplanetsSiO detectionatmospheric retrievalrefractory elementscore accretionTWA 5 Bhigh-resolution spectroscopyexoplanet formation
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The pith

Direct detection of gaseous SiO reveals super-stellar silicon abundance in the atmosphere of TWA 5 B.

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

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.

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

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.

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.

Where Pith is reading between the lines

These are 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.

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.

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.

Figures

Figures reproduced from arXiv: 2606.03824 by Jayne L. Birkby, Luke T. Parker, Matteo Brogi, Siddharth Gandhi, Sophia R. Vaughan, Vatsal Panwar, Vivien Parmentier.

Figure 1
Figure 1. Figure 1: Targets in the CRIMSON survey (Programme ID: 114.27LL.002, PI: Parker), targeting super-Jupiter companions with CRIRES+ M-band, plot￾ted 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 … view at source ↗
Figure 2
Figure 2. 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=… view at source ↗
Figure 3
Figure 3. 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. … view at source ↗
Figure 4
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 convolution with a Gaussian kernel and rescaled based on the maximum depth of their spectral lines, and therefore the relative depths of the spectral… view at source ↗
Figure 5
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 cross￾correlation function (CCF) shows a peak at the velocity (vp) and separation of the companion for each detected molecule. These CCFs are produced using the best fitting models inferred from the atmospheric retrieval (see Section 3.6). The CCF for CO demonstrates cont… view at source ↗
Figure 6
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 metallicity measurements. The predicted abundances of H2O, CO, and SiO from the Sonora Elf Owl model that best fits the properties of TWA 5 … view at source ↗
Figure 7
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-silicate condensation, matching the retrieved atmospheric abundance of SiO, and implying the absence of magnesium silicate clouds at or below… view at source ↗
Figure 8
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 SiO at lower temperatures, the high temperature dissociation of SiO into atomic silicon (Si, also denoted as Si i), and the ionisation of at… view at source ↗
Figure 9
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 stellar C/O ([C/O]★ =-0.09+0.23 −0.27), and sub-stellar O/Si ([O/Si]★ = −0.29+0.17 −0.15) and C/Si ([C/Si]★ = −0.40+0.37 −0.36), but a super-stel… view at source ↗
Figure 10
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 ratios, which is the first order expected composition of TWA 5 B in the case of a star-like gravitational instability formation pathway. The… view at source ↗
Figure 11
Figure 11. Figure 11: Predicted gas phase SiO abundance in the atmospheres of directly imaged planets, under the influence of different magnesium-silicate conden￾sates, generated with FastChemCond rain out condensation (Kitzmann et al. 2024). The model tracks present the expected gas phase abundance of SiO for sub-stellar objects of different temperatures, with each track representing an atmosphere in which only a single cloud… view at source ↗
read the original 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.

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.

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)
  1. [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.
  2. [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)
  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

  1. 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

  2. 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

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.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 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.
axioms (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

pith-pipeline@v0.9.1-grok · 5941 in / 1329 out tokens · 18932 ms · 2026-06-28T08:03:12.197696+00:00 · methodology

discussion (0)

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Reference graph

Works this paper leans on

299 extracted references · 284 canonical work pages · 111 internal anchors

  1. [1]

    doi:10.1111/j.1365-2966.2009.16147.x , Eprint =

    Monthly Notices of the Royal Astronomical Society , author =. 2009 , note =. doi:10.1111/j.1365-2966.2009.14548.x , abstract =

    work page doi:10.1111/j.1365-2966.2009.14548.x 2009

  2. [2]

    Astronomy & Astrophysics , author =

    X-ray spectral modelling of the. Astronomy & Astrophysics , author =. 2014 , note =. doi:10.1051/0004-6361/201322971 , abstract =

    doi:10.1051/0004-6361/201322971 2014

  3. [3]

    The California-Kepler Survey. III. A Gap in the Radius Distribution of Small Planets. , keywords =. doi:10.3847/1538-3881/aa80eb , archivePrefix =. 1703.10375 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/aa80eb

  4. [4]

    , keywords =

    Seeing above the clouds with high-resolution spectroscopy. , keywords =. doi:10.1093/mnras/staa2424 , archivePrefix =. 2008.11464 , primaryClass =

    work page doi:10.1093/mnras/staa2424 2008

  5. [5]

    , keywords =

    Prospects for Characterizing the Haziest Sub-Neptune Exoplanets with High-resolution Spectroscopy. , keywords =. doi:10.3847/1538-3881/abb46b , archivePrefix =. 2008.11299 , primaryClass =

    work page doi:10.3847/1538-3881/abb46b 2008

  6. [6]

    Clouds in the atmosphere of the super-Earth exoplanet GJ 1214b

    Clouds in the atmosphere of the super-Earth exoplanet GJ1214b. , keywords =. doi:10.1038/nature12888 , archivePrefix =. 1401.0022 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature12888

  7. [7]

    , keywords =

    GJ 3090 b: one of the most favourable mini-Neptune for atmospheric characterisation. , keywords =. doi:10.1051/0004-6361/202243975 , archivePrefix =. 2207.14121 , primaryClass =

    work page doi:10.1051/0004-6361/202243975

  8. [8]

    , keywords =

    Carbon monoxide emission lines reveal an inverted atmosphere in the ultra hot Jupiter WASP-33 b consistent with an eastward hot spot. , keywords =. doi:10.1093/mnras/stad1103 , archivePrefix =. 2203.13234 , primaryClass =

    work page doi:10.1093/mnras/stad1103

  9. [9]

    1986, , 98, 609, 10.1086/131801

    An optimal extraction algorithm for CCD spectroscopy. , keywords =. doi:10.1086/131801 , adsurl =

    work page doi:10.1086/131801

  10. [10]

    pycrires: Data reduction pipeline for VLT/CRIRES+

  11. [11]

    A blue-shifted tentative water signal constrains the presence of clouds

    The hot Neptune WASP-166 b with ESPRESSO - III. A blue-shifted tentative water signal constrains the presence of clouds. , keywords =. doi:10.1093/mnras/stad480 , archivePrefix =. 2302.04794 , primaryClass =

    work page doi:10.1093/mnras/stad480

  12. [12]

    VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)

    2003

  13. [13]

    , keywords =

    Constraints on atmospheric water abundance and cloud deck pressure in the warm Neptune GJ 3470 b via CARMENES transmission spectroscopy. , keywords =. doi:10.1093/mnras/stae997 , archivePrefix =. 2404.06648 , primaryClass =

    work page doi:10.1093/mnras/stae997

  14. [14]

    2023, ApJL, 956, L13, doi: 10.3847/2041-8213/acf577

    Carbon-bearing Molecules in a Possible Hycean Atmosphere. , keywords =. doi:10.3847/2041-8213/acf577 , archivePrefix =. 2309.05566 , primaryClass =

    work page doi:10.3847/2041-8213/acf577 2041

  15. [15]

    , keywords =

    Possible Hycean conditions in the sub-Neptune TOI-270 d. , keywords =. doi:10.1051/0004-6361/202348238 , archivePrefix =. 2403.03244 , primaryClass =

    work page doi:10.1051/0004-6361/202348238

  16. [16]

    arXiv e-prints , keywords =

    High-resolution Spectroscopic Reconnaissance of a Temperate Sub-Neptune. arXiv e-prints , keywords =. doi:10.48550/arXiv.2403.18891 , archivePrefix =. 2403.18891 , primaryClass =

    work page doi:10.48550/arxiv.2403.18891

  17. [17]

    arXiv e-prints , keywords =

    JWST Reveals CH _4 , CO _2 , and H _2 O in a Metal-rich Miscible Atmosphere on a Two-Earth-Radius Exoplanet. arXiv e-prints , keywords =. doi:10.48550/arXiv.2403.03325 , archivePrefix =. 2403.03325 , primaryClass =

    work page doi:10.48550/arxiv.2403.03325

  18. [18]

    , keywords =

    High-resolution Transmission Spectroscopy of the Terrestrial Exoplanet GJ 486b. , keywords =. doi:10.3847/1538-3881/acbd39 , archivePrefix =. 2212.11816 , primaryClass =

    work page doi:10.3847/1538-3881/acbd39

  19. [19]

    Search for water in a super-Earth atmosphere: High-resolution optical spectroscopy of 55 Cancri e

    A Search for Water in a Super-Earth Atmosphere: High-resolution Optical Spectroscopy of 55Cancri e. , keywords =. doi:10.3847/1538-3881/aa7133 , archivePrefix =. 1705.03022 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/aa7133

  20. [20]

    , keywords =

    Characterization of the Atmosphere of Super-Earth 55 Cancri e Using High-resolution Ground-based Spectroscopy. , keywords =. doi:10.3847/1538-3881/aba1eb , archivePrefix =. 2007.03115 , primaryClass =

    work page doi:10.3847/1538-3881/aba1eb 2007

  21. [21]

    , keywords =

    A Near-infrared Chemical Inventory of the Atmosphere of 55 Cancri e. , keywords =. doi:10.3847/1538-3881/abe768 , archivePrefix =. 2102.08965 , primaryClass =

    work page doi:10.3847/1538-3881/abe768

  22. [22]

    , keywords =

    No Escaping Helium from 55 Cnc e. , keywords =. doi:10.3847/1538-3881/abe382 , archivePrefix =. 2012.02198 , primaryClass =

    work page doi:10.3847/1538-3881/abe382 2012

  23. [23]

    , keywords =

    The PEPSI exoplanet transit survey (PETS) I: investigating the presence of a silicate atmosphere on the super-earth 55 Cnc e. , keywords =. doi:10.1093/mnras/stac810 , archivePrefix =. 2203.16856 , primaryClass =

    work page doi:10.1093/mnras/stac810

  24. [24]

    , keywords =

    A reflective, metal-rich atmosphere for GJ 1214b from its JWST phase curve. , keywords =. doi:10.1038/s41586-023-06159-5 , archivePrefix =. 2305.06240 , primaryClass =

    work page doi:10.1038/s41586-023-06159-5

  25. [25]

    Atmospheric composition, spin rotation, and radial velocity

    Pictoris b through the eyes of the upgraded CRIRES+. Atmospheric composition, spin rotation, and radial velocity. , keywords =. doi:10.1051/0004-6361/202347846 , archivePrefix =. 2311.13527 , primaryClass =

    work page doi:10.1051/0004-6361/202347846

  26. [26]

    arXiv e-prints , keywords =

    Feasibility of High-Resolution Transmission Spectroscopy for Low-Velocity Exoplanets. arXiv e-prints , keywords =. doi:10.48550/arXiv.2403.18894 , archivePrefix =. 2403.18894 , primaryClass =

    work page doi:10.48550/arxiv.2403.18894

  27. [27]

    , keywords =

    High-resolution Spectroscopic Reconnaissance of a Temperate Sub-Neptune. , keywords =. doi:10.3847/2041-8213/ad3828 , archivePrefix =. 2403.18891 , primaryClass =

    work page doi:10.3847/2041-8213/ad3828 2041

  28. [28]

    , keywords =

    Optimising spectroscopic observations of transiting exoplanets. , keywords =. doi:10.1051/0004-6361/202347398 , archivePrefix =. 2312.08320 , primaryClass =

    work page doi:10.1051/0004-6361/202347398

  29. [29]

    Atomic iron and titanium in the atmosphere of the exoplanet KELT-9b

    Atomic iron and titanium in the atmosphere of the exoplanet KELT-9b. , keywords =. doi:10.1038/s41586-018-0401-y , archivePrefix =. 1808.05653 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41586-018-0401-y

  30. [30]

    Fe II in MASCARA-2b and KELT-9b with FIES on the Nordic Optical Telescope

    Exoplanet atmospheres at high resolution through a modest-size telescope. Fe II in MASCARA-2b and KELT-9b with FIES on the Nordic Optical Telescope. , keywords =. doi:10.1051/0004-6361/202142787 , archivePrefix =. 2203.04969 , primaryClass =

    work page doi:10.1051/0004-6361/202142787

  31. [31]

    Detection of the resolved signatures of a supersonic equatorial jet and cool poles in a hot planet

    CRIRES ^+ transmission spectroscopy of WASP-127b. Detection of the resolved signatures of a supersonic equatorial jet and cool poles in a hot planet. arXiv e-prints , keywords =. doi:10.48550/arXiv.2404.12363 , archivePrefix =. 2404.12363 , primaryClass =

    work page doi:10.48550/arxiv.2404.12363

  32. [32]

    2004, MNRAS, 348, 435, doi: 10.1111/j.1365-2966.2004.07180.x

    Correcting systematic effects in a large set of photometric light curves. , keywords =. doi:10.1111/j.1365-2966.2004.08585.x , archivePrefix =. astro-ph/0502056 , primaryClass =

    work page doi:10.1111/j.1365-2966.2004.08585.x 2004

  33. [33]

    The Sys-Rem Detrending Algorithm: Implementation and Testing

    The Sys-Rem Detrending Algorithm: Implementation and Testing. Transiting Extrapolar Planets Workshop , year = 2007, editor =. doi:10.48550/arXiv.astro-ph/0612418 , archivePrefix =. astro-ph/0612418 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0612418 2007

  34. [34]

    Detection of water absorption in the day side atmosphere of HD 189733 b using ground-based high-resolution spectroscopy at 3.2 microns

    Detection of water absorption in the day side atmosphere of HD 189733 b using ground-based high-resolution spectroscopy at 3.2 m. , keywords =. doi:10.1093/mnrasl/slt107 , archivePrefix =. 1307.1133 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnrasl/slt107

  35. [35]

    Trends in Atmospheric Properties of Neptune-Size Exoplanets

    Trends in Atmospheric Properties of Neptune-size Exoplanets. , keywords =. doi:10.3847/1538-3881/aa9279 , archivePrefix =. 1708.00016 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/aa9279

  36. [36]

    , keywords =

    Clouds and Clarity: Revisiting Atmospheric Feature Trends in Neptune-size Exoplanets. , keywords =. doi:10.3847/2041-8213/ad1b5c , archivePrefix =. 2310.07714 , primaryClass =

    work page doi:10.3847/2041-8213/ad1b5c 2041

  37. [37]

    L., Raymond, S

    The Nature and Origins of Sub-Neptune Size Planets. Journal of Geophysical Research (Planets) , keywords =. doi:10.1029/2020JE006639 , archivePrefix =. 2010.11867 , primaryClass =

    work page doi:10.1029/2020je006639 2010

  38. [38]

    The California-Kepler Survey. VII. Precise Planet Radii Leveraging Gaia DR2 Reveal the Stellar Mass Dependence of the Planet Radius Gap. , keywords =. doi:10.3847/1538-3881/aae828 , archivePrefix =. 1805.01453 , primaryClass =

    work page doi:10.3847/1538-3881/aae828

  39. [39]

    An asteroseismic view of the radius valley: stripped cores, not born rocky

    An asteroseismic view of the radius valley: stripped cores, not born rocky. , keywords =. doi:10.1093/mnras/sty1783 , archivePrefix =. 1710.05398 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty1783

  40. [40]

    Three Possible Origins for the Gas Layer on GJ 1214b

    Three Possible Origins for the Gas Layer on GJ 1214b. , keywords =. doi:10.1088/0004-637X/716/2/1208 , archivePrefix =. 0912.3243 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/716/2/1208

  41. [41]

    Science , keywords =

    Density, not radius, separates rocky and water-rich small planets orbiting M dwarf stars. Science , keywords =. doi:10.1126/science.abl7164 , archivePrefix =. 2209.03871 , primaryClass =

    work page doi:10.1126/science.abl7164

  42. [42]

    A Framework for Characterizing the Atmospheres of Low-Mass Low-Density Transiting Planets

    A Framework for Characterizing the Atmospheres of Low-mass Low-density Transiting Planets. , keywords =. doi:10.1088/0004-637X/775/1/80 , archivePrefix =. 1306.4329 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/775/1/80

  43. [43]

    G., Welbanks, L., Schlawin, E., et al

    Sulfur Dioxide and Other Molecular Species in the Atmosphere of the Sub-Neptune GJ 3470 b. , keywords =. doi:10.3847/2041-8213/ad55e9 , adsurl =

    work page doi:10.3847/2041-8213/ad55e9 2041

  44. [44]

    Exoplanet Atmospheres at High Spectral Resolution

    Exoplanet Atmospheres at High Spectral Resolution. arXiv e-prints , keywords =. doi:10.48550/arXiv.1806.04617 , archivePrefix =. 1806.04617 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1806.04617

  45. [45]

    , keywords =

    Irradiated Ocean Planets Bridge Super-Earth and Sub-Neptune Populations. , keywords =. doi:10.3847/2041-8213/ab9530 , archivePrefix =. 2002.05243 , primaryClass =

    work page doi:10.3847/2041-8213/ab9530 2041

  46. [46]

    , keywords =

    Mass-Radius Relationships for Irradiated Ocean Planets. , keywords =. doi:10.3847/1538-4357/abfa99 , archivePrefix =. 2105.01102 , primaryClass =

    work page doi:10.3847/1538-4357/abfa99

  47. [47]

    , keywords =

    The Runaway Greenhouse on Sub-Neptune Waterworlds. , keywords =. doi:10.3847/1538-4357/acafdf , archivePrefix =. 2212.02644 , primaryClass =

    work page doi:10.3847/1538-4357/acafdf

  48. [48]

    Nature Astronomy , keywords =

    Evidence for the volatile-rich composition of a 1.5-Earth-radius planet. Nature Astronomy , keywords =. doi:10.1038/s41550-022-01835-4 , archivePrefix =. 2212.08477 , primaryClass =

    work page doi:10.1038/s41550-022-01835-4

  49. [49]

    , keywords =

    Unveiling Shrouded Oceans on Temperate sub-Neptunes via Transit Signatures of Solubility Equilibria versus Gas Thermochemistry. , keywords =. doi:10.3847/2041-8213/ac1f92 , archivePrefix =. 2108.04745 , primaryClass =

    work page doi:10.3847/2041-8213/ac1f92 2041

  50. [50]

    , keywords =

    Habitability and Biosignatures of Hycean Worlds. , keywords =. doi:10.3847/1538-4357/abfd9c , archivePrefix =. 2108.10888 , primaryClass =

    work page doi:10.3847/1538-4357/abfd9c

  51. [51]

    S., Fegley, Jr., B., Schaefer, L., & Ford, E

    Atmosphere Origins for Exoplanet Sub-Neptunes. , keywords =. doi:10.3847/1538-4357/ab6ffb , archivePrefix =. 2001.09269 , primaryClass =

    work page doi:10.3847/1538-4357/ab6ffb 2001

  52. [52]

    E., & Young, E

    Chemical Equilibrium between Cores, Mantles, and Atmospheres of Super-Earths and Sub-Neptunes and Implications for Their Compositions, Interiors, and Evolution. , keywords =. doi:10.3847/PSJ/ac68e6 , archivePrefix =. 2107.10405 , primaryClass =

    work page doi:10.3847/psj/ac68e6

  53. [53]

    Exploring the edge of the evaporation desert

    Observability of silicates in volatile atmospheres of super-Earths and sub-Neptunes. Exploring the edge of the evaporation desert. , keywords =. doi:10.1051/0004-6361/202245521 , adsurl =

    work page doi:10.1051/0004-6361/202245521

  54. [54]

    , keywords =

    Distinguishing Oceans of Water from Magma on Mini-Neptune K2-18b. , keywords =. doi:10.3847/2041-8213/ad206e , archivePrefix =. 2401.05864 , primaryClass =

    work page doi:10.3847/2041-8213/ad206e 2041

  55. [55]

    2024 , eprint=

    New insights into the internal structure of GJ 1214 b informed by JWST , author=. 2024 , eprint=

    2024

  56. [56]

    , keywords =

    Water Vapor and Clouds on the Habitable-zone Sub-Neptune Exoplanet K2-18b. , keywords =. doi:10.3847/2041-8213/ab59dc , archivePrefix =. 1909.04642 , primaryClass =

    work page doi:10.3847/2041-8213/ab59dc 2041

  57. [57]

    , keywords =

    Updated Parameters and a New Transmission Spectrum of HD 97658b. , keywords =. doi:10.3847/1538-3881/ab8815 , archivePrefix =. 2004.03601 , primaryClass =

    work page doi:10.3847/1538-3881/ab8815 2004

  58. [58]

    , keywords =

    Transmission Spectroscopy for the Warm Sub-Neptune HD 3167c: Evidence for Molecular Absorption and a Possible High-metallicity Atmosphere. , keywords =. doi:10.3847/1538-3881/abc874 , archivePrefix =. 2011.03470 , primaryClass =

    work page doi:10.3847/1538-3881/abc874 2011

  59. [59]

    , keywords =

    Hubble Space Telescope Transmission Spectroscopy for the Temperate Sub-Neptune TOI-270 d: A Possible Hydrogen-rich Atmosphere Containing Water Vapor. , keywords =. doi:10.3847/1538-3881/aca90b , archivePrefix =. 2211.15576 , primaryClass =

    work page doi:10.3847/1538-3881/aca90b

  60. [60]

    , keywords =

    Water Absorption in the Transmission Spectrum of the Water World Candidate GJ 9827 d. , keywords =. doi:10.3847/2041-8213/acebf0 , archivePrefix =. 2309.10845 , primaryClass =

    work page doi:10.3847/2041-8213/acebf0 2041

  61. [61]

    The GAPS Programme at TNG. LV. Multiple molecular species in the atmosphere of HAT-P-11 b and review of the HAT-P-11 planetary system. , keywords =. doi:10.1051/0004-6361/202347659 , archivePrefix =. 2403.01527 , primaryClass =

    work page doi:10.1051/0004-6361/202347659

  62. [62]

    A Framework for Prioritizing the TESS Planetary Candidates Most Amenable to Atmospheric Characterization

    A Framework for Prioritizing the TESS Planetary Candidates Most Amenable to Atmospheric Characterization. , keywords =. doi:10.1088/1538-3873/aadf6f , archivePrefix =. 1805.03671 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1538-3873/aadf6f

  63. [63]

    arXiv e-prints , keywords =

    Peering above the clouds of the warm Neptune GJ 436b with CRIRES+. arXiv e-prints , keywords =. doi:10.48550/arXiv.2407.06707 , archivePrefix =. 2407.06707 , primaryClass =

    work page doi:10.48550/arxiv.2407.06707

  64. [64]

    Array Programming with NumPy

    Array programming with NumPy. , keywords =. doi:10.1038/s41586-020-2649-2 , archivePrefix =. 2006.10256 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41586-020-2649-2 2006

  65. [65]

    Astropy: A Community Python Package for Astronomy

    Astropy: A community Python package for astronomy. , keywords =. doi:10.1051/0004-6361/201322068 , archivePrefix =. 1307.6212 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201322068

  66. [66]

    The orbital motion, absolute mass, and high-altitude winds of exoplanet HD209458b

    The orbital motion, absolute mass and high-altitude winds of exoplanet HD209458b. , keywords =. doi:10.1038/nature09111 , archivePrefix =. 1006.4364 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature09111

  67. [67]

    , keywords =

    Nightside condensation of iron in an ultrahot giant exoplanet. , keywords =. doi:10.1038/s41586-020-2107-1 , archivePrefix =. 2003.05528 , primaryClass =

    work page doi:10.1038/s41586-020-2107-1 2003

  68. [68]

    , keywords =

    Bioverse: A Comprehensive Assessment of the Capabilities of Extremely Large Telescopes to Probe Earth-like O _ 2 Levels in Nearby Transiting Habitable-zone Exoplanets. , keywords =. doi:10.3847/1538-3881/acd1ec , archivePrefix =. 2304.12490 , primaryClass =

    work page doi:10.3847/1538-3881/acd1ec

  69. [69]

    A Unified Treatment of Kepler Occurrence to Trace Planet Evolution. II. The Radius Cliff Formed by Atmospheric Escape. , keywords =. doi:10.3847/1538-3881/ad434c , archivePrefix =. 2404.15172 , primaryClass =

    work page doi:10.3847/1538-3881/ad434c

  70. [70]

    arXiv e-prints , keywords =

    Chemical mapping of temperate sub-Neptune atmospheres: Constraining the deep-interior H2O/H2 using the atmospheric CO2/CH4. arXiv e-prints , keywords =. doi:10.48550/arXiv.2406.01955 , archivePrefix =. 2406.01955 , primaryClass =

    work page doi:10.48550/arxiv.2406.01955

  71. [71]

    Quantitatively Assessing the Role of Clouds in the Transmission Spectrum of GJ 1214b

    Quantitatively Assessing the Role of Clouds in the Transmission Spectrum of GJ 1214b. , keywords =. doi:10.1088/0004-637X/775/1/33 , archivePrefix =. 1305.4124 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/775/1/33

  72. [72]

    Microphysical Modeling of Mineral Clouds in GJ1214 b and GJ436 b: Predicting Upper Limits on the Cloud-Top Height

    Microphysical Modeling of Mineral Clouds in GJ1214 b and GJ436 b: Predicting Upper Limits on the Cloud-top Height. , keywords =. doi:10.3847/1538-4357/aabee3 , archivePrefix =. 1804.05708 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aabee3

  73. [73]

    Aggregate Hazes in Exoplanet Atmospheres

    Aggregate Hazes in Exoplanet Atmospheres. , keywords =. doi:10.3847/1538-4357/ab074c , archivePrefix =. 1902.05231 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab074c 1902

  74. [74]

    Rotation and winds of exoplanet HD 189733 b measured with high-dispersion transmission spectroscopy

    Rotation and Winds of Exoplanet HD 189733 b Measured with High-dispersion Transmission Spectroscopy. , keywords =. doi:10.3847/0004-637X/817/2/106 , archivePrefix =. 1512.05175 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/817/2/106

  75. [75]

    Search for water vapor in the high-resolution transmission spectrum of HD189733b in the visible

    Search for water vapor in the high-resolution transmission spectrum of HD 189733b in the visible. , keywords =. doi:10.1051/0004-6361/201730814 , archivePrefix =. 1706.00027 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201730814

  76. [76]

    arXiv e-prints , keywords =

    The ESO SupJup Survey II: The ^ 12 C/ ^ 13 C ratios of three young brown dwarfs with CRIRES ^+. arXiv e-prints , keywords =. doi:10.48550/arXiv.2407.07678 , archivePrefix =. 2407.07678 , primaryClass =

    work page doi:10.48550/arxiv.2407.07678

  77. [77]

    A rationale for the characterization of exoplanet atmospheres

    Planet and star synergy at high-spectral resolution. A rationale for the characterization of exoplanet atmospheres. I. The infrared. , keywords =. doi:10.1051/0004-6361/201936566 , archivePrefix =. 1909.11807 , primaryClass =

    work page doi:10.1051/0004-6361/201936566 1909

  78. [78]

    The High-Resolution Transmission Spectrum of HD 189733b Interpreted with Atmospheric Doppler Shifts from Three-Dimensional General Circulation Models

    The High-resolution Transmission Spectrum of HD 189733b Interpreted with Atmospheric Doppler Shifts from Three-dimensional General Circulation Models. , keywords =. doi:10.3847/1538-3881/ab164c , archivePrefix =. 1810.06099 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/ab164c

  79. [79]

    Progress in Modeling Very Low Mass Stars, Brown Dwarfs, and Planetary Mass Objects

    Progress in modeling very low mass stars, brown dwarfs, and planetary mass objects. Memorie della Societa Astronomica Italiana Supplementi , keywords =. doi:10.48550/arXiv.1302.6559 , archivePrefix =. 1302.6559 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1302.6559

  80. [80]

    , keywords =

    WOBBLE: A Data-driven Analysis Technique for Time-series Stellar Spectra. , keywords =. doi:10.3847/1538-3881/ab40a7 , archivePrefix =. 1901.00503 , primaryClass =

    work page doi:10.3847/1538-3881/ab40a7 1901

Showing first 80 references.