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The Roasting Marshmallows Program with IGRINS on Gemini South III: Seeing deeper into the metal depleted atmosphere of a gas-giant on the cusp of the hot to ultra-hot Jupiter transition

T0 review · 3 major / 5 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read The paper claims that WASP-122b has a drastically metal-depleted dayside atmosphere, about 3% of solar metallicity, and that this depletion is what makes its water lines appear in absorption rather than emission, contradicting…

desk verdict A careful first-look dayside characterization of WASP-122b that plausibly finds a very metal-poor, non-inverted atmosphere, but the headline metallicity rests almost entirely on one H2O detection and is not tested against cloud opacity. read the letter →

arxiv 2507.07204 v1 pith:R2OVNHQE submitted 2025-07-09 astro-ph.EP astro-ph.SR

Vatsal Panwar , Matteo Brogi , Krishna Kanumalla , Michael R. Line , Siddharth Gandhi , Peter C.B. Smith , Jacob L. Bean , Lorenzo Pino
show 12 more authors
Arjun B. Savel Joost P. Wardenier Heather Cegla Hayley Beltz Megan Weiner Mansfield Jorge A. Sanchez Jean-Michel Désert Luis Welbanks Viven Parmentier Changwoo Kye Jonathan J. Fortney Tomás de Azevedo Silva
This is my paper · ORCID
classification astro-ph.EPastro-ph.SR
keywords hotJupiterultra-hottransitionhigh-resolutionspectroscopyatmosphericmetallicitythermalinversionwatervaporexoplanetatmospheresDoppler
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 high-resolution infrared spectra of the hot Jupiter WASP-122b, a planet sitting in the temperature gap between hot and ultra-hot Jupiters. It detects water vapor in the dayside and finds that the atmosphere is remarkably metal-poor: about 3% of solar metallicity, with a solar-to-sub-solar carbon-to-oxygen ratio. The low metallicity changes where the observed light is emitted, pushing it to a deep, non-inverted region around 1 bar, so the water lines appear in absorption, opposite to what solar-composition radiative-convective equilibrium models predict. The result suggests that atmospheric metallicity, not just temperature, can control whether a hot giant shows an inverted thermal structure, and it also conflicts with standard core-accretion formation expectations.

What carries the argument

The central object is the contribution function, defined as cf(P,λ) = B(λ,T(P)) Δeτ(λ,P)/Δlog(P), which quantifies which pressure layers emit most of the light at each wavelength. The argument is that low atmospheric metallicity reduces the opacity, pushing the contribution function deeper to about 1 bar, where the P-T profile is non-inverted, so H2O lines appear in absorption. This is supported by high-resolution cross-correlation spectroscopy with IGRINS, the CCF-to-log-likelihood retrieval framework, the GENESIS forward model, FastChem equilibrium chemistry, and a Bézier-spline parametrization of the P-T profile.

What would settle it

Run the same IGRINS data through a retrieval that includes cloud/haze opacity (e.g., a gray cloud deck or haze scattering) and check whether the recovered metallicity stays near -1.5 dex; if the posterior moves toward solar (above about -0.5 dex), the metal-depletion claim is an artifact of unmodeled aerosols.

Watch

Extended reading notes

Core claim

WASP-122b's dayside atmosphere has a metallicity of log10[ZP/Zsun] = -1.48 ± 0.25 dex (0.033 × solar) and a C/O ratio of 0.36 ± 0.22 (3σ upper limit 0.82), based on a detection of H2O in high-resolution IGRINS spectra. Because the atmosphere is so metal-poor, the contribution function—the pressure layers that dominate the emitted spectrum—moves deeper to around 1 bar, where the pressure-temperature profile is non-inverted, causing H2O lines to appear in absorption. This is inconsistent with a solar-composition 1D-RCTE model, which predicts an inverted profile with emission lines; the data show an anticorrelated cross-correlation peak against that model. The measured sub-solar metallicity and solar/sub-solar C/O ratio are inconsistent with standard core-accretion predictions, and the measured Kp and Vsys values are shifted from literature values, in tension with global circulation model predictions.

Load-bearing premise

The forward models and retrievals assume a cloud-free, haze-free gas-phase atmosphere; if aerosols exist at the probed pressures around 0.1 to 1 bar, they could mute the water lines and mimic the inferred low metallicity.

Editorial extensions

If this is right

  • If the atmosphere is truly ~3% solar metallicity, the probed dayside layers are non-inverted, so H2O lines are in absorption; solar-composition RCTE models are ruled out for this planet.
  • The sub-solar metallicity and solar/sub-solar C/O ratio are inconsistent with standard core-accretion formation models, implying alternative formation pathways such as formation beyond the CO/CO2 snow line with carbon partly locked in soot phase.
  • The measured metallicity of 0.033× solar falls in the range of metallicities (0.03–30× solar) needed to explain the scatter in H2O absorption features observed by HST/WFC3 for a sample of hot and ultra-hot Jupiters.
  • The positive ΔKp and large ΔVsys values are in tension with GCM predictions and tidally locked rotation; confirming them would require post-eclipse observations and may indicate strong atmospheric dynamics or systematic effects.
  • A non-inverted P-T profile in the 0.1–1 bar range, with possible weak inversion above 0.1 bar, supports a gradual onset of thermal inversion near Teq ~ 1900 K, but only upper-atmosphere constraints can confirm the transition.

Reading between the lines

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

  • The metallicity–inversion link implies that the hot-to-ultra-hot Jupiter transition may be composition-dependent, not solely temperature-dependent; surveys should treat metallicity as a key variable when predicting emission versus absorption line shapes in this regime.
  • If clouds or hazes are present at 0.1–1 bar, they could mute H2O line contrasts and bias the retrieved metallicity low; a retrieval that includes cloud/haze opacity on the same data would directly test whether the metal depletion is real.
  • Other hot Jupiters with similarly low metallicities might also show water lines in absorption despite high dayside temperatures, predicting a correlation between measured metallicity and line-shape sign across the population.
  • The anomalous velocity shifts, if confirmed with post-eclipse data, would motivate 3D retrieval frameworks and could indicate large-scale atmospheric circulation patterns beyond current GCM predictions.
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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

3 major / 5 minor

Summary. The paper presents high-resolution near-infrared (H/K-band, IGRINS/Gemini South) dayside emission spectroscopy of the hot Jupiter WASP-122b, a planet near the hot-to-ultra-hot Jupiter transition (T_day = 2258 K). The authors detect H2O via cross-correlation with a retrieved model and report a strongly sub-solar atmospheric metallicity log10[Z_P/Z_sun] = -1.48 +/- 0.25 dex, a solar/sub-solar C/O ratio of 0.36 +/- 0.22 (3-sigma upper limit 0.82), and a non-inverted lower-atmosphere P-T profile that places the contribution function near 1 bar. They contrast this with a solar-composition 1D-RCTE forward model that predicts an inverted profile and emission lines, which yields an anti-correlated CCF peak. The retrieval is tested against five P-T parametrizations, free and equilibrium chemistry, PHOENIX versus blackbody stellar spectra, a free v sin i, and a range of PCA components; all yield consistent sub-solar metallicities. The paper also reports a positive Delta-K_P and large negative Delta-V_sys relative to literature values, which is in tension with GCM predictions.

Significance. If the central claim holds, WASP-122b would be a striking data point: an atmosphere at 0.033x solar metallicity, the most metal-depleted gas giant with a well-constrained atmospheric metallicity to date. This would challenge core-accretion expectations and would demonstrate that the emission/absorption character of high-resolution spectral lines depends jointly on composition and thermal structure, reinforcing the need for flexible P-T parameterizations in HRCCS retrievals. The paper is methodologically careful: it includes a controlled collection of robustness tests (Appendices B-D) and an external benchmark in the 1D-RCTE forward model that produces an anti-correlated CCF peak. The claimed detection and parameter constraints are supported by log-likelihood mapping and are reproducible in principle, with data products and code deposited on Zenodo. However, the central metallicity inference rests almost entirely on one molecule (H2O), and the retrieval excludes aerosols, which is a latent alternative explanation for weak line contrasts.

major comments (3)
  1. [Section 4 and Appendices B-D] The retrieval never includes cloud or haze opacity, yet the data are sensitive to pressures around 0.1-1 bar (Fig. 11), where silicate and iron condensates are expected at T ~ 1500-2000 K. In a cloud-free model, a grey or modestly scattering aerosol layer suppresses molecular line contrasts while contributing little narrow-band spectral structure, and the retrieval would compensate by lowering the H2O abundance. Since the metallicity claim is carried almost entirely by the single detected species H2O (Section 4.2, Fig. E1; all other species are unconstrained to the prior bounds), the claimed log10[Z/Zsun] = -1.48 is conditional on an aerosol-free photosphere. This is an internal completeness gap: the robustness tests vary P-T parametrization, stellar spectrum, PCA order, and v sin i, but none admits any aerosol opacity. To make the metal-depletion claim load-bearing, the authors should either include a cloud parameter (e.g., grey or Mie opacity with a base pressure and optical depth) and show that the posterior remains sub-solar, or quantify with a simple injection-recovery test how much cloud optical depth would be required to bias a solar-metallicity truth down to 0.03x solar.
  2. [Section 4.1, Table 2] The equilibrium-chemistry retrieval reports tight constraints on the P-T nodes T2, log10P2, and T0, but several nodes (T1, log10P1, T2 with sigma ~ 900-1000 K) are essentially unconstrained, and the text acknowledges that the nodes are control points rather than physical profile values. The claim that the P-T profile is 'well constrained in the range of pressures we compute the emission spectrum' is supported by the consistency across parametrizations (Fig. 10), and the Delta-ln-Z = 9 preference for a non-inverted linear profile over an inverted one is meaningful. However, the paper should state more explicitly that the retrieved T(P) is only constrained over roughly 0.1-1 bar, and that the upper-atmosphere inversion seen in the Bezier profile is not required by the data (as the linear non-inverted profile with negligible Delta-ln-Z shows). This is partially stated in Section 5.1, but the abstract and conclusions present the non-inverted-versus-inverted narrative more strongly than the posterior support warrants.
  3. [Section 5.3 and Fig. 13] The claim that WASP-122b is 'lowest among all gas-giant exoplanets with well constrained atmospheric metallicity so far' depends on a heterogeneous set of literature values derived from different species (C/H, O/H, (C+O)/H, and (C+O+R)/H) and different techniques. Figure 13 mixes these definitions without, in the main text, a full discussion of systematic offsets (e.g., refractory depletion can depress (C+O+R)/H relative to O/H). The paper should either restrict the comparison to a single metallicity proxy or add a caveat that the ordering may be affected by proxy choice. This does not undermine the internal retrieval result, but it does affect the strength of the population-level statement.
minor comments (5)
  1. [Section 4.2] The CCF peak S/N is reported as 3-sigma for the retrieved model, which is modest. The paper correctly notes that the log-likelihood confidence intervals are the more statistically motivated detection metric, but it would help to report the formal detection significance from the log-likelihood mapping (e.g., Delta-ln-L or the sigma equivalent) alongside the CCF S/N.
  2. [Section 5.4] The measured KP and Vsys shifts are discussed as potential dynamical signatures, but the paper should more prominently state that with only pre-eclipse phase coverage (0.36-0.47), KP and Vsys are strongly correlated and the 1-sigma uncertainties are large; the current phrasing ('significant shift', 'in tension with GCMs') overstates what a single pre-eclipse epoch can establish. The text does acknowledge this at the end of Section 5.4, but the abstract and conclusions should carry the same caveat.
  3. [Section 1 and Fig. 1] The definition of T_day = 2258 +/- 54 K for f = 1.98 is non-standard (f > 1 implies a 'negative' heat redistribution). It would help to explicitly state the corresponding T_eff or T_day for f = 1/2 and f = 2/3, so that the placement of WASP-122b in the hot-to-ultra-hot transition is clear to readers.
  4. [Throughout] There are frequent typographical issues from the LaTeX-to-text conversion (e.g., missing spaces, 'Cóte', 'scenarios' as 'scanrios'), and the citations in the references section are not fully formatted (e.g., several entries are missing journal names or page numbers). The paper would benefit from a careful copyedit; the technical content is readable but the presentation is rough.
  5. [Appendix D] The test with free v sin i is reassuring, but the prior bounds for vrot (1-50 km/s) and the resulting posterior (4.25 +2.43/-1.99 km/s) are broad. The paper says the H2O abundance is unchanged, but it should also state whether the best-fit log10[H2O] shifted by the reported value (-5.05 vs -4.86) is within the quoted uncertainties in a way that accounts for the different P-T parametrization (MS09 vs Bezier), not just the free rotation.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the sub-solar metallicity is a fitted retrieval result checked against an unfitted solar-composition RCTE model, not a prediction that reduces to its input.

full rationale

The paper's central inference is not circular. In Section 3, the authors first compute an unfitted solar-composition 1D-RCTE forward model and cross-correlate it against the data; it produces an anti-correlated CCF peak, showing that the data reject a solar-composition emission-line model independent of any fitted parameters. The retrieval in Section 4 then fits metallicity, C/O, and the P-T profile, and the best-fit model with log10[ZP/Zsun] = -1.48 produces lines in absorption around 1 bar and a positive CCF peak (Figure 4). The statement that low metallicity pushes the contribution function deeper is a forward-model computation (Figure 11) evaluated at the fitted metallicity, not a quantity defined to equal the fitted value. The authors also test alternative P-T parametrizations and a forced non-inverted profile, which is preferred over the inverted profile by Delta ln Z = 9. Self-citations to earlier program papers (Brogi et al. 2023; Smith et al. 2024; Panwar et al. 2024) and to Parmentier et al. (2018) are methodological or empirical inputs, not load-bearing uniqueness claims; the H2O dissociation prescription still leaves the deep H2O abundance as a free parameter. The absence of cloud/haze opacity in the retrieval is a genuine model degeneracy that could bias the H2O abundance low, but it is a completeness/robustness gap rather than a circular reduction: the paper does not fit a cloud parameter and then rename it a prediction. No circular step is identified.

Assumptions & free parameters 6 free parameters · 6 assumptions · 0 invented entities

The central metallicity and C/O constraints come directly from free parameters in the equilibrium chemistry retrieval (metallicity, C/O, plus the P-T nodes) and the H2O abundance in the free chemistry retrieval. The result depends on standard 1D/LTE/equilibrium-chemistry assumptions and on the absence of cloud opacity, which is not tested. No new physical entities are introduced.

free parameters (6)
  • Planet metallicity log10[ZP/Zsun] = -1.48 +0.25/-0.22 (equilibrium chemistry, 4-node Bezier)
    Fitted in equilibrium chemistry retrieval (Table 2); the central claim of metal depletion rests on this parameter.
  • C/O ratio = 0.36 +0.22/-0.22
    Fitted in equilibrium chemistry retrieval; constrains formation scenario (Table 2).
  • KP (planet velocity semi-amplitude) = 205.16 +7.35/-7.61 km/s
    Fitted in retrieval; the significant offset from literature KP is a secondary result.
  • Vsys (systemic velocity) = 25.86 +4.49/-4.24 km/s
    Fitted in retrieval; offset from literature is a secondary result.
  • P-T profile control points (T0, T1, T2, T3, log10P1, log10P2) = Best-fit values in Table 2 (e.g., T0=3315 K, T1=1403 K, log10P1=-2.58, T2=1532 K, log10P2=1.44, T3=3070 K)
    Six free parameters parametrizing the temperature-pressure profile in the 4-node Bezier spline; the inferred non-inverted profile at ~1 bar depends on these.
  • H2O deep abundance log10[H2O] (free chemistry retrieval) = -4.86 +0.14/-0.13
    Free chemistry retrieval constrains H2O abundance; the low abundance drives the metallicity inference.
assumptions (6)
  • domain assumption The planetary atmosphere is 1D, plane-parallel, and in hydrostatic equilibrium.
    GENESIS computes spectra from 1D P-T and VMR profiles; the retrieval does not model 3D structure or phase variations (Section 4).
  • domain assumption Local thermodynamic equilibrium (LTE) holds for the line-forming region.
    GENESIS and the CCF framework assume LTE opacities and source functions; non-LTE effects such as pumping are ignored.
  • domain assumption Equilibrium chemistry (FastChem) accurately predicts abundance profiles for the equilibrium retrieval.
    The equilibrium chemistry retrieval (Section 4) uses FastChem with metallicity and C/O as inputs; the derived metallicity depends on this chemical scheme.
  • domain assumption The CCF-to-log-likelihood mapping (Brogi & Line 2019) provides an unbiased likelihood for the data.
    The retrieval uses this mapping to compute posteriors; any bias in the mapping would propagate to the parameter constraints.
  • domain assumption The stellar spectrum is well represented by PHOENIX (and the blackbody test is a valid cross-check).
    The model planet-to-star contrast uses a PHOENIX stellar model (Section 3); imperfect stellar modeling could bias molecular abundances.
  • domain assumption The planetary orbit is circular and follows the Keplerian velocity equation (1).
    The Doppler shift model assumes a circular orbit with constant KP and Vsys; eccentricity or non-Keplerian effects are not modeled.

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Cite this review

Pith. "Pith review of The Roasting Marshmallows Program with IGRINS on Gemini South III: Seeing deeper into the metal depleted atmosphere of a gas-giant on the cusp of the hot to ultra-hot Jupiter transition." pith.science (2026). https://pith.science/paper/R2OVNHQE

@misc{pith2026250707204,
  author       = {Pith},
  title        = {Pith review of: The Roasting Marshmallows Program with IGRINS on Gemini South III: Seeing deeper into the metal depleted atmosphere of a gas-giant on the cusp of the hot to ultra-hot Jupiter transition},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/R2OVNHQE}},
  note         = {Machine review of arXiv:2507.07204}
}
abstract

Ultra-hot Jupiters are a class of gas-giant exoplanets that show a peculiar combination of thermochemical properties in the form of molecular dissociation, atomic ionization, and inverted thermal structures. Atmospheric characterization of gas giants lying in the transitional regime between hot and ultra-hot Jupiters can help in understanding the physical mechanisms that cause the fundamental transition in atmospheres between the two classes of hot gas giants. Using Doppler spectroscopy with IGRINS on Gemini South (1.4 to 2.5 $\mu$m), we present the day-side high-resolution spectrum of WASP-122b (T$_{\mathrm{day}}$=2258$ \pm$ 54 K), a gas-giant situated at this transition. We detect the signal from H$_{2}$O, based on which we find that WASP-122b has a significantly metal-depleted atmosphere with metallicity log$_{10}$[Z$_{\mathrm{P}}$/Z$_{\odot}$] = $-$1.48$\pm$0.25 dex (0.033$_{-0.016}^{+0.018}$ $\times$ solar), and solar/sub-solar C/O ratio = 0.36$\pm$0.22 (3$\sigma$ upper limit 0.82). Drastically low atmospheric metallicity pushes the contribution function to higher pressures, resulting in the planetary spectral lines to originate from a narrow region around 1 bar where the thermal profile is non-inverted. This is inconsistent with solar composition radiative convective equilibrium (RCTE) which predicts an inverted atmosphere with spectral lines in emission. The sub-solar metallicity and solar/sub-solar C/O ratio is inconsistent with expectations from core-accretion. We find the planetary signal to be significantly shifted in K$_{\mathrm{P}}$ and V$_{\mathrm{sys}}$, which is in tension with the predictions from global circulation models and require further investigation. Our results highlight the detailed information content of high-resolution spectroscopy data and their ability to constrain complex atmospheric thermal structures and compositions of exoplanets.

Figures

Figures reproduced from arXiv: 2507.07204 by the authors.

Figure 1
Figure 1. Surface gravity vs dayside temperature parameter space explored by the Roasting Marshmallows program to measure the dayside emission spectra of hot to ultra-hot Jupiters with IGRINS on Gemini South. General planet population is marked by grey symbols, and the planet names observed by the program in blue (W = WASP, and M = MASCARA, H-P = HAT-P). The symbol size is proportional to the S/N expected for each target rela… view at source ↗
Figure 2
Figure 2. Demonstration of detrending the data to remove the contamination from stellar and telluric lines before cross-correlation. The top panel shows the original raw flux data cube where each row is the 1D spectrum for an exposure, the horizontal axis is the wavelength, and the vertical axis is the orbital phase for each exposure. The middle panel is the PCA detrended data cube. The bottom panel shows the same detrended d… view at source ↗
Figure 3
Figure 3. (Left panel) Vertical abundance (volume-mixing ratio (VMR)) profiles (solid lines) and P − T profile (dashed line) and the emission spectrum from all and individual molecular and atomic species as predicted from 1D radiative-convective thermal equilibrium (1D-RCTE) for WASP-122b. The shaded region in the left panel shows the wavelength integrated contribution function (Knutson et al. (2008)) calculated using GENESIS… view at source ↗
Figures from the paper (11 more)
Figure 4
Figure 4. Figure 4: Model emission spectrum (FP/FS) and the corresponding KP - Vsys maps for the CCF and log-likelihood derived confidence intervals for the 1D-RCTE model (top row) and the retrieved model (bottom row). In the inset are shown the P − T profiles for both cases, with the wav…
Figure 5
Figure 5. Figure 5: Dichotomy between inverted and non-inverted P − T profiles (left panel) and the shape of lines in the corresponding spectra (right panel), both assuming solar composition, with an arbitrary vertical offset between them for clarity. The solid lines in the left panel sho…
Figure 6
Figure 6. Figure 6: Cornerplot showing the 1D and 2D posterior distributions for some of the free parameters constrained by the equilibrium chemistry retrieval (described in Section 4) using both 4 node (blue) and 6 node (red) Bézier spline P − T parametrization. The inset in, two corresp…
Figure 7
Figure 7. Figure 7: Same as [PITH_FULL_IMAGE:figures/full_fig_p010_7.png]
Figure 8
Figure 8. Figure 8: Same as [PITH_FULL_IMAGE:figures/full_fig_p011_8.png]
Figure 9
Figure 9. Figure 9: Vertical abundance profiles from the equilibrium chemistry retrieval, and posteriors for corresponding species from the free chemistry retrieval assuming vertically uniform abundances (except for H2O, see Section 4.) By comparing the inferences for the molecular abunda…
Figure 10
Figure 10. Figure 10: Comparison of the P − T profiles constrained from a range model parametrizations, and from the 1D-RCTE model assuming solar metallicity (dashed black). The solid lines show the best fit P − T profiles obtained from 5 different retrievals, one of which assumes free che…
Figure 11
Figure 11. Figure 11: Wavelength dependent contribution functions for the combination of P − T profile (overplotted) and metallicity for WASP-122b across three cases: (Left panel) 1D-RCTE model P − T profile with solar metallicity, (Middle panel) 1D-RCTE model P − T profile with −2 dex sol…
Figure 12
Figure 12. Figure 12: Best fit emission spectrum model for WASP-122b obtained from the equilibrium chemistry retrieval in comparison with its corresponding H2- H2 and H2-He collision induced absorption (CIA) contribution. The shaded region shows the H and K wavelength bands covered by the …
Figure 13
Figure 13. Figure 13: Atmospheric metallicity of WASP-122b constrained from IGRINS observations in this work in the planet mass vs atmospheric metallicity space along with solar system gas-giants and other gas-giant exoplanets with well constrained metallicity measurements. The values for …
Figure 14
Figure 14. Figure 14: 1D posteriors for the C/O and metallicity of WASP-122b as compared to the solar and stellar values derived from the equilibrium chemistry retrieval (blue posteriors) and free chemistry retrieval (red posteriors). the larger the absolute value of ΔKP. Wardenier et al. …

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Works this paper leans on

98 extracted references · 8 canonical work pages

  1. [1]

    write newline

    " write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.state := if if FUNCTION not #0 #1 if FUNCTION and 'skip pop #0 if FUNCTION or pop #1...

  2. [2]

    Arcangeli J., et al., 2018, @doi [The Astrophysical Journal] 10.3847/2041-8213/aab272 , 855, L30

    doi:10.3847/2041-8213/aab272 2018

  3. [3]

    M., Grevesse N., 2021, @doi [Astronomy and Astrophysics] 10.1051/0004-6361/202140445 , 653, A141

    Asplund M., Amarsi A. M., Grevesse N., 2021, @doi [Astronomy and Astrophysics] 10.1051/0004-6361/202140445 , 653, A141

    doi:10.1051/0004-6361/202140445 2021

  4. [4]

    C., Bean J

    August P. C., Bean J. L., Zhang M., Lunine J., Xue Q., Line M., Smith P. C. B., 2023, @doi [The Astrophysical Journal] 10.3847/2041-8213/ace828 , 953, L24

    doi:10.3847/2041-8213/ace828 2023

  5. [5]

    S., Hauschildt P

    Barman T. S., Hauschildt P. H., Allard F., 2005, @doi [The Astrophysical Journal] 10.1086/444349 , 632, 1132

    doi:10.1086/444349 2005

  6. [6]

    Bartelt D., et al., 2025, @doi [The Astronomical Journal] 10.3847/1538-3881/ad9b95 , 169, 101

    doi:10.3847/1538-3881/ad9b95 2025

  7. [7]

    Baxter C., et al., 2020, @doi [Astronomy and Astrophysics] 10.1051/0004-6361/201937394 , 639, A36

    doi:10.1051/0004-6361/201937394 2020

  8. [8]

    Baxter C., et al., 2021, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/202039708 , 648, A127

    doi:10.1051/0004-6361/202039708 2021

Show all 98 references
  1. [9]

    L., et al., 2023, @doi [Nature] 10.1038/s41586-023-05984-y , 618, 43

    Bean J. L., et al., 2023, @doi [Nature] 10.1038/s41586-023-05984-y , 618, 43

    2023 doi

  2. [10]

    M.-R., 2021, @doi [The Astronomical Journal] 10.3847/1538-3881/abb67b , 161, 1

    Beltz H., Rauscher E., Brogi M., Kempton E. M.-R., 2021, @doi [The Astronomical Journal] 10.3847/1538-3881/abb67b , 161, 1

    2021 doi

  3. [11]

    Beltz H., Rauscher E., Kempton E., Malsky I., Savel A., 2023, Magnetic Effects and 3D Structure in Theoretical High - Resolution Transmission Spectra of Ultrahot Jupiters : the Case of WASP -76b, http://arxiv.org/abs/2302.13969

    2023 arXiv

  4. [12]

    F., 2020, @doi [Journal of Quantitative Spectroscopy and Radiative Transfer] 10.1016/j.jqsrt.2019.106687 , 240, 106687

    Bernath P. F., 2020, @doi [Journal of Quantitative Spectroscopy and Radiative Transfer] 10.1016/j.jqsrt.2019.106687 , 240, 106687

    2020

  5. [13]

    L., 2018, Exoplanet Atmospheres at High Spectral Resolution , http://arxiv.org/abs/1806.04617

    Birkby J. L., 2018, Exoplanet Atmospheres at High Spectral Resolution , http://arxiv.org/abs/1806.04617

    2018 arXiv

  6. [14]

    L., de Kok R

    Birkby J. L., de Kok R. J., Brogi M., de Mooij E. J. W., Schwarz H., Albrecht S., Snellen I. A. G., 2013, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnrasl/slt107 , 436, L35

    2013 doi

  7. [15]

    R., 2019, @doi [The Astronomical Journal] 10.3847/1538-3881/aaffd3 , 157, 114

    Brogi M., Line M. R., 2019, @doi [The Astronomical Journal] 10.3847/1538-3881/aaffd3 , 157, 114

    2019 doi

  8. [16]

    Brogi M., Snellen I. A. G., de Kok R. J., Albrecht S., Birkby J., de Mooij E. J. W., 2012, @doi [Nature] 10.1038/nature11161 , 486, 502

    2012 doi

  9. [17]

    M., Schwarz H., 2017, @doi [The Astrophysical Journal] 10.3847/2041-8213/aa6933 , 839, L2

    Brogi M., Line M., Bean J., Désert J. M., Schwarz H., 2017, @doi [The Astrophysical Journal] 10.3847/2041-8213/aa6933 , 839, L2

    2017 doi

  10. [18]

    Brogi M., et al., 2023, @doi [The Astronomical Journal] 10.3847/1538-3881/acaf5c , 165, 91

    2023 doi

  11. [19]

    Buchner J., et al., 2014, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/201322971 , 564, A125

    2014 doi

  12. [20]

    N., Tennyson J., 2022, @doi [RAS Techniques and Instruments] 10.1093/rasti/rzac004 , 1, 43

    Buldyreva J., Yurchenko S. N., Tennyson J., 2022, @doi [RAS Techniques and Instruments] 10.1093/rasti/rzac004 , 1, 43

    2022 doi

  13. [21]

    A., Charbonneau D., 2007, @doi [The Astrophysical Journal] 10.1086/522834 , 668, L171

    Burrows A., Hubeny I., Budaj J., Knutson H. A., Charbonneau D., 2007, @doi [The Astrophysical Journal] 10.1086/522834 , 668, L171

    2007 doi

  14. [22]

    W., Hunten D

    Chamberlain J. W., Hunten D. M., 1987, Theory of planetary atmospheres. An introduction to their physics andchemistry.. Vol. 36

    1987

  15. [23]

    J., Madhusudhan N., Holmberg M., 2023, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/stad648 , 522, 661

    Cheverall C. J., Madhusudhan N., Holmberg M., 2023, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/stad648 , 522, 661

    2023 doi

  16. [24]

    De Kok R., Brogi M., Snellen I., Birkby J., Albrecht S., De Mooij E., 2013, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/201321381 , 554, A82

    2013 doi

  17. [25]

    K., et al., 2024, @doi [The Astronomical Journal] 10.3847/1538-3881/ad643f , 168, 148

    Deibert E. K., et al., 2024, @doi [The Astronomical Journal] 10.3847/1538-3881/ad643f , 168, 148

    2024 doi

  18. [26]

    P., Bridges M., 2009, @doi [Monthly Notices of the Royal Astronomical Society] 10.1111/j.1365-2966.2009.14548.x , 398, 1601

    Feroz F., Hobson M. P., Bridges M., 2009, @doi [Monthly Notices of the Royal Astronomical Society] 10.1111/j.1365-2966.2009.14548.x , 398, 1601

    2009

  19. [27]

    J., Saumon D., Marley M

    Fortney J. J., Saumon D., Marley M. S., Lodders K., Freedman R. S., 2006, @doi [The Astrophysical Journal] 10.1086/500920 , 642, 495

    2006 doi

  20. [28]

    J., Lodders K., Marley M

    Fortney J. J., Lodders K., Marley M. S., Freedman R. S., 2008, @doi [The Astrophysical Journal] 10.1086/528370 , 678, 1419

    2008 doi

  21. [29]

    Gandhi S., Madhusudhan N., 2017, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/stx1601 , 472, 2334

    2017 doi

  22. [30]

    P., Parmentier V., Welbanks L., Savel A

    Gandhi S., Kesseli A., Snellen I., Brogi M., Wardenier J. P., Parmentier V., Welbanks L., Savel A. B., 2022, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/stac1744 , 515, 749

    2022 doi

  23. [31]

    Garhart E., et al., 2020, @doi [The Astronomical Journal] 10.3847/1538-3881/ab6cff , 159, 137

    2020 doi

  24. [32]

    P., et al., 2020, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/staa228 , 493, 2215

    Gibson N. P., et al., 2020, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/staa228 , 493, 2215

    2020 doi

  25. [33]

    Gressier A., et al., 2025, @doi [The Astronomical Journal] 10.3847/1538-3881/ad97bf , 169, 57

    2025 doi

  26. [34]

    A., Yelle R

    Griffith C. A., Yelle R. V., Marley M. S., 1998, @doi [Science] 10.1126/science.282.5396.2063 , 282, 2063

    1998

  27. [35]

    N., Helled R., Ikoma M., Line M

    Guillot T., Fletcher L. N., Helled R., Ikoma M., Line M. R., Parmentier V., 2022, Giant Planets from the Inside - Out , @doi 10.48550/arXiv.2205.04100 , http://arxiv.org/abs/2205.04100

    2022 doi arXiv

  28. [36]

    R., et al., 2020, @doi [Nature] 10.1038/s41586-020-2649-2 , 585, 357

    Harris C. R., et al., 2020, @doi [Nature] 10.1038/s41586-020-2649-2 , 585, 357

    2020 doi

  29. [37]

    S., Tashkun S

    Huang X., Freedman R. S., Tashkun S. A., Schwenke D. W., Lee T. J., 2013, @doi [Journal of Quantitative Spectroscopy and Radiative Transfer] 10.1016/j.jqsrt.2013.05.018 , 130, 134

    2013 doi

  30. [38]

    W., Freedman R

    Huang X., Schwenke D. W., Freedman R. S., Lee T. J., 2017, @doi [Journal of Quantitative Spectroscopy and Radiative Transfer] 10.1016/j.jqsrt.2017.04.026 , 203, 224

    2017 doi

  31. [39]

    Hubeny I., Burrows A., Sudarsky D., 2003, @doi [The Astrophysical Journal] 10.1086/377080 , 594, 1011

    2003 doi

  32. [40]

    D., 2007, @doi [Computing in Science and Engineering] 10.1109/MCSE.2007.55 , 9, 90

    Hunter J. D., 2007, @doi [Computing in Science and Engineering] 10.1109/MCSE.2007.55 , 9, 90

    2007 doi

  33. [41]

    O., Wende-von Berg S., Dreizler S., Homeier D., Reiners A., Barman T., Hauschildt P

    Husser T. O., Wende-von Berg S., Dreizler S., Homeier D., Reiners A., Barman T., Hauschildt P. H., 2013, @doi [Astronomy and Astrophysics] 10.1051/0004-6361/201219058 , 553, A6

    2013 doi

  34. [42]

    Kanumalla K., et al., 2024, @doi [The Astronomical Journal] 10.3847/1538-3881/ad72f3 , 168, 201

    2024 doi

  35. [43]

    M., Woitke P., Dominik C., 2022, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/202141455 , 667, A147

    Khorshid N., Min M., Désert J. M., Woitke P., Dominik C., 2022, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/202141455 , 667, A147

    2022 doi

  36. [44]

    M., 2023, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/202245469 , 675, A95

    Khorshid N., Min M., Désert J. M., 2023, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/202245469 , 675, A95

    2023 doi

  37. [45]

    A., et al., 2008, @doi [The Astrophysical Journal] 10.1088/0004-637X/690/1/822 , 690, 822

    Knutson H. A., et al., 2008, @doi [The Astrophysical Journal] 10.1088/0004-637X/690/1/822 , 690, 822

    2008 doi

  38. [46]

    Kokori A., et al., 2023, @doi [The Astrophysical Journal Supplement Series] 10.3847/1538-4365/ac9da4 , 265, 4

    2023 doi

  39. [47]

    Kreidberg L., et al., 2014, @doi [The Astrophysical Journal] 10.1088/2041-8205/793/2/L27 , 793, L27

    2014 doi

  40. [48]

    Kreidberg L., et al., 2018, @doi [The Astronomical Journal] 10.3847/1538-3881/aac3df , 156, 17

    2018 doi

  41. [49]

    L., 2018

    Kurucz R. L., 2018. p. 47, https://ui.adsabs.harvard.edu/abs/2018ASPC..515...47K

    2018

  42. [50]

    Lee J.-J., Gullikson K., 2016, @doi [Zenodo] 10.5281/zenodo.56067

    2016 doi

  43. [51]

    E., Rothman L

    Li G., Gordon I. E., Rothman L. S., Tan Y., Hu S.-M., Kassi S., Campargue A., Medvedev E. S., 2015, @doi [The Astrophysical Journal Supplement Series] 10.1088/0067-0049/216/1/15 , 216, 15

    2015 doi

  44. [52]

    R., et al., 2013, @doi [The Astrophysical Journal] 10.1088/0004-637X/775/2/137 , 775, 137

    Line M. R., et al., 2013, @doi [The Astrophysical Journal] 10.1088/0004-637X/775/2/137 , 775, 137

    2013 doi

  45. [53]

    R., et al., 2021, @doi [Nature] 10.1038/s41586-021-03912-6 , 598, 580

    Line M. R., et al., 2021, @doi [Nature] 10.1038/s41586-021-03912-6 , 598, 580

    2021 doi

  46. [54]

    D., Barman T., 2019, @doi [The Astrophysical Journal] 10.3847/1538-4357/ab1485 , 876, 69

    Lothringer J. D., Barman T., 2019, @doi [The Astrophysical Journal] 10.3847/1538-4357/ab1485 , 876, 69

    2019 doi

  47. [55]

    J., Simard L., Takami H., eds, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series Vol

    Mace G., et al., 2018, in Evans C. J., Simard L., Takami H., eds, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series Vol. 10702, Ground-based and Airborne Instrumentation for Astronomy VII. p. 107020Q, @doi 10.1117/12.2312345

    2018 doi

  48. [56]

    Madhusudhan N., Seager S., 2009, @doi [The Astrophysical Journal] 10.1088/0004-637X/707/1/24 , 707, 24

    2009 doi

  49. [57]

    A., Kennedy G

    Madhusudhan N., Amin M. A., Kennedy G. M., 2014, @doi [The Astrophysical Journal Letters] 10.1088/2041-8205/794/1/L12 , 794, L12

    2014 doi

  50. [58]

    Mansfield M., et al., 2018, @doi [The Astronomical Journal] 10.3847/1538-3881/aac497 , 156, 10

    2018 doi

  51. [59]

    Mansfield M., et al., 2021, @doi [Nature Astronomy] 10.1038/s41550-021-01455-4 , 5, 1224

    2021 doi

  52. [60]

    Mansfield M. W., et al., 2024, The metallicity and carbon-to-oxygen ratio of the ultra-hot Jupiter WASP -76b from Gemini - S / IGRINS , @doi 10.48550/arXiv.2405.09769 , http://arxiv.org/abs/2405.09769

    2024 doi arXiv

  53. [61]

    S., Robinson T

    Marley M. S., Robinson T. D., 2015, @doi [Annual Review of Astronomy and Astrophysics] 10.1146/annurev-astro-082214-122522 , 53, 279

    2015 doi

  54. [62]

    K., Masseron T., Hoeijmakers H

    McKemmish L. K., Masseron T., Hoeijmakers H. J., Pérez-Mesa V., Grimm S. L., Yurchenko S. N., Tennyson J., 2019, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/stz1818 , 488, 2836

    2019 doi

  55. [63]

    Mikal-Evans T., et al., 2022, @doi [Nature Astronomy] 10.1038/s41550-021-01592-w , 6, 471

    2022 doi

  56. [64]

    Panwar V., Brogi M., Gandhi S., Cegla H., Lafarga M., 2024, The mystery of water in the atmosphere of tau Bootis b continues: insights from revisiting archival CRIRES observations, @doi 10.48550/arXiv.2410.08178 , http://arxiv.org/abs/2410.08178

    2024 doi arXiv

  57. [65]

    Parmentier V., et al., 2018, @doi [ ] 10.1051/0004-6361/201833059 , https://ui.adsabs.harvard.edu/abs/2018A&A...617A.110P 617, A110

    2018 doi

  58. [66]

    P., Fortney J

    Parmentier V., Showman A. P., Fortney J. J., 2021, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/staa3418 , 501, 78

    2021 doi

  59. [67]

    Pelletier S., et al., 2021, @doi [The Astronomical Journal] 10.3847/1538-3881/ac0428 , 162, 73

    2021 doi

  60. [68]

    Pelletier S., et al., 2023, @doi [Nature] 10.1038/s41586-023-06134-0 , 619, 491

    2023 doi

  61. [69]

    Pelletier S., et al., 2024, CRIRES + and ESPRESSO reveal an atmosphere enriched in volatiles relative to refractories on the ultra-hot Jupiter WASP -121b, @doi 10.48550/arXiv.2410.18183 , http://arxiv.org/abs/2410.18183

    2024 doi arXiv

  62. [70]

    Pelletier S., et al., 2025, @doi [The Astronomical Journal] 10.3847/1538-3881/ad8b28 , 169, 10

    2025 doi

  63. [71]

    Pinhas A., Madhusudhan N., Gandhi S., MacDonald R., 2019, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/sty2544 , 482, 1485

    2019 doi

  64. [72]

    Pino L., et al., 2020, @doi [The Astrophysical Journal Letters] 10.3847/2041-8213/ab8c44 , 894, L27

    2020 doi

  65. [73]

    Piskorz D., et al., 2018, @doi [The Astronomical Journal] 10.3847/1538-3881/aad781 , 156, 133

    2018 doi

  66. [74]

    B., Hubickyj O., Bodenheimer P., Lissauer J

    Pollack J. B., Hubickyj O., Bodenheimer P., Lissauer J. J., Podolak M., Greenzweig Y., 1996, @doi [Icarus] 10.1006/icar.1996.0190 , 124, 62

    1996

  67. [75]

    L., Kyuberis A

    Polyansky O. L., Kyuberis A. A., Zobov N. F., Tennyson J., Yurchenko S. N., Lodi L., 2018, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/sty1877 , 480, 2597

    2018 doi

  68. [76]

    Prinoth B., et al., 2022, @doi [Nature Astronomy] 10.1038/s41550-021-01581-z , 6, 449

    2022 doi

  69. [77]

    E., et al., 2016, @doi [The Astronomical Journal] 10.3847/0004-6256/151/6/138 , 151, 138

    Rodriguez J. E., et al., 2016, @doi [The Astronomical Journal] 10.3847/0004-6256/151/6/138 , 151, 138

    2016 doi

  70. [78]

    Roth A., Parmentier V., Hammond M., 2024, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/stae984 , 531, 1056

    2024 doi

  71. [79]

    S., et al., 2010, @doi [Journal of Quantitative Spectroscopy and Radiative Transfer] 10.1016/j.jqsrt.2010.05.001 , 111, 2139

    Rothman L. S., et al., 2010, @doi [Journal of Quantitative Spectroscopy and Radiative Transfer] 10.1016/j.jqsrt.2010.05.001 , 111, 2139

    2010 doi

  72. [80]

    B., Kempton E

    Savel A. B., Kempton E. M. R., Rauscher E., Komacek T. D., Bean J. L., Malik M., Malsky I., 2023, Technical report, Diagnosing limb asymmetries in hot and ultra-hot Jupiters with high-resolution transmission spectroscopy, https://ui.adsabs.harvard.edu/abs/2023arXiv230101694S ,...

    2023 doi arXiv

  73. [81]

    Schwarz H., Brogi M., de Kok R., Birkby J., Snellen I., 2015, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/201425170 , 576, A111

    2015 doi

  74. [82]

    D., 1998, @doi [The Astrophysical Journal] 10.1086/311498 , 502, L157

    Seager S., Sasselov D. D., 1998, @doi [The Astrophysical Journal] 10.1086/311498 , 502, L157

    1998 doi

  75. [83]

    Smith P., et al., 2023, A Combined Ground -based and JWST Atmospheric Retrieval Analysis : Both IGRINS and NIRSpec Agree The Atmosphere of WASP - 77A b is Metal - Poor , @doi 10.48550/arXiv.2312.13069 , http://arxiv.org/abs/2312.13069

    2023 doi arXiv

  76. [84]

    Smith P. C. B., et al., 2024, @doi [The Astronomical Journal] 10.3847/1538-3881/ad8574 , 168, 293

    2024 doi

  77. [85]

    Snellen I. A. G., de Kok R. J., de Mooij E. J. W., Albrecht S., 2010, @doi [Nature] 10.1038/nature09111 , 465, 1049

    2010 doi

  78. [86]

    Stangret M., et al., 2024, The obliquity and atmosphere of the hot Jupiter WASP -122b ( KELT -14b) with ESPRESSO : An aligned orbit and no sign of atomic or molecular absorption, @doi 10.48550/arXiv.2410.00800 , http://arxiv.org/abs/2410.00800

    2024 doi arXiv

  79. [87]

    W., Kitzmann D., Patzer A

    Stock J. W., Kitzmann D., Patzer A. B. C., Sedlmayr E., 2018, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/sty1531

    2018 doi

  80. [88]

    W., Kitzmann D., Patzer A

    Stock J. W., Kitzmann D., Patzer A. B. C., 2022, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/stac2623 , 517, 4070

    2022 doi

  81. [89]

    Sudarsky D., Burrows A., Hubeny I., 2003, @doi [The Astrophysical Journal] 10.1086/374331 , 588, 1121

    2003 doi

  82. [90]

    D., et al., 2016, @doi [Publications of the Astronomical Society of the Pacific] 10.1088/1538-3873/128/964/064401 , 128, 064401

    Turner O. D., et al., 2016, @doi [Publications of the Astronomical Society of the Pacific] 10.1088/1538-3873/128/964/064401 , 128, 064401

    2016 doi

  83. [91]

    Virtanen P., et al., 2020, @doi [Nature Methods] 10.1038/s41592-019-0686-2 , 17, 261

    2020 doi

  84. [92]

    Wardenier J. P., et al., 2024, Phase-resolving the absorption signatures of water and carbon monoxide in the atmosphere of the ultra-hot Jupiter WASP -121b with GEMINI - S / IGRINS , http://arxiv.org/abs/2406.09641

    2024 arXiv

  85. [93]

    P., Parmentier V., Lee E

    Wardenier J. P., Parmentier V., Lee E. K. H., Line M. R., 2025, From pre-transit to post-eclipse: investigating the impact of 3D temperature, chemistry, and dynamics on high-resolution emission spectra of the ultra-hot Jupiter WASP -76b, @doi 10.48550/arXiv.2502.01606 , http:/...

    2025 doi arXiv

  86. [94]

    Weiner Mansfield M., et al., 2024, @doi [The Astronomical Journal] 10.3847/1538-3881/ad4a5f , 168, 14

    2024 doi

  87. [95]

    F., Hubeny I., Spiegelman F., Leininger T., 2019, @doi [The Astrophysical Journal] 10.3847/2041-8213/ab5a89 , 887, L20

    Welbanks L., Madhusudhan N., Allard N. F., Hubeny I., Spiegelman F., Leininger T., 2019, @doi [The Astrophysical Journal] 10.3847/2041-8213/ab5a89 , 887, L20

    2019 doi

  88. [96]

    Xue Q., Bean J. L., Zhang M., Welbanks L., Lunine J., August P., 2023, JWST transmission spectroscopy of HD 209458b: a super-solar metallicity, a very low C / O , and no evidence of CH4 , HCN , or C2H2 , @doi 10.48550/arXiv.2310.03245 , http://arxiv.org/abs/2310.03245

    2023 doi arXiv

  89. [97]

    van Sluijs L., et al., 2023, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/stad1103 , 522, 2145

    2023 doi

  90. [98]

    I., Murray-Clay R., Bergin E

    Öberg K. I., Murray-Clay R., Bergin E. A., 2011, @doi [The Astrophysical Journal] 10.1088/2041-8205/743/1/L16 , 743, L16

    2011 doi

Pith tools

Reviewed August 6, 2026 · model on record in the stance chip above.