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arxiv: 2606.07497 · v1 · pith:X5XRE54Nnew · submitted 2026-06-05 · 🌌 astro-ph.EP

The Roasting Marshmallows Program with IGRINS on Gemini South V: Atmosphere of MASCARA-1b is Enriched in Refractory Elements

Krishna Kanumalla , Michael R. Line , Martina Chiarella , Matteo Brogi , Peter C. B. Smith , Jorge A. Sanchez , Yayaati Chachan , Joshua Lothringer
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Joost P. Wardenier Hayley Beltz Carlos Saffe Emily K. Deibert Megan Weiner Mansfield Stefan Pelletier Vivien Parmentier Yeon-ho Choi Swaetha Ramkumar Arjun B. Savel Luis Welbanks Jacob L. Bean Vatsal Panwar Tom\'as Azevedo Silva Lorenzo Pino Yuya Hayashi Dongwook Lim Cicero X. Lu Venu M. Kalari Teo Mo\v{c}nik Mark G. Rawlings Heeyoung Oh Ruben J. Diaz Chan Park Jae-Joon Lee Sanghyuk Kim Ueejeong Jeong Hye-In Lee Woojin Park Youngsam Yu Yunjong Kim Moo-Young Chun Jae Sok Oh Sungho Lee Jeong-Gyun Jang Bi-Ho Jang Hyeon Cheol Seong Hyun-Jeong Kim Cynthia B. Brooks Gregory N. Mace Hanshin Lee John M. Good Daniel T. Jaffe Kang-Min Kim In-Soo Yuk Narae Hwang Byeong-Gon Park Hwihyun Kim Brian Chinn Francisco Ramos Pablo Prado John White Andres Olivares Valentina Oyarzun Emma Kurz Hawi Stecher Carlos Quiroz Ignacio Arriagada Thomas L. Hayward Hyewon Suh Jen Miller Siyi Xu Emanuele Paolo Farina Charlie Figura Andrew Stephens Bryan Miller Kathleen Labrie Paul Hirst Edo Tapia Zachary Hartmann
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Pith reviewed 2026-06-27 20:49 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords ultra-hot Jupitersexoplanet atmospheresrefractory elementshigh-resolution spectroscopyplanet formationcross-correlation spectroscopyMASCARA-1bsnowlines
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The pith

MASCARA-1b's atmosphere shows 2.5 times solar refractory abundance while maintaining solar metallicity and C/O ratio.

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

The paper presents a high-resolution cross-correlation spectroscopy analysis of the ultra-hot Jupiter MASCARA-1b using IGRINS data. It detects signals from H2O, CO, OH, Fe I, Mg I, Ca I, and Ti I and applies a chemically consistent retrieval to derive elemental abundances. The results indicate solar overall metallicity and C/O but enhanced refractories relative to volatiles, leading to the conclusion that the planet accreted material between the soot-H2O or H2O-CO snowlines. This links atmospheric composition directly to formation location in the protoplanetary disk.

Core claim

The retrieval yields a solar atmospheric metallicity ([M/H]⊙ = 0.07+0.17−0.13 ≈1.2× solar), solar C/O (0.65+0.08−0.08), enhanced refractory abundance ([R/H]⊙ = 0.40+0.23−0.17 ≈2.5× solar), and super-solar refractory-to-volatile ratio ([R/V]⊙ = 0.36+0.11−0.09 ≈2.3× solar). Comparison with formation models indicates accretion between the soot-H2O or H2O-CO snowlines at 68% confidence, with stellar Ti/Mg, Ca/Mg, and Mg/Fe ratios showing no strong nightside cold trapping.

What carries the argument

Chemically consistent atmospheric inference framework that fits cross-correlation signals from multiple species to retrieve elemental abundances simultaneously.

If this is right

  • MASCARA-1b most likely accreted material between the soot-H2O or H2O-CO snowlines.
  • Atmospheric Ti/Mg and Ca/Mg ratios match stellar values, and Mg/Fe is consistent at 95% confidence.
  • No strong indication of nightside cold trapping is present in the abundance ratios.
  • Expanding homogeneous refractory-to-volatile measurements across UHJs will enable statistical tests of giant planet formation trends.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The same chemically consistent retrieval approach could map snowline accretion locations for a larger sample of ultra-hot Jupiters observed with future facilities.
  • If refractory enrichment turns out to be widespread, it would suggest that disk processing or pebble accretion commonly delivers rock-forming material to giant planet envelopes.
  • Precise stellar abundance comparisons for individual elements like Ti, Mg, and Ca could further constrain whether any species are sequestered on the nightside.

Load-bearing premise

The line lists, temperature-pressure profile, and chemical equilibrium model accurately reproduce the observed cross-correlation signals without significant bias from unmodeled opacity or data artifacts.

What would settle it

An independent retrieval or observation that finds sub-solar refractory abundance or a refractory-to-volatile ratio inconsistent with the snowline accretion region would falsify the formation interpretation.

Figures

Figures reproduced from arXiv: 2606.07497 by Andres Olivares, Andrew Stephens, Arjun B. Savel, Bi-Ho Jang, Brian Chinn, Bryan Miller, Byeong-Gon Park, Carlos Quiroz, Carlos Saffe, Chan Park, Charlie Figura, Cicero X. Lu, Cynthia B. Brooks, Daniel T. Jaffe, Dongwook Lim, Edo Tapia, Emanuele Paolo Farina, Emily K. Deibert, Emma Kurz, Francisco Ramos, Gregory N. Mace, Hanshin Lee, Hawi Stecher, Hayley Beltz, Heeyoung Oh, Hwihyun Kim, Hye-In Lee, Hyeon Cheol Seong, Hyewon Suh, Hyun-Jeong Kim, Ignacio Arriagada, In-Soo Yuk, Jacob L. Bean, Jae-Joon Lee, Jae Sok Oh, Jen Miller, Jeong-Gyun Jang, John M. Good, John White, Joost P. Wardenier, Jorge A. Sanchez, Joshua Lothringer, Kang-Min Kim, Kathleen Labrie, Krishna Kanumalla, Lorenzo Pino, Luis Welbanks, Mark G. Rawlings, Martina Chiarella, Matteo Brogi, Megan Weiner Mansfield, Michael R. Line, Moo-Young Chun, Narae Hwang, Pablo Prado, Paul Hirst, Peter C. B. Smith, Ruben J. Diaz, Sanghyuk Kim, Siyi Xu, Stefan Pelletier, Sungho Lee, Swaetha Ramkumar, Teo Mo\v{c}nik, Thomas L. Hayward, Tom\'as Azevedo Silva, Ueejeong Jeong, Valentina Oyarzun, Vatsal Panwar, Venu M. Kalari, Vivien Parmentier, Woojin Park, Yayaati Chachan, Yeon-ho Choi, Youngsam Yu, Yunjong Kim, Yuya Hayashi, Zachary Hartmann.

Figure 1
Figure 1. Figure 1: Summary of our observations and detrending process. Left inset shows the phase coverage of our observations in pre-secondary eclipse (pink) and post-secondary eclipse (yellow) geometries. The phase range obstructed by the secondary eclipse is shown as the thick black line between these geometries. In the top right panel, we show our median signal-to-noise ratios (SNRs) per order for pre-eclipse (pink) and … view at source ↗
Figure 2
Figure 2. Figure 2: Trail of positive cross-correlation values following the orbital motion (along the faint white lines) of MASCARA-1 b in the observer’s rest frame. The black region denotes the phase range where the planet is eclipsed behind the host star. This trail is generated by cross-correlating a solar composition “full” model template (described in Section 3) with the post-SVD data of pre- and post-eclipse geometries… view at source ↗
Figure 3
Figure 3. Figure 3: Detections from our cross-correlation analyses shown as Kp-∆Vsys maps. Each map has been generated using a solar composition RCTE model template containing a single gas opacity along with the continuum. The top row shows the detection of volatile gases i.e., H2O, CO and OH. The bottom row shows our detections of refractory gases i.e., neutral Fe, Mg, Ca, and Ti. The white perpendicular dotted lines denote … view at source ↗
Figure 4
Figure 4. Figure 4: Summary of the fiducial chemical equilibrium retrieval results. Our obtained medians and 1σ errors on the elemental abundances relative to solar are shown in the top left panel. Elemental abundances are expressed as logarithmic multiplicative factors relative to solar composition. The solar abundance is shown for reference as the dashed gray horizontal line. For elements with measured stellar abundances, w… view at source ↗
Figure 5
Figure 5. Figure 5: shows the distribution of ∆Kp and ∆Vsys values obtained from above-mentioned retrievals using single model templates. As investigated in Wardenier et al. (2025), devi￾ations from expected Kp occur due to the planet’s rotation, and the upper limit on ∆Kp can be derived to be |∆Kp| ≤ 3eq + 3jet. Here, 3eq denotes the equatorial solid body rota￾tion velocity and 3jet denotes the equatorial jet speed. Given th… view at source ↗
Figure 6
Figure 6. Figure 6: Observed elemental ratios of MASCARA-1b (red), WASP-121 b (black), and WASP-189 b (purple) compared with the tracks of formation scenarios from Chachan et al. (2023). Colored lines indicate predicted C/R vs R/H trends for planets forming at different disk locations relative to major snow lines. Within the 1σ region (opaque error bar), the scenario that most agrees with our results is that MASCARA-1b formed… view at source ↗
Figure 7
Figure 7. Figure 7: Refractory elemental ratios in MASCARA-1 b along with WASP-121 b (from Smith et al. 2024a) and WASP-189 b (from Sanchez et al. 2025). We find stellar values for Ti/Fe and Ca/Fe. However, the Mg/Fe is super-stellar but consistent with stellar value at 2σ confidence. From these, we conclude that there is no strong evidence for nightside cold trapping. On the right panel, we have compared the retrieved therma… view at source ↗
Figure 8
Figure 8. Figure 8: Targets of the Roasting Marshmallows survey (GS-2023B-LP-206; PI: M. Line) performed using the IGRINS spectrograph on the Gemini-S telescope. In gravity and temperature space, targets of this survey span across key physicochemical transitions enabling inferences on fundamental properties of exoplanet atmospheres. The marker sizes scale with the level of expected thermal emission signal estimated using the … view at source ↗
Figure 9
Figure 9. Figure 9: Cross-correlation maps, similar to as shown in [PITH_FULL_IMAGE:figures/full_fig_p016_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Our retrieved constraints on elemental abundances and derived composition compared with previous works on MASCARA-1 b by Ramkumar et al. (2025) and Guo et al. (2024). The shaded regions in all panels shows the errors on our constraints. We find that our fiducial results are consistent with these previous analyses. 10 9 10 7 10 5 10 3 10 1 VMR 10 1 10 0 10 1 10 2 10 3 10 4 10 5 10 6 Pressure (bar) [PITH_F… view at source ↗
Figure 11
Figure 11. Figure 11: Median volume mixing ratios (VMRs) and their 1σ regions obtained using random draws of parameters controlling composition and thermal structure in our retrieval. The gray spectrum in the background denotes the estimated photosphere (where τ = 2/3). Beyond the photosphere, the precision of VMRs is low as expected [PITH_FULL_IMAGE:figures/full_fig_p016_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: The full corner plot from our retrieval showing the correlations between parameters and their marginalized posterior distributions. We achieved ≈ 0.2 dex on all elements except Si. We derive our fiducial constraints on composition using the first eight parameters describing chemistry. We constructed the median thermal structure along with the errors using parameters T0-T5. Overall, we conclude that the at… view at source ↗
read the original abstract

Ultra-hot Jupiters (UHJs; $T_{\rm eq} \gtrsim 2000$ K) enable simultaneous detection of volatile (ice-forming) and refractory (rock-forming) species in planetary atmospheres, providing a powerful diagnostic of planet formation and atmospheric processing. We present a comprehensive high-resolution cross-correlation spectroscopy (HRCCS) analysis of the UHJ MASCARA-1b ($T_{\rm eq} \approx 2600$ K) using the IGRINS and IGRINS-2 spectrographs. We detect robust (SNR$>$4) signals from H$_2$O, CO, OH, Fe I, Mg I, Ca I, and Ti I, marking the most complete atmospheric inventory of MASCARA-1b to date. Using a chemically consistent atmospheric inference framework, we constrain elemental abundances to a typical precision of $\approx$0.2 dex, retrieving a solar atmospheric metallicity ([M/H]$_\odot$ $= 0.07^{+0.17}_{-0.13}$ $\approx 1.2\times$ solar), a C/O ratio (C/O $= 0.65^{+0.08}_{-0.08}$) consistent with solar value (C/O $=$ 0.59), an enhanced refractory abundance ([R/H]$_\odot$ $= 0.40^{+0.23}_{-0.17} \approx 2.5\times$ solar; $\approx 3.8\times$ stellar), and a moderately super-solar refractory-to-volatile ratio ([R/V]$_\odot$ $= 0.36^{+0.11}_{-0.09}$ $\approx 2.3\times$ solar). Comparison with formation models suggests that MASCARA-1b most likely accreted material between the soot-H$_2$O or H$_2$O-CO snowlines (at 68$\%$ confidence). We additionally find stellar values for atmospheric Ti/Mg and Ca/Mg ratios (at 68$\%$ confidence). The Mg/Fe is also found to be consistent with stellar value at 95$\%$ confidence. Therefore, we do not find strong indication of nightside cold trapping in MASCARA-1b. As homogeneous refractory-to-volatile measurements expand across the UHJ population, particularly with upcoming Extremely Large Telescopes, these diagnostics will enable statistically robust tests of emerging trends in giant planet formation and atmospheric evolution.

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

1 major / 1 minor

Summary. The paper reports high-resolution cross-correlation spectroscopy of the ultra-hot Jupiter MASCARA-1b with IGRINS, claiming robust (SNR>4) detections of H2O, CO, OH, Fe I, Mg I, Ca I, and Ti I. Using a chemically consistent retrieval framework, it derives solar atmospheric metallicity ([M/H]⊙=0.07+0.17−0.13), solar C/O (0.65+0.08−0.08), enhanced refractory abundance ([R/H]⊙=0.40+0.23−0.17 ≈2.5×solar), and super-solar refractory-to-volatile ratio ([R/V]⊙=0.36+0.11−0.09 ≈2.3×solar), inferring accretion between the soot-H2O or H2O-CO snowlines at 68% confidence, with stellar Ti/Mg, Ca/Mg, and Mg/Fe ratios.

Significance. If the abundance ratios hold, the work supplies one of the most complete UHJ inventories to date and demonstrates the diagnostic power of simultaneous volatile/refractory measurements for formation pathways. The reported 0.2 dex precisions and multi-species SNR>4 detections are concrete strengths that enable direct comparison to snowline models.

major comments (1)
  1. [methods (chemically consistent atmospheric inference)] Chemically consistent retrieval (methods section describing the inference framework): the headline values [R/H]⊙=0.40+0.23−0.17 and [R/V]⊙=0.36+0.11−0.09, together with the 68% snowline probability, are obtained from a single equilibrium-chemistry step that ties all species through a shared T-P profile and line lists. The manuscript does not report free-chemistry retrievals or injection-recovery tests that would isolate whether unmodeled opacities or residual artifacts alter the relative CCF amplitudes of refractory versus volatile species; this assumption is load-bearing for the central formation claim.
minor comments (1)
  1. [abstract and results] The abstract states 'stellar values for atmospheric Ti/Mg and Ca/Mg ratios (at 68% confidence)' and 'Mg/Fe consistent with stellar value at 95% confidence'; the exact definition of 'stellar value' and the reference stellar abundances should be stated explicitly in the results section for reproducibility.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their thorough review and valuable comments on our manuscript. We address the major comment point by point below.

read point-by-point responses

  1. Referee: [methods (chemically consistent atmospheric inference)] Chemically consistent retrieval (methods section describing the inference framework): the headline values [R/H]⊙=0.40+0.23−0.17 and [R/V]⊙=0.36+0.11−0.09, together with the 68% snowline probability, are obtained from a single equilibrium-chemistry step that ties all species through a shared T-P profile and line lists. The manuscript does not report free-chemistry retrievals or injection-recovery tests that would isolate whether unmodeled opacities or residual artifacts alter the relative CCF amplitudes of refractory versus volatile species; this assumption is load-bearing for the central formation claim.

    Authors: We agree with the referee that the manuscript does not report free-chemistry retrievals or injection-recovery tests to specifically validate the relative CCF amplitudes between refractory and volatile species. Although the chemically consistent framework is well-suited for the high-temperature regime of MASCARA-1b, where thermochemical equilibrium is expected, we recognize that demonstrating the robustness against potential unmodeled effects would further support the formation interpretation. Accordingly, in the revised version of the manuscript, we will add comparisons with free-chemistry retrievals and include injection-recovery tests focused on the refractory-to-volatile ratios. revision: yes

Circularity Check

0 steps flagged

No circularity: abundances are direct retrieval outputs from independent HRCCS data

full rationale

The paper's central results ([M/H]⊙, C/O, [R/H]⊙, [R/V]⊙ and snowline probability) are obtained by fitting a chemically consistent atmospheric model to observed cross-correlation signals from multiple species (H₂O, CO, OH, Fe I, Mg I, Ca I, Ti I). No equation or step defines any reported ratio in terms of itself, renames a fitted parameter as a prediction, or reduces the outcome to a self-citation chain; the chemically consistent assumption is an explicit modeling choice whose validity is external to the derivation itself. The derivation chain is therefore self-contained against the spectroscopic dataset.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The abundance ratios rest on the accuracy of the cross-correlation detection pipeline and the chemically consistent retrieval model; no new physical entities are postulated.

free parameters (1)
  • elemental abundances [M/H], [R/H], C/O, [R/V]
    Fitted parameters in the atmospheric retrieval that directly produce the reported ratios.
axioms (2)
  • domain assumption Line lists and opacities for H2O, CO, OH, Fe I, Mg I, Ca I, Ti I are complete and accurate at the relevant temperatures.
    Invoked when converting cross-correlation signals into abundance constraints.
  • domain assumption The planet's atmosphere is in chemical equilibrium and can be described by a single 1D T-P profile.
    Core assumption of the chemically consistent inference framework.

pith-pipeline@v0.9.1-grok · 6367 in / 1551 out tokens · 18814 ms · 2026-06-27T20:49:58.478306+00:00 · methodology

discussion (0)

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