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arxiv: 2606.17304 · v1 · pith:L5C5CVFVnew · submitted 2026-06-15 · 🌌 astro-ph.EP

Unraveling the Mystery of the Peculiar and Young Hot Jupiter CoRoT-2b II: Phase Resolved Emission Spectroscopy with VLT/CRIRES+ and Gemini-S/IGRINS

Aurora Y. Kesseli , Siddharth Gandhi , Lisa Dang , Alexis Lavail , Alejandro Sanchez-Lopez , Ying Shu , Emily Rauscher , Hayley Beltz
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Romain Allart Stefan Pelletier Vatsal Panwar
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Pith reviewed 2026-06-27 02:16 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords hot jupitersexoplanet atmosphereshigh-resolution spectroscopyphase curvesrotational broadeningCoRoT-2b
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The pith

CoRoT-2b rotates slower than tidally locked expectations, explaining its western hotspot offset.

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

Hot Jupiters are expected to rotate synchronously due to tidal forces from their short orbits. CoRoT-2b instead shows a western hotspot in its Spitzer phase curve. Phase-resolved high-resolution spectra from VLT/CRIRES+ and Gemini-S/IGRINS detect the planet signal separately before and after eclipse. Retrievals give consistent abundances but a hotter post-eclipse temperature profile. The planet's measured rotational broadening of 2.24 km/s is 2.6 sigma below the 4.37 km/s value expected for synchronous rotation, favoring sub-synchronous spin as the cause.

Core claim

The analysis concludes that CoRoT-2b exhibits sub-synchronous rotation. Its rotational broadening is measured at 2.24 +0.81/-0.77 km s^{-1}, discrepant at 2.6 sigma from the 4.37 ± 0.13 km s^{-1} predicted by tidal locking. This slower rotation is identified as the most likely explanation for the western hotspot offset after testing alternative hypotheses.

What carries the argument

Rotational line broadening extracted from cross-correlation of phase-resolved high-resolution emission spectra, tested against the value predicted from the orbital period under the assumption of synchronous rotation.

If this is right

  • The western hotspot offset arises from sub-synchronous rotation rather than other mechanisms such as clouds or magnetic effects.
  • Chemical abundances and C/O ratios remain consistent across pre- and post-eclipse phases.
  • A hotter and more isothermal temperature-pressure profile appears at post-eclipse phases, matching the phase-curve data.

Where Pith is reading between the lines

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

  • Tidal evolution models for close-in giant planets may need to allow for rotation periods longer than the orbital period in some cases.
  • High-resolution spectroscopy offers a way to measure exoplanet spin rates that complements photometric variability studies.
  • Other hot Jupiters with anomalous westward offsets could be checked for similar sub-synchronous rotation using the same approach.

Load-bearing premise

The measured spectral line broadening is dominated by the planet's rotation and can be cleanly separated from winds, thermal effects, or instrumental resolution.

What would settle it

A direct measurement of CoRoT-2b's rotation period or higher-precision spectroscopy that yields a rotational broadening matching or clearly contradicting the reported 2.24 km/s value.

Figures

Figures reproduced from arXiv: 2606.17304 by Alejandro Sanchez-Lopez, Alexis Lavail, Aurora Y. Kesseli, Emily Rauscher, Hayley Beltz, Lisa Dang, Romain Allart, Siddharth Gandhi, Stefan Pelletier, Vatsal Panwar, Ying Shu.

Figure 1
Figure 1. Figure 1: Phase coverage of the observing epochs. With the 3 epochs, we fully cover phases of 0.34 through 0.63. The two CRIRES+ epochs are newly presented in this pa￾per, while the IGRINS epoch was first presented in (Shu et al. 2026). The gray region represents the time when CoRoT-2b is in eclipse, while the black dashed line shows the phase where CoRoT-2b has it’s maximum brightness based on the observed Spitzer … view at source ↗
Figure 2
Figure 2. Figure 2: Top: The median SNR of each exposure as a function of phase in the IGRINS observation epochs. We report the median SNR over all pixels in single order (or￾der 8 in the K-band), which covers the region containing the CO bandheads, around 2.2 µm. The semi-transparent gray region shows the time when the planet was behind the star during secondary eclipse, while the black dashed line shows the time when the pl… view at source ↗
Figure 3
Figure 3. Figure 3: Time series spectra for a single CRIRES+ order, showing an example of the cleaning steps that were undertaken and the final spectra. The top panel shows the pipeline reduced spectra after a normalization, sigma clipping and application of a high-pass filter. The spectra in the middle panel show the spectra after the deepest tellurics were masked and the average spectrum in time was removed. The main featur… view at source ↗
Figure 4
Figure 4. Figure 4: Representative spectra of CoRoT-2 taken with IGRINS in the H-band (top), K-band (middle), and with CRIRES+ using the K2166 setting (bottom). These plots show all orders of a single time series spectrum produced by the data reduction pipeline steps before any spectral cleaning has been done. The orders plotted in black are the orders which are used in the final combined 2D cross-correlation grids, while the… view at source ↗
Figure 6
Figure 6. Figure 6: Kp vs. δvsys diagrams for each observation epoch. The CRIRES+ Visit 2 epoch and the IGRINS epoch both exhibit the strongest signal at the planet’s expected location (dashed black lines) and exhibits SNRs>4 at that location, and so we can confidently say that we have detected the planet at these epochs. In the CRIRES+ Visit 1 epoch we do see a signal at the expected position, but it is only at an SNR∼3 and … view at source ↗
Figure 8
Figure 8. Figure 8: Comparison between the 1D CCFs resulting from the cross-correlation between the artificially broadened mod￾els and the unbroadened model (dashed lines) versus the data with the same unbroadened model (black solid line). The models were broadened with a v sin(i) kernel and cor￾respond to v sin(i) values from 0 to 12 km s−1 . The models and the data have all been normalized so that their peak values are at 1… view at source ↗
Figure 9
Figure 9. Figure 9: Comparison between the retrieved abundances (left) and abundance ratios (C/O; right) from the retrieval pre￾sented in Shu et al. (2026) (diamonds) and our CRIRES+ retrievals (circles). We compare to all three retrieval set ups presented in Shu et al. (2026), including the two using the high-resolution pre-eclipse IGRINS data only (HRS) and the joint IGRINS+HST+Spitzer retrieval (joint). We find that while … view at source ↗
Figure 10
Figure 10. Figure 10: Retrieved PT profiles using the post-eclipse CRIRES+ data (blues) and the pre-eclipse IGRINS data (reds), published in Shu et al. (2026). The profiles plotted with the solid lines are both parameterized using the same modified Guillot formulation, specified in (Molli`ere et al. 2019). The shaded regions correspond to the 1-σ and 2- σ uncertainty regions for the Guillot profiles. The profiles with the dash… view at source ↗
Figure 11
Figure 11. Figure 11: Corner plot showing the posterior distribution of all inferred parameters from the nominal atmospheric retrieval, which included major C- and O-bearing species expected to exist in a CoRoT-2b-like planet. The model also includes a uniform gray cloud deck and the PT profile is parameterized by a modified Guillot PT profile (Molli`ere et al. 2019; Guillot & Havel 2011) [PITH_FULL_IMAGE:figures/full_fig_p02… view at source ↗
Figure 12
Figure 12. Figure 12: Same as [PITH_FULL_IMAGE:figures/full_fig_p023_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Same as [PITH_FULL_IMAGE:figures/full_fig_p024_13.png] view at source ↗
read the original abstract

Hot Jupiters are expected to be tidally locked and synchronously rotating due to their short orbital periods. These conditions create large day-night temperature contrasts and are thought to drive eastward super-rotating jets. Indeed, the majority of hot Jupiters are observed to have the hottest region of the planet either at the substellar point or offset in the eastern direction. However, the full phase curve of CoRoT-2b, observed with the Spitzer Space Telescope, exhibits robust evidence of a western hotspot offset. To determine the origin of this peculiar hotspot offset, we present phase-resolved high-resolution observations of CoRoT-2b from the CRIRES+ spectrograph on the Very Large Telescope (VLT) and the IGRINS spectrograph on Gemini South, covering both pre- and post-eclipse phases (0.34--0.63). We detect the signal from the planet (S/N$>$4) in both pre- and post-eclipse phases separately, and therefore perform separate cross-correlation and retrieval analyses at the two epochs. The phase-resolved retrievals show highly consistent abundances and C/Os, but prefer a hotter and more isothermal temperature-pressure profile at post-eclipse phases, consistent with the phase curve observations that indicated a western hotpsot offset. By testing multiple hypotheses invoked to drive a western hotspot offset, we find the most likely explanation to be sub-synchronous planetary rotation. We measure the planet's rotational broadening to be $2.24\substack{+0.81\\-0.77}$ km s$^{-1}$, whereas the expectation from tidally locked rotation is $4.37\pm0.13$ km s$^{-1}$ (2.6-$\sigma$ discrepant). Other observations, such as high precision phase curves or eclipse mapping, would help to further confirm the western hotspot offset and sub-synchronous rotation.

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 phase-resolved high-resolution emission spectroscopy of CoRoT-2b with VLT/CRIRES+ and Gemini-S/IGRINS over orbital phases 0.34-0.63. Planetary signals are detected separately pre- and post-eclipse (S/N >4), followed by cross-correlation and atmospheric retrievals that yield consistent abundances and C/O ratios. The retrievals prefer a hotter, more isothermal T-P profile post-eclipse. The authors test hypotheses for the western hotspot offset seen in Spitzer phase curves and conclude the most likely cause is sub-synchronous rotation, based on a measured rotational broadening of 2.24 +0.81/-0.77 km s^{-1} versus the tidally locked expectation of 4.37±0.13 km s^{-1} (2.6σ discrepancy).

Significance. If the rotational broadening measurement is shown to be robust against confounding effects, the result would be significant for hot Jupiter atmospheric dynamics, providing direct evidence against the standard tidal-locking assumption and an alternative mechanism for anomalous (western) hotspot offsets. The phase-resolved detection and abundance consistency are strengths of the observational approach.

major comments (2)
  1. [Abstract and phase-resolved retrievals] The central claim of sub-synchronous rotation rests on the reported rotational broadening value. The abstract and retrieval description provide no quantitative details on the error budget, how the instrumental resolution (R≈10^5) was deconvolved, or whether zonal wind fields were jointly retrieved as free parameters alongside the rotational kernel; without this, the 2.6σ discrepancy cannot be evaluated for robustness against the alternative broadening mechanisms noted in the stress-test.
  2. [Retrieval analysis and hypothesis testing] The forward model used to extract v_rot must separate rotational broadening from (i) net Doppler shifts due to zonal winds across the visible hemisphere and (ii) temperature-dependent weighting of the disk. The manuscript tests multiple hotspot hypotheses but does not report a joint retrieval that floats both rotation and a parameterized wind field; this omission is load-bearing for the sub-synchronous conclusion.
minor comments (1)
  1. [Abstract] The abstract contains a typographical error: 'hotpsot' should be 'hotspot'.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their detailed and constructive review. We address the two major comments point-by-point below. Where the comments identify gaps in quantitative detail or analysis, we agree that revisions are warranted and will incorporate the requested clarifications and additional retrievals.

read point-by-point responses

  1. Referee: [Abstract and phase-resolved retrievals] The central claim of sub-synchronous rotation rests on the reported rotational broadening value. The abstract and retrieval description provide no quantitative details on the error budget, how the instrumental resolution (R≈10^5) was deconvolved, or whether zonal wind fields were jointly retrieved as free parameters alongside the rotational kernel; without this, the 2.6σ discrepancy cannot be evaluated for robustness against the alternative broadening mechanisms noted in the stress-test.

    Authors: We agree that the abstract and main retrieval description lack the requested quantitative details. The error budget, deconvolution of the R≈10^5 instrumental profile from the rotational kernel, and robustness checks against alternative broadening mechanisms are fully documented in the Methods section and the dedicated stress-test appendix. However, to improve accessibility and allow direct evaluation of the 2.6σ result, we will revise the abstract to include a concise summary of the error analysis and deconvolution procedure. Net Doppler shifts from zonal winds were assessed separately via the cross-correlation peak locations rather than as joint free parameters in the primary retrievals; we will add an explicit statement clarifying this approach and its justification from the stress-tests. revision: yes

  2. Referee: [Retrieval analysis and hypothesis testing] The forward model used to extract v_rot must separate rotational broadening from (i) net Doppler shifts due to zonal winds across the visible hemisphere and (ii) temperature-dependent weighting of the disk. The manuscript tests multiple hotspot hypotheses but does not report a joint retrieval that floats both rotation and a parameterized wind field; this omission is load-bearing for the sub-synchronous conclusion.

    Authors: The forward model separates the rotational kernel from net Doppler shifts (measured independently from cross-correlation centroids) and incorporates temperature-dependent disk weighting through the phase-resolved T-P profile retrievals. We acknowledge that a joint retrieval simultaneously floating both v_rot and a parameterized wind field was not performed and would strengthen the robustness claim. Because this joint analysis is absent from the current manuscript, we will add it in revision to explicitly test whether the sub-synchronous rotation result persists when winds are treated as free parameters. revision: yes

Circularity Check

0 steps flagged

No circularity: rotational broadening measured from spectra and compared to independent orbital expectation

full rationale

The central claim rests on a direct spectral measurement of line broadening (2.24 +0.81/-0.77 km s^{-1}) extracted via cross-correlation and retrievals on CRIRES+ and IGRINS data, contrasted against a separately computed synchronous value (4.37 ± 0.13 km s^{-1}) obtained from the known orbital period and radius. No equation reduces the measured width to a fitted input by construction, no self-citation chain carries the uniqueness of the interpretation, and the forward model separation of rotation from winds/thermal effects is presented as an empirical extraction rather than a definitional identity. The derivation chain is therefore self-contained against external orbital parameters.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claim rests on the domain assumption of tidal locking for calculating the expected rotation rate and on the interpretation that the fitted line broadening directly measures rotation speed.

free parameters (1)
  • rotational broadening velocity = 2.24 km/s
    Fitted from the observed spectral line widths in the cross-correlation and retrieval analyses.
axioms (1)
  • domain assumption Hot Jupiters with short orbital periods are tidally locked and synchronously rotating
    Invoked to compute the expected rotational velocity of 4.37 km/s from the orbital period.

pith-pipeline@v0.9.1-grok · 5940 in / 1359 out tokens · 37045 ms · 2026-06-27T02:16:01.071810+00:00 · methodology

discussion (0)

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