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Unraveling the Mystery of the Peculiar and Young Hot Jupiter CoRoT-2 b. II. Phase-resolved Emission Spectroscopy with Very Large Telescope/CRIRES+ and Gemini South/IGRINS

  • Authors: Aurora Y. Kesseli, Siddharth Gandhi, Lisa Dang, Alexis Lavail, Alejandro Sánchez-López, Ying Shu, Emily Rauscher, Hayley Beltz, Romain Allart, Stefan Pelletier, Vatsal Panwar

Aurora Y. Kesseli et al 2026 The Astronomical Journal 172 .

  • Provider: AAS Journals

Caption: Figure 7.

1D coadded CCFs in the planet’s rest frame at four different phase epochs. The CCFs are offset by a constant coefficient for clarity. The two bottom CCFs (orange and red lines) are both from the IGRINS visit, while the two top CCFs (purple and blue) are from CRIRES+ Visit 2. We do not measure a significant planet signal for preeclipse phases less than 0.4, but measure significant peaks at the other phase bins (with SNRs of 4.6, 4.0, and 4.2 for the CCFs from top to bottom). For all three phase bins our measured radial velocity offset is consistent with zero to within 1.5σ, although we do measure a nonsignificant slight blueshift preeclipse and slight redshift posteclipse.

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