Figure 4 from Detection and Bulk Properties of the HR 8799 Planets with High-resolution Spectroscopy

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Detection and Bulk Properties of the HR 8799 Planets with High-resolution Spectroscopy

Authors: Jason J. Wang, Jean-Baptiste Ruffio, Evan Morris, Jacques-Robert Delorme, Nemanja Jovanovic, Jacklyn Pezzato, Daniel Echeverri, Luke Finnerty, Callie Hood, J. J. Zanazzi, Marta L. Bryan, Charlotte Z. Bond, Sylvain Cetre, Emily C. Martin, Dimitri Mawet, Andy Skemer, Ashley Baker, Jerry W. Xuan, J. Kent Wallace, Ji Wang, Randall Bartos, Geoffrey A. Blake, Andy Boden, Cam Buzard, Benjamin Calvin, Mark Chun, Greg Doppmann, Trent J. Dupuy, Gaspard Duchêne, Y. Katherina Feng, Michael P. Fitzgerald, Jonathan Fortney, Richard S. Freedman, Heather Knutson, Quinn Konopacky, Scott Lilley, Michael C. Liu, Ronald Lopez, Roxana Lupu, Mark S. Marley, Tiffany Meshkat, Brittany Miles, Maxwell Millar-Blanchaer, Sam Ragland, Arpita Roy, Garreth Ruane, Ben Sappey, Tobias Schofield, Lauren Weiss, Edward Wetherell, Peter Wizinowich, and Marie Ygouf

2021 The Astronomical Journal 162 148.

Provider: AAS Journals

Caption: Figure 4.

The 1D extracted spectra (black) from the fiber placed on each planet and the best-fitting forward model from echelle order 33. The forward model (blue) has been deconstructed into its two constituent parts: the stellar model (cyan) built from a linear combination of on-axis stellar spectra and the planet model generated from the BT-Settl atmospheric models (red). The residuals to the fit are plotted as gray circles and appear to be dominated by uncorrelated noise. A zoomed-in version of this plot is available in Appendix B.

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