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Deep Limits on Planets Exterior to HR 8799’s Known Planetary System with the James Webb Space Telescope

  • Authors: Bryden Geoffrey, Llop-Sayson Jorge, Beichman Charles A., Balmer William O., Kammerer Jens, Leisenring Jarron M., Ygouf Marie, Krist John, Faramaz-Gorka Virginie, Greenbaum Alexandra Z., Girard Julien, Perrin Marshall, Pueyo Laurent, van der Marel Roeland, Meyer Michael, Johnstone Doug, Hodapp Klaus, Rieke Marcia

Bryden Geoffrey et al 2026 The Astronomical Journal 171 .

  • Provider: AAS Journals

Caption: Figure 5.

The emission from planets c (top), d (middle), and e (bottom) in the F356W filters is fit to a simulated PSF. As in Figure 4, the planet emission (left) is well fit by the model PSF (center) and clean residuals (right), except that planets c and d are clearly visible in the residuals for planet e (lower right). For the planets closest to the central star (d and e) the star remains in the frame (asterisks). The photometry and astrometry for all extracted point sources are given in Table 4.

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