1RXS J1609b), confirming the feasibility of direct spectrographic studies of exoplanets.[2][8]
Spectra
The spectrum of the planet HR 8799 c. The spectrum of the star and the planet was obtained with the NACO adaptive optics instrument on ESO’s Very Large Telescope.
Near infrared spectroscopy from 995 to 1769 nanometers made with the Palomar Observatory show evidence of ammonia, perhaps some acetylene but neither carbon dioxide nor substantial methane.[9] High resolution spectroscopy with the OSIRIS instrument on the Keck Observatory show numerous well resolved lines of molecular absorption in the planet's atmosphere in the K band. Although methane is absent, the planet's atmosphere contains both water and carbon monoxide; the carbon-to-oxygen ratio of HR 8799 c is higher than that of its star, suggesting that the planet formed through the core accretion process.[10][11]
Later, in November 2018, researchers confirmed the existence of
23h 07m 28.7150s, +21° 08′ 03.302″.jpg)
Media related to HR 8799 c at Wikimedia Commons
