Bibcode
Birkby, J.; Alonso, R.; Hoyer, S.; Lopez-Morales, M.
Referencia bibliográfica
American Astronomical Society, AAS Meeting #229, id.202.06
Advertised on:
1
2017
Número de citas
0
Número de citas referidas
0
Descripción
High-resolution spectroscopy (R>100,000) is a robust and powerful
tool for directly characterizing exoplanet atmospheres that is
applicable to both transiting and non-transiting planets, as well as
those with relatively large projected separation angles. In the
infrared, the technique has unambiguously revealed the presence of
complex molecules, such as water, in hot Jupiters, as well as measuring
exoplanet rotation rates and their day-to-night winds. In the optical,
the technique is highly suited to characterizing the atmosphere of our
nearest rocky neighbor, Proxima b, by detecting the Doppler shift and
modulation of its host star spectrum as reflected by the planet’s
dayside. However, the technique is currently not yet robustly proven at
optical wavelengths. Here, we present new results on the non-transiting
hot Jupiter, 51 Peg b, using 5 half nights of optical HARPS-N
spectroscopy from the 3.5m TNG telescopes. We aimed to detect reflected
light from the planet’s dayside and obtain one of the most
detailed exoplanet reflection spectra to date, spanning 387-691 nm in
bins of 50nm. Our goal is to strongly constrain previous claims of a
very high albedo or highly inflated radius for 51 Peg b and assess the
potentially cloudy nature of the planet. This will also guide us in
using high-resolution spectroscopy to characterize Proxima b in the era
of the extremely large telescopes.This work was performed in part under
contract with the California Institute of Technology/Jet Propulsion
Laboratory funded by NASA through the Sagan Fellowship Program executed
by the NASA Exoplanet Science Institute.