Figure 13.
Using advanced
imaging techniques and
the special capabilities
of the Gemini Planet
Imager (GPI), the light
from β Pictoris has been
suppressed in these
images using GPI’s Y,
J, H, K1, and K2 filters.
The arrow indicates
the location of the
exoplanet β Pictoris b in
in all but the left image.
Based on the GPI data, combined with
planetary evolution and atmospheric mod-
els, Chilcote suggests a “hot-start” planet
formation scenario for β Pictoris b, which
has a surface temperature of about 1,724
K. He adds, “This is consistent with the disk
instability formation mechanism for wide-
orbit giant exoplanets.” However, the char-
acteristics for the atmosphere of β Pictoris
b found in this work best matches that of
a low-surface-gravity (L2±1) brown dwarf,
not a planet.
John Blakeslee is the Chief Scientist at Gemini Ob-
servatory and located at Gemini South in Chile.
He can be reached at: [email protected]
Peter Michaud is the Public Information Out-
reach Manager of Gemini Observatory. He can
be reached at: [email protected]
The team studied β Pictoris b during the
verification and commissioning of the
Gemini Planet Imager, and as part of an
astrometric (position) monitoring program
designed to constrain the orbit of the exo-
planet (Figure 13). This work is also part of
a Gemini Large and Long Program.
“With GPI, the Gemini Observatory is at
the forefront of exoplanet exploration,”
says Chilcote. He adds, “Direct imaging al-
lows for the discovery of planets on solar-
systems-scale orbits, provides new insight
into the formation and characteristics of
extrasolar systems, and enables direct
spectroscopic observations of their atmo-
spheres.”
The full results are accepted for publica-
tion in The Astrophysical Journal Letters. A
preprint is available here.
48
GeminiFocus
January 2018 / 2017 Year in Review