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MINERVA control software effortlessly
alters robotic telescope operations
Achieving sub-millimagnitude precision
with one MINERVA telescope
Meeting the challenge of bright star photometry
with MINERVA
· 4 telescope array
· 0.7m diameter per telescope
· Doppler Shift precision < 1 m/s
· Photometric precision < 1 mmag
Fig. 2: After observing these two defocused bright stars
(undergoing no exoplanet transit) via 1 telescope, a
photometric precision of 2.7 mmag was achieved [1].
Fig. 3: Once binned down to timescale of ~200s (or 3 min),
the observational scatter of the 16 Cyg A light curve
is < 1 mmag [1].
References
[1] Swift et al., 2015, JATIS 1, 2
Acknowledgements
This work is supported by the
National Science Foundation
Want More Details?
https://mwilson1.github.io/research/projects.html
Maurice Wilson
My code allows us to conduct automated observations such as this example.
To avoid saturating the CCD with our bright targets, we use the defocusing technique.
Timescale (s)
RM
S (
mm
ag)
Rel
ativ
e M
agni
tude
(m
mag
)
Time since start (minutes)
· Location: Mt. Hopkins in Arizona
· Mission: Detect, confirm, and characterize nearby Earth-like exoplanets
· Optimize control software of robotic telescopes for photometric and spectroscopic observations
High Precision Photometry of Bright Transiting Exoplanets
with MINERVA
Fig. 1: Demonstration of MINERVA’s 4 telescopes observing distinct
regions of the sky (Credit: Miguel Claro). With MINERVA, 3 additional
telescopes can be used to find the bright comparison stars needed to
conduct relative photometry.
Maurice Wilson, Jason Eastman, John Johnson
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; [email protected]
MINERVA specs MINERVA objectives
Graduate Research Fellowship Program.