MINERVA Small planets from small telescopes Jason T Wright 1 , John Asher Johnson 2 , Nate McCrady 3 , Rob Wittenmyer 4 Jon Swift, Mike Bottom, Reed Riddle (Caltech), Phil Muirhead (BU), Ming Zhao 1 Center for Center for Exoplanets and Habitable Worlds 1 2 3 4 MINERVA’s first telescope, T1 at its commissioning home in Pasadena (Photo credit Mike Wong) MINERVA will use at least 4 PlaneWave CDK-700’s for an effective aperture of 1.24-m (Photo credit Mike Wong) MINERVA will reside at The Ridge on Mt. Hopkins (the site of the decommissioned VERITAS telescope) WASP12b −50 0 50 100 Normalized Flux − 1 (ppt) P = 1.0914225 d R p /R * = 0.1308 +/− 0.0020 t 0 = 2456621.95685 +/− 0.00059 JD T dur = 2.983 +/− 0.0397 h b = 0.30 ρ * (fit) = 0.449 g/cc ρ * (init.) = 0.440 g/cc LD lin = 0.458 LD quad = −0.229 χ r 2 = 1.024 −0.05 0.00 0.05 0.10 Time from Mid−Transit (d) −10 −5 0 5 10 Residuals (ppt) Detection of WASP-12b by T1 from Pasadena with a commissioning camera. Derived depth is within 1-σ of literature value. Each MINERVA telescope will have a photometric camera at the Nasmyth port opposite the fiber for transit photometry and educational / public outreach use MINERVA is funded by its partner institutions (1-4, at top); NASA EPSCoR under cooperative agreement NNX13AM97A; Australian Research Council grant LE140100050; and the UNSW Major Research Equipment and Infrastructure Initiative MINERVA will be fully automated and robotic, with heritage from Robo-AO (software architecture designed by Reed Riddle) and the MEarth and HAT programs at Mt. Hopkins Monte Carlo simulation results for a nominal 3 year survey with 4 dedicated telescopes on 80 bright G, K, and early M dwarfs. Conservative extrapolation of Kepler results with realistic weather and jitter yields 14 ± 4 planets, with 3 ± 1 in Habitable Zone. The gray region is MINVERA’s new search space around these well-studied bright stars. The four telescopes will independently and simultaneously feed a stabilized, iodine-calibrated spectrograph, which will achieve 0.8 m/s single-shot precision. Key optics will be in vacuum and the entire spectrograph will be temperature stabilized to ±0.01 K. Shown here, ray trace diagram and mechanical design of KiwiSpec-M (Barnes et. al., SPIE 2012, 8446, 88), similar to final MINERVA design. Fiber-Aquisition Unit (FAU) design, one of the only elements not off-the-shelf (design and construction by P. Muirhead). Each of the four MINERVA telescopes guides and collects starlight independently. The four fibers each produce an independent trace in the echelle spectrograph
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MINERVASmall planets from small telescopes
Jason T Wright1, John Asher Johnson2, Nate McCrady3, Rob Wittenmyer4 Jon Swift, Mike Bottom, Reed Riddle (Caltech), Phil Muirhead (BU), Ming Zhao1
Center forExoplanets and Habitable Worlds
Center forExoplanets and Habitable Worlds
1 2 3 4
MINERVA’s first telescope, T1 at its commissioning home in Pasadena
(Photo credit Mike Wong)
MINERVA will use at least 4 PlaneWave CDK-700’s for an effective aperture of 1.24-m (Photo credit Mike Wong)
MINERVA will reside at The Ridge on Mt. Hopkins (the site of the decommissioned VERITAS telescope)
WASP12b
−50
0
50
100
Nor
mal
ized
Flu
x −
1 (p
pt)
P = 1.0914225 dRp/R* = 0.1308 +/− 0.0020t0 = 2456621.95685 +/− 0.00059 JDTdur = 2.983 +/− 0.0397 hb = 0.30
ρ* (fit) = 0.449 g/ccρ* (init.) = 0.440 g/ccLD lin = 0.458LD quad = −0.229χr
2 = 1.024
−0.05 0.00 0.05 0.10Time from Mid−Transit (d)
−10−5
05
10
Res
idua
ls (p
pt)
Detection of WASP-12b by T1 from Pasadena with a commissioning camera. Derived depth is within 1-σ of literature value. Each
MINERVA telescope will have a photometric camera at the Nasmyth port opposite the fiber for transit photometry and
educational / public outreach use
MINERVA is funded by its partner institutions (1-4, at top); NASA EPSCoR under cooperative agreement NNX13AM97A; Australian Research Council grant
LE140100050; and the UNSW Major Research Equipment and Infrastructure Initiative
MINERVA will be fully automated and robotic, with heritage from Robo-AO (software architecture designed by Reed Riddle) and the MEarth and HAT programs at
Mt. Hopkins
Monte Carlo simulation results for a nominal 3 year survey with 4 dedicated telescopes on 80 bright
G, K, and early M dwarfs. Conservative extrapolation of Kepler results with realistic weather and jitter
yields 14 ± 4 planets, with 3 ± 1 in Habitable Zone. The gray region is MINVERA’s new search
space around these well-studied bright stars.
The four telescopes will independently and simultaneously feed a stabilized, iodine-calibrated spectrograph, which will
achieve 0.8 m/s single-shot precision. Key optics will be in vacuum and the entire spectrograph will be temperature stabilized to ±0.01 K. Shown here, ray trace diagram and mechanical design of KiwiSpec-M (Barnes et. al., SPIE 2012, 8446, 88), similar to final MINERVA design.
Fiber-Aquisition Unit (FAU) design, one of the only elements not off-the-shelf (design and construction by P. Muirhead). Each of the four MINERVA telescopes guides and collects starlight independently. The four fibers each produce an independent trace in the echelle spectrograph
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