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Magellan Planet Finder Spectrograph. Jeff Crane (OCIW) Steve Shectman (OCIW) Paul Butler (DTM). Background. Extrasolar planet search using the iodine absorption cell Doppler method Currently ~6 MIKE observing runs/year
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Magellan Planet Finder Spectrograph Jeff Crane (OCIW) Steve Shectman (OCIW) Paul Butler (DTM)
Background • Extrasolar planet search using the iodine absorption cell Doppler method • Currently ~6 MIKE observing runs/year • Want an instrument that is more optimized than MIKE for velocity measurement SAC Meeting
PFS vs. MIKE • Higher resolution (R4 grating vs. R2) • Better optical quality • Better thermal control • Very high quality flat-fielding (TDI) • Careful slit and pupil illumination SAC Meeting
Numbers • R4 reflection grating • R ~ 40,000 / arcsec • 0.7” x 3.5” slit, could go as small as 0.2” • 4096 x 4096 15mm pixel CCD • 0.09”/pixel • Complete coverage for 3900<l<6200Å • Goal is sv ~ 1 m/s SAC Meeting
Optical layout – spectrograph Optical design similar to one MIKE channel SAC Meeting
Echellogram SAC Meeting
Optical layout – fore optics • Functions: • Focal reduction from f/11 to f/5 • Slit viewing/centering • Slit focus SAC Meeting
Mechanical design *** Overall structure not yet finalized. One possibility SAC Meeting
PFS on the telescope • Clay telescope nasmyth mount • Static • 3-point ¼” thick mount points welded to nasmyth platform SAC Meeting
Operations Day(s?) before each run: • Refresh dewar vacuum • Possibly enable active thermal control • Day of the run: • Instrument change – alignment easy (!?) • During the run: • lN2 each morning SAC Meeting
Timeline Currently: • Optical design complete • Solid model design ~1/3 complete • Upcoming: • Optical figuring begins within weeks • Machining begins late Summer First Light: Fall 2006 ish SAC Meeting
Fore optics – slit focus SAC Meeting
Fore optics – slit centering SAC Meeting