For more detailed information than the summary specs presented below,
please see the SPIE papers. Note that PFS is undergoing upgrades in 2018
that include a new detector (installed February 2018) and a fiber-based
pupil slicer (to be installed Fall 2018)|
Wavelength range: Fixed format covering 391 to 734nm.
Slits and Resolving Power:
Scale and Dispersion: 0.054 arcsec/pixel, ~0.009 Angstroms/pixel
|Width (")||Length (")||Resolving Power
|0.3||2.5||127,000||Default as of 2018|
|0.5||2.5||76,000||Default prior to 2018|
|0.7||3.9||N/A||For Wide Flats|
|0.3||-||N/A||Pinhole; For Focus|
Velocity precision: 1 meter/sec
Detector: STA1600 CCD, 10K x 10K, 9 micron pixels.
Slit viewer field of view: 38x38 arcsec
|Speed||Read Noise (e-)||Gain (e-/ADU)
||Readout time (sec)|
|Normal (250 kHz)||3.59||2.29||62|
|Turbo (100 kHz)||4.14||2.30||26|
Calibration sources: Thorium Argon lamp, Quartz lamp, Iodine
Practical faint magnitude limit: Somewhere between V=15 and V=16,
limited by star visibility in slit viewer
Efficiency: Peak instrumental efficiency is around 23%
Instrumental efficiency from entrance aperture to detector.|
This does not include slit losses, telescope efficiency, or atmospheric
absorption, but does include the QE of the CCD.
AB magnitude zero point.|
This is the AB magnitude of an object from which one expects to receive 1
electron/sec/Angstrom at 1 airmass without a slit. Depending on the airmass,
seeing, and choice of slit, actual count rates will be lower.