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Because TEXES is background photon noise limited and both the instrumental response and the background flux depend on wavelength, the instrument sensitivity depends strongly on wavelength and spectral resolution. Proposers are encouraged to contact TEXES team members for sensitivity estimates for observations at specific wavelengths, but can make initial estimates based on the table below.
When performing electrical troubleshooting at Gemini North telescope facility on Wednesday, February 26, one of our electrical specialists accidentally contacted a powered circuit and received an electrical shock. He was evacuated and evaluated at the nearest medical facility, and he has been released and advised that he could go back to work.
Gemini Observatory invites its community to propose scientific investigations for the 2014B semester, 1 August 2014 - 31 January 2015.
The original GMOS-N detector array consisted of three 2048x4608 EEV chips arranged in a row. This array was replaced by e2v deep depletion devices in October 2011.
The table below gives a summary of the original EEV detector/controller characteristics.
GPI Public Data Early Release Readme
Wavelength Calibration Accuracy & Flexure
This page is focussed on the wavelength calibration accuracy and the IFS flexure compensation.
Extended Objects: Europa Observations
Europa, satellite of Jupiter was observed on November 18, 2013 from 08:42:16 (airmass=1.63) to 08:48:16 (airmass=1.64) under average seeing conditions (DIMM seeing~0.6-0.8) in K1 band, and direct mode (no coronagraph, no apodizer). Eleven data cubes with a true integration time of 8.73 s were processed by M. Perrin using the recipe listed below.
Recipy used to process Europa Data