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The gaps between the three detectors in GMOS cause gaps in the spectral coverage, see the example. The size of the gaps in wavelength space depends on the grating used, but is typically a few nanometers. If continuous spectral coverage is essential for your program, consider using two configurations of the grating with central wavelengths 3-5 nm different.
The GMOS-North light curve (top panel) and Fourier transform (bottom panel) for the optical companion to PSR J1738+0333. A comparison star is shown in blue, offset by -7%. We mark the 4 sigma and 3 sigma significance level as dashed green and blue lines, respectively. The three significant pulsations are marked with red lines in the bottom panel and the frequency solution is illustrated in the top panel.
Journey through the Universe 2015
This patch release of the "commissioning" release of the Gemini IRAF data reduction package is being made available to assist in the reduction of the Hamamatsu data, pending the next stable release of the Gemini IRAF package. In addition, this release is to allow users to provide valuable feedback as to the status of the data reduction package for GMOS-S Hamamatsu data. Please provide any feedback, comments or questions etc., via the Gemini HelpDesk system as described in the notes below for the v113_COMM release.
Detector characteristics are given in this section. Note that the GMOS-South detectors have been upgraded in 14B. Note also that the telescope optics are now silver-coated, reducing the system throughput in the blue.
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Due to ongoing problems with its cold heads, GNIRS is about to be removed from the telescope and warmed up for closer inspection. We should know by Friday October 10th whether this intervention has been successful. The instrument will not be available for observations during this period, and NIRI will be installed on the GNIRS telescope port instead (see the 2014B telescope schedule: http://www.gemini.edu/sciops/metrics/gn2014Boverview.html).
This information refers to the EEV detectors at GMOS-S. These were removed in May 2014 and are no longer available. The Hamamatsu detectors were installed in June 2014.
The GMOS South detector array consists of three 2048x4608 EEV chips arranged in a row. The table below gives a summary of the current detector/controller characteristics.
Gemini Observatory is pleased to announce the release of the Gemini Instrument Feasibility Studies Request for Proposals (RfP).
Please visit this page for full details.