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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.
Figure 1. Stellar Kinematic Maps of M60-UCD1 showing clear rotation and a dispersion peak. Panels a and b show the measured radial velocities (bulk motions towards & away from us) and velocity dispersions (random motions) of the stars in M60-UCD1 with typical errors of 6 km/s. Black contours show isophotes in the K band stellar continuum.
Example bias images are available for the following instrument/detector combinations:
The current version of the GMOS Mask Making software (GMMPS) is v0.4.1, released in 2014-08-27 for Linux and Mac OS X. This is an interim version to provide support for the new Hamamatsu detectors in GMOS-S. It is not yet fully backwards compatible (see below).
!! VERY IMPORTANT NOTE for GMOS-S users, concerning the Hamamatsu detector upgrade -- PLEASE READ !!
Figure 1. Part of MACS J0416-2403 seen by GSAOI. The average angular resolution is about 80 milliarcseconds, the full field-of-view of the data released is nearly twice as large as shown here.
The latest version of the Gemini MOS Mask Preparation Software (GMMPS 0.4.1) is now available. Please see the GMMPS web page for more information and download links.
Calibrations for GNIRS consist of the following measurements.
The table below gives gain/read-noise values for the current GMOS Hamamatsu CCDs measured in September 2014.
Note: GMOS South data
obtained before May 19, 2014 should use the previous gain/read-noise values.
|SDSU Gain number||