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In a milestone statement distributed moments ago by the GPI Pre-delivery Acceptance Review Committee, Chair Stephen Goodsell announced that GPI is now clear for shipment from the University of California Santa Cruz to Gemini South in Chile.The Committee’s final report is slated for release on July 26th, but a statement sumarizing the results of the review is available now - GPI Review Committee: Final Day Statement 41 KB
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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.
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.
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.