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The GNIRS team strongly recommends that users start from the automatically-generated OT templates and the GNIRS OT library when preparing GNIRS observations. The library contains detailed instructions for customising the template observations: changing targets, standard stars, slit widths, wavelengths, etc. This web page is intended to explain the various OT components in more depth:
This page provides instructions for completing Phase II Science Programs for all Gemini North and Gemini South instruments. It includes submission details and notes of any procedural changes. Please read this page carefully!
The table below summarises the classically-scheduled programs that have been awarded time on Gemini North and South, as well as programs from the Gemini community awarded Exchange time on Subaru. Jump directly to the schedule for:
The 2016B Gemini Observing Tool is now available for download. This update is required to access the Gemini Observing Databases.
Gemini North and South are accepting proposals for the Fast Turnaround (FT) program. Here, we give information specific to this proposal cycle. Please see the other FT pages - particularly the rules - for general information about the program. FT-specific proposal templates must now be used for all FT proposals; see the "PIT information" section below.
Figure 1. (Left:) Zoom-in images on HD 95086 b obtained with GPI at the first and last epochs. The magenta crosses show the measured positions (for clarity, the size of the symbol is not representative of the precision). Significant orbital motion is detected within the GPI data. (Right:) Deepest image obtained on HD 95086 with GPI at K1 on April 8, 2015.
Before low-medium mass stars become white dwarfs they pulsate wildly and eventually spew their outer layers into space – often forming beautiful planetary nebulae. The same stars are predicted to continue pulsating during their transformation to a white dwarf, if they have helium in their atmospheres. A team from the University of Oklahoma used Gemini North, in conjunction with the 1.2-meter FLWO telescope in Arizona, to observe a much-sought-after link between these pulsations and helium in the star’s atmospheres.