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We currently anticipate completing integration and testing of our data reduction software with AstroConda in November this year. In the meantime, our recommended platform is still Ureka 1.5.1 or 1.5.2.
Gemini North and W.M. Keck images of Io at different near-infrared wavelengths; the name of the filter is indicated in the black box at the start of each section. The bright spots are thermal emissions from Io’s myriad volcanoes. Note the increasing number of hot spots detected at longer wavelengths, i.e. towards the bottom of the figure. Credit: Katherine de Kleer and Imke de Pater, UC Berkeley/Gemini Observatory/AURA/W.M. Keck Observatory
An in depth discussion of the satellite spots can be found in GPI Observational Calibrations VIII: Characterization and Role of the Satellite Spots. by Wang et al.
GPI Contrast and sensitivity
Achieved sensitivity is a function of many parameters, including contrast, inner working distance, brightness of the central star (if any), observing mode (dithered, sky-offset, sky-rotation), and, weather conditions.
Contrast as function of I-magnitude of the star
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.
The purpose of these page is to give quick guidelines to both Contact Scientists, NGO's and PI's to make sure that the defined observations in the OT are correctly defined.
The Phase II check point of view GPI consists of 4 components as these are driving the Phase II checking.