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False-color image of SPT-CL J0546–5345 at z = 1:067. Gemini GeMS/GSAOI Ks (this work) = red, HST ACS F814W = green, HST ACS F606W = blue. The red polygon shows the approximate sky coverage of the GSAOI pointings. PSF stars are indicated by white circles. The star near the top of the image with two circles is a binary star. The inset at lower left is a zoom-in of the cluster core.
Gemini encourages collaborations and will provide a forum for those seeking additional partners to complete a team for this work. Groups interested in Instrument Upgrades who may lack the expertise needed to complete the work should submit a notice of intent and use this forum to find additional partners for the work.
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