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Imagen en el infra-rojo cercano del cúmulo globular Liller1 obtenida con el sistema de óptica adaptiva GeMS en el telescopio de Gemini Sur, en Chile.
To properly reduce GPI observations one must download the proper calibrations. This document describes how the user can download all types of calibrations from the GSA. The user should read the instructions here on how to access the GSA, these instructions are only details on how to access GPI particular data.
Figure 1. Image of HD 115600 showing a bright debris ring viewed nearly edge-on and located just beyond a Pluto-like distance to the star. One or more unseen solar system-like planets are causing the disk center (diamond) to be offset from the star's position (cross).
This section contains instructions for configuring GPI at phase II. It is organised as follows:
A Gemini Facility Calibration Unit (GCAL) is available on each Gemini telescope, providing continuum and line emission light sources for wavelength and flat-field calibrations. Each GCAL is located permanently on one port of the instrument support structure and light is directed into an instrument by the science fold mirror. The GCAL optics simulate the f/16 telescope beam, illuminating the instrument pupil in the same way as light from an astronomical source.
This section describes both the data format for all Gemini instruments, including GMOS, and the Gemini IRAF Package, which supports imaging, as well as long-slit, multi-object, and IFU spectroscopic data from both GMOS-N and GMOS-S.
Gemini is pleased to announce the launch of 4 feasibility studies as a result of the GIFS RfP process. The four studies (alphabetically) are GEONIS, GMOX, MOVIES, and OCTOCAM. Below is a brief synopsis of each study:
Left: J-band polarized intensity (P⊥) images. Right: P⊥ scaled by r2, where r is the distance in pixels from the central binary, corrected for projection effects. Both images are shown on a linear scale and oriented north up and east left. The coronagraph is represented by the black filled circles.