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Figure 1. Artist's rendition of UY Aur's probable outflow system. Credit: National Astronomical Observatory of Japan, All Rights Reserved.
The following table shows a summary of GCAL emission line plots for two lamps (Ar and Xe) at near IR wavelengths. The spectra all have the same integration time. Wavelengths are in vacuum. See also the general wavelength calibration page for more line lists etc.
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.
The GPI Pipeline
The Gemini Planet Imager Data Pipeline allows transformation of raw data from GPI into calibrated spectral and polarimetric data cubes. It also provides some basic capabilities for PSF suppression through differential imaging, and for astrometry and spectrophotometry of detected sources.
Priority Visitor observing will be expanded beyond Large and Long Programs (LLP) in 2015A and offered to investigators of regular semester queue programs. Investigators wishing to have their program considered for PV observing should indicate their desire to participate in the Technical Design portion of their 2015A queue proposal.
GPI programs selected for Early Science Observations
The table below summarizes the programs that have been approved for GPI Early Science observations.