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Semester 2017B

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!

 


 

2016 Annual Report and 2017 Program Plan of the Gemini Observatory

Long-slit Spectroscopy

Long slit spectroscopy can be obtained in either normal or Nod-and-Shuffle modes using GMOS standard slits or custom slits.

Gemini Tracks Distant Star Cluster with Adaptive Optics

Figure 1: Gemini Multi-Object Spectrograph (GMOS-South) of the Pyxis field (left image), with the center of the cluster marked with a red star. A zoom of the pseudo color image of Pyxis observed with the Gemini South Adaptive Optics Imager (GSAOI) used with the Gemini Multi-conjugate adaptive optics System (GeMS) is shown at right. The field of view of GMOS is 5 x 5 arcminutes, 85 x 85 arcseconds for GeMS.

GMOS-North Fringing

The GMOS-N E2V DD CCDs, used between Nov 2011 and Feb 2017, had much weaker fringing than the original GMOS-N EEV CCDs or the new Hamamatsu CCDs. This page shows examples of fringe frames in imaging mode.

Spectroscopy Overview

Three types of spectroscopy are possible with each GMOS and its selection of gratings.

 

 

Fringing

The GMOS-N and GMOS-S EEV detectors had significant fringing in the red. The GMOS-N DD E2V detectors, which were in operation until February 2017, and the new GMOS-N and GMOS-S Hamamatsu detectors exhibit much less fringing than the original EEV detectors. The pages in this section show examples of fringe frames in imaging mode as well as science data before and after correction for fringing.

 

  • GMOS-North
  • GMOS-South