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The OCTOCAM study was led by Antonio de Ugarte Postigo and managed by Pete Roming and Christina Thöne. The project was coordinated from the Instituto de Astrofisica de Andalucia (IAA-CSIC), with main collaborators at the Southwest Research Institute, Fractal SLNE, and George Washington University. The study began in April 2015 and concluded in October 2015.
This page describes the steps to properly configure the instrument using the OT. Generally the user should use the skeleton templates that are created in Phase II and apply them to obtain the proper sequences. Instructions on for the general use of the OT can be found on the OT page and related links, as this page describes particular details for using OT with GPI. There is a GS-GPI-library available that contains complete examples of various modes and setups. Use the OT and select "libraries" and the program can be downloaded.
Figure 1. Color composite-image of IMS J2204+0111 at z=6 (about 1 billion years after the Big Bang). IMS J2204+0111 is the red object at the center and its distance from us is 12.8 billion light years. Because of the expansion of the universe, distant objects like IMS J2204+0111 move away from us almost at the speed of the light, making their light to shift into near-infrared wavelength (phenomenon, called “redshift”).
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.
GPI limiting magnitudes are determined by several components, the AO WFS (I-band), the LOWFS (H-band), and the IFS (selected filter). In addition the observing conditions add another layer of limits. Thus the brightest of the science object is limited in I band from the AOWFS, in H-band from the LOWFS (not a constraint in DIRECT mode as then no coronographic mask is used and no LOWFS is possible). It should be noted that it is NOT possible to observe without the AOWFS and Coronographic modes are NOT possible to observe without the LOWFS.
Gemini South optical engineers inspect the primary mirror after 7-hour coating process.
The 8.1 meter primary mirror suspended on the 4th floor, before descending to the stripping/coating area on the first floor of the observatory building.
The Gemini-S telescope is now back into operation following the planned maintenance shutdown.
30"x30" color composite g+r+i image using data from both Gemini and the NOT, highlighting the three brighter lensed quasar images for which time delays have now been measured. Image C leads all other images of the quasar by several years, and hence predicts the future behaviour.