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The GeMS / GSAOI laser run that was planned to take place this week had to be canceled. Unfortunately the laser and the Canopus Real Time Control system were not operational and in spite of intense efforts to resolve these problems in time for the laser window there was just not sufficient time to get the system in an operational state. We will continue to work towards ensuring that the upcoming January GeMS / GSAOI run will be a success.
Figure 1. Image of Cheshire Cat gravitationally lensed galaxies produced by combining Chandra X-ray data with Hubble Space Telescope optical data. Gemini spectroscopy provided critical spectroscopic data for characterizing the foreground lensing cluster and understanding its history and likely fate as a "fossil group." Image Credit: Hubble Space Telescope and Chandra X-ray Observatory
Gemini Observatory is pleased to announce the release of the public GIFS reports.
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National Gemini Offices
Gemini is operated by a partnership including the United States, Canada, Chile, Brazil, Argentina and the University of Hawaii. Each partner maintains a “National Gemini Office”.
Contact information for each of the partners:
Dr. Lydia S. Cidale
Facultad de Ciencias Astronómicas y Geofisicas
Universidad Nacional de La Plata
Instituto de Astrofísica La Plata (CONICET-UNLP)
Paseo del Bosque - B1900FWA - La Plata - Buenos Aires Argentina
Tel: +54-221-4236593 (ext: 153)
The Brazilian Gemini Office
Dr. Eder Martioli
Laboratório Nacional de Astrofísica
Rua Estados Unidos, 154
37504-364 Itajubá - MG
Phone: (+55)-35-3629-8220 (direct)
Phone: (+55)-35-3629-8110 (LNA general)
The Chilean Gemini Office
Prof. Edgardo Costa
The Chilean National Gemini Office
Programa de Astronomía
Comisión Nacional de Investigación Científica y Tecnológica de Chile
Bernarda Morin 551, Providencia, Santiago
Additionally, Gemini may have “limited-term partners” - countries or institutions who have acquired temporary access to a subset of the telescope’s operating modes. These may or may not maintain an NGO.
Contact information for the current limited-term partners (if none, contact the observatory directly):
K-GMT Science Program Office
Dr. Narae Hwang
Center for Large Telescopes
Korea Astronomy and Space Science Institute
776 Daedeokdae-Ro Yuseong-Gu
Daejeon 34055 Rep. of KOREA
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.
The GPI in the OT can be broken down into the following components:
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.