Change page style: 

Cancelation of the November GeMS run

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.

Gemini Characterizes Cheshire Cat

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 Instrument Feasibility Study (GIFS) reports available.

Gemini Observatory is pleased to announce the release of the public GIFS reports.

Contact Us

Gemini Observatory
Northern Operations Center
670 N. A'ohoku Place
Hilo, Hawaii, 96720, USA
Phone: (808) 974-2500
Fax: (808) 974-2589
Gemini Staff Directory

Gemini Observatory
Southern Operations Center
c/o AURA, Casilla 603
La Serena, Chile
Phone: 56-51-220-5600
Fax: 56-51-220-5650
Gemini Staff Directory

General Inquiries
Safety
Operations general (science and engineering)
Development
Administration
Science Operations South
Science Operations North
Science user support inquiries including HelpDesk and Archive
Engineering & Mountain Operations South
Engineering & Mountain Operations North
Telescope Performance
Adaptive Optics Performance
Research Activity at Gemini
Public Information and Outreach
Instrumentation South
GPI
GeMS/GSAOI
GMOS-S
FLAMINGOS-2
Instrumentation North
NIRI
NIFS
GRACES
GNIRS
GMOS-N
General Inquiries
Logistics - North
Logistics - South


Polycom Videoconference Directory

Contact information for Gemini Polycom videoconference systems.



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:

United States | Canada | Chile | Argentina | Brazil | University of Hawaii

The United States Gemini Office
Dr. Verne Smith
National Optical Astronomy Observatory
PO Box 26732, Tucson, Arizona 85726, USA
vsmith@noao.edu

The Canadian Gemini Office
Dr. Stéphanie Côté
National Research Council Canada
5071 W. Saanich Road
Victoria BC, V9E 2E7, CANADA
Phone: 250-363-0026
Stephanie.Cote@nrc-cnrc.gc.ca

The Argentinian Gemini Office

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)
Fax: +54-221-4236591
argo@fcaglp.unlp.edu.ar

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)
brgo-head@lna.br

The Chilean Gemini Office
Prof. Edgardo Costa
The Chilean National Gemini Office
Programa de Astronomía
Comisión Nacional de Investigación Científica y Tecnológica de Chile
(CONICYT)
Bernarda Morin 551, Providencia, Santiago
CHILE
costa@das.uchile.cl


University of Hawaii Gemini Office
Roy Gal
Institute for Astronomy
University of Hawaii
2680 Woodlawn Dr.
Honolulu, HI 96822
(808) 956-6235
rgal@ifa.hawaii.edu


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):


The Australian Gemini Office
Dr. Stuart Ryder
Australian Astronomical Observatory
P.O. Box 915
North Ryde, NSW 1670, AUSTRALIA
Phone: 61 (02) 9372-4843
ausgo@aao.gov.au


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
Phone: +82-42-869-5822
Email: kgmtprop@kasi.re.kr

OCTOCAM Feasibility Study

Introduction

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.

Gemini Planet Imager Exoplanet Survey – One Year into the Survey

GPI OT Details

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: 

Illumination of the Early Universe by Quasars: Korea's 1st Result as Limited Gemini Partner

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”).

GPI Phase II Checks

Purpose

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. 

Background

The Phase II check point of view GPI consists of 4 components as these are driving the Phase II checking.

 

Limiting magnitudes for instrument and internal wavefront sensors

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.