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Sakurai’s Object: Stellar Evolution in Real Time

TEXES Sensitivities and Overheads


Because TEXES is background photon noise limited and both the instrumental response and the background flux depend on wavelength, the instrument sensitivity depends strongly on wavelength and spectral resolution. Proposers are encouraged to contact TEXES team members for sensitivity estimates for observations at specific wavelengths, but can make initial estimates based on the table below.

Accepted programs and status

GPI programs selected for Early Science Observations


The table below summarizes the programs that have been approved for GPI Early Science observations.


2014A Observing Tool update released

An updated to the 2014A Observing Tool (2014A.1.2.10) has been released and is available from the downloads site. This is an optional but recommended update.  This version fixes several bugs and improves performance and stability, especially when working with large programs and multiple science program editors. Be sure to sync local changes or save programs to XML before updating. You will have to reenter authentication keys.

Electrical Accident at Gemini North Closes Road, Injury Minor

When performing electrical troubleshooting at Gemini North telescope facility on Wednesday, February 26, one of our electrical specialists accidentally contacted a powered circuit and received an electrical shock. He was evacuated and evaluated at the nearest medical facility, and he has been released and advised that he could go back to work.

2014B Call for Proposals Announced

Gemini is now accepting proposals for observing time in Semester 2014B. The submission deadline varies with partner and ranges from MONDAY MARCH 31, 2014 to TUESDAY APRIL 1, 2014. A new version of the Phase I Tool (PIT) has been released to support proposal submissions.

Semester 14B Call for Proposals

Gemini Observatory invites its community to propose scientific investigations for the 2014B semester, 1 August 2014 - 31 January 2015.

GMOS-N Array (EEV)

The original GMOS-N detector array consisted of three 2048x4608 EEV chips arranged in a row. This array was replaced by e2v deep depletion devices in October 2011.

The table below gives a summary of the original EEV detector/controller characteristics.

Detector Array

Detector characteristics are given in this section. Note that the GMOS-South detectors will be upgraded for 14B. Note also that the telescope optics are now silver-coated, reducing the system throughput in the blue.

Public Data Readme

GPI Public Data Early Release Readme