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Semester 2014B Time Distribution


The time available on each of Gemini North and South is distributed according to the Observatory partners' shares . To maintain overall balance amongst the partnership, the allocations are adjusted each semester as a result of actual time charged in prior semesters. The allocations are approved at the Operations Working Group meeting prior to the Call. Historically, around 5% of each semester's science time is used to complete highly ranked programs from the previous two semesters to which the ITAC granted rollover status.

Semester 2014B Important Dates

Key dates and events in the proposal process are shown below. The Phase I and Phase II deadlines are highlighted.

2014B Instrument Availability and Target Accessibility

This page provides best estimates, at the time of the Call for Proposals, of instrument availability and target (RA, dec) restrictions for 2014B.


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Observing Constraints

To reach the desired instrument performance GPI is constrained both in the suitable weather conditions and the elevation of the target being observed. 

Spectroscopic Accuracy

Spectroscopic Accuracy

The spectroscopic accuracy has been evaluated using the white dwarf orbiting HD 8049 discovered by Zurlo et al (2013), believed to have a temperature of 18800+/-2000 K. Observations were performed during the second commissioning run on December 12, 2013. The recipes, calibration files, and reduced cubes used to create the plots in this section are available as part of the first light data release. For this data, zero-point offsets to the wavelength solutions were determined using an Argon arclamp image taken immediately after the exposures.

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). 


For faint targets(I magnitude ≤9.0), GPI is expected to achieve 5-σ sensitivity at H=21 in one hour in spectroscopic mode. Achieved sensitivity is a function of many parameters, including contrast, inner working distance, brightness of the central star (if any), observing mode (dithered, sky-offset, sky-rotation) and it is not yet possible to provide estimates for all modes.

March GeMS Run Cancelled

The Gemini South laser suffered a fault towards the end of the last GeMS run in February. The laser power has been lost to a level that prohibits useful science. Unfortunately, despite all the efforts of the laser team, we were not able to recover the laser during the run. The problem has been identified and a plan is under development to recover, which involves replacement of key hardware parts and realignment of the system. Internal and external specialists will collaborate to complete this work and return the laser to the level required to do science.

Limits on Binarity of Exoplanet Host Stars

Gemini North Back On-sky: Dome Repairs Complete

After a very involved repair to a drive unit for the shutter of the Gemini North dome, Gemini North is back on the sky for regular science operations. See more at: .