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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. 

Back on the Sky at Gemini South

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.

Gemini-S shutdown work completed

The Gemini-S telescope is now back into operation following the planned maintenance shutdown.

Time Delay in Lensed Quasar: First Fast Turnaround Result

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.

Autoridades Locales Dan Inicio a Semana de Viaje al Universo






Una novedad para este año es la visita del grupo de reconocidos científicos y comediantes españoles Big Van “Científicos sobre Ruedas.”

Credit: Gemini Observatory/AURA

Gemini Launches Local Students on an Exciting Week-long Viaje al Universo






A special addition to this year’s programming is a week-long visit by the renowned science entertainers, Big Van “Scientists on Wheels.”

Credit: Gemini Observatory/AURA

Mysterious Starburst Unshrouded in Nearby Galaxy

Figure 1. Color composite image of the central region of NGC 253, from Flamingos 2 images using the filters J (blue), H (green) and Ks (red). This region of the edge-on viewed galaxy appears completely veiled in optical images due to the presence of large amounts of dust (so dense that it is still obscuring some regions at the near-infrared spectral range). The wavelength range covered by F-2 goes from 1 to 2.5 μm. The field of view is 420 x 144 arcseconds.

GNIRS Sensitivity Estimates

If you want to consult the monitoring of GNIRS sensitivity and throughput since 2011, please go here.

RFP for Gemini Instrument Upgrades: Small Project

Gemini is seeking to upgrade its operational instruments to keep them scientifically competitive. Gemini’s development program will provide funding to upgrade existing operational instrumentation, creating new instrument capabilities at the Gemini North and/or South telescopes. The Observatory is seeking community-created, science-driven instrumentation upgrade proposals, and will consider any area that fits the set of IUSP requirements provide in the RFP.

Gemini Sodium Laser Guide Star RFQ

AURA is seeking to replace the current continuous wave (CW) mode-locked 50 Watt laser at the Gemini South facility with a more robust alternative Laser (the subject of this RFQ, hereafter called the “Laser”) providing a photon return equivalent to or greater than currently received by its 5 laser guide star Multi-Conjugate Adaptive Optics system, GeMS.