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Figure 1. (Left:) Zoom-in images on HD 95086 b obtained with GPI at the first and last epochs. The magenta crosses show the measured positions (for clarity, the size of the symbol is not representative of the precision). Significant orbital motion is detected within the GPI data. (Right:) Deepest image obtained on HD 95086 with GPI at K1 on April 8, 2015.
Before low-medium mass stars become white dwarfs they pulsate wildly and eventually spew their outer layers into space – often forming beautiful planetary nebulae. The same stars are predicted to continue pulsating during their transformation to a white dwarf, if they have helium in their atmospheres. A team from the University of Oklahoma used Gemini North, in conjunction with the 1.2-meter FLWO telescope in Arizona, to observe a much-sought-after link between these pulsations and helium in the star’s atmospheres.
The Association of Universities for Research in Astronomy, Inc. (AURA), on behalf of Gemini Observatory is soliciting proposals to design, fabricate, assemble, test, deliver, and commission Gemini Observatory's next facility class instrument, Gen 4#3. Gen 4#3 will be a wide-band medium-resolution spectrograph designed to take advantage of the Large Synoptic Survey Telescope (LSST) follow up opportunities.
Gemini North and South are accepting proposals for the Fast Turnaround (FT) program. Here, we give information specific to this proposal cycle. Please see the other FT pages - particularly the rules - for general information about the program. FT-specific proposal templates must now be used for all FT proposals; see the "PIT information" section below.
CLICK HERE for a complete list of the Gemini research staff.
GNIRS was built by NOAO in Tucson, Arizona and delivered to Cerro Pachon in late October 2003. Commissioning of the majority of the modes took place in stages during 2004. GNIRS was first made available for science use in 2004B. The instrument was damaged in 2007 while at Cerro Pachon and was repaired at Gemini North. Since 2010 it has been available for use on the Gemini North telescope.
FLAMINGOS-2 spectrometer/imager on Gemini South.
Comparison of the central portions of the sparse NGC 1600 galaxy group (right) with the dense Coma Cluster (left) which is at least 10 times more massive than the NGC 1600 group. The two closest companion galaxies of NGC 1600 (NGC 1601 and NGC 1603), are nearly 8 times fainter than NGC 1600 (center of right image). The Coma Cluster contains over 1,000 known galaxies. Both images are from the Second Palomar Observatory Sky Survey.