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Left: GPI J band (top) and K1 band (bottom) polarized intensity (Qr) images of the TW Hya disk. Right: Qr(i; j) scaled by r2(i; j), where r(i; j) is the distance (in pixels) of pixel position (i; j) from the central star, corrected for projection effects. All images are shown on a linear scale. The coronagraph is represented by the black filled circles and images are oriented with north up and east to the left.
Figure 1. The massively star-forming galaxies analyzed in this study have clumpy, turbulent gas shown on the left (Hubble Telescope data). Through a unique combination of Gemini-GMOS and Keck-OSIRIS observations, the scientists were able to measure the velocity of these galaxies in each point, such as shown on the right in false colors.
A new version of the Gemini IRAF package (v1.13.1) has been released. This version is recommended to anyone processing GMOS-S data but is required to reduce GMOS-S Hamamatsu CCD data obtained after the August 2015 work on the instrument. Updated configuration files and examples are included. Please see the Processing Software page for more information.
Gemini to support AstroConda in place of Ureka later this year
The 2016A Gemini Observing Tool is now available for download. This update is required to access the Gemini Observing Databases.
Figure 1. Image of HD 100546 obtained with the Gemini Planet Imager at near-infrared wavelengths (1.6 microns). The cross shows the position of the star, the green hatched lines show the region interior to which GPI's coronagraph blocks our view of the system. HD 100546 b appears as a bright point source sitting on a finger of disk emission.
Observations using the Gemini Planet Imager are featured prominently at the Extreme Solar Systems III meeting ongoing this week (Nov. 29 - December 4) in Waikoloa Hawai‘i. Below are two results from a press conference on December 1, 2015.