Change page style:
Gemini South Telescope with the Milky Way above.
Today, in the journal Science, Australian scientist Keith Bannister announced findings that might help solve a 30-year old mystery.
In preparation for the start of 2016A, all Fast Turnaround (FT), Director's Discretionary (DD) time, and Poor Weather (PW) proposals must use the 2016A Phase I Tool (PIT). See the PIT Version Table for more information and download links.
AstroDay Chile es uno de los programas de extensión con mayor tradición que organiza Gemini anualmente.
Computer simulation of gas distribution (left) and stars (right) after the Milky Way is perturbed by the dwarf satellite. Download the entire animation here.
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.