Change page style:
Expires on: TBD
gemini_python is a new Python-based data reduction platform under development at Gemini. It was developed to support the Quality Assessment Pipeline.
Figure 1. All of the images shown in Figure 2 were “stacked” in this image of Comet 67P. Background stars are expanded and fuzzy due to the use of a “median” filter when stacking the images while keeping the comet centered.
Figure 1. Images of P/2013 P2 (left) obtained using the Gemini North telescope on September 4, 2013 when it was 3.2 AU from the sun, and of P/2014 S3 obtained using the CFHT telescope in late September 2014 when it was 2.1 AU from the sun. Both images have been processed to remove most of the background stars and galaxies to enhance the visibility of the faint dust tails.
Left panel: the velocity vs. clustercentric radius phase space of galaxies in the nine GCLASS clusters. The velocities are in units relative to the individual cluster velocity dispersions and the radii are relative to the position of the brightest cluster galaxy scaled by the R200 of the cluster. The shaded regions are arbitrarily defined but are indicative of increasing time since infall (see text).
Official Data Processing Software
The data reduction software approved for scientific purposes is the Gemini IRAF package.
On the 31st October Gemini Observatory will host an interactive remote Bidders Conference for participates to learn more about the GIFS RfP.
Participants can attend by phone or by polycom. Gemini will host two equivalent sessions to allow for participation across many different time zones.
Session 1: 11:00 – 13:30 CLST
Session 2: 19:00 – 21:30 CLST
If you plan on attending one of the sessions, please email firstname.lastname@example.org and inform us which session you plan on attending and how. (i.e. my phone or polycom)
The current version of the GMOS Mask Making software (GMMPS) is v0.4.2, released in 2014-10-28 for Linux and Mac OS X. This is an interim version to provide support for the new Hamamatsu detectors in GMOS-S. It is not yet fully backwards compatible (see below).
Version 0.4.2 fixed several memory leaks and other bugs that could prevent GMMPS from creating the ODF FITS tables we need to cut the masks. This has occurred with newer gcc compilers.
The gaps between the three detectors in GMOS cause gaps in the spectral coverage, see the example. The size of the gaps in wavelength space depends on the grating used, but is typically a few nanometers. If continuous spectral coverage is essential for your program, consider using two configurations of the grating with central wavelengths 3-5 nm different.
The GMOS-North light curve (top panel) and Fourier transform (bottom panel) for the optical companion to PSR J1738+0333. A comparison star is shown in blue, offset by -7%. We mark the 4 sigma and 3 sigma significance level as dashed green and blue lines, respectively. The three significant pulsations are marked with red lines in the bottom panel and the frequency solution is illustrated in the top panel.