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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.
NASA SSERVI director Yvonne Pendleton used coin faces to help students visualize how the moon rotates as it orbits the Earth, keeping the same side facing the "Earth".
Hilo High students observed various light sources through filters that separate the light into a rainbow of colors.
Three GMOS (North and South) spectra obtained at different times of the z =2.47 quasar J0230 show the variability of the absorption features, especially the CIV near rest-frame wavelength 1550Å. The spectra have been normalized based on measurements in the shaded regions.
Figure 1. GMOS-South image of the center of the Abell 85 galaxy cluster. The brightest galaxy in the middle was thought to hide a supermassive black hole in its core based on prior lower-resolution data.
Figure 1. Left: Y dwarfs imaged in the CH4S filter. For each object two panels are shown, with the left displaying a 0.8×0.8 arcsecond sub-image centered on the Y dwarf, and the right showing a nearby reference star. All images are north up and east to the left.
Since November 2015, all science data and the associated calibrations are stored in, and accessed via, the Gemini Observatory Archive (GOA), which is operated by the Observatory. All Gemini data has been transferred into the new archive and can be accessible from the GOA. The GOA is described here. Detailed instructions to search and retrieve science data and associated calibrations are given in the GOA Help web page.
Our observed spectrum of PSO J318.5−22 (black) compared to the forward model with our best fit parameters (red). The median residual of the fit is 0.079 (in normalized Fλ units), which is larger than the median uncertainty (0.048) of our observed spectrum. The rms of the residuals (0.12) indicates systematic uncertainties of ≈10%.
The PWFS2 is available for observing non-siderial targets or when a suitable OIWFS star is not available. There are a few drawbacks with using the P2WFS instead of the OIWFS which are:
- The probe vignettes the F2 FOV.
- The flexure between the probe arm and the detector has not been quantified