The DMS begins at the data acquisition interface between camera and telescope subsystems and flows through to the data products accessed by end users. On the way, it moves through three types of managed facilities supporting data management, as well as end user sites that may conduct science using Rubin Observatory data or pipeline resources on their own computing infrastructure.

Cerro Pachón, a mountain peak in northern Chilé, has been selected as the site for the Large Synoptic Survey Telescope.

The Rubin Observatory summit facility is currently under construction in north-central Chile, on the Cerro Pachón ridge in the foothills of the Andes Mountains. The entire Cerro Pachón area, including the Rubin Observatory site, and the Gemini-South and SOAR telescopes, lies on a tract of land owned by the Association of Universities for Research in Astronomy (AURA), Inc.

M1M3 Monolith

In the Rubin Observatory optical design, the 8.4 m primary (M1) and 5.0 m tertiary (M3) mirrors form a continuous surface. Because the two mirrors curve differently, a slight cusp is formed where they meet, as seen in the picture below. This design makes it possible to fabricate both the primary and tertiary mirrors from a single monolithic substrate, the M1M3 monolith.

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Usually the redshift of a galaxy is measured spectroscopically. The spectrum of the galaxy is observed: Emission or absorption lines are identified and their wavelengths are measured. These measured wavelengths are then compared with the rest wavelengths to determine the redshift. Photometric redshifts (also known as "color redshifts" or "photo-z") utilize broad-band photometry to measure the redshifts of galaxies rather than spectroscopy.