The data processing pipeline that maps CCD pixel coordinates to celestial coordinates. The detailed workings of this pipeline are described in the Astrometry section of the algorithms pages, or the Pi [..]

The fits binary tables containing photometrically and astrometrically calibrated quantities from the imaging pipeline. Available in the SAS.

A method of measuring object shapes (i.e., fitting those shapes to ellipses). These moments are close to optimal for measuring the shapes of faint galaxies, and have been used for weak lensing studies [..]

A philanthropic nonprofit institution (www.sloan.org) established in 1934 by Alfred Pritchard Sloan, Jr., then President and Chief Executive Officer of the General Motors Corporation. An early award f [..]

A neural network technique for selecting quasars for spectroscopy in the BOSS survey. It is one of the techniques used in the BONUS quasar sample. The algorithm is described in Yèche et al. 2010.

Apache Point Observatory, located in Sunspot, New Mexico. This is the location of the 2.5m SDSS telescope as well as the Photometric Telescope (PT), as well as other non-SDSS telescopes, such as the A [..]

The Apache Point Observatory Galactic Evolution Experiment, one of four surveys included in SDSS-III. This is using a high-resolution (R~22,500) H-band spectrograph fed by 300 fibers. The spectrograph [..]

Astrophysical Research Consortium. Incorporated in the State of Washington. Members include the University of Washington; New Mexico State University; The University of Chicago, Princeton University; [..]

Magnitudes within SDSS-I/II are expressed as inverse hyperbolic sine (or "asinh") magnitudes, sometimes referred to informally as luptitudes. The transformation from linear flux measurements [..]

FITS binary table with astrometric transformations for every field in a single imaging run. It transforms frame (row,col) coordinates to great circle (μ,ν) coordinates for a given inclination. Availab [..]