The Seventh Data Release of the Sloan Digital Sky Survey

TL;DR

The Seventh Data Release of SDSS provides comprehensive imaging and spectroscopic data covering over 11,600 square degrees, including millions of objects, with improved calibration, deeper coadded imaging, and enhanced data processing techniques.

Contribution

This release completes the SDSS-II goals, expands data coverage, and introduces improvements in data calibration, reduction, and analysis methods for large-scale astronomical surveys.

Findings

Over 1.6 million spectra collected, including galaxies, quasars, and stars.

Improvements in astrometry reduce positional errors to 45 milliarcseconds.

Deeper coadded imaging reaches two magnitudes fainter than the main survey.

Abstract

This paper describes the Seventh Data Release of the Sloan Digital Sky Survey (SDSS), marking the completion of the original goals of the SDSS and the end of the phase known as SDSS-II. It includes 11663 deg^2 of imaging data, with most of the roughly 2000 deg^2 increment over the previous data release lying in regions of low Galactic latitude. The catalog contains five-band photometry for 357 million distinct objects. The survey also includes repeat photometry over 250 deg^2 along the Celestial Equator in the Southern Galactic Cap. A coaddition of these data goes roughly two magnitudes fainter than the main survey. The spectroscopy is now complete over a contiguous area of 7500 deg^2 in the Northern Galactic Cap, closing the gap that was present in previous data releases. There are over 1.6 million spectra in total, including 930,000 galaxies, 120,000 quasars, and 460,000 stars. The data release includes improved stellar photometry at low Galactic latitude. The astrometry has all been recalibrated with the second version of the USNO CCD Astrograph Catalog (UCAC-2), reducing the rms statistical errors at the bright end to 45 milli-arcseconds per coordinate. A systematic error in bright galaxy photometr is less severe than previously reported for the majority of galaxies. Finally, we describe a series of improvements to the spectroscopic reductions, including better flat-fielding and improved wavelength calibration at the blue end, better processing of objects with extremely strong narrow emission lines, and an improved determination of stellar metallicities. (Abridged)