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Published December 2001 | Published + Accepted Version
Journal Article Open

The 2dF Galaxy Redshift Survey: spectra and redshifts

Abstract

The 2dF Galaxy Redshift Survey (2dFGRS) is designed to measure redshifts for approximately 250000 galaxies. This paper describes the survey design, the spectroscopic observations, the redshift measurements and the survey database. The 2dFGRS uses the 2dF multi-fibre spectrograph on the Anglo-Australian Telescope, which is capable of observing 400 objects simultaneously over a 2° diameter field. The source catalogue for the survey is a revised and extended version of the APM galaxy catalogue, and the targets are galaxies with extinction-corrected magnitudes brighter than b_J = 19.45. The main survey regions are two declination strips, one in the southern Galactic hemisphere spanning 80° x 15° around the SGP, and the other in the northern Galactic hemisphere spanning 75° x 10° along the celestial equator; in addition, there are 99 fields spread over the southern Galactic cap. The survey covers 2000 deg² and has a median depth of z = 0.11. Adaptive tiling is used to give a highly uniform sampling rate of 93% over the whole survey region. Redshifts are measured from spectra covering 3600A-8000Å at a two-pixel resolution of 9.0Å and a median S/N of 13 pixel⁻¹. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q ≥ 3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km s⁻¹. The overall redshift completeness for Q ≥ 3 redshifts is 91.8%, but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS database is available on the WWW at this http URL: http://www.mso.anu.edu.au/2dFGRS

Additional Information

© 2001 RAS. Accepted 2001 August 9. Received 2001 July 30. The 2dF Galaxy Redshift Survey was made possible through the dedicated efforts of the staff of the Anglo-Australian Observatory, both in creating the 2dF instrument and in supporting the survey observations.

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Published - 328-4-1039.pdf

Accepted Version - 0106498.pdf

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September 15, 2023
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