The SDSS Collaboration et al. 2000 The Astronomical Journal 120 1198 doi:10.1086/301540
The SDSS Collaboration (Philippe Fischer1,18, Timothy A. McKay2, Erin Sheldon2, Andrew Connolly3, Albert Stebbins4, Joshua A. Frieman4,5, Bhuvnesh Jain6, Michael Joffre5, David Johnston5, Gary Bernstein1,18, James Annis4, Neta A. Bahcall7, J. Brinkmann8, Michael A. Carr7, István Csabai6,9, James E. Gunn7, G. S. Hennessy10, Robert B. Hindsley10, Charles Hull11, Željko Ivezić7, G. R. Knapp7, Siriluk Limmongkol12, Robert H. Lupton7, Jeffrey A. Munn13, Thomas Nash4, Heidi Jo Newberg14, Russell Owen12, Jeffrey R. Pier13, Constance M. Rockosi5, Donald P. Schneider15, J. Allyn Smith2, Chris Stoughton4, Alexander S. Szalay6, Gyula P. Szokoly6, Aniruddha R. Thakar6, Michael S. Vogeley16, Patrick Waddell12 and David H. Weinberg17 and Donald G. York)5
Show affiliationsWe present measurements of galaxy-galaxy weak lensing from 225 deg2 of early commissioning imaging data from the Sloan Digital Sky Survey (SDSS). We measure a mean tangential shear around a stacked sample of foreground galaxies in three bandpasses (g', r', and i') out to angular radii of 600'', detecting the shear signal at very high statistical significance. The shear profile is well described by a power law γT = γT0(1'/θ)η, with best-fit slope of η = 0.7–1.1 (95% confidence). In the range θ = 10''–600'', the mean tangential shear is approximately 6 ± 1 × 10-4 in all three bands. A variety of rigorous tests demonstrate the reality of the gravitational lensing signal and confirm the uncertainty estimates. In particular, we obtain shear measurements consistent with zero when we rotate the background galaxies by 45°, replace foreground galaxies with random points, or replace foreground galaxies with bright stars. We interpret our results by assuming that all matter correlated with galaxies belongs to the galaxies. We model the mass distributions of the foreground galaxies, which have a mean luminosity
L(θ < 5'')
= 8.7 ± 0.7 × 109 h-2 Lg'
, 1.4 ± 0.12 × 1010 h-2 Lr'
, 1.8 ± 0.14 × 1010 h-2 Li'
, as approximately isothermal spheres characterized by a velocity dispersion σv and a truncation radius s. The velocity dispersion is constrained to be σv = 150–190 km s-1 at 95% confidence (145–195 km s-1 including systematic uncertainties), consistent with previous determinations but with smaller error bars. Our detection of shear at large angular radii sets a 95% confidence lower limit s > 140'', corresponding to a physical radius of 260 h-1 kpc, implying that the dark halos of typical luminous galaxies extend to very large radii. However, it is likely that this is being systematically biased to large value by diffuse matter in the halos of groups and clusters of galaxies. We also present a preliminary determination of the galaxy-mass correlation function, finding a correlation length similar to the galaxy autocorrelation function and consistency with a low matter density universe with modest bias.
The full SDSS will cover an area 44 times larger and provide spectroscopic redshifts for the foreground galaxies, making it possible to improve greatly the precision of these constraints, to measure additional parameters such as halo shape and halo concentration, and to measure the properties of dark matter halos separately for many different classes of galaxies.
dark matter; galaxies: fundamental parameters; galaxies: halos; gravitational lensing; large-scale structure of universe
Issue 3 (2000 September)
Received 1999 November 15, accepted for publication 2000 May 15
The SDSS Collaboration et al. 2000 The Astronomical Journal 120 1198
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