Candidate RR Lyrae Stars Found in Sloan Digital Sky SurveyCommissioning Data*

Abstract

We present a sample of 148 candidate RR Lyrae stars selected from Sloan Digital Sky Survey (SDSS) commissioning data for about 100 deg 2 of sky surveyed twice with Δ t = 1.9946 days. Although the faint-magnitude limit of the SDSS allows us to detect RR Lyrae stars to large Galactocentric distances (∼100 kpc, or r * ∼ 21), we find no candidates fainter than r * ∼ 20, i.e., farther than ∼65 kpc from the Galactic center. On the assumption that all 148 candidates are indeed RR Lyrae stars (contamination by other species of variable star is probably less than 10%), we find that their volume density has roughly a power-law dependence on Galactocentric radius, R -2.7±0.2 , between 10 and 50 kpc and drops abruptly at R ∼ 50–60 kpc, possibly indicating a sharp edge to the stellar halo as traced by RR Lyrae stars. The Galactic distribution of stars in this sample is very inhomogeneous and shows a clump of over 70 stars at about 45 kpc from the Galactic center. This clump is also detected in the distribution of nonvariable objects with RR Lyrae star colors. When sources in the clump are excluded, the best power-law fit becomes consistent with the R -3 distribution found from surveys of bright RR Lyrae stars. These results imply that the halo contains clumpy overdensities inhomogeneously distributed within a smooth R -3 background, with a possible cutoff at ∼50 kpc.

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Affiliated Institutions

• University of Chicago US
• United States Naval Research Laboratory US
• Pennsylvania State University US
• Eötvös Loránd University HU
• Princeton University US
• United States Naval Observatory US
• University of Michigan US
• Tokyo University of Science JP
• Rensselaer Polytechnic Institute US
• Fermi National Accelerator Laboratory US
• University of Washington US
• Johns Hopkins University US
• Institute for Advanced Study US
• The University of Tokyo JP
• National Astronomical Observatory of Japan JP
• Leibniz Institute for Astrophysics Potsdam DE

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