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Figure 1: Imaging Sky Coverage for the SDSS EDR. A box defined by raMin, raMax, decMin, and decMax is filled in for each Field object.

  
Figure 2: Spectroscopy Sky Coverage for the SDSS EDR. A circle defined by ra, dec and a diameter of is filled in for each Plate object.

  
Figure 3: Overview of data products and distribution for SDSS EDR. The left column contains all of the data products available. The second column contains the servers that hold data. Note that not all data products are contained in each of the servers. The third column contains the interfaces we provide to these servers. Choose which interface to use based on the results you wish to obtain, listed in the fourth column.

  
Figure 4: Preliminary 2.5-m telescope filter responses, in u, g, r, i, and z. The upper curve in each case is the filter reponse including the quantum efficiency of the CCD and the reflectivity of the primary and secondary, ignoring the atmosphere, and the lower curve assumes an airmass of 1.3. Scattering within the thin chips affects the r and i band; this has no effect on extended objects, and the corresponding response curve is given by the dashed line in these two cases.

  
Figure 5: Quantum efficiency of atmosphere/telescope/fiber/spectrograph combination for each of the four spectroscopic chips, as measured from F stars with calibrated photometry.

  
Figure 6: Typical astrometric residuals, comparing positions between the astrometric and photometric chips for objects in common. The line going through the points is a spline fit to these residuals, attempting to remove atmospheric fluctuations.

  
Figure 7: The width of the PSF is a strong function of position in the imaging camera, even on the scale of a single CCD. Each square represents one of the photometric CCDs. The colors indicate the PSF width across the camera at a single moment of relatively poor seeing; the variations are due to time variability during the 55 second integration, plus effects in the telescope optics. The stretch is linear, from 1.4 to 2 arcsec.

  
Figure 8: The seeing (psfWidth) measured in the r filter in each of the imaging runs in the six camera columns, as a function of field number (lower axis) and (upper axis). A symbol for each field along the bottom indicates the quality of each field: Acceptable, Good, or Hole. Vertical marks indicate the location of MT secondary patches used for photometric calibration.

  
Figure 9: The aperture magnitude correction (apCorrRunErr) for the five filters, in each of the imaging runs in the six camera columns, as a function of field number (lower axis) and (upper axis). Vertical marks indicate the location of MT secondary patches used for photometric calibration.

  
Figure 10: Zeropoint deviations as a function of 2.5m CCD column. This plot contains data from comparisons of 22,972 stars from runs 752 and 756 between the PT and 2.5m telescopes and shows the 2.5m magnitude - PT magnitude (which is equal to the zeropoint determined from each star). Scattered light creates deviations as great as 10% in the u band in columns 1 and 6.

  
Figure 11: In runs 752 and 756, for objects that are measured in each run in the overlap region of camera column 3, we show the difference of magnitude as a function of field number. We inspect the complete set of these plots, six camera columns for each pair of overlapping runs. This set is typical, showing RMS scatter of 0.02 mag in , , , and 0.03 mag in and .

  
Figure 12: Location of the break in the stellar locus between K and M stars in the color-color diagrams, for runs 752 and 756 of the EDR.

  
Figure 13: Color-color plots of quasars and stars as measured in the SDSS colors. Black contours and black dots are stellar sources. Red contours and red dots show the distribution of quasars in the EDR data.

  
Figure 14: Redshift histogram for spectra classified as galaxies.

  
Figure 15: Pie diagram of main galaxies and LRGs with spectra in the EDR. The annuli are labeled with the comoving distance, assuming , , and .

  
Figure 16: Redshift histogram for spectra classified as quasars.

  
Figure 17: Pie diagram of quasars in the EDR. The annuli are labeled with the comoving distance, assuming , , and .