Data Set Overview : The data set consists of ground-based images of comet 9P/Tempel 1 in the R and HB filters taken at the Kitt Peak Mayall 4m telescope from July 2-9, 2005 around the Deep Impact encounter. The Kitt Peak Mayall 4m telescope with the MOSAIC camera at Prime focus was used for all observations. Harris broad-band filters optimized for the Landolt broad-band colors were used, as well as narrowband HB filters. The comet was tracked at non-sidereal rates. However, occasionally, the tracking failed and some comet images are smeared.  Raw, as well as reduced images are included. Corresponding calibration frames (dome flats and bias frames) are included. All the data were bias subtracted, flat fielded, corrected for crosstalk, and the pupil contamination was removed when necessary following the data reduction guide by Buell Jannuzi, Jenna Claver, and Frank Valdes, available at http://www.noao.edu/noao/noaodeep/ReductionOpt/frames.html  As the MOSAIC camera has been replaced since our observations, the relevant manual has been included in this archive for reference. Note that the MOSIAC camera consists of 8 CCDs arranged in a 4x2 pattern. The corresponding raw fits files have therefore 8 extensions (from 1 to 8). As the comet did not cover the entire MOSAIC field, it was always placed on the same chip (#2). The reduced data were therefore trimmed to a much smaller size. The corresponding fits files do not contain extensions.  Note that sometimes (but rarely) there are no corresponding reduced images due to e.g. tracking errors, filters not used for Temepl 1, or the objects not being placed in chip #2).  Landolt standard fields are available in photometric nights.  The observing logs, as well as additional hand-written logs are included in the archive, although some logs are incomplete.  Tables listing the centers (x,y) of the Landolt standard stars in the reduced images are also included. NOTE that the origin is (1,1). The centers for the HB standard stars are not included as they are always the brightest object in the image and easy to identify. The centers for comet 9P/Tempel 1 are also not given, as it is always the brightest extended object in the image and easy to identify.  For the photometric nights, tables relating the counts of individual images to calibrated flux units for the broadband R as well as the HB comet filters are also included.  f(X) : counts/sec * f0(X) * 10^(-0.4*(m0-ZP(X)-coeff(X)*airmass))  where m0:25mag is the zero point offset of the magnitude scale, ZP(X) the zero point, coeff(X) the airmass coefficient, and counts/sec is the DN value read from the image / exposure time.  Therefore  f(X) : DN value * f0(X) * conversion factor  where the conversion factor is  1/exptime * 10^(-0.4*(m0-ZP(X)-coeff(X)*airmass))  These conversion factors are given in tables. For the broadband R filter, X:R and f0(R):2.23E-09 erg s^-1 cm^-2 Angstrom^-1 (converted from Bessel 1979). The error in f0(R) is 0.02E-09 due to the difference in effective wavelength between the Cousins Filter and the Harris filter. The filter response curves however look very similar to each other.  For the narrowband HB filters, the values for f0(X) in 10E-9 erg s^-1 cm^-2 Angstrom^-1 (Farnham et al. 2000) are: f0(OH):10.560 f0(CN):8.6 f0(C2):3.887 f0(UC):7.802 f0(BC):6.210 f0(GC):3.616 f0(RC):1.316   The archiving of this data set was supported by NASA's Planetary Mission Data Analysis Program.   References:  Bessell, M.S. 1979. UBVRI Photometry II: The Cousins VRI system, its temperature and absolute flux calibration, and relevance for two-dimensional photometry. PASP 91, 589-607.  Farnham, T.L., D.G. Schleicher, M.F. A'Hearn 2000. The HB narrowband comet filters: Standard stars and calibrations. Icarus 147, 180-204.

Confidence Level Overview : The errors in the conversion factors given in the tables for 9P/Tempel 1 are about 2%.  The comet was tracked non-sidereally. However, sometimes the tracking failed, and some comet images are trailed.