Data Set Overview ================= KPNO Images of Comet 9P/Tempel 1 from February to June 2005 The data set consists of ground-based images of comet 9P/Tempel 1 in the R and HB filters taken at the Kitt Peak 2.1m telescope between February and June 2005 prior to the Deep Impact encounter. The Kitt Peak 2.1m telescope at f/7.5 with the F3KB (3kx1k) chip 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. Raw, as well as reduced images are included. Corresponding calibration frames (dome flats, bias frames, and dark frames) are included. All the data were bias subtracted and flat fielded with the dome flats and some of the data were dark corrected. The F3KB has some LED effects in the corners of the CCD. The KPNO observing logs as well as additional handwritten logs are also included in pdf format. The KPNO observing logs are named kp05mmdd_log.pdf where mmdd are the numerical month and day of the observing log. The handwritten logs are named 2005_Mon_dd.pdf where Mon is the 3-letter abbreviation of the month and dd the day of the observing log. The observing dates in 2005 were: February 2-5, March 11-14, April 9-14, May 14-17, and June 4-7. The following nights were photometric: February 2 & 3 (but see note below), March 11-13, April 10, 11, & 14, May 14 & 16, and June 5-7. NOTE that all the data from the February run were affected by a sticky shutter. We therefore could not flux calibrate those data, although the standard star images are still included in the data set. Landolt standard fields are available in photometric nights. Often frames of fields where the comet was/will be located from previous/subsequent nights were also taken in order to tie non-photometric nights to photometric nights. Such images are also included. Tables listing the centers (x,y) of the Landolt standard stars and the object in the reduced images are also included. NOTE that the origin of the coordinate system is (1,1). The centers for the HB standard stars are not included as they are very bright stars and are almost always the only object in the frame. They were always placed near the center of the CCD and are 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)*air1mass)) 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 1E-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 Some of the comet data were affected by obvious guiding problems (which are not always noted in the logs). Some of these images were still archived but were not flux calibrated. If images are not in the archive (but are mentioned in the log files), then there was something wrong with them (e.g. obvious guiding errors, wrong field, saturated standards, etc.). Conversion factors of images that could not be flux calibrated in photometric nights (due to various problems) are not included in the conversion files. The fits headers often show the filter number but not the filter name. The following table shows the correspondence of the filter number to the filter name. This is valid for all the observing runs. Filter number Filter name Description 1 OH HB OH 2 UC HB UV continuum 3 CN HB CN 4 BC HB blue continuum 5 C2 HB C2 6 GC HB green continuum 7 RC HB red continuum 8 R broad-band R Directory Structure: The data were archived into raw and reduced directories for the raw and reduced data respectively. Each of these directories have sub-directories with the data in the form of 2005_monthdd where month is feb, march, april, may, or june, and dd the day. These sub-directories contain the tables listing the centers and the conversion tables, and are divided further into subdirectories called calibrations, calibration_fields, comet_9p_tempel_1, and standard_stars. Not all of these sub-directories are present in every directory. The 'calibrations' directory contains bias, flat, and dark frames. The 'calibration_fields' directory contains frames where the comet was/will be located from previous/subsequent nights. The 'comet_9p_tempel_1' directory contains images of comet 9P/Tempel 1. The 'standard_stars' directory contains images of the standard stars. All the image names are of the following convention: kp05mmdd_nnn.fit, where mm is the 2-digit month, dd the 2-digit day and nnn a sequential integer number starting at 001. Preliminary results from this data set were reported at the DPS meeting (Farnham 2005). Some results from this data set were included in the overview paper by Meech et al. (2010). Farnham et al. (2007) reported on observations of comet C/2004 Q2 (Machholz) taken during the same observing runs as the Tempel 1 data. Users of this archive might find it useful for background information and more details about the telescope/instrument used. The archiving of these data 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. Farnham, T.L., B.E.A. Mueller, M.M. Knight, N.H. Samarasinha 2005. Narrowband observations of Comet Tempel 1 in support of the Deep Impact mission. AAS, DPS meeting #37, #43.05. Farnham, T.L., N.H. Samarasinha, B.E.A. Mueller, M.M. Knight 2007. Cyanogen jets and the rotation state of Comet Machholz (C/2004 Q2). AJ 133, 2001-2007. Meech, K.J., and 57 colleagues 2011. Deep Impact, Stardust-NExT and the behavior of Comet 9P/Tempel 1 from 1997 to 2010. Icarus 213, 323-344. Confidence Level Overview ========================= The data from the February run are affected by a sticky shutter. These data therefore cold not be flux calibrated. Some of the comet data were affected by guiding problems. The images were still archived but are not flux calibrated. The conversion factors to relate counts to flux densities have an error of about 2%.