All Tables

Table 1: Instrument filter setup and filter properties during the DI observations at ESO. The broadband filters are annotated following the standard photometry designation. Note that $R_{\rm special}$ is a modified R Bessell filter - see http://www.eso.org/instruments/fors1/ for further details. The names of the narrowband gas filters (CN, C₂, C₃, NH₂) refer to the respective gaseous species that emit light in the filter passband. Dust continuum filters are labeled BC for "blue continuum'' and RC for "red continuum'', a narrowband OII filter was used to measure the dust continuum in the UV. A special Na filter was installed for imaging of the comet in the wavelength range of the sodium D lines.
Table 2: Log of the DI broad- and narrowband observations at the ESO observatories in Chile. For ESO Chile the observing window of the comet started around 23:30 UT (Sun about 18 deg below horizon) and lasted until 04:20 UT (comet at 20 deg elevation). The following notations are used for the sky conditions: CLR = clear sky; THN = thin cirrus clouds; COUT = clouded out. The seeing values are measured by a dedicated seeing-monitoring telescope on-site.
Table 3: Coma structure geometry caused by normal activity of comet 9P/Tempel 1 around the time of the DI event. Near-nucleus position angles PA, curvature and minimum extension are determined from BVRI images of the comet obtained between 4 and 8 July 2005. The results are cross-checked with data obtained through narrowband filters during the same time interval. The jet-like structures are labeled in Fig. 1. Accuracy of the PA values is $\pm$ 5 deg. Active regions, tentatively associated with the jets, are labeled AR1, AR2, AR3a, AR3b, AR3c, and AR4. Abbreviations and notes: C = clockwise curvature, CC = counterclockwise curvature, S = straight, no curvature. (*) Structure B may also be due to comet tail phenomena. (**) Structure C is detached from the nucleus, but overlaps with jet D at an projected nucleus distance of about 3500 km. It extends almost parallel to structure B into tail direction. (***) Structures G, H, I evolved from the nucleus at about the same PA, but show different curvatures which indicates that they may originate from 3 different active regions at the nucleus with slightly different latitudes: G located slightly South of H and the latter being slightly South of I. The PA difference between GHI and the projected rotation axis suggests that the related active regions may be located close to the equator of the nucleus.
Table 4: The DI dust cloud ``mass spectrometer'': Apex distance, radiation pressure factor $\beta$ and initial velocity as determined from the DI dust ejecta envelope.
Table 5: Fluxes, molecule production rate&production rate ratios and dust continuum reddening of 9P/Tempel 1 during 2-10 July 2005. The fluxes F and reddening slopes R are measured in circular apertures of fixed radii centered at the brightness peak in the coma. $Q_{\rm mean}$ and $R_{\rm mean}$ are mean values of the production rates and reddening slopes, respectively, obtained from the flux and slope measurements with radii 5000, 10 000, 15 000, and 20 000 km. The continuum filter image used for dust continuum subtraction in the gas filter images is indicated in table column DCONT; if two filters are given, the flux and production rate numbers are the mean values obtained from measurements using either of the two filter images as reference for the dust continuum subtraction. The table lists logarithmized values for fluxes and production rates. "NM'' means "no useful measurement obtained''. Flux F is measured in erg/s/cm²/Å, production rates Q in molecules/s, reddening slope R in %/100 nm, aperture radii are in km at the distance of the comet. All results are based on narrowband filter imaging of the comet obtained with the EMMI instrument at the ESO NTT telescope in La Silla. Measurements, obtained at very high airmass where the flux calibration may be badly affected by extinction, are indicated by symbol *.