"... In PAGE 7: ... The Parsec-Scale Radio Continuum Figures 3, 4 and 5 show naturally-weighted 5, 8 and 22 GHz images of the parsec-scale continuum emission in the nucleus of NGC 3079. Table2 lists the tted parameters of the compact continuum sources identi ed at each of these frequencies. Figure 6 compares the flux densities of the two brightest continuum components, A and B.... In PAGE 7: ... Due to the limited (u; v) coverage of the 5 GHz VLBI observation, no substructure was resolved in either component. Note that while the flux density of B in 1992 is approximately the same as that measured by IS in 1986, component A appears to have faded somewhat ( Table2 ). However, given the quoted uncertainties in the flux density measurements of IS, it is not possible to determine with this observation whether either component is in fact variable at 5 GHz.... In PAGE 7: ... However, component A exhibits an extension to the W at the 15 level (Figure 3), and there is some indication of emission that is undersampled by our shortest baselines. We report the detection of a third continuum component (labelled D in Figure 3 and Table2 ), located 4pcSEofBalong the A-B axis. Component D is not visible at the 0.... In PAGE 11: ...but not coincident with, the assumed position of the central engine. Its position also agrees within the measurement errors with the position of continuum component C of IS; however, that source was observed at 5 GHz, and was considerably larger ( Table2 ), so it is not clear that they are the same. Component C is unusual in that it was only detected at 22 GHz, which suggests an inverted spectrum extending to high frequencies.... ..."

"... In PAGE 12: ... None of the derived abundances di er signi cantly from the template apos;s. While deviations of individual abun- dances could be detected only with reasonable ( gt; 2:5 ) signi cance when log gt; 0:2 dex, the scatter of the dif- ferential abundances derived for di erent ions ( Table5 ) is fully consistent with the hypothesis that #128 and #201 have identical abundances. This makes it unlikely that sev- eral of the studied abundances deviate by more than 0.... In PAGE 12: ...04 dex. Table5 shows that also in this star any di erence in abundance pattern relative to #201 remains below the present level of detectability. Figure 8 visualizes the spectral changes as a consequence of abundance changes of 0.... ..."

"... In PAGE 6: ... (Gray 1985)describes collaboration as the process through which parties who see different aspects of a problem can constructively explore their differences and search for solutions beyond their own limited vision of what is possible . Mulford amp; Rogers (1982) describe the collaboration continuum from the perspective of cooperation through to various strategies of managed coordination in Table1 . Spatial data sharing arrangements exist at all levels of the continuum defined by Mulford amp; Rogers.... ..."

"... In PAGE 35: ...oes not equate with community-driven. Consequently, there was little sustainability. Active (or proactive) community participation should thus be differentiated from passive (or coerced) participation. Table1... ..."

"... In PAGE 7: ...a 25% error in one of the continuum fluxes introduces only an error of 0:1in the continuum slope index . Errors in are predominantly systematic and hard to estimate, but from the self consistency of objects for which we have multiple observations, and the residuals to power-law ts to the continuum ( Table3 ), we estimate them to be of order 0:1. A power-law continuum is tted (by least-squares minimisation) to the corrected continuum fluxes; the resultant power-law indicies are listed in Table 3.... In PAGE 7: ... Errors in are predominantly systematic and hard to estimate, but from the self consistency of objects for which we have multiple observations, and the residuals to power-law ts to the continuum (Table 3), we estimate them to be of order 0:1. A power-law continuum is tted (by least-squares minimisation) to the corrected continuum fluxes; the resultant power-law indicies are listed in Table3 . A histogram of these continuum slopes in shown in Figure 2.... In PAGE 7: ... A histogram of these continuum slopes in shown in Figure 2. The power-law t is generally a good one; the scatter around the ts ( Table3 ) is consistent with the photometry and correction errors. Note however that in the absence of R or I-band photometry, we have little sensitivity to large-scale departures from a power-law continuum shape.... ..."

"... In PAGE 5: ... For 2:4 lt; z lt; 3 however, the B-band ux was corrected, the correction factor being chosen from visual inspection of the spectrum. Corrected continuum uxes are shown in Table2 . Correction factors are typically 0:3 magnitudes or less.... ..."

"... In PAGE 8: ... The one exception is the detector background, which is discussed in the following section. The sensitivity calculation for Andromeda is illustrated in Table4 . The observation time, #1C, has been taken as 2 #02 10 4 seconds, the detector area, A, as 2200 cm 2 , the detection signi#0Ccance is 3, and the energy bandwidth, #01E=E, as... ..."

"... In PAGE 10: ... That we are not victims of coincidences will be very clear from Fig. 5 below and also from Table2 which gives the analogous results for = 0:90. Here, since we are much closer to the phase transition line, the level structure is much more involved.... ..."

"... In PAGE 13: ... To nd the H2 column density NH2, an abundance ratio of [CO]/[H2] = 8 10?5 (Frerking, Langer, amp; Wilson 1982) was assumed: NH2 = NCO V vobs 8 10?5 (1) where vobs is the observed FWHM of a Gaussian t to the CO J = 2 ! 1 line. Table2 summarizes the results of the CO modeling. The average kinetic temperature, hydrogen volume and column densities at the continuum sources are: Tk = 56 11 K, log nH2 (cm?3) = 3:5 0:3, and NH2 (1022 cm?2) = 7 4, respectively (quoted errors are the standard deviation among the sources).... ..."

"... In PAGE 8: ... 1980). These three parameters are listed in Table1 . The grains polarizing in the optical show a range of polarization e ciencies up to a maximum value of p(%)/EB?V =9.... In PAGE 8: ...0 (or pmax= V 0:032) along those lines of sight where conditions for alignment are optimal (Serkowski, Mathewson amp; Ford 1975). For both HD 197770 and HD 147933-4, pmax is well below this maximum value for the measured reddening ( Table1 ). Figure 2 shows the linear polarization data.... In PAGE 11: ... The ts, displayed in Figure 3, are quite good. Using also the basic data in Table1 and 2, we construct the ratios of polarization to extinction for the continuum, pc/ c and for the feature, p= at the nominal center of the extinction bump, 4.6 m?1.... In PAGE 24: ... The solid line represents the three-parameter Serkowski law t to the visible and infrared data only, while the dotted line illustrates the extrapolation of this t into the ultraviolet (see x 2.2 and Table1 ). The error bars are statistically 1{ , and are not shown for those smaller than the symbols.... ..."