"... In PAGE 19: ... The values were obtained with excited fermion masses of 165 GeV/c2. channel e ` ! ` 46 50 45 ! 46 46 46 channel ps =172 GeV ps =161 GeV ` ! W 17 14 ! `W 12 12 Table1 0: E ciencies for the double production modes at ps = 161; 172 GeV. The values were obtained with excited leptons masses of 70 GeV/c2.... In PAGE 20: ...6 80.1 Table1 1: Lower limits (in GeV/c2) at 95 % con dence level on the excited leptons masses from the double production modes. leptons are given in table 11.... ..."

"... In PAGE 6: ... We compute CCD6CPCS making use of UV fluxes derived from archived International Ultraviolet Explorer (IUE) data of Castor A and B. In Table3 we tabulate the IUE fluxes of each of the two binaries at the wavelengths corresponding to the excita- tion energy between the upper levels of the CU and the CX line for oxygen and neon. Making use of the distance (BDBI pc), stellar ra- dius (derived from the Stefan-Boltzmann law), and limb dark- ening (from Table 1 of Diaz-Cordoves et al.... ..."

"... In PAGE 14: ... Note that it would be more appropriate to estimate optical property and aging uncertainty at monthly resolution, as with SCF, but this would require an excessive number of off-line SNICAR runs. [65] The range in mean Fs,snow estimated with these approaches is shown in Table4 . Uncertainty in emissions has the largest bearing on BC/snow forcing, closely followed by snow aging.... ..."

"... In PAGE 4: ...| (following pages) Normalized spectrum of HS 1700+6416 obtained with the echelle spectrograph on the KPNO 4m telescope, plotted as a function of vacuum heliocentric wavelength. Absorption lines due to extragalactic metals are marked with a number that identi es the line in column 1 of Table1 . At lt; 4560 A, most of the absorption lines are due to the Ly forest.... In PAGE 15: ...ripp et al. 1996). We have used this ratio of the HS 1700+6416 spectrum to the HS 1946+7658 spectrum to identify telluric lines only; for all other measurements reported in this paper we use the coadded spectrum shown in Figure 1 (which has not been divided by the HS 1946+7658 spectrum). Table1 lists all statistically signi cant (W 4 ) extragalactic absorption lines detected in the KPNO HS 1700+6416 spectrum. Table 1 also lists the heliocentric vacuum wavelength of the centroid of each absorption line and a line number which identi es the absorption line in Figure 1.... In PAGE 15: ... Table 1 lists all statistically signi cant (W 4 ) extragalactic absorption lines detected in the KPNO HS 1700+6416 spectrum. Table1 also lists the heliocentric vacuum wavelength of the centroid of each absorption line and a line number which identi es the absorption line in Figure 1. Identi cations of the line species derived from the Morton (1991) nding list are tabulated in column 4 of Table 1, and Table 2 summarizes by redshift the heavy element systems we detect in the spectrum of this quasar.... In PAGE 15: ... Table 1 also lists the heliocentric vacuum wavelength of the centroid of each absorption line and a line number which identi es the absorption line in Figure 1. Identi cations of the line species derived from the Morton (1991) nding list are tabulated in column 4 of Table1 , and Table 2 summarizes by redshift the heavy element systems we detect in the spectrum of this quasar. We have detected 13 heavy element absorbers in the direction of this quasar, 6 of which also produce detectable Lyman limits in the FOS spectrum of HS 1700+6416 obtained by Reimers et al.... In PAGE 15: ... (1992). There are several absorption features in Table1 for which we could not nd positive identi cations (labeled \UID quot; in column 4 of Table 1). Most of these unidenti ed lines are weak ( lt; 5 ), so they could be the C IV 1548.... In PAGE 15: ... (1992). There are several absorption features in Table 1 for which we could not nd positive identi cations (labeled \UID quot; in column 4 of Table1 ). Most of these unidenti ed lines are weak ( lt; 5 ), so they could be the C IV 1548.... In PAGE 17: ... Table1 |Continued Line vac W W Identi cation zabs log N b log Na Number ( A) ( A) (cm?2) (km s?1) (cm?2) (1) (2) (3) (4) (5) (6) (7) (8) 21 5121.89 0.... In PAGE 18: ... Table1 |Continued Line vac W W Identi cation zabs log N b log Na Number ( A) ( A) (cm?2) (km s?1) (cm?2) (1) (2) (3) (4) (5) (6) (7) (8) 38 5747.49 0.... In PAGE 19: ... (1996), and this error is added in quadrature to the error from photon counting and read noise to get the total uncertainty in Na(v). Integrated apparent column densities of all metals detected in the HS 1700+6416 spectrum are given in column 8 of Table1 . For further information on the apparent column density method, see Savage amp; Sembach (1991), Jenkins (1996), and references therein.... In PAGE 19: ... For further information on the apparent column density method, see Savage amp; Sembach (1991), Jenkins (1996), and references therein. For most of the lines in Table1 we use oscillator strengths and wavelengths from Morton (1991). However, for some transitions we use the oscillator strength revisions summarized in Tripp et al.... In PAGE 19: ...8 A) simultaneously, but we have tted di erent elements and di erent ionization stages independently. The column densities, Doppler parameters, and redshifts obtained by tting Voigt pro les in this fashion are listed in columns 5, 6, and 7 of Table1... In PAGE 22: ... However, the weaker Mg II 2803.5 A line yields an integrated column density in good agreement with the column density from pro le tting (see Table1 ), so this magnesium doublet is only weakly saturated. Reimers et al.... In PAGE 23: ...nd Reimers et al. (1992) nd that log N(H I) = 16.85. The Mg II 2796.4 and 2803.5 A lines at this redshift are recorded at high signi cance levels in the KPNO spectrum (see lines 40 and 41 in Figure 1 and Table1 ). The integrated apparent column densities of these Mg II lines are in agreement, but inspection of the Na(v) pro les suggests that they are undersampled, and the higher column density from pro le tting indicates that the lines may be moderately a ected by unresolved saturation.... In PAGE 24: ...85. Inspection of the Na(v) pro les indicates that these C IV lines are not signi cantly a ected by saturation, and this conclusion is supported by the good agreement of the column densities from pro le tting and Na(v) integration (see Table1 ).... In PAGE 28: ...2, 1550.8 A doublet (lines 26 and 27 in Figure 1 and Table1 ). Comparison of the Na(v) pro les indicates that these C IV lines are not substantially a ected by unresolved saturated component structure.... In PAGE 28: ...igure 1), which corresponds to 2.432 lt; zabs lt; 2.441. Figure 4 shows an expanded plot of this region of the KPNO spectrum along with the component t which gives the pro le parameters listed in columns 5-7 in Table1... In PAGE 29: ....| (opposite page) The normalized absorption pro les of the C IV complex at 2.432 lt; zabs lt; 2.441 (lines 28-33 in Figure 1 and Table1 ), plotted versus vacuum Heliocentric wavelength (bottom axis) and velocity in the zabs = 2.43877 rest frame (top axis).... In PAGE 29: ... Here each C IV doublet is indicated with a single thin vertical line at the measured redshift. The line identi cation numbers from Table1... In PAGE 33: ...2, 1550.8 A doublets at this redshift (see lines 3-4 and 38-39, respectively, in Table1 and Figure 1).... In PAGE 44: ...eems like a high metallicity for zabs = 2.315. However, it may not be. Recently, several high quality abundance measurements for intervening damped Ly QSO absorbers have appeared in the literature (Lu et al. 1996 and references therein, see their Table1 6). In Figure 8 we show the Si and Al abundances measured in these damped Ly absorbers with open circles.... In PAGE 51: ... Finally, we comment that these photoionization models are highly simpli ed, and there are some indications that the real absorbers are more complicated than the assumed models. Consider the Doppler parameters derived from pro le tting in Table1 . These b-values can be expressed as a sum with a term due to thermal motions (bt) and a term which includes all non-thermal motions (bnt) such as bulk motions and turbulence, b2 = b2 nt + b2 t = b2 nt + 2kT m = b2 nt + (0:129)2T A ; (4) where m is the mass and A is the atomic weight of the element and b is measured in km s?1.... ..."

"... In PAGE 9: ... 5. To illustrate its accuracy for the FIRE II #0Dow conditions, Table2 compares it to the NEQAIR code of Park. 14 NEQAIR is a detailed line-by-line nonequilibrium radiation model.... ..."