"... In PAGE 14: ... The accretion disk parameters (and 1 errors) derived using the Smak pro le ts for GRO J0422+32 are compared to those derived for the XRN A0620-00 and X-ray Nova Muscae 1991 (Orosz et al. 1994) in Table2 . We see that the r1 values derived for A0620-00 and GRO J0422+32 are very similar, and are a factor of two larger than that found for Nova Muscae.... ..."

"... In PAGE 12: ... Three of the functions are able to rank the X-ray structure first for individual proteins but no energy function can consistently rank X-ray structures highly for all proteins. However, some trends in the data of Table6 are discernible. To see these more easily we calculated the quality factor, Q(r) for each rank (see Methods), and then averaged these values Q(r) over different proteins for the same function ( Qf ) and over different functions for the same protein ( Qp ).... In PAGE 12: ... This discrepancy is an indication that our ensembles are a more challenging test of certain energy functions. The Z-scores averaged over different proteins also show that the energy functions, VdW(MJ), VdW(HL) and Histogram, do better than the three others, paralleling what is seen in Table6 using Q-scores. Finding near-native folds As important a characteristic of a potential function as being able to identify the X-ray conformation from a group of incorrect confor- mations is, it is perhaps more important for a potential function to be able to identify native-like conformations.... ..."

"... In PAGE 2: ... The adopted thresholds result in less than one spurious source in the eld of view of each de- tector. The nal X-ray catalog contains 28 HRI sources po- sitionally matched with at least one PSPC source, 13 HRI sources with no PSPC counterpart and 37 PSPC sources with no HRI counterpart, for a total of 78 X-ray sources, reported in Table1 . We have used the notation Pxx and Hxx, where xx are two digits, for the PSPC-only and HRI- only X-ray sources, and four digits for sources detected both in PSPC and HRI, with the rst two digits giving PSPC source number.... In PAGE 5: ...OSA T Observ ations of NGC 2422 5 Table1 . Continued src RA2000 Dec2000 X-o set o ax psnr hsnr PSPC ux HRI ux Lx log(fx=fv) optid sp mpg MPastr MPph O-o set (hour) (deg.... In PAGE 6: ...Barb era et al. Table1 . Continued src RA2000 Dec2000 X-o set o ax psnr hsnr PSPC ux HRI ux Lx log(fx=fv) optid sp mpg MPastr MPph O-o set (hour) (deg.... In PAGE 8: ... A few of the sources have as most likely counterparts dMe/dKe stars. Spectral types derived from the collected optical spec- tra are reported in Table1 . Photographic magnitudes were derived from aperture photometry applied to the Digitized Sky Survey plates, using the photometric cali- brations given by Lasker et al.... In PAGE 8: ... (2000). We have identi ed as having high photometric mem- bership probability (\H quot; ag in Table1 ) all stars within 0.8 mag from the ZAMS of the cluster.... In PAGE 10: ...tars observed at the 1.5 m ESO telescope. For 18 X-ray sources with multiple optical counterparts we have used visible to X-ray ux ratios and distances between the X- ray source and the optical counterparts as discriminating factors in the counterpart identi cation process. The six right-most columns of Table1 report the op- tical identi cation number of matched sources, spectral type when available, photographic magnitude, astromet- ric membership ag (Sect. 3.... ..."

"... In PAGE 2: ... 3. Analysis of the X-ray spectra In Table1 we have listed some characteristics of the X-ray observations. Two observations of Procyon are available in the pub- lic ROSAT archive: the rst one comprises two exposures, separated by about one year; the second observation has been performed 6 months after the end of the rst one.... In PAGE 4: ...ig. 1. Upper panels: ROSAT PSPC spectra of the sample stars and best- t 2-T models. Dotted and dashed lines indicate the contribution due to the cool and the hot component, respectively; the total spectrum is represented with a solid line. The spectrum of Procyon is relative to the data segment #3 (see Table1 ). The best- t model for HR 3625 is the one obtained assuming NH = 5 1019 cm?2 (see Table 2).... ..."

"... In PAGE 16: ...e give the hardness ratios H21 and H31 as de ned in x 4.4. The fractional contribution of resolved, unresolved, and truly di use emission to the counts within each band is given. Finally, the unabsorbed luminosity for each component and band are given, based on the best- t spectra for each component (x 6 and Table3 below). Within one e ective radius, 61% of the counts and 71% of the X-ray luminosity is resolved into individual X-ray sources for the total band.... In PAGE 20: ...72{10 keV energy range after subtraction of background, is shown in Figure 11. We rst t the spectrum assuming the same spectra properties and properties as were used to t the total ASCA plus ROSAT spectrum in ISB (row 1, Table3 ). The normalizations of the hard (bremss) and soft (MEKAL) components were allowed to vary.... In PAGE 21: ... However, the abundance in the MEKAL model was essentially unconstrained, and there is no clear evidence for emission lines in the spectrum, so we adopt a blackbody model for the soft component. Rows 10 and 11 of Table3 show the ts without and with the soft component. The ux of the soft component is small, but it improves the t signi cantly.... In PAGE 32: ... The total X-ray luminosity of the gas may be too low to be consistent with a global cooling in ow involving the total stellar mass loss rate of the galaxy. The total bolometric luminosity of the gas is Lbol 3:6 1040 ergs s?1, assuming the best- t soft component model for the unresolved emission ( Table3 ). Given its optical luminosity and assuming a normal elliptical galaxy stellar mass loss rate, the total rate of stellar mass loss is about 0.... In PAGE 54: ...ig. 11.| The data points in the upper panel are the cumulative X-ray spectrum of all of the resolved sources in the inner e ective radius of NGC 4697. The solid histogram is the best- t model spectrum (row 3 in Table3... ..."

"... In PAGE 4: ... The best t model provides, along with the best- t values of the other free parameters, the centre of the Gaussians in each axis; these numbers provide a surpris- ingly robust measure for the location of the centre of each cluster.The cluster X-ray centres calculated in this way are pre- sented in Table2 [columns (2), (3)]. This procedure also pro- vides the errors of the determined cluster centre, which are given in Table 2 [column (4)].... In PAGE 4: ...The cluster X-ray centres calculated in this way are pre- sented in Table 2 [columns (2), (3)]. This procedure also pro- vides the errors of the determined cluster centre, which are given in Table2 [column (4)]. The results and their position on the X-ray images were also examined by eye, to make sure that the adopted centre had not been unduly in uenced by any residuals from the subtraction of the point sources.... In PAGE 6: ... For each system, the error in mainly depends on the accuracy of the position of the cluster centre; the position of the optical galaxy has been measured with an accuracy of 1 arcsec (Ledlow amp; Owen 1995b). For the sources for which a measurement of the error for the position of the cluster centre exists, the error in is calculated and presented in Table2 . Generally, the largest inaccuracies of correspond to sources which lie very close to the cluster centre, since a small change in the position of such a source corresponds to a large change in angle.... ..."

"... In PAGE 21: ...nd we therefore calculated it on the photon energy range 0.1 to 2.4 keV from the best t models. In Table6 we list these luminosities, along with the ratio LX=LBol, which has been found to be about 10?7 for O stars (Pallavicini et al. 1981).... In PAGE 30: ... The primary result of the inclusion of wind attenuation is that the total X-ray luminosity generated in the wind does not escape. In Table6 and Figure 2 we show for the three relevant stars the adjustments to the LX=LBol values that are caused by including wind attenuation. One can only assume that this correction is larger still for the O stars due to their denser winds.... ..."

"... In PAGE 7: ... The greyscale is proportional to the square root of the X-ray surface brightness, and the values vary between 1 and 25 cts pixel?1. The numbers identify the detected sources in this regions as listed in Table1 below. The optical center of the galaxy coincides with the position of Src.... In PAGE 7: ... For comparison, Figure 4 shows the Digital Sky Survey optical image of the same region as shown in Figure 3. The circles indicate the positions of individual X-ray sources which are identi ed in x 4 and Table1 below. The distribution of X-ray point sources in Figure 1 appears to be elongated at the same position angle as the optical image of this E6 galaxy (67 ; Jedrzejewski, Davies, amp; Illingworth 1987; Faber et al.... In PAGE 8: ... All of the source detections were veri ed by examining the image. Table1 lists the 90 discrete sources detected by this technique, sorted in order of increas- ing distance d from the center of NGC 4697. Columns 1-9 give the source number, the IAU name, the source position (R.... In PAGE 9: ... These should be spread out fairly uniformly over the S3 image (Figure 1), except for the e ects of the reduced exposure and increased PSF at the outside of the eld. Thus, the unrelated sources should mainly be found at larger distances from the optical center of NGC 4697 (the bottom part of Table1 ), while the sources associated with NGC 4697 should be concentrated to the center of the galaxy. Within 20 of the center of NGC 4697 (roughly the region covered by Figure 2 in Paper 1), 2 of the 60 the detected sources would be expected to be unrelated to NGC 4697.... In PAGE 9: ... All but one of these sources lie within a few arcsec of strong sources which we detect with Chandra. The identi cations of these sources (the sources numbers in Table1 from ISB) are listed in column 10 of Table 1. ISB Src.... In PAGE 10: ...mage of this region (Fig. 4). Eleven of the sources had possible faint optical counterparts on this image; four others appear on deeper optical images discussed below. These are all marked with note \e quot; in Table1 . The possible faint optical counterparts of Srcs.... In PAGE 10: ...3 associations to occur at random. Thus, it is likely that all of the 7 associations of X-ray sources with optical globular cluster candidates in Table1 are real. However, at the distance to NGC 4697, globular clusters are not resolved in ground-based optical images, and the candidate globulars were identi ed by luminosities and (possibly) colors.... In PAGE 11: ... (Of course, some of the sources are background and foreground objects and not at the distance of NGC 4697.) The resulting X-ray luminosities are given in column 9 of Table1 , and range from about 5 1037 to 2:5 1039 ergs s?1. The cumulative luminosity function of all of the sources is shown as a histogram in Fig- ure 5, under the assumption that all of the sources are located at the distance of NGC 4697.... In PAGE 13: ....2 s periodicity on the events imposed by the ccd readout. Applying the KS test, we found that 11 sources (Srcs. 2, 9, 18, 26, 36, 51, 52, 55, 58, 64, amp; 84) were inconsistent with a constant ux at gt;90% con dence; these sources are noted in Table1 . This is not very strong evidence for variability, since with a total of 90 sources, one might expect 9 sources to show variations at the 90% con dence just as a result of statistical uctuations.... In PAGE 45: ... (The ACIS pixels are 0: 00492 square.) The positions of detected sources in the image are indicated by their source numbers in Table1 . Src.... ..."