f flare or other obvious variability is seen in the source light curve; * additional source notes follow: 5 1T model gives a high but uncertain temperature kT>=4keV. 15 HLL-131 is a likely IR counterpart, but there is a ~4" positional offset 15 even after correcting for systematic differences between CXO and HLL 15 coordinates. 16 HLP-54 is a likely IR counterpart, but there is a ~4" positional offset 16 between CXO and HLP coordinates. 18 Flare spectrum gives kT=5.4^+0.0^_-2.2_keV and logLX=31.58ergs/s 18 (unabsorbed). 27 Flare spectrum gives kT=4.2^+0.6^_-0.7_keV and logLx=30.99ergs/s 27 (unabsorbed). (Fig. 7) 36 Variability is present throughout the observation. Complex or rapidly 36 varying temperature structure suspected. 39 Source lies in CCD gap. Flux is uncertain. 41 Weak flare whose spectrum gives kT=2.6^+1.0^_-0.5_keV and logLx=30.80ergs/s 41 (unabsorbed). 52 Weak flare. Insufficient counts to accurately determine flare parameters. 75 1T models give {chi}^2^_red_=1.09 but 2T models give a slightly better fit 75 with {chi}^2^_red_=1.05 and converge to NH=1.7^+0.2^_-0.2_*10^22^cm^-2^, 75 kT_1_=0.6^+0.3^_-0.2_keV, kT_2_=2.7^+0.4^_-0.3_keV, and logLx=31.50ergs/s 75 (unabsorbed). 81 Flare spectrum gives kT=9.8^+0.0^_-4.5_keV and logLx=31.08ergs/s 81 (unabsorbed). (Fig. 7) 85 Flare spectrum gives kT=3.8^+0.5^_-0.5_keV and logLx=31.34ergs/s 85 (unabsorbed). (Figs. 7 & 10) 93 Flare spectrum gives kT=3.5^+2.1^_-1.1_keV and logLx=30.98ergs/s 93 (unabsorbed). 94 Slow variability is present throughout the observation. DEM model shows a 94 double-peaked structure with cool and hot components. 99 1T models give {chi}^2^_red_=0.94 but 2T models give a slightly better fit 99 with {chi}^2^_red_=0.92 and converge to a larger absorption 99 NH=2.7^+0.4^_-0.6_*10^22^cm^-2^. 104 Declining count rate may indicate decay phase of a flare. 105 Weak flare. Insufficient counts to accurately determine flare parameters. 108 Flare spectrum gives same temperature kT=3.3^+1.0^_-0.6_keV and 108 logLx=31.01ergs/s (unabsorbed). 114 Declining count rate may indicate decay phase of a flare. Possible spectral 114 contamination from nearby source. 120 Source may be affected by moderate pileup (~10-15%) during short periods 120 when the count rate fluctuated to levels of ~0.15cts/s. 123 Count rate increased throughout the observation (Fig. 7). 133 1T models are only marginally acceptable with {chi}^2^_red_=1.35. DEM model 133 peaks near 1.7keV but shows substantial emission up to ~4keV. Declining 133 count rate may indicate decay phase of a flare. 139 Slowly rising variability and outburst spectrum gives kT=4.2^+0.0^_-1.6_keV 139 and logLx=30.79ergs/s (unabsorbed). 141 The spectrum used to determine NH, kT excludes data from a weak flare that 141 occurred during the last 5ksec of the observation. 145 No reliable spectral fit because of contamination from nearby source 145 no. 148. Possible optical counterpart is GSC 04771-00589. 148 No reliable spectral fit because of contamination from nearby source no. 145 152 1T models are only marginally acceptable with {chi}^2^_red_=1.38. DEM model 152 peaks near 1.4keV. 153 1T models are not acceptable with {chi}^2^_red_=1.91 but 2T models are 153 acceptable with {chi}^2^_red_=1.00. NH is from 2T model (kT_1_=0.8keV, 153 kT_2_=3.4keV). 160 Weak flare. Insufficient counts to accurately determine flare parameters. 174 Flare spectrum gives kT=4.5^+0.6^_-0.7_keV and logLX=31.45ergs/s 174 (unabsorbed). Moderate pileup may have occurred near flare peak. (Fig. 7) 175 Long duration flare with a secondary peak during decay phase (Fig. 7). Flare 175 spectrum gives kT=5.2^+2.6^_-1.3_keV and logLx=31.47ergs/s (unabsorbed). 182 The counterpart name IRS 2b is from Nisini et al. (1994A&A...290..463N). 182 Spectral fit parameters are uncertain because of possible contamination 182 from source 183 located 1.7" to the north (Fig. 2). Some improvement is 182 obtained with 2T models which place most of the emission measure in a cool 182 component at kT_1_ ~0.2keV and require a larger absorption column 182 NH_=5.5^+2.5^_-2.0_*10^22^cm^-2^. 183 Weak flare. Insufficient counts to accurately determine flare parameters. 183 Spectral fit parameters are uncertain due to possible contamination from 183 source 182. 187 1T models give {chi}^2^_red_=1.10 but 2T models give a slightly better fit 187 with {chi}^2^_red_=0.88 and converge to a higher absorption 187 NH=6.1^+4.9^_-2.7_*10^22^cm^-2^, kT_1_=0.6^+1.0^_-0.3_keV, and a hotter 187 component with uncertain temperature kT_2_>=3keV. 188 Weak flare. Flare spectrum gives kT=3.2^+0.8^_-0.6_keV and same 188 logLx=31.25ergs/s (unabsorbed). 189 1T models are not acceptable ({chi}^2^_red_=1.52) nor are 2T models 189 ({chi}^2^_red_=1.68). Hard heavily-absorbed spectrum with uncertain 189 temperature. 192 Slowly rising outburst (Fig. 7) with high absorption. The X-ray temperature 192 shortly after onset reached values of at least kT~6keV, and possibly as 192 high as kT ~10keV. The unabsorbed luminosity varied from a pre-outburst 192 value logLx=30.5ergs/s to at least logLx=31.8ergs/s during the outburst. 192 Source is affected by moderate pileup (~27%) near end of observation. 193 Declining light curve may indicate decay phase of a flare. 196 1T models give a high but uncertain temperature kT>=3.1keV. 207 Slowly rising outburst (Fig. 7). Very hard source. Time-averaged outburst 207 spectrum gives kT=7.8^+0.0^_-3.3_keV and logLx=31.4ergs/s (unabsorbed). 207 Temperature peaked about 4 hours after onset followed by a general decline, 207 but there is evidence for at least one reheating event. DEM model of 207 outburst spectrum suggests that most of the emission measure comes from 207 plasma above ~4keV. Insufficient counts to analyze pre-outburst spectrum. 210 Declining light curve during first ~20ksec of observation may indicate decay 210 phase of a flare. Decay spectrum gives kT=4.9^+1.7^_-1.1_keV and 210 logLx=31.59ergs/s (unabsorbed). Source may be affected by moderate pileup 210 (~16%) at beginning of observation. 222 Weak flare. Insufficient counts to accurately determine flare parameters. 223 A faint IR source is visible at the X-ray position in 2MASS H and K-band 223 images (2MASS J05415068-0153063), but is flagged as a filter glint 223 artifact. Because of the close positional agreement with CHANDRA, the IR 223 source flagged as an artifact may be real. 232 1T models are only marginally acceptable with {chi}^2^_red_=1.39. 234 Declining light curve may indicate decay phase of a flare. 258 Possible double source. 269 Count rate declined throughout the observation (Fig. 7). 272 Soft source (low absorption). 1T models underestimate the flux below 1keV 272 and are not acceptable ({chi}^2^_red_=3.2). 2T models give improved fits 272 when the Fe abundance is allowed to vary ({chi}^2^_red_=1.24), converging 272 to Fe=0.8 solar with kT_1_=0.77keV and kT_2_=1.9keV. DEM model peaks near 272 0.7keV. 274 1T models are only marginally acceptable with {chi}^2^_red_=1.42. DEM model 274 peaks near 2keV. Variability is present throughout the observation.