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Transcribe page 6 of 38
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[[start page]] [[preprinted]] 8 [[/preprinted]] [[underline]] Saturday, October 28, 1905 [[/underline]] The Small Magellanic Cloud. Certain Variables re-examined B20655 | No.60 = 14.4? Diff. | | No.291 15.3? Extremely diff B20678 No.60 = 13.6? Image very poor - Diff. A6984 N0.290 = 15.7? There is a defect near im. of alpha making meas. diff 6985 15.4? Image very sharp 6986 16.5? [[strikethrough]]Ims.[[/strikethrough]] 6987 15.3 7016 15.0 A2189 No.[[strikethrough]]60[[/strikethrough]]15 14.0 | No.60 14.0 2187 "[[ditto for No.15]] 14.0 13.7 B34116 No.60 13.6 No.391 14.[[strikethrough]]3[[/strikethrough]]7 [[strikethrough]]Moving star ims. before?[[/strikethrough]] B20638 No.391 [[strikethrough]]14.2[[/strikethrough]] 15.0? [[strikethrough]]""""[[ditto for Moving star ims. before?]][[/strikethrough]] B20645 No.391 [[strikethrough]]14.1[[/strikethrough]] 16.0? 20678 No.391 14.[[strikethrough]]0[[/strikethrough]]7 Observation of No.391 on Plate B20645 very uncertain. All observations on this group of plates are difficult for this star. A3393 No.391 15.3 A6981 ""[[ditto for No., ditto for 391]] 15.7 A2183 ""[[ditto for No., ditto for 391]] 15.6? B10746 No.60 13.8 B9625 No.60 13.9? Images of [[nu?]] and [[?]] poor B28831 No.60 14.2 A6860 No.60 13.9 A6913 No.60 14.1 A2149 [[end page]] [[start page]] [[preprinted]]9[[/preprinted]] [[underline]]Thursday, November 1, 1905[[/underline]] The Small Magellanic Cloud A6984 No.391 | 15.9? diff A2149 No.391 | Too poor 14.7? B20645 ""[[ditto for No., ditto for 391]] 15.7? B20678 ""[[ditto for No., ditto for 391]] 14.8? B20650 ""[[ditto for No., ditto for 391]] 14.7 B20655 ""[[ditto for No., ditto for 391]] 15.0? diff. B20638 | 14.7? A3393 | 15.4? diff. On all Bache plates No.391 is too near limit of visibility of plates for satisfactory observation The original obs in A3393 15.1 was certainly too bright. Taking mean of obs. on page 8 and obs. above, 15.4 may be [[later?]] to represent nearly the magnitude A6981 On this plate the variable is certainly extremely faint. The image[[strikethrough]]s[[/strikethrough]] [[strikethrough]]are[[/strikethrough]] is less sharp than those of comparison stars alpha, beta and gamma. Probably 15.9 would be a better estimate of [[the?]] brightness than 15.7, [[twice?]] observed. No.15. Re-examination of Plates B9625, B9808 and B10746 show that the variable was in each case faint, as recorded. This seems to give no opportunity for maximum brtness J.D. 2620 and J.D. 2820. [[end page]]
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