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I thought, would be a permanent and measurable record of the 

 quantity of the eclipse for future reference. Having obtained 

 the negatives, the next thing was to watch for the final contact. 

 Not only was the sun's image less steady at this period, but also 

 an alarm of tire somewhat disturbed tlie observation, so that it 

 was not so certain as the first, still I do not think it can be more 

 than two seconds out. The final contact took place at 1 h. 54 m. 

 30 s. p.m. By these times of first and final contact I find that 

 the second photo I took at 12 h. 36 m. 4 s. was 1 m. 42-5 s. 

 earlier than the centre of the eclipse, but the nearest thereto. 

 From this I have made a photographic enlargement, six and a- 

 half inches in diameter. By applying the accompanying scale of 

 hundredths to this photo, we see at once that the encroachment 

 or overlapping measures 40-5 hundredths. Allowing for the 

 photo not being exactly central, a very small amount should, of 

 course, be added. Being so near the centre of the eclipse, the 

 advance made would be very small (not more than half one of 

 the divisions of the scale), so that the whole amount of the ob- 

 scuration may fairly be set down as 41 hundredths of the sun's 

 diameter. As proof of this, it may be added that the third 

 negative, taken at 12 h. 40 m. (being 2 m. 13-5 s. later than the 

 centre of the eclipse), measures just perceptably less than the 

 former. It may be stated as a proof of the absence of anything 

 in the way of distortion that the photos taken previous to the 

 eclipse are perfectly circular. The enlargement is so sharp that 

 on close examination some of the protuberances on the moon's 

 limb can be readily distinguished. 



