454 



Lieut. HerscheFs Examination of [June 18, 



star in the central patch (sketched) . This star was frequently 

 in the spectroscopic field, but no lines were seen : a haziness 

 suspected. 



April 26. Continuous spectrum : readily found owing to the 

 central star. 



No. 4361. April 17. Very remarkable ; very bright ; extremely large ; 



extremely irregular figure ; with large cluster."] A large 

 nebulous area visible in finder ; not examined with telescope ; 

 spectrum linear, but feeble. D + r98. Some doubt about 

 the reading of D. 



No. 4390. April 16. ["Planetary; very bright; very small; round; little 

 hazy."] Seen in spectroscope as a short bright line with 

 a second fainter one ; a third suspected. Measurement 

 D-h2-34. 



No. 4403. April 26. [" Very remarkable ; bright ; extremely large ; ex- 

 tremely irregular figure."] I should say this is as bright an 

 object as any of the larger nebulse T have seen. It is a 

 striking object (detailed account of appearance and sketch), 

 and the various parts could be recognized as they were brought 

 on the slit. Measurements, D being read by reflected light 

 from soda-flame : — 



tll]^''' D = 2-48| j3_^2-10. 

 4-59 4-59 =2-44 J 



No. 4628. April 26. ["Remarkable; planetary; very bright; small; 



elliptic."] Easily seen in telescope, and confidently looked 

 for in spectroscope. Spectrum as bright and distinct as any 

 yet seen ; lines measured by ohliteration with cross-wires in 

 a dark field, D being obtained from a reflected soda-flame. 

 4-61. 4-81, ; 5-16, D = 2'41, 



or D + 2-20, +2-40, +275. 



No. 4510. May 3. [" Planetary; bright; very small; round."] I am rather 

 surprised to find this described as "bright, very small;" I 

 should have expected very bright, pretty large. Its spectrum 

 is the first in which I have suspected a new character. In 

 the first place, there is no trace of a third line, and the second 

 is more uncertain, as though there were more than one fainter 

 companion. The brightness, of the principal line is considerable, 

 making measurements by estimation behind the wires in a dark 

 field not very difficult. , The following measures are, I believe, 



trustworthy: D = | ^132 } 2-32, Neb. line = ^.'gg | 4-64. 



In the second place, therefore, here is a reliable measure- 

 ment, differing widely from the rest (too widely, as I think, 



