OF ARTS AND SCIENCES. 381 



year. Father Hagen has begun a systematic search for variables of 

 the fourth class in a great circle whose pole is 12'' 40", +28°, and 

 has examined the DM. chart No. 32 in accordance with suggestions 

 given in "Variable Stars of Short Period." See these Proceedings, 

 XVI. 277, 281. He suspects the following stars to be variable: 

 DM. +55° 2587, +44° 3368, +44° 3402. Dr. Hartwig has not 

 made any statement with regard to his observations in 1886. Pro- 

 fessor Safarik has been prevented by illness from making a complete 

 statement of his work, but has sent a list containing a large number of 

 observations, which are entered as usual in Tables I. and II. State- 

 ments have also been received from some observers who have not 

 contributed to previous reports. The additional abbreviations thus 

 required in Tables I. and II. are explained in the following para- 

 graphs. 



Bj. These observations were made by Mr. Joseph Baxendell, at 

 Birkdale, Southport, England. The telescope used in the observa- 

 tions is an achromatic refractor of 6 inches' aperture, made by Cooke 

 and Sons, of York ; and the magnitudes of the variables are determined 

 by comparisons with neighboring stars whose magnitudes have been 

 determined by the method of limiting apertures. 



B,. These observations were made by Mr. Joseph Baxendell, Jr. 

 The place, instrument, and method of observation were the same as 

 described under the heading Bj. 



Eq. These observations were made with the equatorial telescope 

 of the Observatory of Harvard College. The aperture and focal 

 length of the instrument are respectively 15 and 279 inches. The 

 magnifying power employed was ordinarily 103. The observers were 

 Messrs. Arthur Starle and 0. C. Wendell. The observations consist 

 in measurements, made with the wedge photometer, of the comparison 

 stars known to have been employed by previous observers ; but when 

 the variable stars themselves were visible, they were incidentally com- 

 pared with others by estimate, according to the method of Argelander, 

 and were also observed with the wedge. The work will be continued 

 during the coming year, and it is desired to make it include as many 

 as possible of the comparison stars which have been em{)loyed by any 

 observer. The list now in use is chiefly derived from the published 

 work of Argelander, Schonfeld, and Oudemans. Observers are re- 

 quested to send lists of the comparison stars not included in these pub- 

 lications which they have themselves employed, or which have been 

 employed to their knowledge by others. It is very desirable that 

 not only the places of these stars, but also their designations in the 



