2 7 480 I 28 At the present time the photometric measures for this fourth magnitude spectroscopic binary are open to some question. The three spectroscopic orbits by Harper, FKlson and Daniel agree fairly well, except that the first found certain faint lines on his plates that he attributed to the spectrum of the secondary star '), while the Lick z, and Allegheny 3, observers find no trace of the second spectrum. Upon a request from the writer, Prof. Campbell, Dr. Moore and Dr. Uaynes made a

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... cial examination of Lick Observatory plates but failed to find any definite indication of the secondary. The earlier photometric observations at Princeton gave what seems to be definite evidence of light variability of the eclipse character4). The later series of measures, however, gave some doubtful results. Though much care was taken, the observations were uncertain to some extent and difficult, because the whole range of variation is apparently small Das Minimum, zu ~o m o im S (oder 9m6 im R), fallt auf den 1 0 . Okt. 1 9 1 4 (J. D. 2 4 2 0 4 1 6 ) ; das Maximum, zu 3m8 im B (oder 4mo mit blofiem Auge), auf den 29. Januar 1 9 1 5 (J. D. 2420527) und also 328 Tage nach dem vor-