The Astrophysical journal . » O O t-» O H w ro++++ + + .-J- — r^. co sC r*« O N vO Oi ir> t^*sO 3 t^ O ** n 0 CO 2 i|l C K B M s B ° 0 o O ip 1^ PC O -1 CO \C Uj v. 0 H C? 1^; n m co 0 0 pc 0 pc pc pc tt m r^co 0 Pi 1 PC «o OOwvCr^rc- CO i^h mPi ?*? tJ- mO ih m Own pcpcpcpcpcpc pc rr-i-i PCCO pi X r~-O Pi 00 >PjvO ^1-0 0 0 « 0 F> 0 Z O ti - f> O PC m (n in m 0 a -r ~ - -r 0 h1- pj re n OOpCOOpiO pi « i c^ - T J -OOO IP C IP; IP; *C t^- r^ c ~ X o> vCt^-X g -f IT, IP, IP, IT, C CT ~ O O O — — — pi pc r^ PC Pi-to ip. pc -rO r^ t^X CO CO 00- pi n « pi PQ pc c BBSS PQ pq -t- irv r-»
The Astrophysical journal . » O O t-» O H w ro++++ + + .-J- — r^. co sC r*« O N vO Oi ir> t^*sO 3 t^ O ** n 0 CO 2 i|l C K B M s B ° 0 o O ip 1^ PC O -1 CO \C Uj v. 0 H C? 1^; n m co 0 0 pc 0 pc pc pc tt m r^co 0 Pi 1 PC «o OOwvCr^rc- CO i^h mPi ?*? tJ- mO ih m Own pcpcpcpcpcpc pc rr-i-i PCCO pi X r~-O Pi 00 >PjvO ^1-0 0 0 « 0 F> 0 Z O ti - f> O PC m (n in m 0 a -r ~ - -r 0 h1- pj re n OOpCOOpiO pi « i c^ - T J -OOO IP C IP; IP; *C t^- r^ c ~ X o> vCt^-X g -f IT, IP, IP, IT, C CT ~ O O O — — — pi pc r^ PC Pi-to ip. pc -rO r^ t^X CO CO 00- pi n « pi PQ pc c BBSS PQ pq -t- irv r-»X O* <*3 0 0 o- o- 0- 0 ^--pc<3:< ca <pq< •tC N X 00 PC-+U-5 m< ca<cc 0 »-- X O PJ 344 SEBASTIAN ALBRECHT For each star the probable error of a single plate was found to be± km. The probable error of measurement of a single spectrumline was ± km. From this alone we should expect a smaller + 15 km. Grades 17 Fig. 2.—T Vulpeculae value for the probable error of a plate. If we remember, however,that large accidental variations in the positions of individual lineswere not uncommon (see p. 334), the value found for the probable errorof a plate is readily accounted for. Also, in such long exposures as Y OPHIUCHI AND T VULPECULAE 345 were employed on these variables, the chances become greater foran incomplete correspondence between the star- and the comparison-spectra. The upper part of Fig. 2 shows the velocity-curve computed withthe elements above, while the lower part of the figure gives the light-curves by several observers. For Pickerings light-curve the range ofvariation is smaller than for the other observers. For Wilkensphotographically determined light-curve the photographic range ofvariation was reduced to the visual range by his ratio of photographicto visual range, which for this star was The visually determinedlight-curves agree fairly well in regard to the epoch
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Keywords: ., bookcentury1800, bookdecade1890, booksubjectspectru, bookyear1895
