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1903Aj 23 . . . 22K 22 the Asteojsomic Al 22 THE ASTEOJSOMIC AL JOUENAL. Nos- 531-532 22K . Taking into account the smallness of the weights in- concerned. Through the use of these tables the positions . volved, the individual differences which make up the and motions of many stars not included in the present 23 groups in the preceding table agree^very well. catalogue can be brought into systematic harmony with it, and apparently without materially less accuracy for the in- dividual stars than could be reached by special compu- Tables of Systematic Correction for N2 and A. tations for these stars in conformity with the system of B. 1903AJ The results of the foregoing comparisons. have been This is especially true of the star-places computed by utilized to form tables of systematic corrections for ISr2, An, Dr. Auwers in the catalogues, Ai and As. As will be seen Ai and As. In right-ascension no distinction is necessary by reference to the catalogue the positions and motions of between the various catalogues published by Dr. Auwers, south polar stars taken from N2 agree better with the beginning with the Fundamental-G at alo g ; but in decli- results of this investigation than do those taken from As, nation the distinction between the northern, intermediate, which, in turn, are quoted from the Cape Catalogue for and southern catalogues must be preserved, so far as is 1890. SYSTEMATIC COBEECTIOEB : CEDEE OF DECLINATIONS. Eight-Ascensions ; Cokrections, ¿las and 100z//xtf. Declinations; Corrections, Æs and IOOzZ/x^. B — ISa B —A B —N2 B —An B —Ai âas 100 â[is âas 100 âgô âSs 100 jfs â8s lOOJu's âSs loo d S'* + 85 o!ooo + o!o68 + o!o29 + 0A49 + 90 0.00 0.00 0.00 0.00 80 -0.017 + 0.040 + 0.026 + 0.127 85 0.00 0.00 0.00 0.00 75 -0.025 + 0.004 + 0.017 + 0.092 80 0.00 0.00 + 0.07 + 0.44 70 -0.028 -0.018 + 0.007 + 0.061 75 0.00 + 0.10 + 0.14 + 0.84 + 5 -0.21 -0.99 65 -0.027 -0.031 -0.005 + 0.031 70 0.00 + 0.14 4-0.17 + 0.79 0 -0.21 -0.89 + 60 -0.028 -0.040 -0.021 -0.002 + 65 -0.04 + 0.10 + 0.18 + 0.61 - 5 -0.21 -0.92 55 -0.026 -0.047 -0.028 -0.019 60 -0.09 + 0.01 + 0.17 + 0.43 10 -0.21 -0.99 50 -0.023 -0.048 -0.029 -0.022 55 -0.14 -0.05 + 0.15 + 0.23 15 -0.16 -0.97 45 -0.019 -0.042 -0.026 -0.020 50 -0.19 -0.10 + 0.12 -0.03 20 -0.05 -0.88 40 -0.013 -0.033 -0.023 -0.016 45 -0.23 -0.16 + 0.04 -0.38 -25 + 0.17 -0.79 + 35 -0.007 -0.021 -0.020 -0.015 + 40 -0.27 -0.20 -0.09 -0.83 30 -0.005 -0.013 -0.017 -0.018 35 -0.27 -0.20 -0.19 -1.12 25 -0.004 -0.006 -0.014 -0.022 30 -0.25 -0.17 -0.22 -1.20 20 -0.003 -0.003 -0.010 -0.022 25 -0.23 -0.16 -0.24 -1.22 15 -0.002 0.000 -0.005 -0.018 20 -0.23 -0.18 -0.24 -1.24 + 10 -0.002 0.000 0.000 -0.009 + 15 -0.25 -0.20 -0.21 -1.23 + 5 -0.002 0.000 + 0.005 + 0.004 10 -0.28 -0.22 -0.17 -1.13 0 -0.002 -0.001 + 0.009 + 0.016 + 5 -0.31 -0.23 -0.13 -0.99 — 5 -0.002 0.000 + 0.010 + 0.023 0 -0.33 -0.24 -0.07 -0.89 10 0.00Q + 0.005 + 0.009 + 0.025 - ,5 -0.34 -0.23 + 0.01 -0.92 + 0.010 + 0.028 -10 -0.34 -0.20 + 0.11 -0.99 -15 + 0.005 + 0.014 B —A 20 + 0.013 + 0.031 + 0.013 + 0.036 15 -0.33 -0.16 + 0.26 -0.97 // s 25 + 0.020 + 0.044 + 0.021 + 0.054 20 -0.28 -0.09 + 0.43 -0.88 -20 -0.22 -0.73 30 + 0.025 + 0.054 + 0.031 + 0.077 25 -0.19 + 0.06 + 0.61 -0.79 25 -0.20 —0.55 35 + 0.032 + 0.063 + 0.037 + 0.090 30 -0.12 + 0.10 + 0.83 -0.71 30 -0.15 -0.35 -40 + 0.040 + 0.070 + 0.042 + 0.097 -35 -0.06 + 0.16 35 -0.08 -0.15 45 + 0.045 + 0.076 + 0.043 + 0.096 40 0.00 + 0.36 40 -0.03 0.00 50 + 0.045 + 0.081 + 0.038 + 0.084 45 + 0.03 + 0.55 45 + 0.03 + 0.17 55 + 0.037 + 0.087 + 0.026 + 0.071 50 + 0.04 + 0.63 50 + 0.05 + 0.27 60 + 0.019 + 0.094 + 0.016 + 0.068 55 + 0.03 + 0.71 55 + 0.10 + 0.43 — 65 + 0.009 + 0.097 + 0.011 + 0.080 -60 + 0.10 + 0.93 60 + 0.20 + 0.71 70 + 0.016 + 0.096 + 0.012 + 0.093 65 + 0.15 + 0.97 65 + 0.33 + 0.91 75 + 0.035 + 0.092 + 0.012 + 0.100 70 + 0.13 + 0.67 70 + 0.40 + 0.83 80 + 0.032 + 0.069 + 0.006 + 0.086 75 + 0.06 + 0.18 75 + 0.40 + 0.53 -85 0.000 0.000 -0.034 -0.034 80 0.00 0.00 80 + 0.29 + 0.22 -85 0.00 0.00 85 + 0.10 -0.08 -90 0.00 0.00 -90 0.00 -0.30 © American Astronomical Society • Provided by the NASA Astrophysics Data System 531-532 THE ASTRONOMICAL JOURNAL. 23 CM ^ SYSTEMATIC CORRECTIONS ORDER OE R. A. past epochs can only be improved through a new reduction Nj Kiglit-Ascension Declination of the older catalogues. It would therefore seem to be the : b — n2 b — a B — R2 B —A Ada lOOJ/Za Ada A [la al too J/+ al ioo¿y* part of wisdom fco select, for the increase of our list of // // // a Oh-!o02 -!o0o +S.027 -K098 + .02 +.04 +.08 +.10 standards, those stars which have been well observed in 1 —.003 -.007 4-.026 +.095 + .03 +.05 +.06 +.09 the first sixty years of the nineteenth century, irrespective 2 -.004 -.009 +.025 +.092 + .03 +.05 +.04 +.08 of the attention which they have received since that time. 1903AJ. 3 —.004 -.011 +.024 +.088 + .03 +.06 +.02 +.06 The force of this is all the greater on account of the 4 -.004 -.011 +.023 +.084 + .03 +.05 .00 +.04 5 -.004 -.011 +.022 +.081 + .03 +.05 -.02 +.02 prevalent idea in regard to the supposed advantages, more 6 -.004 —.010 +.022 +.078 + .02 +.04 -.04 -.01 imaginary than real, in adherence for a long term of years 7 -.003 -.008 +.022 +.076 + .02 +.03 -.06 -.04 to the use of some one standard catalogue. If our standard 8 -.002 -.006 +.022 +.074 + .01 +.01 -.07 -.06 catalogues were to be revised as often as they should be, 9 —.001 -.004 +.023 +.074 .00 .00 -.08 -.08 the necessity for high weight as to the adopted proper 10 .000 -.001 +.024 +.074 — .01 -.01 -.09 -.09 11 +.001 +.002 +.026 +.076 -.02 -.03 -.08 -.10 motions, though still important, would not be of such vital 12 +.002 --.005 +.027 +.078 -.02 -.04 -.08 -.10 consequence. 13 +.003 +.007 +.028 +.081 — .03 -.05 -.06 -.09 The names of several well known stars will be missed 14 +.004 -Í-.009 +.029 +.084 -.03 -.05 -.04 -.08 from the present collection. Nearly all of these are open 15 +.004 +.011 +.030 +.088 -.03 -.06 -.02 -.06 to proof, or at least to well grounded suspicion, of periodic 16 +.004 +.011 +.031 +.092 — .03 -.05 .00 -.04 17 +.004 i-.Oll +.032 +.095 -.03 -.05 +.02 -.02 variation in proper motion. The duplicity of some of these 18 +.004 -^-.010 +.032 +.098 — .02 -.04 +.04 +.01 stars also constitutes an objection to their use as standard 19 +.003 +.008 +.032 +.100 — .02 -.03 +.06 +.04 stars. Among them are : ^ Cassiopeae, a Can. Majoris, 20 +.002 +.006 +.032 +.102 -.01 -.01 +.07 +.06 a Geininorunij a Can.min.¿ y Virginia, £ Bootis, £ 11 er culis, 21 +.001 +.004 +.031 +.102 .00 .00 +.08 +.08 61 Cygni, a Crncis, and a Centauri. It is scarcely neces- 22 .000 +.001 +.030 +.102 + .01 +.01 +.09 +.09 23 -.001 -.002 +.028 +.100 + .02 +.03 +.08 +.10 sary to urge that these stars should still be included in 24 -.002 -.005 +.027 +.098 + .02 +.04 +.08 +.10 observing lists where absolute determinations are intended, Notes Relating- to the Catalogue. and also in those wherein differential determinations for The subjoined catalogue of 627 stars is divided into three the bright stars is the object in view. sections, the limits of which are indicated in the respective From —20° to —40° of declination there is a rapid fall- captions. The selection of these stars was made with the ing off in the precision with which the places of the princi- idea that these would be best adapted to serve as a con- pal stars are known ; so that the mean weiglit of g and /+ necting link between the various catalogues of observation.
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