ASTRON 0 MIS CHE N ACHRI CHTEN.

Gill 383 distances ; 65 position angles > Finlay 270 B 35 *

-Yacocly 128 B

\ Ambronn 106 >

Yale Chase 309 B

Gottingen \ SC/ZUY I27 B

Band 130.

166 distances ; 36 position angles I 1 2 ‘5 .v D

5 2 2

124 3

57 > 33

B

N2 3107-08.

four pointings, - two in each of the opposite positions If the segments.

A few position angles measured at Yale and Gottingen were not employed as they were not sufficiently numerous to be completely discussed.

The meridian observations, together with a large num- ber of additional observations, made to secure uniformity in the determinations of the positions, have been completely discussed by Professor A. A~wers, and the results of his discussion, communicated in October I 89 I, have been taken

mary of the results of combining the Meridian and Helio-

doing. The general plan of the Triangulation will be ob- vious by looking on the list of the 37 stars, Table I, and

paper.

as the basis Of this work. The following iS a brief Sum-

meter observations, and Of the methods in so

the measures of distances, Table 11, at the end of this Measures of distance have been chiefly employed.

To give rigidity to the figure as a whole two auxiliary stars E = BD. -605201 and F = BD. -6?5294

All the distances measured by each Heliometer ob-

were intro- duced. These stars were not observed at the 2 2 observa- tories.

11-12.

scale value for each instrument, and corrected for refraction, aberration and proper motion to the Equinox 1889.0 and Epoch 1889.55.

A complete set of observations on any night should, according to the programme of work, contain three mea- sures of the Standard distance (the distance between the stars t-p) one at the beginning, one in the middle, and one at the end of the set.

If Z0 is the adopted value of the standard distance Z1 S2 and & the three observed values

and and distances in the triangulation observed simultaneously with

of 61

2a and respectively; then if & Xa and Z3 are observed without error the true values

and will be

0, + !% ( 2 0 - 2,)

0 3 + 3 ( 2 0 - 4)

2 6

4 2 0

2 0

62 + - ( 2 0 - 23)

On the definitive places of the Stars used for comparison with the Planet Victoria in the observations for parallax 1889.

By David GiZZ, LL. D., F. R. S., H. M. Astronomer at the Cape.

The relative positions of the comparison stars em- ployed in the observations of Victoria in 1889, are ndw, thanks to the generous and hearty cooperation of a large number of Astronomers, more accurately known than those of any other group of stars in the heavens, and may there- fore be advantageously used for determining the optical dis- tortion and scale-value of our photographic telescopes, and testing the various methods for the Braccordement des plaques q .

The following resume of results is therefore communi- cated in advance of the full details (which will afterwards appear in a complete form in connection with. the deter- mination of the Solar Parallax) in order that advantage may be taken of the opportunity of making the necessary

photographs during the current year, and of utilizing them without delay.

The definitive positions of the 37 stars are based on the following data :

3 7 66 Meridian observations of Right Ascension 3771 > > of Declination

made at the following observatories : Algiers, Berlin, Bordeaux, Cape of Good Hope, Cam-

bridge (Engl.), Cambridge (Mass.), Cincinnati, Cordoba, Dublin, Greenwich, Hamburgh, Mt. Hamilton, Konigsberg, Leiden, Leipzig, Melbourne, Naples, Oxford (Radcl. Obs.), Paris, Pulkowa, Vienna (Kuffner’s Obs.), Washington ;

also upon the following Heliometer observations :

subject only to the accidental errors of measurement, and a final systematic correction on account of possible error in the adopted value of X0.

But q 4 and G~ cannot be strictly simultaneously observed with 2, z9 and and it becomes a Dractical

than on real changes of scale-value, then method I would be best, but if they depend chiefly on true variations of scale value then method I1 should be adopted. The obser- vations were reduced independently by both methods, and in some cases method I seemed the better, in others method

The different observers' measures were compared with distance depends more on accidental errors of pointing GiZZ's, each pair of stars affording an equation of the form i If the variation of the measures of the standard

& I

question I* whether the mean Of the three (20-21)'

11. whether their values should be interpolated by means

the ordinate and abscissa are the sidereal time and the corresponding value of (2, - 2).

(E,, - &) and (Z0 - 2;) should be adopted, or

of a curve drawn through points On a diagram Of which

+ (" - 400<)y + (6 - 4000" - ) ' a = G - 0 with the weight Pg ~ * P o Pg +Po 1000 1000

11, but for all the observers the probable errors were on the whole nearly identical for both methods, and the mean of the two better than either. Accordingly the mean was adopted.

The next step was to ascertain whether, in spite of

outstanding systematic differences between the various ob- servers.

this correction to a common value, there remained

where G is the distance according to Gild, 0 according to another observer, Pg and Po the weights of Gill's and the other observer's measures, depending on the number of observations.

The resulting corrections to Gill were:

Distance 1000"

3000 4000 5000

6000 7000

2000

FinZay +!o3'

.oo

.02 - - ,04 ' - .06 - .o 7 - -.08

Yacoby +!23

+.I2

+.03 - .06 -.I3 -.I8 -.23

Chase +!13 t.07 +.02

-.03 -.07

. 10'

.I2

- -

Sckur +!I2 2

+.13 +.os

--.04' -.06* - .06

.OI -

Ambronn +!lo6

- .06 .o I -

. I 0

.12'

- - -.I4 - . r 4

These corrections having been applied and the means taken having regard to a preliminary system of weights found for the observations of different distances by different observers, and Tabular distances having been computed with their weights from the data of Azwers' discussion of the meridian observations, the observed and computed distances were compared by equations of the form

' 2 6 - 4000" d - 4000" s inp (ma - ml) u + s inp (mZ2 - mla) w - x - )y-(-=) 2 = 0.-c.

where ml is the magnitude of the brighter star (reckoned from K O ) , ma of the fainter star of the pair, p the position angle reckoned from the brighter star as origin, u , w , x , y , a constants to be determined. Each equation received a

. The resulting corrections were: weight = ~

$0 x Pc %+PC C o r r e c t i o n s t o t h e M e r i d i a n K A . (arc) Correc t ion t o t h e H e l i o m e t e r D i s t a n c e s

omitting w with w Stars mag. 5.7 -!'083 -!098 Distances I 000" +!lo 2 9

6.0 -.072 -.080 2000 t.019 1.0 -.036 -.031 3000 t.009 8.0 .ooo .ooo 4000 .ooo

The term w was found to be -Yo085 with mean error f.'o157. The results of a solution without w were therefore adopted.

5000 -.009 6000 -.or8 7000 -.024

These Heliometer corrections are applicable to Gill's observations, and have to be further added to the reductions to Gill for the other observers. This done the mean error of each observer's work was derived, not from his own observations in te r s e but from the agreement of the observations for the same distance by the different observers, and the following Table of weights was derived, in which an estimated m e a n e r r o r of f o l 2 corresponds with weight unity.

3 107

Its 'romthe der. obs.

only

4.5 3 3 3.1 4.8 4.9 4.8 4.1 3.3 3.8 4.0 3.1

3.8 3.1 7.0 5.8 4.0

7.0

4.7

3.7

166

AB

-__ - 7 0 2 0

i--o77 +.035 -.023 -.020

+.or1

+.033' +.oo4* +.029 -.038*

-.or6 -.076 +.032' +.080 -.047

--.029

+.047

-*044

+,045

W e i g h t of a s ingle n o r m a l o b s e r v a t i o n b y e a c h o b s e r v e r . Distance GiZZ FinZay 'jfacoby Chse Scbur Ambrortn

I o 00" 3.0 2 2.70 0.1 5 0.60 1.50 1.09 3000 1.42 1 .27 0.40 0.50 0.69 0.56

7000 0.67 0.52 0.14 0.30 0.27 0.25 5 000 0.89 0.78 0 . 2 0 0.39 0.3 5 0.35,

ts 'rom the ler. obs.

only

3.7 4.5 5.6 5.3 4.9 4.5 3.1 3.3 4.2 4.3 3.9 3.6 3.9 4.1 3.3 3.1 3.0 6.0

The observations were then combined with the above weights, and these weights then received small corrections corresponding to the uncertainty of the correction for proper motion to 1889.55.

Adopting these combined weights as true, it , was found from the discordances between the observed and computed distances that Auwers' original weights for the Meridian Right Ascensions should be multiplied by 0 .7 I and those of the Declinations by 1.33.

x = Aa cos d y = Ad

Now putting

each of the 37 observed Right Ascensions gives an equation of the form

x = Correction for magnitude, each of the 37 Declinations observed in the Meridian gives an equation of the form

y = o and these equations have the weights assigned by Auwers [after reduction to our system of weights) multiplied by the

AB

+YO45 - .025 -.o13. -.o14 + . O I I

+.006 -.032 -.088 -.030 t . 0 2 2 .

+.or2 -.086 +.027 t . 0 9 2 t.010 -.068 +.or3 + .020

There were observed in all 173 distances with the Heliometers - each of which gives an equation of the form

I s i n p x 1 + C O S P Y l \ = 0. - c. - sinp x2 - cospy2 J

where x1 ") refer to the two stars of the pair, and 25

pairs measured in position angle, each of which, when the residuals are reduced to seconds of arc on the great circle, gives an equation of the form

I - c o s p x 2 + sinpya J = O* - c. From these 2 7 2 equations normal equations were formed

having regard to the weights of the equations, the total num- ber of these normals being 78 (viz. x a n d y for each of the 37 comparison stars and the two auxiliary stars). These 78 unknowns were eliminated with their weights, the results will be found in the following Table.") The additional weights given in the Table are the weights of the meridian obser-

Yl Y2

c o s p x, - sinpy, \

2 R Z

n

p q Y

t

M?

above mentioned factors. I vations employed in the solution.

Def in i t ive c o r r e c t i o n s f r o m t h e c o m p l e t e d i s c u s s i o n t o t h e meridi .an o b s e r v a t i o n s a s r e p r e s e n t e d b y Auwers' d i s c u s s i o n of t h e m alone.

+ . O I I

+ . 0 2 2 - .198 - .053 - .136

0 - .I14 - . 027

+ .050 + .129

s - .030 -0.013

Wei irom Hel. : Mer. obs :ombined

17.0 I 1.8 I 9.0 2 2.4 30.0 38.6 25.0

I 8.8 30.2

6. I 5 1.8 23.1 20.5

50.5 45.8 16.8 25.3 45.5

22.1

Wei 'rom Hel. : Mer. obs :ombined

17.6 21.3

30.8 26.8. 29.4' 2 2.4 19.6 19.2 27.2

16.5 33.1 2 1.4 17.7 34.1 26.2 2 6.8 28.3 3 5-3

22.2

I t s +om the fier. obs.

only

11.0

10.8 10.4 1 2 . 2

1 2 . 2

I 1.6 I 0.6 8. I 9.7

10.8 8.2

I 2.4 10.3 8.9

16.6 14.6

9.3 17.2

10.0

- * -

U V Ee X

Y

a B Y 6

5 e

2

&

17

L X R P

Au.cos b

-0!'025

+- .078 + *039 - .138 + .048 + .081 - .006 + .lo8 - -057 - .046 + . 0 2 0

- .042 - .067 + .119 + .07I + .116 -0.073

. I 1 I -

Wei, +om Hel. ! Mer. obs. combined

30. I 36.0 34.1 30.8 23.8 2 3.9 '9.9 14.7 I 8.2 18.9.

I 2.9 I 3:1 I 8.8

5.7 I 2.5 16.4

--

21.2

1 2 . 0

An estimated mean error of +0!'20 Eorresponds with weight unity.

Wei, +om Hel. L Mer. obs. combined

17.5 18.3 23.7 25.3 22.4 25.0 18.3 13.8 15.5 22.5

25.0

1 7 . 2 2 1.3 10.3 19.1 20.4 21.7

_-

17.9

ts 7rom the ler. obs.

only

9.6 10.8 13.8 I 3.8 12.5 11.7 8.4 7.8

I 0.9 10.8

9.6 9.0 9.4

10.1

8.5 8.2 6.2

I 5.2

*) The elimination of the unhowns and their weights was effected by a series of approximations of which an account mill be after- wards given.

I I"

3 107 I 68 * 67 When the values of x and y for the different stars

are substituted in the corresponding equations of condition, the residuals given in Table 11 at the end of this paper are found (in the column marked ,Mean<).

The other columns represent the comparison of the definitive computed distance with the distaace as observed by each observer and corrected for systematic error.

The corresponding weight is given beside each value of c. - 0.

From the residuals of the 2 7 2 equations we get

To the 78 unknown quantities eliminated from the normals must be added the terms u , x , r and z expressing the corrections of the Meridian observations in Right Ascen- sion on account of magnitude, and the corrections of the Heliometer distances for systematic error, which, strictly speaking, should have entered into the simultaneous solution, but which were more conveniently, and without sensible error, eliminated before and gave the results tabulated p. 163, 164.

The total number of unknown quantities is therefore - rn = 8 2 .

Whence

[pvv] = 8 . 3 8 2 5 .

- [Pvv] = 0.0441 = Ea n - m and E = +0:'210

the assumed value was + 0 . 2 0 0 .

The accordance between the estimated and actual errors is not so precise for the various classes of obser- vations. If each class had proper weight one should have

n - wz - 190

n1 n 212 [ P 4 = $2.X - 0 . 0 4 X - = 0.0279

where nl is the number of observations belonging to each special class.

Instead we find: [p.v] Corresp. mean ?Zl *, error for weight I

Heliometer Distances I 7 3 .0329 f l 2 1 6 2 Pos. Angles 2 5 .0415 f . 2 4 2

Meridian Right Ascensions 37 .0253*) f .189 2 Declinations 37 .0193 f . 1 6 6

The overestimate of the weight of the position angles is probably due to an increase of small systematic errors in particular pairs consequent upon the unfavourable charac- ter of Heliometer images for measures in position angle. The underestimate of the weights of the meridian obser- vations is traced to the neglect of small systematic errors in the Heliometer observations of distance (peculiar to dif- ferent pairs of stars) which are not eliminated in the mean. Auwers' weights of the Right Ascensions should have been diminished instead of 3 0 0 / ~ , and the weights of the Declinations increased 7 0 0 / ~ instead of 3o0IO. It is shown that a new discussion with rigorous weights would not sen- sibly affect the results. The solution as it stands is accepted.

The mean error of an observation of weight unity is found to be in the mean

for Distances 600" to 3000" f Y 2 0 7 3000 P 5000 f . 1 9 5 5000 s 7300 f . 2 2 6

For the various observers:

Distance GiL? FinZay Yacoby Chase Schur Ambronn 600" to 3000" f:'223 (32) +!'244 (32) f!'209 ( 2 5 ) f!'217 (31) +!'234 (15) +!'211 ( 1 8 )

3000 B 5000 .221 (65) *239 (64) -194 (42) * 2 1 9 (64) * 198 (39) . ~ I I (31) 5000 B 7300 a213 (74) -214 ( 7 5 ) -204 (47) -236 (67) -236 (29) - 2 1 7 (46)

Accepting these results as representing sufficiently the weights assigned to the different distances, the combined residuals of each observer give

Weight df Factor [p- Factor

Y l l

Gill .0361 - 7 7 356 FinZay -0405 - 6 9 230 y'acoby .0286 *98 36 Chase - 0 3 92 - 7 1 I 2 2

Schur .0361 - 7 7 67 Ambronn .0338 3 3 43

The factors are the quantities by which must

be multiplied to give 0.0279 - or in other words the factors by which the weights of the table pag. 165 have to

n1

be multiplied. The weights of the factors are the sums of the weights which have been' assigned to each observer. Having regard to these weights the resulting mean factor is

0.76

The corresponding factor from the combined observations of distance is

Thus whilst the measures of the individual observers are affected by systematic errors which diminish their weight 24OIO on the average, the weight of the mean of the ob- servers is affected by only 1 5 0 / ~ - a proof that the per- sonal errors are to a sensible extent eliminated in the mean of several observers.

The corresponding p r o b a b l e e r r o r s are given in the following table.

0.85.

P r o b a b l e e r r o r of a s ing le n o r m a l o b s e r v a t i o n . Distance Gih? FinZay yacoby Chase Schur Ambronn 1000" - + Yo88 f!'099 * ? I 5 7 - + Y206 - + l 1 2 5 - +!141

5000 .162 . I 83 .302 - 2 5 5 .260 .250 3000 . 1 2 8 .I44 .216 .225 . 1 8 4 *I97

7000 . I87 . 2 2 5 -369 .294 a294 .294

*) If the magnitude corrections are omitted for the Right Ascension becomes 0.0287. m

These probable errors include the effect of errors in the measurement of the Standard stars (producing errors of scale-value) and all outstanding systematic errors personal and instrumental.

- *

~

a b

d e

g k i K I

n

P P

c

f

m

0

Y s t U V

W

Distance C. - 0. Weight

1500 n 2500 - .o14 104.8 2500 s 3500 - .005 131.2

600" to I 500" -01008 52.7

3500 4500 + . O I 2 142.2 The mean residuals in distance are represented in - .o I 5 111.8

groups as follows:

If no systematic corrections had been applied to the original observations of the different observers their ob- servations would be represented thus :

c. - 0. Distance

6oo"to 1500" 1500 s 2500

2 5 0 0 n 3500 3500 $ 4500 4500 * 5500 5500 n 6500 6500 s 7300

P +lo3 26.1 +.or 58.5 +.or 62.7 +.or 68.5 -.06 52.8 -.04 51.6

.oo 35.9

Filt Cay P

+!lo7 21.5 .oo 36.6

-.04 39.8 .oo 48.2

-.13 31.8 - -05 34.5

-.I2 17.5

Yacoby P

+!'I8 4.3 t . 1 3 6.8 t . 1 3 8.0

.oo 7.2

-.21 3.0 - . I S 4.8

- . I 2 ' 2.1

These results depend on no assumed law, but represent the quantities required to reduce the u n c o r r e c t e d original observations of each group to zero. They prove conclu- sively the necessity for systematic corrections very similar with those which have been actually employed.

The residuals of Table I1 for the individual observers

Chase P

+!'.14 6.5 +.08 14.6 +.08 24.0 -.OI 25.8

.I0 22.1 - - .I8 19.1 -.08 12.2

SChUY P

t l 2 o 7.8 t . 0 3 11.3 t . 0 9 20.0

-.08 13.6 -.01 4.3 -.I2 5-9 -.07 4.2

stances possibly arise from a peculiarity in the images (a difference of colour) of the Standard stars, which appears to produce a small personality in their observation by dif- ferent observers. For the positive corrections for short distances no satisfactory explanation can presently be given. A closer examination of these points must be reserved for

refer to the c o r r e c t e d observations. the more detailed publication. The negative corrections required for the large di-

Table 'I. Def in i t ive p l a c e s of the Vic tor ia C o m p a r i s o n Stars .

Equinox 1889.0. Epoch 1889.55. -- Mag.

7.8

8.5 8.4 8.3 7-5 8.5 7-8 7.7 7.9 8.0 5.7 6.6 7.6 7.6 8.4 7.9 1.9 7.9 8.0 6.7 8.2

8.2

a

~9~ 2 im251200

23 2.485 24 6.225 25 17.932 25 40.295 2 7 50.504 28 37.608 29 2 0 . 7 2 7

30 41.136 30 53.379- 31 22.109 31 53.995 34 26.876 34 53.498 35 56.005 39 23.665 40 59498 41 53.285 43 4.463 43 43.816 44 56.178

r9 47 27.184

6

-5" 57' 20186 6 24 0.52 5 9 5.82 5 54 12.54 5 2 1 2.34 4 58 48.96 4 41 23.26 4 33 5-37 5 1 2.44 4 32 43.39 3 43 18.95 4 53 40.08 5 42 7.34 4 1 7 21.16 4 32 49.33 4 41 22.28 3 56 0.58 5 30 22.53' 4 46 18.32 4 48 25.24' 4 58 27-07.

-4 5' 32.35

Prec

1850 1900

5?2046 ,2029 .2142 .2123 -1864 .1846 , 2 0 2 7 .zoo9 .1905 .1887 .I820 .I801 *I755 *I737 .1724 .1705 .1823 .1804 . I 7 2 0 .I701 .1540 .1523 -1794 *I775 I964 . I944

.1658 .1639

.1712 .1692 *I758 -1737 . I 5 7 2 .I552 .1go6 .1884 *I747 . I 7 2 5 *I753 *I731 .1786 .1764 1.1757 *I734

Ambronn

+:I14 4.0 t . 0 2 10.4 -.I1 4.9 - . I I 6.5 - . I S 8.1 -.22 5.6 -.21 3.6

P

+6l805 +7!'023 6.938 7.156 7 .027 7.242 7-124 7.340 7 . 1 5 5 7.370 1.332 7.546 7.396 7.610

7.563 7.776 7.580 7.792

7.455 7-668

7.620 7.831 7.662 7.874 7.866 8.079 7.904 8.114 7.987 8.197

8.392 8.599 8.264 8.472

8.461 8.670 8.556 8.763 8.608 8.815 8.703 8.909

f8.901 t 9 . 1 0 6

Pa Pa

--Zoo06 -!'OIO

-.0012 t . 0 0 3 -.0036 +.016 -.0004 -.o08 -.0038 -.062 -.0012 t.004 +.ooro t . 0 1 5 -.0005 -.013 -.003) +(.oI) t . 0 0 2 4 -.024

+.0056 -.045 -.0007 .ooo +.0012 f.014 -.0014 +.004 -.OOIO +.oo'l +.OOOI .ooo -.OOII +.or4 - . O O O ~ -.or6 -.0025 -.004 - .0002 --.004 -.0032 +.015

-.OOI) -(.02)

Probable Errors a(arc) 8 p(arc)

- +!o32 f!032 .039 .029

.028 .024

.025 -026

. 0 2 2 .025

.027 ,028

.029 .030

.o31 .031

.024 .026 -055 -033 .or9 .023 .028 .026 .030 .032 .o19 .023 .o20 .026 .033 .026 .027 .025 .o20 .023 .025 .032 .02z .032

f .023 f . 0 2 7

.03I .028

- +lo13 .o I 5 . 0 2 2

.020

.o I8

.024

*049

.040

.oo 7

.o I I

.OI I

.020

.OI I

. 0 2 2

.OI I

.o I I

.o I I

.o I 3

.o I 3

.009 - +.022

.o I I

3 '07 1 7 2

x I 8.1 y 8.1

a 8.0 x 8.5

19h48d222375 5 1 25.861 52 3.490 52 18.113

lu, 8 Precession I I850 I900 I I 8 5 0 I900

$1855 .1831

.is77 .1852

.2121 .2094

.1690 .1666

. 2 i 1 ~ .2090

. 1828 .1803

. 'I52 . 1 7 2 7

.1702 .1676

.2415 .2444

. 2 2 3 0 . 2 2 0 0

13.2596 .2562

. I774 . I 7 5 0

. I703 .I679

.2388 .2358

1 .215I .2122

-5" 19'59:'89

5 28 58.91 4 58 53.86

6 38 55.75 4 39 16.34 4 36 52.23

5 1 7 48.65 6 40 49.00

8 o 14.38 4 56 27.93 6 53 57.31 4 4 4 4.02 8 29 59.20 7 20 32.96

-9 10 12.56

+ 8!973 + 91'178 +Zoo33 +!'OII 9.212 9.415 +.002I -.045 9.260 9.463 (-.OOI) (+.I) 9.278 9.483 -.0036 --.OOI

9.485 9.686 -.0003 -.023

9.537 9.741 - . 0 0 2 2 + . 0 2 1

9.587 9.788 +.OOII -.025

9.670 9 . 8 7 0 ~ -.0041 + . 0 1 7

9.929 10.127 +.oo21 -.006 9.949 10.151 +.0014 - . 0 2 2

10.079 10.279 -.oor7 - - . 0 2 0

+10.257 +10.458 1 +.OOOI .ooo

9.305 9.508 -.OOZ9 +.035

9.645 9.849 ~ .OOOO -.lo

9.823 10.0251 -.OOZI -.053

E

5 9 d L

Iz P

x

Probable Errors u(arc) 8 p(arc)

6.6 56 17.659 8.0 51 4.779 8.1 5 7 21.729 8.4 19 59 23.785 7.0 1 2 0 o 44.858

8.1 I 2 45.811 7.5 I I 3.695

6.5 1 2 0 5 8.919

- +:'024 f!'o27 +!016 .028 .028 ,013 '.028 .027 .038 -030 .032 . O I I

-035 .036 .or3 .032 .034 .009 .o31 .028 . o i l .029 - 0 2 7 .or3 .038 .032 .033 .037 .032 . O I I

.031 .029 .007

.056 .042 .OII

.038 .031 . O I 1

.033 .030 . O I ~

f .039 f . 0 2 9 k.007

zi 1.86 1.44 0.89 1.55 2.88

3.01 2.44

1.80 1.38 1.32

2.48

4.86 2.32 1.58 1.67

5.42

2.79

1.54

3.96

1.20

2.00

1.42 2.29

1.41

1.24

The Precessions and Proper motions of the above Table were communicated by Dr. Auwers. The probable errors of the proper motions are so comparatively large that it is desirable to obtain the photographs for determining scale value, distortion (ec. as soon as possible.

The approximate places of the two auxiliary stars used in the Triangulation are, for Eq. 1889.0: E 870 1 9 ~ 3om30fo -6" 12' 55" F 873 1 9 ~ 4 7 ~ 2 6 f 4 -6" 1 7 ' 24".

Table 11.

C o m p a r i s o n of t h e H e l i o m e t e r o b s e r v a t i o n s o f D i s t a n c e with t h e D i s t a n c e s c o m p u t e d f rom t h e D e f i n i t i v e C o o r d i n a t e s .

___ -

-:22

+.oo' - . I 3 +.12

+ . I 5 -.04

+.XI +.OI

-.02

+ .22

+ . X I

+.24

-.21

+ .20

t . 0 3 -.09

-.23 -.29 +.07 -.27

-.37

- .OO'

-.O4'

+.I4

--.IO

- .22

- Ko-

.ation No.

f n I

2

3 4 5 6 7 8 9

I 0 1 1

I 2

' 3 I 4 '5 16 1 7 18 '9 2 0 2 1

2 2

23 24 25 26

1 64641'881

c. - 0.

1.48 2.26 1.62

3.89 1.08 0.77 0.95 1.73 2.64 4.34

- -

-.24* -- - - - - --

, -

I! I ,

2.14 2.34 1.53 0.99 1.16 1.27 2.02

1.27 1.15

I - I - - - -

-.37 -.40 -.I9

1 -.45

-~

+!'3 I

+.23' + * 3 2 +.OI

-.05 -.I4'

f . 3 2

.oo -.OI

+.oo. +.08

+.05 -.OI

-.06 -.23 +.02

+*04 - .og -.22

+.03 f.08 -.05 -.06 +.02

+.o I

+.I2

da d E

t F $ 7 6 %

I x m k mn

t Y

2.8

a x Z E X S

X E

ki

5327.079

I 4188.115

6721.389 7280.782 5950.193

4433.861 1549.3'7 3696.760

1 3471.413

3549.61'

3404.129

3345.678 3854.403 5843.512 7099.830 2995.443 1708.871

+Yo9 t . 6 9 . +.09 -.36 +.25 -.06 -.07'

-.08 - .I8 +.20.

+.or -.42 - - -

-.29 -.03 +-37 +.02

-.14 - . 2 7

+a09 -

+.OI

t.05 -a43

0.96 +Yo4 0.48 - 0.64 f . 2 7

0.39 0.88 t . 1 7

-

1.92 1 -.07

1.41 + . I I

0.64 -

1.20 -

- t . 2 5 - -.69 - -.03

0.84 - . z 5 1.14 - .07 0.92 -.28 0.96 t . 3 9

0.50 0.56 ~ - - 0.50 1 - 0.48 1 -

0.29 -

0.29 -.43 - -.04

0.94

2.44 ~

- -

- 1.28 1 -

- - j -.I1 1.20 1 - -

~ t . 2 9 .

- +.25 1.18 -

0.52 - 0.60 - 1.22 0.45 I

1 ~

- -

2.46 1 - 1.12

1.24 - -

-- .05

- 1 +.53

__

-

-

0.27

0-35 - -

- 0.32

0.37

0.26

-

-

- - - - - - - -

0 . 3 ~ 0 . 5 ~ 0.56 0.88 0.56 0.50

Mean

+y035 f . 2 2 2

+.090 -.018 +.236 -.018 --.I35 +.006 -.052 f .039 +.026 +.005

+.110 -.118 -.036 --.068 --075 +.038 +*03 5 -.053

-.089 -.100

- . I 78 - - .022

-.I I 2 -.r06

-

5.8 3 . 1

3.6 I .9'

3.9 7.4 7.5 5.4 6.3 5.4 7.4 3.3 2.5' 3.0 5.' 6.8 9.8 6.1,

3.8 3.5 2.9'

3.4 2.8

3.2 3.6 3.4

* 73

'

3 107

R0- tation

No.

28 29 30 3 ' 32 33 34 35 36 37 38 39 40 4 1 4 2

43 44 45 46 47 48 49 5 0 5 ' 5 2

53 5 4 55 56 5 7 58 59 60 61 62 63 64 65 66 67 68 69 7 0 7 ' 7 2 73 74 7 5 76 7 7 78 79 80 81 82 83

1. 74

Definitive Distance

4930'(463 2 734.1 7 7 6401.850 6479.911 3970.402 4383.267 2095.474 6706.1 87 3986.304 5 7 15.462 4535.736

5623.594 6687.227 2087.464 2458.1 59 4 104.430 2 294.5 5 5 4'76.213 5101.719 2063.291 4594.263 2 159.5 70 25 53.233 6740.367 3224.962 4525.105 3413.786 3398.7 18 4651.565 4386.949

6701.289 5 505.42 7

6940.902 2697.65 I 1821.767 2850.02 I 3429.02 5 4 4 8 2.34 2 69 14.024 5601.102 3457.027 1175.229 4362.95 I

4699.460 5898.7 73 1896.207 5245.191 1385.581 6052.330 I 596.850

3006.023 4476.612 4014.870 6364.028

4202.502

6443.400

GiZZ ___

- :'02 -.05

-.06 -.07

t . 0 3 +.03 t . 0 3 t . 0 5 -.13

-.03 -.16 -.19 -.I8 +.02

t. 19 +.16 - - 4 4 +.oo* -.07

t . 2 7

+.I 3' -.27

+.or -.23 +:05 t . 0 9 t.04' t . 0 6 +.2 I

- .27

-.04 +.05 - .05 --.16. +.02

+.O I

+.I0 - .08 -.08 -.03 -.16 t.05 --.08 -.I8 +.19 - -03 t . 2 8 -.32

-.29 +.04 - .04

+.04

.2 0' -

+ - I 7

+.05

- . 0 2

__

1.3t I . I (

I .41 3 . 2 ~ 4.8L 0.5'

I .9f 1.32 2.14

3.6t 3.95 2.55 I .6E I .24 I .oq

I .95 1 . 7 ~ 1.19 2 . 7 ~

2.06

4.95 I .92 5.73 I .64 2.07

5.2e

o.gE 3,72 3.72 I .44

2.03

1.57 3.26 3.75 2.48 I .g8 2.70

4.15 1.23

3.54 5.50

3.09 I .go 1.58 t.22

2.59 1.14 2.39 1.08 a.84 3.49 r.34 3.90

1.11

I .oc

3.22

Fin Cay

-Yo5 t . 0 3 t.04 +. 16 t . 0 5

. I0 - t . 0 7

- .07 -.06 t . 0 6 - 4 7 -047 -.09 -.31

t . 2 2

t . 2 0 '

+ .OI

-.08 -.26

-.02

.2 I -

. I0 -

- .OI

+* I9 +.og -.04 -.31 -.27' -.09 +.03 +.22.

-.65 +.08 - .07

+.26 t . 0 9 '

+.OI -.03

f . 0 9 f . 1 9 -.06 -.16 t . 1 5

f . 0 9

.2 I -

-

. 2 0 -

f . 0 4

-.02

-.02

-.06 -*33 f . 1 7 -.25

f.33 --.OI

__

0.79 0.35 1.16 1.14 2.94 0.89 1.74 0.54 1.45 1.70 1.94 0.40 I .60 0.88 0.81 1.74 1.54 0.82 I .63 0.93 1.14 0.88 1.68 1.70 I 4 8 0.53

0.86 1.73 1.73 0.83 0.45 0.52 I .40 I .g2

1.15

0.78 1.23 1.14 2.52 1.34 1.r5 1.66 0.65 2.33 0.75 2.32 0.62

1.2'

2.01

-

2.12

0.58

1.27 1.30 0.97 0.58

Yacoby

-

0.44 - - -

0.2(

0.55

0 . 3 ~ -

- - - - - -

3.55 0.48 - - - - - - - 3.47 - - 3.50

3.36 3.36 3.23 3.26 3.14 3.48 3.60 3.43 3.36 3 .25

3.14

3.36

3.26

-

-

- - ). 16 - 3.19 3.67

3.63

1.40 3.25

-

-

- -

Chase

-Y25 - .o I -

-.16 - .27

-.16

-.23 +.I1 -.07 - . I7 t . 2 3

-.07

t . 2 6 +.04 t . 1 3 t . 1 5 ' -.14 t . 6 I -.71

+.3 2

t . 3 3 t . 3 6 t . 0 3 +.18*

-.41 t . 2 3 ' t . 0 8

. I I -

.oo

- .OI

.oo

-.22

. 2 0

. I I

- - -.04

+.22 '

- . 2 6

t . 6 4 -*37

t . 2 6 t . 3 I -.04

-.23 t . 0 9 -.26 -.13 +.16 t . 2 5 -.16

-.2I

- .20

- .OI

+.I4 t . 0 3 -.07

-*59

-_ 0.7f

0.65 o.6r 0.gc 0.6:

0.51 0.62 '.3f I .4c I .6E 0.9: 0 . 7 ~ 0.72 0.93 0.55 0.53 0 . 8 2

I .06

0.44 0.77 0.55 0.82

I .oe 0 . 5 2

0 . 6 ~ I .47 0.84 I .44 I .44 0.41 0.86 0.gc 1.03

1.53 0.96 0.84 0.90 c.72 0.48 0.59 1.29

D.82 ~1.69

-

1.12

D.88

1.1 I

3.38 1.16 3.34 3.57 3.32

3.84 3.45 3.32

I .oo

Sckur Anztrronn --

- +!'I I

-.06 +.22

+.32

+.08 t . 4 6 -.29

-.30

-

-

- . O I

-

- .oo

--43 - . I 8 -.04 --.08* +.30 -.36 t . 0 7 t . 0 1

+.03

--59 -.30 t.58' --44

-

- - - - - - - - - - - - - - - - -

+a35 t . 0 1 +.I 0

-.29 -.Ol

- - 5 5

+.24 -.01

- 4 9

.o I -

_- -

0.6s

0.2t

0.8t

-

- 0.78 0.26

0.43 0 . 3 ~ 0.35

0.31

0.2t o.7E 0.65 0.38 0.72 0.4 t 0.34 0.75 0.37 o.7t

0.26

3.53 3.38 0.50

-

-

-

- - - - - - - - - - - - - - - - - 1.66 3.32

3.97 3.28

3.91 3.26 1.56

3.39 3.43 3.27

Mean

-Yo86 t . 0 5 0 -.026 -.029 t . 0 2 7 -.107 t . 0 4 5 --034 --.037

-so54 -.091 --.274 -no79 - .08 2 +.I02 -.160 +-074 -.o16 t . 1 6 4 +.or2 -.I08 t.08 I

t . 0 3 9 t.005 +.05 I

- a 0 5 3 -.003 t . 0 8 I

+.014

.o 10 -

t . 0 4 2

.I I 0

+a038 -

t . 0 0 6 -.065 t.007 t . 0 0 8 --.099 +.05 I -.050

+.006 +*034 t . 0 1 5 - a049

t-004 t . 0 4 4 - . 0 2 0

+*o30

. I 2 2 -

-.031

-.326 + a 2 5 -.r61 +.098 --.I 7 7

+-I04

2.4 2.;

3.7 3.8 5.8 2.0

4.3 2.7

5.4 6.6 7.2 3.9 3.7 2.9 2.8 5.' 4.7 2.9

5 . ' 2.5 3 .o 3.6 4. I

7.7 2.9 3 3 8.0 3.6 7.3 7.5

2.8 3.7 5 .o 8.2 8.0 5 . 5 3.2 4.7 4.6 3.5 3.8 8.5 3.8 3.3 2.8 6.7 1.7' 6.3

5.6

5.2

3. I

3 . 0 I .9

2.2

2.2

2.1

I 7 5

RO- tation No. -

84 85

87

89

86

88

90 91 92 93 94 95 96 91 98 99

I00

I01

I 0 2

'03 104 '05 I 06 1 0 7 108

I09 I I 0 I11

I 1 2

"5 116 "7 118 1 '9 I 2 0

I 2 2

124 '25 126 '27 I 28 129 '30 131 1 3 2 '33 I34 135 136 I37 138 '39 I40 '41 142

'43

3 107 I 76 - Stars

Definitive Distance

4265!696 49'5.113 6890.039

5241.838

5 7 18.762 6786.124 6 I 70.524

1237.641 365 1.896 5526.064 7 0 56. I 39 '3' 7.341 5013.854 6731.595 5504.030 4451.882 5 7 85.060 5162.402

5054.101

3 3 36.5 1 7

3163.057

67 76.484 4247.997 5383.282 4064.637 6444.042 3707.61 I 7 193.4 59 3 5 94.1 7 1 2 190.700 4314.118 3545.292

5154.003 3343346 2 358.3 I 9

3010.540

7231.412 4313.571 7000.763 3939.444 3026.568 3026.879 45 34.7 87 6464.942 5823.259 1598.901 5803.086 6076.853 5'52.924 399' * O 78 667 8.95 6

3889.100 58 I 9.612 6069.776

5048.697

6OI.775

GidZ

+!'I4 -.19 +.03 -.06 -.I8 +.03 -.05

f . 0 8 --47 +.16 +.02

+.05 +.29 -.32

+.13 -.03* -.14 -.14

.oo

. 20

-.I0

-

+.05 +.28 +.I5 +.20

-.17

+*33 +.18 -.23

+.3 I

+.03 -.06 t . 0 3 -.07

+.05 -.07

-.OI

- .OI

.oo +.I4 t.08 +.2 7 +.2 2

+.19 -.04

+.05

-.04 +.03 t.48 -*34 -.08

- .OI

-

- .02

+.30 . 2 1 -

--

r.53 "73

1.33 1.74 2.54 1.63 1.36 ).74 2.26

5.52

5.27 I .68 ).67

1.01

5.36 3.56 2.75 t .68 3.99

1.74 3.06

1.70 I .06 ~ . 7 2 1.73 3.66 1.19 1.87

3.80

1.02

I .02

1 .20

2.84 1.74 2.55 5.16 2.64 I .oo 0.67 I .62 1.41 1.41 0.98 0.71

2.3s 0.8c

2.6: 1.6~ 0.65 1.72 1.6! 3.2( 1.5: 1.7c

1 . 2 C

-

Finlay

+!60 t . 1 6 f . 3 0 -.26 - .o I fa39 f . 3 8 f . 0 2

f . 3 4 +.I1

-.03 f - 0 4 f .26 -.03 -.I5 -.08* - .07 f - 3 2 -*44 f.16 t . 0 6 +.I5 -.23 f.08 +.I0

f . 43 -.09 +.23

+. I7 f.16

t . 4 4 -.45 f .06 +.27 +.I1

+.I 1 -.31 -.30 -.I5

+.16 -.31 +.25

-.13 -.03 + . I7 + . 2 I

+.o I

-.05

+.26 - .06

--.I0

-.02

- .02

+-24

.oo

- 2 0 -

-

J.9 I I .60 ~ . 6 6 J.77

1.76

'.53 3.60 2.08 2.46 t.34 1.43 3.52

2.40 "73 I .88 3.71

3.66 1.50 3.93 3.91 3.73 0.96 ~ 5 8 0 .53 0.51

1.68 0.9 I 1.68 1.27

0.75 0.58 2 . 4 ~ 0.5 I 0.85 0 . 5 2

0.48 I .zt I .zt 0.8C 0.5; 0.3:

0.6t 0.6: 0.7! 0.9: 0.5: 1.1:

2.3

6.4'

1.12

1 .02

J.88

1.lC

2.1:

I .O(

I .2.

Yacoby

- +!o3

+a33

-

- - -

-.39 - .05 f . 2 7 f . 0 2

-.07 -

f . 4 1 .oo

f . 2 0

f . 2 3 ' -

f . 2 0

+.I7

-*59 +.I5

-.07

+ * I 9 +a48

. I 0 -

f . 2 3 +.83 -.48

f . 3 2 t . 3 3 -.I5 - 1.03 +.I5 -.04 +.08

+.20

+ . 2 0

-.13 +.49 -.03

-.26

f . 1 3

.oo

-

.oo +.04 +.19 + . I 2

- .I7 -.47 -.14 +.38 -.31 + . I 1

-.13

-

- 3.21 - 3.20

- - -

3.14 3.16 3.64 3.70 3.68 -

3.14

0.69

0.14

0.26 0.16 0.19 0.14

0.19

0 . 3 ~ 0.23 0.32 0.14 0.34 0.52 0.27

0.35 0.4~

0.3t 0 . 5 ~

0.2t

3.20

-

0.28

0.2c

0. I 1

0.11

0.3' 0.4' 0.4' 0.2' -

O . t (

0.6: 0.1:

O.I( 0.2(

0.31 0. I.

0 . 2

0.3 0.11

0.11

0.81

Chase

+!'32 +.25

. I0

- . I 2

-

- . I 7 +.35 -.04

-.31 -.04

+.I0

f . 0 9

+ . 3 2

.I0 -

- -.18 -.03

.2 I ' - -.02

+.04 - - .04

-.29 -.18 - . S O

+.28 +.26

-.08 -. 1 7 -.29

-.08 -.I5 +.06 -.14

+.01

- .40 +. I3 +.26 -.36

-037

-

- .22

-

- .02

+.37 +.02

- .04 +.04 -.46 -.09 +.02

+-5 3 -.06 + .OI

+.33 + . I5

. 2 0 -

~

0.44 1.18 3.60 0.78 3.76 0.96 0.72 0.60 0.33 1.15

1.18 1.41 ~ 3 6

1.17 r.17

).73 1.84

3.38 ~.60 3.44 3.37 J.45 1.32 1.46

3.47 3.54 3.43 J.47

3.76 ~ . 9 6 1.59

3.43 0.30 0.45 3.50

0.50

0.41 0.31 0.35 0.57 0.35 0.34 0.77 0.4: 0 . 3 ~ 1.1;

0.gc 1.7: 0.31

-

L.22

-

-

I .oo

-

I .2:

SCkUY Ambronn

-!I2 7 -.I9 +.26 -*39 -.24 - -

+.16 - .04 -.14 +.05

-.28 -

.oo - . I1

+a42 - - - - - - - - -

-.23 + . O I

- .03 +.06 -.41 - *57

+.I I

-.09 -.14 -.30

-

-

- - - -- -

-.24 -1- .25

-.05 +.oz -.61

+ . 0 2

+*3 5 +.70 +.27

__

-

- - __

Mean

+*236

t . 092 - . I28

-.I37 t . 1 6 9 +.I 2 7 +.lo7

+.I 15 -.or6 +.008 +.I35 - . 0 1 5

-.058 +.025 - .086 -a049 t.08 I -.229 -.008

f . 0 5 2 f . 0 7 0

t . 0 2 7

f . 0 3 8 f.100

f . 2 I 9 f . 0 7 2 --.of32

f . 0 9 3

-.002

-.I 2 2

f . 0 0 4

- - .02I

- .022 - . O I 2

-.028 -.056 +.03' - a045 +.046 +.063 +.043

+.108 + . 2 2 1

-.092

+.025

- . O I 2

t . 0 6 7

-.267 -.036 +.046 +.322 -.070

+*039 -.138 i - 3 8 4 - so49

-

1.4 Lo t.4 5.2'

3.9 j.4 3.5 2.6

5.3 9.3 3.8 2.8

1.5 3.7 1.5' 6.2 3 .o 3.' 1'5 3.8 4.6 2.4 2.3 2.5

3.4

3 .o 2.9

3.9 5.5 3.6 4.2 8.9 3.4 2.8 1.8 3.0 3.7 3. I 2.7 1.7 1.9 6.0

2.0 '

2.0

I .2

2.2

2.0

I .4 3.9 3.5 I .8 4.7 4.5 6.9 3.2 1.1

I77

unter dem Titel >Resultate aus den in Pulkowa angestellten Vergleichungen von Procyon mit benachbarten Sternencr (Memoires de 1'AcadCmie ImpCriale des sciences de St. PCters- bocrg V I P serie, Tome XXXI, No. 2). Diese Schrift enthiilt u. a. auch eine Bearbeitung der von 0. Struve in den Jahren I 85 1-1 882 angestellten mikrometrischen Vergleichungen von Procyou rnit zwei kleinen Sternen in seiner Nachbarschaft.

3108

formig vorausgesetzten, Bahn des Procyon urn den Schwer- punkt seines Systems hochst wahrscheinlich kleiner ist, als ihn die bekannte, von Auwers aus Meridianbeobachtungen ab- geleitete Bahn (Monatsberichte der K. Preussischen Akademie der Wissenschaften zu Berlin, Mai 1873) angiebt. Allerdings zeigen die von Auwers aus den Rectascensionen und Decli- nationen gesondert abgeleiteten Resultate verhiiltnissmassig

- Stars

Definitive Distance

260217 1 1 5 138.599 4572.962 4504.656

814.563

59I4.165 6195.865 59'0.509 55 17.645 3560.857

7050.633

6933.942 5 0 1 2.382

6038.157

6020.077

2910.765

6640.65 7 3340.138

5141 -134 6289.293 3 150.220 500 I .a54 2018.006 6404.2 7 2

1890.544 5320.028 5042.418 2049.7 74 402 9-45 6 3827.938 4366.019

1260.625 5 290.05 2

65 74-1 '9

GiZl 1 -~

+!I0

f . 3 1 -.04 +.Ol -. 13 -.13

+ . I O '

- , O I

-.13' -.02

-.05'

+.I8 +.13 +.I1

- .25

+ a 0 7

-.08 - . I 6 -.09 -.06

-.14 - . I 8

- . 05 +.22 -.13 -.07

.oo

-.02

.I0 -

-.02

.I1 - -a34 + . r 2

+.29

1.98

1.54 ).28

'.77 1.78 1.68 1.78 2 . 5 2

2.94 0.67 3.14 2.52

0.67 3.11

0.81 1.47 3.38 0.89 4.06 2.52

1 .72 1.78 0.50

3.20 4.20

3.50 0.86 4.11 0.70

I .20

2 : I I

Finlay

-Y19 -.29 f . 0 4 -.ox t . 2 6 -.OI -.OI

f.33' f.01'

-.06 -.03' - .05 +.I I'

-.26

-.06 -.OI

.I0 - +.38 -.27 -.13 -.I8 t . 1 6 - .19 - .03 -.26 -.I4 t.08 +.OI -.19 +.08

+.25

- . I 5

.02 -

t . 2 7

-

1.45 1.76 1.84 1.86 3.63 2.91

3.31 3.64 I .06 0.64 1.43

1.31 0 . 5 2

I .64

0 .52

1.5t 0.6; 0.6~ 2.4t 0.72 1.75 1.71 I .81 0.7, I .gr 2.6,

I .9: 2.51 2.2:

0.7~ 2.4! 0 . 5 !

1.11

1.15

Yacoby

t Y 2 I -.I I

f . 3 I

--34 -.13 f . 2 0

-.25

+.5 3 -.16* --.07

+.05 +.56' +.64 +.45 + . I 8 -.09 +.63

+.24'

-.02

- .04

- .40 +.09 -.13 +.I0

+.42

.I 2 -

+.I4 -.13 t . 5 I

.2 I - -

-*97 --33' +.56

1.14

1.16 1.18 1.34 ).41 1.14 1.14

3.36 3.14

3.40

3.17

0.16 0.38

0.57 0.15

0.59 0.19

0.57 0.30 0.32

o.ig 0.70 0.15

0.20

0.20

-

-Yo1

+*41 -.24

-.27 -.06 t . 5 1 t . 4 8 ' f . 5 I'

- .04' -.28 -.40* f . 4 6 + . I 2

f . 2 2

+.28 f . 1 4 +.r9

-.2I

-.OI

. I 2

. I 2

- -

-a34 +.IS

-.32 -.47 +.I I -.07

-.16 t . 2 3 +.O$

t . 0 4 -*59

--.20

-

-~ 1.52 +!'03 1.39 .oo 1.82 +.04 1.42 - 1.34 1.60 --.IT

).34 1.34 1.60 +.06* 3.34 1.08 - . IS '

3.47 -.07 1.00 -.04' 0.30 -.09 1.55 +.58 0.97 +.21 0.30 - 0.39 0.35 0.33

0.39 1.10 -.25 1.28 +.35 0.55 + .21

0.75 1.17 -

-

- - -

- - -

1.47 -.O4 -

-

0 . 5 5 ' +.04 0.45 -.08 0.92 - .22

- - j -.04

0.59 1 - 0.31 I -

Ambvom

- -

-Yo9 -.16 +.47

-.19 t . 6 1 .

t.81

-

- - - -- -

+. I1

+.I0 +.OI -.04 -.36 -.09

-.36 -

- - -

+.07 -.06

t . 3 9 -*35

-

.- -

+.I7 -.92

1.38 1.28 ~

1.28

1.28

1.28

-

-

- - - - 3.26 D.5'

0.25

0.70 0.29 0.28

0.35 -

- - -

0.32

0.35

0.43 0.45

-

- -

1.01

0.26

Mean --

-Yo36 t . 0 8 1 - a 0 3 1 -.064 - .009 -.064 t . 0 3 4 t . 3 2 7 t.083 f . 0 7 2 - .05 I

f - 0 4 4 f .099 f.05 7 -a035 +a039

-.I50 --.096

-.085 -.130 -.090 - .09 I

. I 2 0

+ . I 2 3 --.or7 -.o60 - . P O 3 -.040 -.140 +.I31

- .oo 2

+*I03

- .I02

-

.I11 -

-

1.5 I. I

1.1 :.7 !.8 i.8 1.8

5.5

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In conclusion, I desire to convey to the Astronomers and Directors of Observatories who have shared this work, an expression of my warm thanks for their hearty and ready cooperation - and also gratefully to acknowlege the aid received towards the cost of the reductions by a grant from the Bruce Fund.

Royal Observatory, Cape of Good Hope, 1892 June 2 7 . David GiZl.