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Wolf, Harry J (corap.)

Common methods of
determining latitude
and azimuth.

^^z?mmn of f.;iH.i<i

'olume Thirteen

•^ Number Three

^ I

-^ ^or fn the

Quarterly

OF THE

Scho ol QF Mines

icrosoft Corporal

JULY, 1918

Issued Quarterly by the Colorado School of Mines

Entered as Second-Class Mail Matter, July 10, 1906, at the Postofficc at
Golden, Colorado, under the Act of Congress of July 16, 1894.

Volume Thirteen

Number Three

Quarterly

OF THE

School of Mines

JULY, 1918

Issued Quarterly by the Colorado School of Mines

Entered as Second-Class Mail Matter, July 10, 1906, at the Postoffice at
Golden, Colorado, under the Act of Congress of July 16, 1894.

QUARTERLY

OF THE

Vol. Thirteen JULY, 1918 Number Three

Common Methods of Determining Latitude and
Azimuth Useful to Engineers and Surveyors

COMPILED BY HARRY J. WOLF.
Professor of Mining.

I. LATITUDE.
1. By Observing Altitude of the Sun at Noon.

(a) Set up transit before local apparent noon. The standard time
corresponding to local apparent noon at the point of observation may
be found by adding or subtracting from 12 h the equation of time as
directed in the Nautical Almanac or Solar Ephemeris.

(b) Find the maximum altitude of the upper or lower limb of the
sun by keeping the middle horizontal cross hair tangent to the limb
as long as it continues to rise. When the observed limb begins to
drop below the cross hair read the vertical angle.

(c) Level the telescope and determine the index error. Apply
this error to the observed vertical angle to obtain the true vertical angle.

(d) From a table of refractions in altitude determine the refraction
correction for the vertical angle obtained, and subtract this correction
from the true vertical angle to obtain the altitude of the limb observed.

(e) From a table of semi-diameters of the sun determine the semi-
diameter for the date of observation, and add this correction if the
lower limb was observed, or subtract it if the upper limb was observed,
to obtain the altitude of the sun's center.

(f) From a table of the sun's parallax determine the parallax for
the observed altitude, and add this correction to obtain the true altitude
of the sun's center. In view of the limits of accuracy of the surveyor's
transit this correction is usually neglected.

(g) From the Nautical Almanac or Solar Ephemeris determine the
sun's declination at the instant the altitude was taken. If the longitude
of the place is known, increase or decrease the declination for the instant
of Greenwich apparent noon by the hourly change multiplied by the
number of hours in longitude. If the longitude is not known, but stand-
ard time is known, increase or decrease the declination for the instant
of Greenwich mean noon by the hourly change multiplied by the num-
ber of hours since Greenwich mean noon.

(h) Latitude = 90° — Altitude -\- N. Declination, or
Latitude = 90° — Altitude — S. Declination.

^

4 COLORADO SCHOOL OF MINES QUARTERLY.

EXAMPLE:

(a) Transit was set up before local apparent noon on June 26, 1918.
From Solar Ephemeris the equation of time is 2 m 27.73 s, and the differ-
ence for 1 h is 0.525 s. Transit was set up about 11:50 A. M., which was
12 m to 13 m before the sun's meridian transit.

(b) Upper limb of the sun was observed.
The vertical angle was:=

(c) Telescope was leveled. Index error =

True vertical angle =

(d) The refraction correction was =

Altitude of sun's upper limb =:

(e) Sun's semi-diameter was =

Altitude of sun's center

(f) Sun's parallax was =

True altitude of sun's center = 73° 38' 0'

(g) Sun's apparent declination at Greenwich apparent

noon on June 26, 1918 = N. 23° 23' 14.2'

The longitude of the place is 105° 32' 33", which = 7.04 h

(15° = 1 h) . Difference in declination = 7.04 x 4.38" = —30.8'

73°

54'

30"
30"

73°

54'

0"
17"

73°

53'

43"

15'

46"

73°

37'

57"
3"

Sun's apparent declination at point of observations N. 23° 22' 43.4"
(h) Compute latitude by formula: Lat = 90°— Alt + N. Dec.

90" 0' 0"
Subtract altitudes 73° 38' 0"

16° 22' 0'
Add N. Declinations 23° 22' 43'

Latitude of places N. 39° 44' 43"

2. By Observing Altitude of Polaris at Culmination.

(a) Set up transit before upper or lower culmination. The standard
time of culmination may be found by interpolation from a table of time
of culmination of Polaris in the Nautical Almanac.

(b) Focus on the star and follow it with the horizontal cross hair as
long as it continues to rise if upper culmination is observed, or as long
as it continues to fall if lower culmination is observed. When the desired
culmination is reached read the vertical angle.

(c) Level the telescope and determine the index error. Apply this
error to the observed vertical angle to obtain the true vertical angle.

(d) From a table of refractions in altitude determine the refraction
correction for the vertical angle obtained, and subtract this correction
from the true vertical angle to obtain the altitude of the star.

(e) JFYom the Nautical Almanac or Ephemeris determine the polar
distance of Polaris, either from a table of polar distances or by subtract-
ing the apparent declination from 90°.

(f) Latitude s Altitude of the Pole.

Latitude s Altitude of Polaris at upper culmination — polar

I distance.

Latitude = Altitude of Polaris at lower culmination -|- polar
distance.

Q8

\^\o^

COLORADO SCHOOL OF MINES QUARTERLY. 5

EXAMPLE:

T^nri^l Ti'^i^^'^'^^^, ^.^^ .VP b^^o^e lower culmination on June 1, 1918.
From a table of culminations of Polaris, the local mean time of lower
??}^J,^^H?^i« 8 H 51.3 m P. M. for longitude 90° W. For longitSde lol'
ilox^^ n^- l^^ M?'® ^o"ld ^6 8 h 51.1 m P. M. (0.16 m earlier for each
15 ) The transit was set up about 8:30 P. M. which is about 20 m be-
fore lower culmination.

(b) Observed vertical angle = 3go 33, q«

(c) Index errors y ^^

True vertical angle =

(d) Subtract refraction corrections

Altitude of Polaris =

(e) Polar distance on June 1, 1918

Latitude of place (altitude of N. Pole) = N. 39* 44' 47"

38°

38'

0"

1'

XZ"

38°

36'

47"

1°

8'

0"

II. AZIMUTH.
1. By Observing Altitude of the Sun.

(a) Observe the sun at any time except when it is within 10° of the
horizon (because the refraction is relatively large and uncertain) or when
it is near the meridian (because small errors in observed altitude pro-
duce relatively large errors in azimuth). Set up transit over one end of
the line whose azimuth is desired. Sight along the line with the verniers
set at 0°. With the lower clamp tightened and the upper clamp loosened
sight on the sun with a colored shade glass on the eye piece or focus the
sun's disc, and the cross hairs of the instrument, on a screen held behind
the eye piece.

If the observation is made in the forenoon place the sun's disc in the
upper left-hand quadrant, and tangent to the vertical and middle horizon-
tal cross hairs, and record the vertical and horizontal angles and the time.
Then reverse the instrument and make similar observations with the
sun's disc in the lower right hand quadrant. If the observation is made
in the afternoon, place the sun's disc first in the upper right-hand quad-
rant and then, with the instrument reversed, in the lower left-hand
quadrant. The mean of the vertical angles and the mean of the hori-
zontal angles may be assumed to correspond to the position of the sun's
center at the instant indicated by the mean time reading.

The direct and reversed observations should be made within a short
period of time, say 2 or 3 minutes. If the instrument is in perfect adjust-
ment, the observation may be simplified by centering the intersection of
the vertical and middle horizontal cross hairs on the sun's disc, with the
assistance of diagonal cross hairs, stadia hairs, or concentric circles
placed on a screen upon which the sun's disc is focused.

(b) From a table of refractions in altitude determine the refraction
correction for the mean vertical angle of the sun's center, nnd subtract
this correction from the vertical angle to obtain the altitude of the sun's
center.

(c) From a table of the sun's parallax determine the parallax for
the observed altitude, and add this correction to obtain the true altitude
of the sun's center. In view of the limits of accuracy of the surveyor's
transit this correction is usually neglected.

(d) Fj:'om the Nautical Almanac or Solar Ephemeris determine the sun's
declination at the instant the altitude was taken. If the longitude of the
place is known, increase or decrease the declination for the instant of Green-

wich apparent noon by the hourly change multiplied by the number of
hours in longitude. If the longitude is not known, but standard time is
known, increase or decrease the declination for the instant of Greenwich
mean noon by the hourly change multiplied by the number of hours since
Greenwich mean noon.

(e) The azimuth of the sun from the NORTH may be computed from
any one of the following formulae:

Where A =: sun's azimuth from north

S= y2 (codec + colat + coalt)

(1) sin 1/^ A = / sin(S — colat) sin(S — coalt)
\ sin colat sin coalt

4

(2) cos Vz \= ^| sin S sin(S — codec)
sin colat sin coalt

(3) tan Vz A = / sin(S — colat) sin(S — coalt)
\ sin S sin (S — codec)

Or from any one of the following formulae:

where A = sun's azimuth from north

8 = 1^ (codec + lat + alt)

(4) sin Yz A = / sin Vz (lat + coalt — dec) cos Vz (lat + coalt + dec)
\ cos lat sin coalt

(5) sin 1/2 A^= sin (s — alt) sin (s — lat)
\ cos lat cos alt

(6) cos 1/2 A^= j/ cos s cos (s — codec )
\ cos lat cos alt

(7) tan Yz A = / sin (s — lat) sin (s — alt)

\ cos s cos(s — codec)

(8) vers A — cos (^^t — alt) — sin dec

^ cos lat cos alt

The azimuth of the sun from the SOUTH may be computed from any
one of the following formulae:

where A =: sun's azimuth from south

s

S = % (codec -f colat + coalt)

(9) sin Yz A = / sin(S — codec) sin(S — colat

\ sin codec sin colat

(10) cos 1/2 A^= / sin S sin (S — coalt)
\sin codec sin colat

(11) tan Y2 ^ = / sin (S — codec) sin (S — colat)

^ \ sin S sin(S — coalt)

(12) cos A = - ^^^ ^^^ — tan lat tan alt

'' cos lat cos alt

COLORADO SCHOOL OF MINES QUARTERLY. 7

Note— If the observation is made north of the equator the declination
IS + when north and — when south. If the observation Is made south
of the equator the declination is + when south and — when north. If
the sun is observed when north of the prime vertical in the northern hem.
isphere, or south of the prime vertical in the southern hemisphere, the
first term will be greater than the second term. Equation (13) is an-
other form of equation (12).

(13) cos A = — ^^^ dec — sin lat sin alt

^ cos lat cos alt

(14) vers A = cos (lat + alt) + sin dec

^ cos lat cos alt

The azimuth of the sun from the NORTH may be computed from
the following formulae:

where Aj^ = sun's azimuth from the north

(15) cos A^=tan Ci tan lat = tan C, tan lat

C, = 1/2 coalt + ^ (Ci — a)

when latitude is less than declination and on the same
side of the equator.

C,= Mi coalt— ^^(Ci — C^)

when latitude is greater than declination and on the
same side of the equator, or when latitude and declina-
tion are on opposite sides of the equator.

tan iA(Ci — C2) =cot 1^ (lat + dec) tan 1^ (lat — dec) cot % coalt

EXAMPLE:

(a) Transit is set up over B.M. on June 4, 1918.
Sighted on Flagstaff with verniers at 0°.

Telescope pointed at sun, and the following observations re-
corded

Quadrant Time ~ Horizontal Angle Vertical Angle

Upper right 2:52 P.M. 294° 15' 50" 3'

Lower left 2:54P.M. 295° 34' 49" 6'

Sun's center 2:53P.M. 294° 54' 30" 49° 34' 30"

(b) Refraction correction = 49"
Altitude of sun's center = 49° 33' 41"

(c) Parallax correction = 6"
True altitude of sun's center = 49** 33' 47"

(d) 1. If the Solar Ephemeris gives the sun's declination at Green-
wich MEAN noon proceed as follows:

Sun's apparent declination at Greenwich MEAN noon on June 4,
1918 = N. 22° 22' 22.0". The difference in declination for 1 h = 18.03".

8

The place of observation is west of longitude 105° W. and 105tli meridian
time is used. 105° = 7 h. The standard time of the observation was
2 h 53 m P. M. = 2.883 h, which is 7 h + 2.883 h = 9.883 h after Greenwich
Mean Noon. The difference in declination at the instant of observation
is 18.03" X 9.883 = 178.2" = 2' 58.2". The declination at the instant of ob-
servation is 22° 22' 22.0" + 2' 58.2" = N. 22° 25' 20.2". The difference is
added because the north declination is increasing,

(d) 2. If the Solar Ephemeris gives the sun's declination at Green-
wich APPARENT Noon, proceed as follows:

Sun's apparent declination at Greenwich APPARENT Noon on June
4, 1918 =N. 22° 22' 21.4". The difference in declination for 1 h = 18.03".
The equation of time is 2 m 1.51 s, and the difference in the equation of
time for 1 h = 0.416 s. The place of observation is west of longitude
105° W. and 105th meridian time is used. 105° =: 7 h. The standard time
of the observation was 2 h 53 m P. M. = 2.883 h, which I's 7 h + 2.883 h
= 9.883 h after Greenwich Mean Noon. The equation of time at the
instant of observation was 2 m 1.51s — (0.416 sx 9.883)= Im 57.4 s =
0.033 h, which must be applied to standard time to obtain apparent time.
The difference in declination at the instant of observation is 18.03" x
9.883 + 0.033) =178.8" = 2' 58.8". The declination at the instant of
observation is 22° 22' 21.4" + 2' 58.8" = N. 22° 25' 20.2". The difference
is added because the north declination is increasing.

By previous observation, or from a map, the latitude of the place of
observation has been determined = N. 39° 44' 45".

(e) 1. Computation by formula (2)

cos 1/^ A

\ SI

sin S sin(S — codec)

sin colat sin coalt
S = 3^ (codec -f colat + coalt)

codec = 67° 34' 40'

colat = 50° 15'

15"

coalt = 40° 26'

13"

2S =158° 16'

8"

S = 79° 8'

4"

log sin S

= 9.9921434

log sin (S — codec)

= 9.3017612

colog sin colat

= 0.1141368

colog sin coalt

= 0.1880158

2)9.5960572

log cos 1/2 A ^

= 9.7980286

V2A„

= 51° 5' 24

^n =

102° 10' 48"

horizontal angle =

294° 54' 30"

397° 5' 18"

-360°

Bearing

= N. 37° 5' 18" W.

(e) 2. Computation by formula (12)

cos A

+ sin dec

cos lat cos alt

log sin dec =

colog cos lat =

colog cos alt =

log 1st term =

log tan lat =

log tan alt =

2nd term
1st term

— tan lat tan alt

= 9.5814136
= 0.1141368
= 0.1880158

9.8835662

9.9198979
0.0694691

log 2nd term = 9.9893670

= —0.975814
= +0.764832

nat cos Ag
log cos Ag

horizontal angle =294° 54' 30"

= — 0.210982
= 9.3242454
= 77° 49' 12"

217'
180'

5' 18'

Bearing

= N. 37° 5' 18" W.

Note: It is customary to make a series of five observations, compute
the azimuth indicated by each, and take as the azimuth required the aver-
age of not less than three computations that check within one minute of
arc. For this purpose formula (12) is the most convenient.

(e) 3. Computation by formula (15)
cos A = tan Co tan lat

C, = 1/2 coalt — 1^ (Ci — C,)
tan i^(Ci — C) =cot y2(lat + dec) tan ^ (lat — dec) cot % coalt

alt= 49° 33' 47"

coalt = 40° 26' 13"

dec = N. 22° 25' 20"

lat = N. 39° 44' 45"

(lat + dec)=62° 10' 5"

(lat — dec)=17° 19' 25"

i^(lat + dec)=31° 5' 2.5"

^(lat — dec)= 8° 39' 42.5"

1/2 coalt = 20° 13' 6.5"

log tan 1/2 (lat — dec) = 9.1828120
log cot 1/2 coalt = 0.4338048

log tan V2(C, — C,) = 9.8364015

10 COLORADO SCHOOL OF MINES QUARTERLY.

y2(Cx— a)

^ coalt

= N

34° 27' 17.6"
20° 13' 6.5"

log tan C2
log tan lat

-14° 14' 11.1"
9.4043466
9.9198979

log cos Ajj

\
horizontal angle

9.3242445

102° 10' 48"
294° 54' 30"

397° 5' 18"
-360°

Bearing =

. 37° 5' 18" W.

By Equal A. M. and P. M. Altitudes of the Sun.

n

2.

(a) Set up transit over one end of line whose azimuth is desired.
Sight along the line with the verniers at 0°. With the lower clamp tight-
ened and the upper clamp loosened sight on the sun. If the upper and
left-hand limbs are sighted in the forenoon, then sight on the upper and
right-hand limbs in the afternoon. Use the same vertical angle in both
observations, and record the horizontal angle and the time in each case.
The mean of the two horizontal angles, corrected for the effect of change
in declination, is the desired azimuth from the south.

(b) The angle between the meridian and the mean of the two hori-
zontal angles is found by the formula:

Half the change in declination between
the two observations
Correction

cos lat X sin half the hour angle between
the two observations

EXAMPLE:

Latitude =:N. 39° 45' 36" Date = July 11, 1918.

Observations: A.M. P.M.

Angle on desired course = 0° " 0°

Vertical angle on upper limb = 63° 18' 63° 18'

Horizontal angle z= 240° 3' (left) 352° 18' (right)
Time of observation = lOh 30m Ih 12m

Half the time between observations, or hour angle. = Ih 21m

= 1.35h

Half the change in declination = 19.37" x 1.35h = 26.15"
log 26.15" = 1.4174717
colog cos lat = 0.1142261
colog sin 20° 15' = 0.4607770

= 20° 15'

log correction = 1.9924748

correction = 98.282" = V 38"

mean horizontal angle =63° 49' 30'

corrected angle = 63° 47' 52"
Bearing = S. 63° 47' 52" W.

r

COLORADO SCHOOL OF MINES QUARTERLY. 11

Note: It is customary to take a series of observatioua in the fore-
noon at suitable intervals, and corresponding observations in the after-
noon, in order to check their accuracy and increase precision.

3. By Observing Polaris at Elongation.

(a) Set up transit over one end of the line whose azimuth is desired,
about half an hour before elongation, and sight along the line with the
verniers set at 0°. The standard time of elongation may be- found by
interpolation from a table of the time of elongation of Polaris. If such a
table is not available, then the hour angle may be computed by the fol-
lowing formula:

tan latitude
cos hour angle'^: tan declination

This hour angle may be converted into sidereal time by the following
formula:

Sidereal time =: hour angle + right ascension.

This sidereal time may be converted into loqal mean time by the
following formula:

Local mean time ^ sidereal time — mean sun's right ascension — in-
crease in sun's right ascension.

This local mean time may be converted into standard time by ex-
pressing the longitude between the local meridian and the standard merid-
ian in units of time (15° = lh), and adding this correction if the local
meridian is west of the standard meridian, or subtracting the correction
if the local meridian is east of the standard meridian.

The declination and right ascension of Polaris, and the mean sun's
right ascension and the increase in sun's right ascension, may be found in
the Nautical Almanac.

(b) Focus on the star and follow it with the vertical cross hair as
it moves towards its greatest elongation. Near the elongation the star
appears to move vertically. When the desired elongation is reached read
the horizontal angle.

(c) From a table of azimuth of Polaris at elongation determine the
azimuth corresponding to the latitude of the place of observation. If such
a table is not available, then the azimuth may be computed by the fol-
lowing formula:

si n polar distance
sin azimuth = cos latitude

s in codeclination
or sin azimuth = cos latitude

(d) Bearing = horizontal angle + azimuth at W. elongation,
or Bearing= horizontal angle — azimuth at E. elongation.

EXAMPLE:

(a) Transit is set up over point A, July 16, 1918, in latitude N. 39*
44' 45'' From a table of elongations of Polaris the time of western elon-
gation is found by computation to be llh 59.3m P. M. Point B is sighted
with the verniers set at 0°.

(b) With the lower clamp tightened and the upper clamp loosened
the star is observed at western elongation, and the horizontal angle is
86° 47' 30".

12 COLORADO SCHOOL OF MINES QUARTERLY.

(c) From a table of azimuth of Polaris at elongation the azimuth
for latitude N. 39" 44' 45" is 1° 28' 27". Or the azimuth may be computed
as follows:

Polar distance = 1° 8' 2". log sin polar distance = 8. 2964195
Latitude =39° 44' 45". log cos latitude =9.8858632

log sin azimuth =8.4105563

azimuth = 1° 28' 27"

(d) Horizontal angle = 86° 47' 30"
Azimuth at W. elongation = 1° 28' 27"

Bearing of line A-B= N. 88° 15' 57" W.

4. By Observing Polaris at Culmination.

(a) Compute the exact standard time of culmination, and provide a
watch reading correct standard time. Set up transit, before upper or
lower culmination, over one end of the line whose azimuth is desired.
Sight along the line with the verniers set at 0°. With the lower clamp
tightened and the upper clamp loosened observe the star.

(b) Focus on the star and follow it with the vertical cross hair until
an assistant reading the watch calls the time of culmination. The hori-
zontal angle is the desired azimuth from the north.

EXAMPLE:

(a) Transit is set up before lower culmination on June 1, 1918. From
a table of culmination of Polaris, the local mean time of lower culmina-
tion is 8h 51m 18s P. M. for longitude 90° W. For longitude 105° 32' 33" W.
the local mean time would be (0.16m earlier for each 15°) 8h 51m 8s P. M.
The longitude between the local meridian and the standard meridian
(105°) is 32' 33", which expressed in units of time (15°=lh)=2m 10s.
Standard time = 8h 51m 8s + 2tii 10s = 8h 53m 18s.

(b) The horizontal angle at 8h 53m 18s P. M. is 88° 16'. Hence the
desired bearing is N. 88° 16' W.

5. By Observing Polaris at Any Hour Angle.

(a) Set up transit, at any time when Polaris is visible, over one end
of the line whose azimuth is desired. Sight along the line with the ver-
niers set at 0°. With the lower clamp tightened and the upper clamp
loosened observe the star.

(b) Focus on the star and follow it with the intersection of the ver-
tical and the middle horizontal cross hairs. Take a series of readings
and record the time, horizontal angle, and vertical angle for each obser-
vation. Determine the index error of the transit if necespary. If the
instrument is not in perfect adjustment, make the observations in pairs,
with telescope direct and inverted, and average the two sets of angles,
and determine the mean time.

(c) The azimuth may be computed by the following formulae:

sin % hour p»gi. - J ^^^^ Ccoalt -j- lat - dec) sin 1/2 (coalt - lat + dec)
\ cos lat cos dec

. , sin hour angle

and tan azimuth = r~r~L ^ , — 7~z z 7—

cos lat tan dec — sin lat cos hour angle

^

COLORADO SCHOOL OF MINES QUARTERLY. 13

EXAMPLE:

Transit is set up at 8:30 P. M., June 27, 1918. Observations are made
from 8:40 P. M. to 9:20 P. M. At 9:00 P. M. standard time in longitude
105° 32' 33" W., the observed horizontal angle Was 88° 56', and the ob-
served vertical angle was 38° 45'. The refraction correction is 1' 12".
Hence the true altitude is 38° 45' — 1' 12" = 38° 43' 48".
Coaltitude = 90° — 38° 43' 48" = 51° 16' 12"
Latitude = N. 39° 44' 45"

Declination = 90° — 1° 8' 3" = 88° 51' 57" (Refer to table of polar
distances or declinations of Polaris)
Computation for hour angle:

VaCcoalt + lat — dec)= 1° 4' 30"! log sin = 8.2732604
Vg (coalt — lat + dec) = 50° 11' 42". log sin = 9 . 8854899

colog cos lat = 0.1141368
colog cos dec = 1.7034741

2) 9.9763612

log sin Vz. hour angle = 9.9881806

lA hour angle = 76° 41' 36"
hour angle = 153° 23' 12"

Computation for azimuth;

log cos lat = 9.8858632
log tan dec = 1.7002091

log sin hour angle ^9. 6512462

1.5860723 =log 38.55426

log sin lat = 9.8057611
log cos hr =9.9513618

9.7571229 = log .57164

log 37.98262 =1.5795849

log tan • azimuth =8.0717613

azimuth east of meridian = 0° 40' 33"

horizontal angle to star = ^° 56' 0"

horizontal angle to pole =88° 15' 27"
Bearing of line =N. 88° 15' 27" W

Note: Culminations of Polaris for latitude, or elongations of Polaris
for azimuth, may be observed without knowledge of the time if advan-
tage is ta,ken of the fact that Zeta Ursa Majoris (the star at the bend in
the dipper handle), the north pole, Polaris, and Delta Cassiopeiae (the
star at the bottom of the first stroke of the W) are nearly in a straight
line, with Polaris between the pole and Delta Cassiopeiae. When this
line is horizontal Polaris is at elongation, and when the line is vertical
Polaris is at culmination, the elongation or culmination being in the direc-
tion towards Delta Cassiopeiae.

t

n

W. F. ROBINSON PTO. CO., DENVER

f

^^WMcrsitylj^ Toronto
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