1600
1615
1630
1650
B. 1615
The standard meridian
The international date line
That of Greenwich
Both (a) and (c) of above
f/H sec θ
f sec θ/H
f/H
f/H cos ½θ
High oblique
Low oblique
Vertical
None of these
Ursa Minor's remains always north of pole star
Polar star remains always north of Polaris
Polaris remains always north of Ursa Minor's
Ursa Minor's pole star and Polaris are the names of the same star
Elevation of the elevated pole
Declination of the observer's zenith
Angular distance along the observer's meridian between equator and the observer
All the above
At east elongation
At upper culmination
At west elongation
At lower culmination
80°
70°
60°
40°
1600
1615
1630
1650
365
365.2224
365.2422
366.2422
Sidereal time
Apparent solar time
Mean solar time
All the above
March 21 to June 21
June 21 to September 21
September 21 to December 21
Both (a) and (b) of above
Positive for points above datum
Negative for points below datum
Zero for points vertically below the air station
All the above
80°
70°
60°
50°
Satellite station
Eccentric station
False station
Pivot station
Hour angle
Azimuth
Right ascension
Declination
H. f
H/f
f/H
H + f
Reduction to mean sea level
Correction for horizontal alignment
Correction for slope
All the above
1 in 12
1 in 10
1 in 8
1 in 6
Northward
Southward
From south to north of the equator
From north to south of the equator
Every angle is less than two right angles
Sum of the three angles is equal to two right angles
Sum of the three angles less than six right angles and greater than two right angles
Sum of any two sides is greater than the third
1000 km
800 km
600 km
500 km
Co-declination
Co-altitude
Co-latitude
Polar distance
Opposite corners of a photograph
Nodal points of the camera lens
Corresponding points on the ground and photograph
Plumb points of stereo pair of photographs
Standard meridian
Greenwich meridian
Equator
180° longitude
1°
2°
3°
4°
At culmination
At elongation
Neither at culmination nor at elongation
Either at culmination or at elongation
The star's movement is apparent due to the actual steady rotation of the earth about its axis
The stars move round in circular concentrated parts
The centre of the circular paths of stars is the celestial pole
All the above
h/H f tan θ
h/H f² tan θ
h/H f² sin θ
h/H f cos θ
Optical projection
Optical mechanism projection
Mechanical projection
All the above
Nadir point
Iso centre
Principal point
All the above