To determine the altitude and azimuth of a celestial body, we could make calculations by using mathematical formulae; we could compute them with the aid of sight reduction tables; we could use star globes and star charts or we could use computer software. However, all of these procedures only tell us what the altitude and azimuth of the chosen body would be at our assumed position which is only an approximate position. The only way that we can determine the altitude and azimuth of a celestial body at our true position is by making accurate measurements with a sextant and an azimuth-compass or similar equipment. However, before we can do this, we must obviously be able to locate the body in the sky.

The ‘Where To Look’ Method enables us to quickly and easily calculate which stars and planets will be above our horizon at the time that we wish to make a ‘fix’. It is quite a useful method, especially in the cramped confines of a chart-table, in a rough sea.

It is emphasised that this is not intended to be a method of accurately pin-pointing the position of a star or planet but a simple and quick method of establishing whether or not the body is likely to be visible at the time an observation is required and if so, what its approximate position will be in the sky.

The following extract is taken from ‘Astronomy for Astro Navigation’ which is a companion book to ‘Astro Navigation Demystified’.

** ****Method. **To find if a star or planet will be above the horizon at our position at the time of the planned observations, we need to take two things into account, its local hour angle and its declination.

** ****Local Hour Angle (LHA).** For a star or planet to be visible, its meridian must be within 90^{o} east or west of our estimated longitude at the time of the planned observations.

- If a body’s LHA is greater than 0
^{o }and less than 90^{o }or if LHA is greater than 360^{o}and LHA – 360^{o}is less than 90^{o}then body will be above the western celestial horizon. - If a body’s LHA is greater than 270
^{o }but less than 360^{o }then 360^{o}– LHA will be less than 90^{o}and the body will be above the eastern horizon.

We can formulate the above statements as follows:

Body is above western horizon if: LHA = 0^{o} TO 90^{o }or LHA – 360^{o} = 0^{o} TO 90^{o}

Body is above eastern horizon if: LHA = 270^{o} to 360^{o} or 360^{o} – LHA = 0^{o} TO 90^{o}

In the following example, we have plotted the positions of stars X and Y in terms of their LHA and declination which are as follows:

Star X: LHA 22^{o}, Dec. 65^{o}N Star Y: LHA 295^{o}E, Dec. 20^{o}N.

Point O is the position of an observer on the Earth’s surface at latitude 50^{o}N.

NS is the meridian of the observer and in terms of LHA is 0^{o}.

WE is the celestial equator.

The limits of the observer’s western and eastern horizons are at LHA 90^{o} and LHA 270^{o} which are both 90^{o} from the observer’s meridian.

Since the LHAs of these bodies is either less than 90^{o} or greater 270^{o}, they will be visible above the horizon.

Bodies whose LHAs are greater than 90^{o} but less than 270^{o} would be below the celestial horizon and therefore would not be visible.

**To Calculate Azimuth**. Once we have ascertained the LHA and declination of a celestial body, we can make a rough approximation of the azimuth by plotting the LHA and declination in relation to the observer’s assumed position on the azimuth diagram.

If we join the positions of X and Y to the position of the observer, we will see that the approximate azimuths are as follows:

X: Approximate Azimuth = N30^{o}W Y : Approximate Azimuth = N110^{o}E

The full procedures for making these calculations is shown in detail in the books Astronomy for Astro Navigation and Astro Navigation Demystified.

**Declination. **To ascertain whether or not a celestial body will be above the horizon, we have to take into account its declination as well as its LHA. To be visible above the horizon, its declination must be within 90^{o} of the latitude of our position. If our latitude is north, then the declination must be within the range 90^{o} north to (90^{o} – latitude) south. If the latitude is south, then the declination must be within the range 90^{o} south to (90^{o} – latitude) north.We can formulate the above statements as follows:

Latitude North: visible range = 90^{o}N to (90^{o} – Lat)S.

Latitude South: visible range = 90^{o}S to (90^{o} – Lat)N.

We can explain the reason for this rule with the aid of another diagram which shows the declinations of the celestial bodies X, Y together with a third body, planet V. Please note that the diagram is for illustrative purposes only; for this reason, it is not drawn to scale and angles are not drawn accurately.

**Summary of data relating to stars X and Y and planet V which are represented in the diagram:**

Assumed Position of observer: Lat. 50^{o}N Long. 135^{o}W

Star X: Declination = 65^{o}N LHA = 22^{o}

Star Y: Declination = 20^{o}N LHA = 295^{o}

Planet V: Declination = 10^{o}S LHA = 190^{o}

O is the position of the observer at latitude 50^{o}N and Z is the zenith at that position.

The line PQ forms part of the visual horizon at point O and is tangential to the circumference of the Earth.

C is the centre of the Earth and the line CZ is perpendicular the visual horizon.

The line ACB is the celestial horizon which is perpendicular to CZ and therefore horizontal to the visual horizon.

The celestial horizon will cut the circumference of the Earth at latitudes that are 90^{o} to the north and to the south of the observer’s latitude (in this example, latitude 40^{o}N and latitude 40^{o}S).

##### X is the position of the star X in the celestial sphere and X_{1} is its geographical position on the Earth’s surface.

Y is the position of the star Y in the celestial sphere and Y_{1} is its geographical position.

V is the position of planet V in the celestial sphere and V_{1} is its geographical position.

The diagram shows that although the geographical positions of X and Y are below the visible horizon and therefore out of sight to the observer, the bodies themselves are above the celestial horizon and therefore since they are within the limits for LHA and declination, they will be visible above the horizon at the observer’s assumed position.

The diagram also shows that V would have been above the celestial horizon but for one thing. Because its LHA is 190^{o} which is greater than 90^{o} but less than 270^{o}, it is outside the LHA limits and therefore will not be above the horizon.

**Estimating Approximate Altitude. **This method enables us to calculate the approximate altitude of a celestial body when it lies over the meridian of the observer; in other words when LHA equals 0^{o} or 360^{o}. When the LHA of a body is greater than 0/360 (i.e. when it is not over the observer’s meridian) adjustments have to be made to the calculated altitude.

**Calculating the Altitude of Stars X and Y and planet V at noon. **We can modify the previous diagram to help us with these calculations.

**Relevant Data:**

Latitude of observer’s assumed position = 50^{o}N

Star X: Declination = 65^{o}N

Star Y: Declination = 20^{o}N

Planet V: Declination = 10^{o}S

In the diagram, Angle ACN is the angle between the Celestial Horizon and the direction of North and NCX is the angle between the direction of North and the direction of X. Angle ACX is equal to the sum of these angles and represents the altitude of X which is 85^{o}.

Angle BCE is the angle between the Celestial Horizon and the Celestial Equator and ECY is the angle between the direction of East and the direction of Y. BCY is equal to the sum of these angles and represents the altitude of Y which is 60^{o}.

Angle BCV is equal to angle BCE minus the declination of V and represents the altitude of planet V which is 30^{o}. However, as discussed earlier, V would not be visible because it is outside the limits for LHA.

** ****Summary.**

**Altitude X = 85**^{o}

**Altitude Y = 60**^{o}

**Altitude V = 30**^{o}

With a little practice, it will become an easy task to estimate the azimuth and altitude of a body without the aid of diagrams.

**Calculating altitude when LHA is not zero.** We must remember that the altitudes we have calculated above would apply when the celestial bodies are over the observer’s meridian (i.e. when LHA is 0^{o}). Therefore, when the LHA is other than 0^{o}, we have to re-calculate the altitude.

The altitude of a celestial body is 0^{o} when it rises at LHA 270^{o} and increases to its maximum when LHA is 360^{o}/ 0^{o} before descending again to 0^{o} when it reaches LHA 90^{o}

**Re-calculation of altitude of star X for LHA 22**^{o}:

The diagram above shows that the altitude of star X is 85^{o}.

Therefore, Altitude = 85^{o} when LHA = 360^{o}

But Altitude = 0^{o} when LHA = 270^{o}

Thus 90^{o} worth of LHA = 85^{o} of altitude

But LHA = 22^{o}

Therefore, 22^{o} of LHA = (85 / 90) x 22 = 20.7^{o} of altitude.

Therefore, when LHA X = 22^{o}, altitude = 85 ^{o}– 20.7^{o} = 64.3^{o}

**Therefore Estimated altitude of X when LHA is 22**^{o} = 64.3^{o}.

**Re-calculation of Altitude of star Y for LHA 80**^{o}:

The diagram shows that the altitude of star Y is 60^{o}.

Therefore, Altitude = 60^{o} when LHA = 360^{o}

But Altitude = 0^{o} when LHA = 270^{o}

Therefore 90^{o} worth of LHA = 60^{o} of altitude

But LHA = 280^{o }= 80^{o} E.

Therefore 80^{o} of LHA = (60 / 90) x 80 = 53.3^{o} of altitude.

Therefore, when LHA = 80^{o}, altitude = 60^{o }– 53.3^{o} = 6.7^{o}

**Therefore, Estimated altitude of Y when LHA is 80**^{o} = 6.7^{o}.

We cannot make a recalculation for planet V because its LHA is outside LHA limits.

Of course we cannot find an accurate solution to a spherical problem with straight-line, two dimensional, drawings such as these which do not take account of phenomena such as refraction and parallax or the fact that the Earth is not a perfect sphere. However, this method does give us a good idea where to look in the sky for a celestial body that we have selected to use for an accurate position fix.

It is also stressed that the drawings above are for illustrative purposes only, are not drawn to scale and that angles are not accurately drawn.

The procedures for making these calculations are shown in detail in the companion books Astronomy for Astro Navigation and Astro Navigation Demystified.

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