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STANDARD - Survey Instrument Antique Center!

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look around it by moving the eye around it in such a manner as to see the entire circumference,<br />

and bring the cross-wires on the four sides of the image normal to their<br />

respective sides, by means of the motion hi azimuth and the motion of the solar<br />

telescope, as above described. This being attained, the optical axis of the main telescope<br />

should be in the astronomical meridian. Refer to an azimuth mark, and repeat<br />

the operation. The above is called a direct observation.<br />

(h.) To make a reverse observation. Having made the direct observation, turn the<br />

whole instrument 180 in azimuth, and set the co-latitude off on the opposite side<br />

of the vertical arc. Also turn the solar telescope 180 , and proceed as before. The<br />

object of repetition is to eliminate personal non-precision and nossible errors in<br />

manipulation, while the object of reversing is to eliminate any possible remaining<br />

errors of adjustment of the instrument. The prudent surveyor will not trust his work<br />

without such verification, and he will take the mean of both observations.<br />

Remarks.<br />

(1.) To unscrew the solar attachment from the packing-piece in the box, first<br />

release the clamp and tangent screw, and then turn carefully the milled-edged disk or<br />

base plate a few turns to the left. To screw the solar attachment to the instrument,<br />

turn this milled-edged disk from left to right around the screw on top of the main<br />

telescope without revolving the solar attachment. To insure a perfect contact of<br />

screw-shoulder against the flange, on which depends the permanency of the adjustment<br />

of the polar axis to the main telescope, it is necessary that these parts be free<br />

from dust, grit, or dirt of any kind.<br />

(2.) The auxiliary or latitude level, if one is ordered, attaches in the same manner<br />

to the end of the cross axis on the side of the vertical circle.<br />

(3.) The latitude level is used to facilitate during repeated observations the resetting<br />

of the polar axis to the co-latitude, assuming that the polar axis has been previously<br />

set to be at right angles to the main telescope by its milled capstan-headed<br />

screws and the solar level, the polar axis being placed in its position for an observation<br />

with more facility and precision with this level than by reading the vertical arc.<br />

(6.) The latitude having been found for the initial point of a survey, it may be<br />

found for other points within moderate limits by allowing 92 chains of northing or<br />

southing for 1' of latitude.<br />

(7.) The object of bringing the main telescope into the meridian by means of<br />

motion on the outer spindle is to have the zero line of the horizontal plate hi the<br />

meridian, so that the azimuth or bearing of lines can be referred to that line.<br />

(8.) If for any cause one is obliged to work with an uncertain latitude, it is better<br />

c<br />

to so with the sun as far from the meridian as practicable, for the following<br />

8<br />

to dc<br />

reasons :<br />

It is only when the sun is in the pole of the meridian that it has its maximum<br />

efficiency in pointing out the direction of the meridian.<br />

Hence a large hour-angle, and a small declination, are conducive to the elimination<br />

of errors resulting from an incorrect latitude.<br />

Indeed, with the sun precisely in the pole of the meridian, the meridian is determined<br />

independently of latitude.<br />

(9.) In making the several adjustments, or rather in verifying them, the student<br />

should have a true meridian established by some other means than by the " solar<br />

transit," as from the North Star, by some of the methods given in works on surveying.<br />

He should compare the results of his observations with this meridian at different<br />

times in the day, and under different states of the atmosphere, till he has learned any<br />

peculiarity of the instrument and the utmost precision obtainable with it, as well as the<br />

ordinary limit of non-precision,<br />

NOTE. The great utility of this auxiliary, or level attachment, is seen in the setting ofgrades. Two of<br />

these levels being applied to the telescope of a pivot-levelling instrument one on each side or one on each<br />

nd of the cross-axis of a transit telescope, and one of them being adjusted to the up, the other to the down<br />

, the engineer may work in either direction on his grade with the same facility that he would on a level

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