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it follows that if a certain magnitude of effect is observed when the telescope points in a given direction, exactly the same effect will be obtained when the interferometer has been rotated 180° and the telescope points in the opposite direction. The interferometer observations determine the line in which the motion takes place but do not distinguish between the plus and minus directions of the motion in this line; the choice between the plus sign, northward, and the minus sign, southward, must be determined from the consistency of the result when this motion is combined with the known orbital motion of the earth. For simplicity in the presentation of the formulae, they will be given for an apex having a north declination and for an observatory located in the northern hemisphere. If the final solution requires a motion to the southward, the new apex will be diametrically opposite the one first determined; its right ascension will be the right ascension of the first apex minus 12 hours and its declination will have the same numerical value as that for the first apex but with the minus sign. For an observatory located in the southern hemisphere there would be certain systematic differences in the formulae which need not be given here. The apex of the absolute motion determined from the magnitude of the ether-drift effect It is shown in the paper by Nassau and Morse, what is also evident from a study of the model, Fig. 17, that the sidereal time, when the component of motion in the plane of the interferometer is a minimum, θ α = θ It is evident that the component of motion in the plane of the interferometer is υ = V sin z, V being the velocity of the absolute motion and z the zenith distance of its apex. If δ ≥ 90° – φ, it may be seen from the model that the minimum value of v occurs when z is equal to δ – φ, that its maximum value occurs when z is equal to 180° – (δ +φ) and that the maximum and minimum values occur at times separated by twelve sidereal hours. If the observations cover the entire sidereal day, the maximum and minimum effects may be obtained. Let R be the ratio of minimum to maximum observed velocities; then R = v from which the declination of the apex of the absolute motion is derived: tan δ = [(1 +R) / (l – R)] tan φ. If δ < 90° — φ, the line of motion will coincide with the plane of the interferometer twice in each day and the maximum observed velocity, v v and ## δ = φ ± sin
| As the azimuth of the effect in the interferometer, which corresponds to the azimuth of the apex, oscillates across the meridian, it reaches a maximum displacement, first to the east and then to the west in each sidereal day. When δ ≥ φ, this maximum azimuth may be treated as the azimuth of a circumpolar star at its eastern or western elongation. It is shown in treatises on spherical and practical astronomy that the azimuth of elongation depends in a very simple way upon the declination of the star and upon the latitude of the observatory. The relation is: sin Amax = cos δ /cos φ, whence cos δ = sin A When δ ≤ φ, the azimuth of the apex swings completely around the horizon in a sidereal day. If θ tan δ = tan φ cos (θ Presuming that the orbital velocity of the earth is known, the formulae now provided are sufficient for the determination in general of the apex and velocity of the absolute motion of the earth, from observations of the relative motion of the earth and ether as made with the interferometer. These observations, giving simply the maximum displacement of the interference fringes as the apparatus turns on its axis, together with the azimuth at which this maximum displacement occurs, must adequately cover the period of one sidereal day for a given epoch. A complete set of such observations gives one determination of the velocity of the absolute motion and two independent determinations of the apex of the motion. The determination of the direction of the earth’s absolute motion is dependent only upon the direction in which the telescope points when the observed displacement of the fringes is a maximum; it is in no way dependent upon the amount of this displacement nor upon the adjustment of the fringes to any particular width or zero position. The actual velocity of the earth’s motion is determined by the amplitude of the periodic displacement, which is proportional to the square of the relative velocity of the earth and the ether and to the length of the light path in the interferometer. The two effects, magnitude and azimuth of observed relative motion, are quite independent of each other. Harmonic analysis of the fringe displacements The records of the actual interferometer observations for the Mount Wilson cycle consist of three hundred and sixteen pages of readings of the positions of the interference fringes, of the form shown in Fig. 8. Each set contains readings for twenty or more turns of the interferometer. The twenty or more readings for each of the sixteen observed azimuths are averaged and the averages are compensated for the slow linear shift of the whole interference system during the period of observation, as explained previously in connection with Fig. 9. The average readings for each set are then plotted on coordinate paper, to a large scale, for the purpose of harmonic analysis. The graphs, I, II, III, and IV, Fig. 21, show the readings for four successive sets of observations made on April 2, 1925. The plotted points are positions of the central black fringe of the interference pattern with respect to the fiducial point, as the interferometer makes one complete turn. The unit for the scale of ordinates is one-hundredth of a fringe width, while the abscissae correspond to azimuth intervals of 22 |