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un:radio-inter [2024/09/08 22:39] – [1.2 Correlation interferometer] asad | un:radio-inter [2024/09/08 23:26] (current) – [1.2 Correlation interferometer] asad | ||
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which can be reduced to only a fringe (interferential) term | which can be reduced to only a fringe (interferential) term | ||
- | $$ R_{AB}(\tau) = \frac{1}{2} \langle V_AV_B\cos\omega\tau. \rangle $$ | + | $$ R_{AB}(\tau) = \frac{1}{2} \langle V_AV_B\cos\omega\tau \rangle $$ |
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+ | where the total-power terms are absent, unlike the equation for the adding interferometer, | ||
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+ | {{: | ||
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+ | The dotted and dashed curves represent two signals (detected by two antennas) phase-shifted with respect to each other, the solid curve shows their multiplication and the solid line the corresponding time-average. As the direction toward the source changes (due to the rotation of the earth), $\tau$ changes and so does the relative phase. At the top phase shift is close to zero, in the middle it becomes $90^\circ$, and at the bottom $180^\circ$. The //fringe amplitude// varies from $+0.5$ to $-0.5$. One cycle of the RF phase shift corresponds to one //fringe cycle//. | ||
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+ | {{: | ||
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+ | Here you see the fringe oscillations (cycles) for a point source located on the celestial equator observed by a two-element interferometer lying along the terrestrial equator creating a 15-$\lambda$ long east-west baseline. | ||
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+ | The fringes oscillate around a zero mean and there are exactly 15 maxima on each side of the center, where $\theta=0^\circ$. The fringes near the center are more sinusoidal because there the small-angle approximation ($\sin\theta=\theta$) is more applicable. As $b_\lambda=15$, |
un/radio-inter.1725856766.txt.gz · Last modified: 2024/09/08 22:39 by asad