The basic equation we need is for the effect of a plane linear gravitational wave on a beam of light. Suppose the angle between the direction of the beam and the direction of the plane wave is . We imagine a very simple experiment in which the light beam originates at a clock, whose proper time is called , and is received by a clock, whose proper time is . The beam and gravitational-wave travel directions determine a plane, and we denote the polarization component of the gravitational wave that acts in this plane by , as measured at the location of the originating clock. The proper distance between the clocks, in the absence of the wave, is . If the originating clock puts timestamps onto the light beam, then the receiving clock can measure the rate of arrival of the timestamps. If there is no gravitational wave, and if the clocks are ideal, then the rate will be constant, which can be normalized to unity. The effect of the gravitational wave is to change the arrival rate as a function of the emission rate by
In order to use such an arrangement to detect gravitational waves, one needs two very stable clocks. The best clocks today are stable to a few parts in 1016 , which implies that the minimum amplitude of gravitational waves that could be detected by such a two-clock experiment is . However, this equation is also fundamental to the detection of gravitational waves by pulsar timing, in which the originating ‘clock’ is a pulsar. By correlating many pulsar signals, one can beat down the single-pulsar noise. This is described below in Section 4.4.2.
An arrangement that uses only one clock is one that sends a beam out to a receiver, which then reflects or retransmits (transponds) the beam back to the sender. The sender has the clock, which measures variations in the round-trip time. This method has been used with interplanetary spacecraft, which has the advantage that the only clock is on the ground, which can be made more stable than one carried in a spacecraft (see Section 4.4.1). For the same arrangement as above, the return time varies at the ratethree-term relation, the third term being the wave strength at the time the beam returns back to the sender.
But the sensitivity of such a one-path system as a gravitational wave detector is still limited by the stability of the clock. For that reason, interferometers have become the most sensitive beam detectors: effectively one arm of the interferometer becomes the ‘clock’, or at least the time standard, that variations in the other arm are compared to. Of course, if both arms are affected by a gravitational wave in the same way, then the interferometer will not see the wave. But this happens only in very special geometries. For most wave arrival directions and polarizations, the arms are affected differently, and a simple interferometer measures the difference between the round-trip travel time variations in the two arms. For the triangular space array LISA, the measured signal is somewhat more complex (see Section 4.4.3 below), but it still preserves the principle that the time reference for one arm is a combination of the others.
Ground-based interferometers are the most sensitive detectors operating today, and are likely to make the first direct detections . The largest detectors operating today are the LIGO detectors , two of which have arm lengths of 4 km. This is much smaller than the wavelength of the gravitational wave, so the interaction of one arm with a gravitational wave can be well approximated by the small- approximation to Equation (43), namely for first corrections to the short-arm approximation.) To analyze the full detector, where the second arm will normally point out of the plane we have been working in up till now, it is helpful to go over to a tensorial expression, independent of special coordinate orientations. The gravitational wave will act in the plane transverse to the propagation direction; let us call that direction and let us set up radiation basis vectors and in the transverse plane, such that lies in the plane formed by the wave propagation direction and the arm of our gravitational wave sensor, which lies along the -axis of the detector plane, whose unit vector is . (For a picture of this geometry, see the left-hand panel of Figure 3, where for the moment we are ignoring the -arm of the detector shown there.)
With these definitions, the wave amplitude is the one that has and as the axes of its ellipse. The full wave amplitude is described, as in Equation (6), by the wave tensor
. The interferometer responds to the difference between these times,
. By analogy with the wave tensor, we define the detector tensor by 
It is conventional to re-express this measurable in terms of the stretching of the arms of the interferometer. Within our approximation that the arms are shorter than a wavelength, this makes sense: it is possible to define a local inertial coordinate system that covers the entire interferometer, and within this coordinate patch (where light travels at speed 1) time differences measure proper length differences. The differential return time is twice the differential length change of the arms:
For a bar detector of length lying along the director , the detector tensor is
When dealing with observations by more than one detector, it is not convenient to tie the alignment of the basis vectors in the sky plane with those in the detector frame, as we have done in the left-hand panel of Figure 3, since the detectors will have different orientations. Instead it will usually be more convenient to choose polarization tensors in the sky plane according to some universal reference, e.g., using a convenient astronomical reference frame. The right-hand panel of Figure 3 shows the general situation, where the basis vectors and are rotated by an angle from the basis used in the left-hand panel. The polarization tensors on this new basis,
Then one can write Equation (51) asantenna pattern functions for the two polarizations defined on the sky-plane basis by
These are the antenna-pattern response functions of the interferometer to the two polarizations of the wave as defined in the sky plane . If one wants the antenna pattern referred to the detector’s own axes, then one just sets . If the arms of the interferometer are not perpendicular to each other, then one defines the detector-plane coordinates and in such a way that the bisector of the angle between the arms lies along the bisector of the angle between the coordinate axes . Note that the maximum value of either or is 1.
The corresponding antenna-pattern functions of a bar detector whose longitudinal axis is aligned along the direction, are
Any one detector cannot directly measure both independent polarizations of a gravitational wave at the same time, but responds rather to a linear combination of the two that depends on the geometry of the detector and source direction. If the wave lasts only a short time, then the responses of three widely-separated detectors, together with two independent differences in arrival times among them, are, in principle, sufficient to fully reconstruct the source location and gravitational wave polarization. A long-lived wave will change its location in the antenna pattern as the detector moves, and it will also be frequency modulated by the motion of the detector; these effects are in principle sufficient to determine the location of the source and the polarization of the wave.
Since the polarization angle of an incoming gravitational wave would generally be expected to be unrelated to its direction of arrival, depending rather on the internal orientations in the source, it is useful to characterize the directional sensitivity of a detector by averaging over the polarization angle . If the wave has a given amplitude and is linearly polarized, then, if we are interested in a single detector’s response, it is always possible to align the polarization angle in the sky plane with that of the wave, so that the wave has pure -polarization. Then the rms response function of the detector isantenna pattern. For a resonant bar, the antenna pattern is
The polarization amplitudes of the radiation from an inspiraling binary, a rotating neutron star, or a ringing black hole, take a simple form as follows:
where is an overall (possibly time-dependent) amplitude, is the signal’s phase and is the angle made by the characteristic direction in the source (e.g., the orbital or the spin angular momentum) with the line of sight. In this case, the response takes a particularly simple form:
Note that , just as , takes values in the range [0, 1]. In this case the average response has to be worked out by considering all possible sky locations, polarizations (which drops out of the calculation) and source orientations. More precisely, the rms response is
The right-hand panel of Figure 4 shows the percentage area of the sky over which the antenna pattern of an interferometric detector is larger than a certain fraction of the peak value. The response is better than the rms value over 40% of the sky, implying that gravitational wave detectors are fairly omni-directional. In comparison, the sky coverage of most conventional telescopes (radio, infrared, optical, etc.) is a tiny fraction of the area of the sky.
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