12. The search is not equally sensitive over the entire sky.

As described earlier, the signal from a pulsar is modulated by the Earth's rotation about its axis and its motion around the Sun. The amount and type of this modulation depends upon sky location. Because the detector's output contains instrument noise artifacts which are purely sinusoidal (for example, 60 Hz harmonics and violin modes of the optical suspension wires) this means that our search is more sensitive in some regions of the sky than in others.

Shown in the following two figures are plots which are similar to the previous figures but in the band of frequencies around the violin modes of the optical suspensions (340-350 Hz). The violin modes of the optical suspensions produce quite prominent false events. (For example, just compare the number counts in these two figures with the figures in the previous section for the 300-325 Hz frequency band.)

The all-sky map (a) shows that the violin modes produce a noisy ``belt'' on the sky. Along this belt, spectral line artifacts appear like a pulsar signal (See the next section for the reason why!). Essentially, we do not have much sensitivity to a signal in this region.

The frequency - declination plot shows that although the violin modes make a moderately large region of the sky insensitive to gravitational waves from a pulsar, the obscured region only covers a narrow range of frequency and still leaves large sensitive areas in parameter space.

Figure 12.1: Color map of the number of coincidences among sixty 10-hour data segments in the frequency range 340-350 Hz. The first harmonics of the violin modes (340-350 Hz) produce quite prominent false events. (a) All-Sky map. (b) Frequency declination plane.

(a) All-Sky map	(b) Declination - Frequency map

In the next section, we explain why sinusoidal noise sources in the instrument produce these characteristic patterns (great circles) on the Celestial Sphere.

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Einstein@Home S3 Analysis Summary	Last Revised: 2005.09.11 16:22:17 UTC
Copyright © 2005 Bruce Allen for the LIGO Scientific Collaboration	Document version: 1.97