Results

The sky region of the observations is shown in Figure 1, where the horizontal axis denotes the A — As between 90° and 120°, and the vertical axis means the (3 between 0° and 20°. It was expected that the dust trails appear in 6°</?<ll° (150< pixels <275), as shown by the solid line in Figure 1. After removing other contributions to the sky brightness from the observed raw data, the zodiacal light was extracted by using the same method as described in [2]. Then we used Fourier filtering to enhance the structure with an angular scale between 0.7° and 5°. This filtering process removes the large scale structure like the smooth component of the zodiacal light.

We have performed the scan of signals along the line perpendicular to the orbit of Phaethon, and in order to enhance the significance of the signals, we summed up the scan results of brightness along the line parallel to the orbit (see Figure 2). In Figure 2, the horizontal axis denotes the separation distance from the orbit of Phaethon, and the vertical axis means the averaged brightness over the Fourier-filtered image from Figure 1. No significant enhancement of brightness larger that 1 S\[email protected] appears near the orbit of Phaethon. The scattering of the resulting data may be caused by noise, with a magnitude of about O.6S'io0.

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