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Figure 1: The ux density distribution of confusing sources in the IDV sample
for 1.4 GHz. Smax is the maximum ux density in a confusing source. N
corresponds to the number of confusing sources detected in 101 images of the
IDV sample target sources (no beam shape correction applied).
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(a) 2.4 GHz (b) 4.8 GHz
Figure 2: The number distribution of modulation indices,  of the total ux den-
sity calculated over the duration of each observing run: May 1994 and August
1994. The distributions of  are shown for (a) 2.4 GHz and (b) 4.8 GHz. The
distribution for November are signicantly broader than for May and August.
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Figure 3: Distribution of the fractional linear polarization averaged over a du-
ration of each observing session (May and August 1994) for all sources in the
sample.
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Figure 4: Upper panel: the number distribution of instantaneous spectral indices
 4:8
2:4
of all sources for May 1994 (full line) and August 1994 (dashed line). Middle
panel: the number distribution of the spectral indices  5:0
2:7
calculated from the
ux densities provided in the Parkes catalogue. Lower panel: The scatter plot
of Parkes spectral indices  5:0
2:7
versus instantaneous spectral indices  4:8
2:4
of all
sources for May 1994 (dots) and August 1994 (triangles).
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(a) (b)
(c) (d)
(e) (f)
Figure 5: A comparison of ux densities measured at dierent times between
days and decades. (a) and (b) show the scatter between the mean ux densi-
ties measured one day apart with the ATCA at 2.4 and 4.8 GHz respectively,
triangles correspond to August 1994 data, dots are May 1994 data (c) and (d)
are the scatter plots of average ux densities measured 3 months apart with
the ATCA, (e) and (f) show ux densities measured with ATCA in May 1994
versus ux densities listed in the Parkes catalogue.
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Figure 6: The distribution of modulation indices calculated over 72 hours. The
distributions are combined over two observing sessions, May and August 1994
for all frequencies.
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(a) (b)
(c) (d)
(e) (f)
Figure 7: Distribution of the fractional dierence in average ux density between
two observing sessions in May and August 1994. Left panels: the data for
the point sources in the Survey sample. Right panels: only IDV sources from
table ?? are included.
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Figure 8: The number distribution of the rms in polarized ux densities at 8.6,
4.8 and 2.3 GHz from top to bottom.
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(a) (b)
(c) (d)
(e) (f)
(g) (h)
Figure 9: Distribution of day-to-day dierences in polarized ux densities. Fig-
ures (a), (c), (e) and (g) show May 1994 data for 8.6, 4.8, 2.4 and 1.4 GHz
respectively. Figures (b), (d), (f) and (h) show August 1994 data for frequen-
cies in the same order.
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(a) 1.4 GHz (b) 2.4 GHz
(c) 4.8 GHz (d) 8.6 GHz
Figure 10: The scatter plot of average polarized ux density in May versus
August 1994
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(a)
(b)
Figure 11: Distribution in respect to Galactic plane, of the IDV sources which
show the peak of variability at given frequency (a) as compared with the distri-
bution of the whole sample in Galactic coordinates (b). Data points are shown
for May 1994. The total number of sources at dierent frequencies varies, only
sources satisfying 'pointlikeness' criteria (see Table ??) were included. The 1.4
GHz data is not included here due to the larger uncertainties in ux density
measurements. The thick curve shows the limits of the Survey, ф = +10 ф .
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(a) IDV sources (b) Whole sample
Figure 12: Redshift distribution of IDV sources compared with the whole sam-
ple. Sources with unknown redshift were excluded.
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