Table 8
Image noise properties for small and natural output pixel sizes.
| Unit: Jy | Small pix | Natural pix | Error ratio | ||
| Image | σ sky |
|
σ sky |
|
|
|
|
|||||
| HIP 103389 70 | 3.32e-03 | 1.02e-03 | 3.84e-03 | 2.31e-03 | 1.01 |
| HIP 103389 100 | 2.02e-03 | 3.62e-04 | 1.50e-03 | 8.64e-04 | 1.06 |
| HIP 107350 100 | 1.34e-03 | 3.42e-04 | 1.46e-03 | 8.73e-04 | 1.14 |
| HIP 114948 100 | 1.23e-03 | 3.48e-04 | 1.01e-03 | 8.18e-04 | 1.05 |
| HIP 103389 160 a | 1.08e-02 | 2.48e-03 | 6.18e-03 | 6.42e-03 | 1.23 |
| HIP 103389 160 b | 3.15e-03 | 1.17e-03 | 3.32e-03 | 2.94e-03 | 1.19 |
| HIP 107350 160 | 5.76e-03 | 1.07e-03 | 4.40e-03 | 2.68e-03 | 1.19 |
| HIP 114948 160 | 4.11e-03 | 1.18e-03 | 3.56e-03 | 3.11e-03 | 1.25 |
Notes.σsky and
σpix have been estimated for several fields using
clean square areas of 22″ and 44″ sizes at 100 and 160 μm,
respectively. The number after the stellar Hipparcos catalogue number is
the wavelength: 70, 100 and 160 μm. Two different 160
μm images were available for HIP 103389. The correlated noise is
clearly revealed by σsky being always larger than
for the small output pixels. The correlated factors included in PIC-ME-TN-037 have
been used to compute the error ratios 
.
The ratios are always close to 1.0, which means that the factors in PIC-ME-TN-037
account for the difference in correlated noise between the natural and standard
output pixel sizes. See text and Table 9 for
more details on the correlated noise factor for natural output pixel sizes.
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