MIPS : Sensitivity

Point Source Sensitivity for MIPS Scan AOT

• For the three scan rates shown, the individual points are located at the effective integration times for 1, 2, 3, 4, .... scans over the same point at 24 and 70 microns. These integration times are "on-source," such that they equal the total time any sky location spends on the 24 and 70 micron arrays during one or more scans (figure).

• Because the 160 micron array does not sample the sky multiple times during a single scan (figure), the "integration" times shown for the 160 micron band are those achieved in 2, 4, 6, 8, .... scan passes at the fast rate, and in 1, 2, 3, 4, ... passes at the slow and medium rates. To achieve full sampling of the scan track at the fast scan rate, two scans at 160 microns must be made (see the MIPS Observing Mode Descriptions).

• With the frame overlap in a scan leg (see figure; or without, in the case of the 160 micron array, see figure), the three scan rates result in integration times per point on the sky in one scan leg (24 and 70 microns/160 microns) of 100/10 seconds (slow), 40/4 seconds (medium), and 15/3 seconds (fast; 160 micron fully is fully sampled in two scan legs at the fast rate). The implementation of the 160 micron reset interval is not final. See the Spitzer Observer's Manual for full details of the MIPS Scan Map AOT.

• Background point source confusion is a function of the location on the sky. The confusion limits shown should be considered optimistic lower limits. See note on confusion limits here.

Scan Map Sensitivities:

Low Background:

24 micron
70 micron
160 micron

Medium Background:

24 micron
70 micron
160 micron

High Background:

24 micron
70 micron
160 micron

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