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Cosmic Origins SpectrographInstrument Handbookfor Cycle 22 > Chapter 10: Bright-Object Protection > 10.4 Source V Magnitude Limits

10.4
In the following tables, the screening limits in Table 10.1 are converted into V magnitude limits for a variety of sources. These values are not meant to be a substitute for the ETC, but rather an indication of whether a given object may be near the limit. The most sensitive spectroscopic setting and lowest rate limit (global or local) determine the listed values. Stellar spectra are assumed to be unreddened. Table 10.2 corresponds to spectroscopy through the PSA, Table 10.3 through the BOA, and Table 10.4 to NUV imaging for both apertures.
0.1
1.2
3.4
4.8
0.5
0.4
0.1
0.8
1.5
1.4
0.7
0.8
2.3
3.1
1.1
2.3
4.5
0.5
5.4
3.9
2.3
3.1
5.0
1.4
7.0
5.1
3.1
1.5
4.2
1.9
1.0
1.0
3.2
1.2
0.3
0.2
0.6
2.9
1.0
Fλ ~ λ1
Fλ = const surface brightness
Fλ = const point source
 
0.1
0.3
2.5
0.4
5.6
0.7
0.6
0.7
6.7
1.6
0.6
1.2
0.8
0.8
8.8
3.7
2.4
2.0
1.4
1.0
10.2
5.0
3.6
2.5
1.7
1.1
3.6
6.1
1.9
4.3
3.1
1.5
2.3
5.9
0.6
5.2
3.6
2.0
1.2
5.6
6.4
4.7
2.7
6.9
6.9
5.2
6.3
4.8
3.1
6.1
7.8
4.4
8.7
6.9
5.1
1.3
7.6
10.0
5.9
11.1
9.7
8.2
2.2
8.5
10.5
6.8
12.6
10.9
9.0
2.8
5.1
7.0
3.4
9.7
7.7
7.0
2.8
5.4
6.5
3.7
8.8
7.0
6.4
2.3
5.6
6.1
3.8
8.6
6.8
5.2
2.6
Fλ ~ λ1
Fλ = const surface brightness
Fλ = const point source
Table 10.4: V Magnitude Bright-Object Limits for Imaging
Fλ ~ λ1
Fλ= const surface brightness
Fλ= const point source

Cosmic Origins SpectrographInstrument Handbookfor Cycle 22 > Chapter 10: Bright-Object Protection > 10.4 Source V Magnitude Limits

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