As described in MAMA Bright-Object Limits, the MAMA's are subject to absolute brightness limits, above which sources cannot be observed or they would potentially damage the detectors. In Table 14.38,we present the complete set of bright object point source and integrated magnitude screening limits for the MAMA imaging modes. These screening magnitudes are presented as a guide. Whether or not an individual source can be observed is determined by whether the desired configuration and the spectrum of that source is predicted to exceed the global and local absolute observing count rate limits, as described in Chapter 7. Remember, sources cannot be observed in configurations where they exceed the absolute bright object limits. The information presented here should be used in conjunction with the material presented in Chapter 7.
A few important points to note.
| Spectral Type |
FUV-MAMA |
NUV-MAMA |
|||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|
| 25MAMA (clear) |
F25SRF2 (longpass) |
F25QTZ (longpass) |
F25LYA (Ly  ) |
25MAMA (clear) |
F25SRF2 longpass |
F25QTZ longpass |
F25CIII (CIII) |
F25CN182 (182 cont) |
F25CN270 (270 cont) |
F25MGII (MgII) |
|
| Surface Brightness1 |
1.4x10-12 |
3.1x10-12 |
6.0x10-12 |
5.6x10-11 |
3.1x10-13 |
3.9x10-13 |
3.7x10-13 |
2.1x10-11 |
3.1x10-12 |
2.8x10-12 |
1.1x10-11 |
| Point Source Flux2 |
3.3x10-15 |
7.3x10-15 |
1.4x10-14 |
1.4x10-13 |
7.5x10-16 |
9.3x10-16 |
8.8x10-16 |
5.1x10-14 |
7.5x10-15 |
6.7x10-15 |
2.7x10-14 |
| O5 V3 |
20.2 |
19.3 |
18.1 |
16.5 |
20.2 |
19.9 |
19.9 |
16.0 |
18.2 |
17.1 |
15.4 |
| B1 V |
19.9 |
18.8 |
17.8 |
15.7 |
19.8 |
19.5 |
19.5 |
15.5 |
17.8 |
16.7 |
15.0 |
| B3 V |
19.5 |
18.4 |
17.3 |
15.0 |
19.4 |
19.2 |
19.1 |
15.2 |
17.3 |
16.5 |
14.7 |
| B6 V |
18.4 |
17.5 |
16.6 |
13.8 |
18.8 |
18.5 |
18.5 |
14.6 |
16.7 |
15.9 |
14.2 |
| B9 V |
17.2 |
16.3 |
15.5 |
12.3 |
17.9 |
17.6 |
17.6 |
13.5 |
15.7 |
15.2 |
13.6 |
| A1 V |
16.0 |
15.6 |
14.7 |
10.8 |
17.3 |
17.2 |
17.2 |
13.0 |
15.2 |
14.8 |
13.2 |
| A3 V |
14.8 |
14.2 |
13.8 |
8.5 |
16.9 |
16.7 |
16.6 |
12.6 |
14.6 |
14.4 |
12.8 |
| A5 V |
13.6 |
13.2 |
13.0 |
6.7 |
16.6 |
16.3 |
16.3 |
12.1 |
14.2 |
14.2 |
12.7 |
| A9 IV |
11.4 |
10.8 |
11.1 |
3.8 |
15.8 |
15.8 |
15.8 |
11.3 |
13.3 |
13.6 |
12.3 |
| F2 V |
10.1 |
9.8 |
9.8 |
2.5 |
15.4 |
15.2 |
15.2 |
10.5 |
12.8 |
13.3 |
11.8 |
| F4 V |
9.3 |
9.1 |
9.0 |
1.7 |
15.2 |
15.0 |
15.0 |
10.2 |
12.2 |
13.1 |
11.7 |
| F6 V |
8.8 |
8.3 |
8.7 |
0.9 |
15.0 |
14.8 |
14.8 |
9.7 |
11.8 |
12.9 |
11.5 |
| F8 V |
7.9 |
7.8 |
7.8 |
0.2 |
14.8 |
14.7 |
14.6 |
9.2 |
11.5 |
12.7 |
11.4 |
| G2 V |
6.5 |
6.8 |
6.6 |
-1.2 |
14.6 |
14.3 |
14.3 |
8.5 |
10.8 |
12.5 |
11.1 |
| G5 IV |
5.4 |
5.2 |
5.3 |
<-2.0 |
14.3 |
14.0 |
14.0 |
7.8 |
10.1 |
12.2 |
10.8 |
| G7 IV |
4.7 |
4.2 |
4.4 |
|
14.1 |
13.9 |
13.9 |
7.6 |
9.8 |
11.9 |
10.7 |
| K0 IV |
3.8 |
2.2 |
2.2 |
|
13.8 |
13.4 |
13.3 |
7.0 |
9.4 |
11.6 |
10.5 |
| K4 V |
-0.9 |
-1.9 |
-1.8 |
|
13.2 |
12.8 |
12.8 |
6.6 |
8.6 |
11.2 |
10.3 |
| K8 V |
<-2.0 |
<-2.0 |
<-2.0 |
|
12.7 |
12.2 |
12.2 |
6.1 |
7.8 |
10.8 |
10.2 |
| M2 V |
|
|
|
|
11.9 |
11.7 |
11.7 |
5.7 |
7.3 |
10.3 |
10.0 |
| M4 V |
|
|
|
|
11.5 |
11.5 |
11.5 |
5.6 |
7.0 |
10.0 |
9.9 |
| M6 V |
|
|
|
|
10.8 |
11.0 |
11.0 |
5.4 |
6.7 |
9.8 |
9.8 |
| T~50000oK4 |
20.1 |
19.2 |
18.0 |
16.3 |
20.1 |
19.8 |
19.8 |
16.0 |
18.2 |
17.1 |
15.3 |
 -1 5 |
16.5 |
15.8 |
14.9 |
12.7 |
18.0 |
17.6 |
17.6 |
13.3 |
15.3 |
15.1 |
13.5 |
| Integrated Magnitude6 |
13.4 |
13.3 |
11.4 |
9.6 |
13.5 |
13.2 |
13.2 |
9.2 |
11.4 |
10.4 |
8.7 |
| 1 Peak allowed diffuse source surface brightness in ergs sec-1 cm-2 Ĺ-1 arcsec-2. 2 Peak allowed point source flux in ergs sec-1 cm-2 Ĺ-1. 3 Limits given are V magnitudes, for unreddened stars. 4 Limits calculated for a black body at 50,000 degrees K. 5 Limits calculated for a source with spectrum F proportional to -1.6 Maximum integrated magnitude of all stars in field, assuming all are O stars. |
|
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