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Cosmic Origins SpectrographInstrument Handbookfor Cycle 22 > Chapter 13: Spectroscopic Reference Material > FUV Grating G130M with CENWAVE=1055 or 1096

FUV Grating G130M with CENWAVE=1055 or 1096
Description
When used with a central wavelength of 1055 or 1096 , grating G130M samples wavelengths between about 900 and 1200 . Its resolution and effective area are higher than those of the G140L grating, but lower than those of G130M when used at longer central wavelengths.
Special Considerations
The COS sensitivity rises steeply between 1070 and 1150 . To observe bright targets near the Lyman limit, turn off detector segment A and use only segment B.
Resolving
Power
R = λ/Δλ
Dispersion
(m pixel–1)
FP-POS
Step
( step-1)
G130M Segment A
G130M Segment B
Figure 13.8: Wavelength Ranges for the G130M/1055 and 1096 Modes
G130M/1055 and 1096 Point-Source Sensitivity
Table 13.5: G130M/1055 and 1096 Point-Source Sensitivity for PSA
Sensitivity
(counts pixel-1 sec-1 per
erg cm-2 sec-1 -1)
Figure 13.9: G130M/1055 and 1096 Point-Source Sensitivity for PSA
The sensitivity through the BOA is not shown, as its MgF2 filter is opaque at these wavelengths.
G130M/1055 and 1096 Signal-to-Noise Ratio
Figure 13.10: Point-Source Signal-to-Noise as a Function of STMAG for G130M at 1030
The top axis displays constant Fλ values corresponding to the STMAG units (V+STMAGλ) on the bottom axis. Recall that STMAG = 0 is equivalent to Fλ = 3.63E-9 erg cm-2 s-1 -1. Colors refer to exposure times in seconds. The edge of the shaded area corresponds to the bright-object screening limit. Use of the PSA is assumed.

Cosmic Origins SpectrographInstrument Handbookfor Cycle 22 > Chapter 13: Spectroscopic Reference Material > FUV Grating G130M with CENWAVE=1055 or 1096

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