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Monitoring

Sensitivity

Spectral Resolution

Background

The primary background sources that affect COS observations are detector dark count, earthshine, zodiacal light, and airglow emission; neither of the COS detectors suffers from read noise. For more information on COS background performance see Section 7.4 of the COS Instrument Handbook. For information on high S/N observations of the geocoronal Lyman-alpha line, please see the COS Airglow page.

Detector Dark Count     Earthshine     Zodiacal Light     Airglow Emission

 

Throughput

COS is considerably more sensitive than STIS and earlier-generation HST instruments at comparable spectral resolutions, particularly in the far ultraviolet. At FUV wavelengths, the peak effective area is ~3000 cm2 near 1300 Å with the G130M grating. At NUV wavelengths, the peak effective area is expected to reach ~850 cm2 near 2250 Å with the G230L grating.

For further information, see Section 5.1.1 of the COS Instrument Handbook.

FUV High Voltage History

The COS FUV detector is a high-gain, cross delay line microchannel plate (MCP) detector. In the following links we present the high voltage history of each segment.

 

FUV History

LAST UPDATED: 06/17/2019

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https://hsthelp.stsci.edu.