10.1 Introduction
Both the FUV XDL and the NUV MAMA detectors are subject to damage or destruction by excessive illumination. An excessive local count rate can permanently reduce the sensitivity of the affected detector region. The most likely causes are a bright spectral emission line (XDL or MAMA) or a bright source observed in direct imaging (MAMA). A global over-illumination of the detector can result in its loss. To protect the detectors, onboard software monitors the local and global count rates. It shutters the instrument in case of a local violation and lowers the high voltage if a global count-rate violation is detected. The local rate is checked before an exposure is begun, while the global rate is monitored continuously during the exposure. Under certain circumstances damage can result despite the onboard safety measures, and in any event lowering the high voltage will disrupt the HST schedule and operations. Therefore, all proposed COS observations must meet count-rate screening limits with safety margins to allow for uncertainties. COS is currently the only HST instrument to use UV detectors for target acquisitions. Such acquisitions must be screened, as well, including special procedures for imaging acquisitions of extended sources; see Section 8.10.2. It is the responsibility of the observer to screen all proposed targets and fields during Phase II
preparation, and of STScI to check and enforce these limits. The COS Bright Object Protection (BOP) policies and procedures are described in this chapter.
Table 10.1: COS Count-Rate Screening Limits.
Detector | Source type | Type of limit | Limiting count rate (counts/s) |
---|---|---|---|
FUV | predictable | global | 15,000 per segment1 |
local | 0.67 per pixel2 | ||
irregular | global | 6,000 per segment1 | |
local | 0.67 per pixel2 | ||
NUV | predictable | global | 170,000 (imaging) or 30,000 per stripe (spectroscopic)1 |
local | 50 per pixel3 (imaging) or 70 per pixel (spectroscopic) | ||
irregular | global | 68,000 (imaging) or 12,000 per stripe (spectroscopic)1 | |
local | 50 per pixel (imaging) or 70 per pixel (spectroscopic) |
1 The global data-rate limit for observations using TIME-TAG
mode is 30,000 counts/s, as discussed in Section 5.2.1.
2 This local count-rate screening limit is not applicable to the 1055 and 1096 cenwaves of the COS G130M grating. For these modes the limiting count rate is 0.2 count/s/pixel for both source types.
3 For imaging acquisitions, a count rate of 360 count/s in the 9 × 9-pixel box surrounding the target (as computed by the COS Imaging Acquisition ETC) represents an equivalent safe upper limit.
-
COS Instrument Handbook
- Acknowledgments
- Chapter 1: An Introduction to COS
- Chapter 2: Proposal and Program Considerations
- Chapter 3: Description and Performance of the COS Optics
- Chapter 4: Description and Performance of the COS Detectors
-
Chapter 5: Spectroscopy with COS
- 5.1 The Capabilities of COS
- • 5.2 TIME-TAG vs. ACCUM Mode
- • 5.3 Valid Exposure Times
- • 5.4 Estimating the BUFFER-TIME in TIME-TAG Mode
- • 5.5 Spanning the Gap with Multiple CENWAVE Settings
- • 5.6 FUV Single-Segment Observations
- • 5.7 Internal Wavelength Calibration Exposures
- • 5.8 Fixed-Pattern Noise
- • 5.9 COS Spectroscopy of Extended Sources
- • 5.10 Wavelength Settings and Ranges
- • 5.11 Spectroscopy with Available-but-Unsupported Settings
- • 5.12 FUV Detector Lifetime Positions
- • 5.13 Spectroscopic Use of the Bright Object Aperture
- Chapter 6: Imaging with COS
- Chapter 7: Exposure-Time Calculator - ETC
-
Chapter 8: Target Acquisitions
- • 8.1 Introduction
- • 8.2 Target Acquisition Overview
- • 8.3 ACQ SEARCH Acquisition Mode
- • 8.4 ACQ IMAGE Acquisition Mode
- • 8.5 ACQ PEAKXD Acquisition Mode
- • 8.6 ACQ PEAKD Acquisition Mode
- • 8.7 Exposure Times
- • 8.8 Centering Accuracy and Data Quality
- • 8.9 Recommended Parameters for all COS TA Modes
- • 8.10 Special Cases
- Chapter 9: Scheduling Observations
-
Chapter 10: Bright-Object Protection
- • 10.1 Introduction
- • 10.2 Screening Limits
- • 10.3 Source V Magnitude Limits
- • 10.4 Tools for Bright-Object Screening
- • 10.5 Policies and Procedures
- • 10.6 On-Orbit Protection Procedures
- • 10.7 Bright Object Protection for Solar System Observations
- • 10.8 SNAP, TOO, and Unpredictable Sources Observations with COS
- • 10.9 Bright Object Protection for M Dwarfs
- Chapter 11: Data Products and Data Reduction
-
Chapter 12: The COS Calibration Program
- • 12.1 Introduction
- • 12.2 Ground Testing and Calibration
- • 12.3 SMOV4 Testing and Calibration
- • 12.4 COS Monitoring Programs
- • 12.5 Cycle 17 Calibration Program
- • 12.6 Cycle 18 Calibration Program
- • 12.7 Cycle 19 Calibration Program
- • 12.8 Cycle 20 Calibration Program
- • 12.9 Cycle 21 Calibration Program
- • 12.10 Cycle 22 Calibration Program
- • 12.11 Cycle 23 Calibration Program
- • 12.12 Cycle 24 Calibration Program
- • 12.13 Cycle 25 Calibration Program
- • 12.14 Cycle 26 Calibration Program
- • 12.15 Cycle 27 Calibration Program
- • 12.16 Cycle 28 Calibration Program
- • 12.17 Cycle 29 Calibration Program
- • 12.18 Cycle 30 Calibration Program
- • 12.19 Cycle 31 Calibration Program
- Chapter 13: COS Reference Material
- • Glossary