10.1 Phase I Proposing
At this point you should have assembled all the information you need to submit your Phase
I HST observing proposal. During the course of this process you should review the items listed below.
For All Proposals:
- Check the catalog of previously executed and accepted programs to search for any duplications, and if present, provide a justification for duplicate observations.
- Justify any special requirements (e.g.,
SHADOW, interactive acquisition, CVZ, target-of-opportunity, time critical scheduling, or the re-use target capability).
- Consider any special calibrations (e.g., unusually accurate wavelength determination requiring additional non-automatic wavecal exposures, fringe flats, or slitless spectroscopy), and account for their time in your request.
- Check your exposure times and configurations to ensure they are sufficient to provide the desired signal-to-noise ratios and accuracies, without saturation.
- Check that no visit is longer than 3 orbits.
- Allocate time for a target acquisition with appropriate centering accuracy. If a pre-acquisition image is needed, include the necessary extra orbit in the total orbit time request.
- Include all applicable overheads so that in Phase II you will have enough orbits available to successfully implement your observations.
- Make sure that all configurations used in your proposal are included in the summary table.
- If applicable, justify the use of any available-but-unsupported modes, and explain how you plan to deal with calibration issues.
For CCD Observations:
- Check that you are not exceeding the CCD full well counts/pix limit for pixels (emission lines or objects) of interest.
- Allow time for
CR-SPLITobservations and dithering, as needed.
For MAMA Observations:
- Check that your source does not exceed the absolute bright object count rate limits for MAMA exposures. For target-of-opportunity programs, explain how you plan to show that the target does not exceed the bright object limits.
- Check that you are not exceeding the MAMA 65,536 counts/pix buffer imposed limit over pixels (emission lines or objects) of interest.
- Check that your proposal does not violate the policy that restricts the mixing of CCD and MAMA observations in the same visit, (see Section 2.7). Be sure that you are requesting sufficient orbits to allow the MAMA and CCD observations to be done in separate visits. Provide a justification if the scientific needs of your program require violating this policy.
- If early acquisition images in support of MAMA bright object checking are necessary, they must be included in the Phase I orbit request.
- Remember that MAMA pure parallels are not allowed (see Section 2.8).
- Be aware of the limits on the number of targets for STIS/MAMA and COS snapshot and survey programs (see Section 2.9).
If you have visits with both CCD and MAMA observations, check that there is less than 30 minutes of science observing time (including overheads) with the CCD, or that the target is observed for only one orbit (See Section 2.7).
I Orbit Allocation Examples
I orbit allocation examples are presented in the HST Primer. Additional examples of Phase
I orbit estimations are worked through in this Handbook (see Section 1.2.2, Section 6.8, and Section 9.3).
STIS Instrument Handbook
- • Acknowledgments
- Chapter 1: Introduction
Chapter 2: Special Considerations for Cycle 28
- • 2.1 STIS Repair and Return to Operations
- • 2.2 Summary of STIS Performance Changes Since 2004
- • 2.3 New Capabilities for Cycle 28
- • 2.4 Use of Available-but-Unsupported Capabilities
- • 2.5 Choosing Between COS and STIS
- • 2.6 Scheduling Efficiency and Visit Orbit Limits
- • 2.7 MAMA Scheduling Policies
- • 2.8 Prime and Parallel Observing: MAMA Bright-Object Constraints
- • 2.9 STIS Snapshot Program Policies
- Chapter 3: STIS Capabilities, Design, Operations, and Observations
- Chapter 4: Spectroscopy
- Chapter 5: Imaging
- Chapter 6: Exposure Time Calculations
- Chapter 7: Feasibility and Detector Performance
- Chapter 8: Target Acquisition
- Chapter 9: Overheads and Orbit-Time Determination
- Chapter 10: Summary and Checklist
- Chapter 11: Data Taking
Chapter 12: Special Uses of STIS
- • 12.1 Slitless First-Order Spectroscopy
- • 12.2 Long-Slit Echelle Spectroscopy
- • 12.3 Time-Resolved Observations
- • 12.4 Observing Too-Bright Objects with STIS
- • 12.5 High Signal-to-Noise Ratio Observations
- • 12.6 Improving the Sampling of the Line Spread Function
- • 12.7 Considerations for Observing Planetary Targets
- • 12.8 Special Considerations for Extended Targets
- • 12.9 Parallel Observing with STIS
- • 12.10 Coronagraphic Spectroscopy
- • 12.11 Coronagraphic Imaging - 50CORON
- • 12.12 Spatial Scans with the STIS CCD
Chapter 13: Spectroscopic Reference Material
- • 13.1 Introduction
- • 13.2 Using the Information in this Chapter
- • First-Order Grating G750L
- • First-Order Grating G750M
- • First-Order Grating G430L
- • First-Order Grating G430M
- • First-Order Grating G230LB
- • Comparison of G230LB and G230L
- • First-Order Grating G230MB
- • Comparison of G230MB and G230M
- • First-Order Grating G230L
- • First-Order Grating G230M
- • First-Order Grating G140L
- • First-Order Grating G140M
- • Echelle Grating E230M
- • Echelle Grating E230H
- • Echelle Grating E140M
- • Echelle Grating E140H
- • PRISM
- • PRISM Wavelength Relationship
- • 52X0.05 Aperture
- • 52X0.05E1 and 52X0.05D1 Pseudo-Apertures
- • 52X0.1 Aperture
- • 52X0.1E1 and 52X0.1D1 Pseudo-Apertures
- • 52X0.2 Aperture
- • 52X0.2E1, 52X0.2E2, and 52X0.2D1 Pseudo-Apertures
- • 52X0.5 Aperture
- • 52X0.5E1, 52X0.5E2, and 52X0.5D1 Pseudo-Apertures
- • 52X2 Aperture
- • 52X2E1, 52X2E2, and 52X2D1 Pseudo-Apertures
- • 52X0.2F1 Aperture
- • 0.2X0.06 Aperture
- • 0.2X0.2 Aperture
- • 0.2X0.09 Aperture
- • 6X0.2 Aperture
- • 0.1X0.03 Aperture
- • FP-SPLIT Slits 0.2X0.06FP(A-E) Apertures
- • FP-SPLIT Slits 0.2X0.2FP(A-E) Apertures
- • 31X0.05ND(A-C) Apertures
- • 0.2X0.05ND Aperture
- • 0.3X0.05ND Aperture
- • F25NDQ Aperture
- 13.5 Spatial Profiles
- 13.6 Line Spread Functions
- • 13.7 Spectral Purity, Order Confusion, and Peculiarities
- • 13.8 MAMA Spectroscopic Bright Object Limits
Chapter 14: Imaging Reference Material
- • 14.1 Introduction
- • 14.2 Using the Information in this Chapter
- 14.3 CCD
- 14.4 NUV-MAMA
- • 25MAMA - FUV-MAMA, Clear
- • 25MAMAD1 - FUV-MAMA Pseudo-Aperture
- • F25ND3 - FUV-MAMA
- • F25ND5 - FUV-MAMA
- • F25NDQ - FUV-MAMA
- • F25QTZ - FUV-MAMA, Longpass
- • F25QTZD1 - FUV-MAMA, Longpass Pseudo-Aperture
- • F25SRF2 - FUV-MAMA, Longpass
- • F25SRF2D1 - FUV-MAMA, Longpass Pseudo-Aperture
- • F25LYA - FUV-MAMA, Lyman-alpha
- • 14.6 Image Mode Geometric Distortion
- • 14.7 Spatial Dependence of the STIS PSF
- • 14.8 MAMA Imaging Bright Object Limits
- Chapter 15: Overview of Pipeline Calibration
- Chapter 16: Accuracies
Chapter 17: Calibration Status and Plans
- • 17.1 Introduction
- • 17.2 Ground Testing and Calibration
- • 17.3 Ground Testing and Calibration
- • 17.4 Cycle 7 Calibration
- • 17.5 Cycle 8 Calibration
- • 17.6 Cycle 9 Calibration
- • 17.7 Cycle 10 Calibration
- • 17.8 Cycle 11 Calibration
- • 17.9 Cycle 12 Calibration
- • 17.10 SM4 and SMOV4 Calibration
- • 17.11 Cycle 17 Calibration Plan
- • 17.12 Cycle 18 Calibration Plan
- • 17.13 Cycle 19 Calibration Plan
- • 17.14 Cycle 20 Calibration Plan
- • 17.15 Cycle 21 Calibration Plan
- • 17.16 Cycle 22 Calibration Plan
- • 17.17 Cycle 23 Calibration Plan
- • 17.18 Cycle 24 Calibration Plan
- • 17.19 Cycle 25 Calibration Plan
- • 17.20 Cycle 26 Calibration Plan
- Appendix A: Available-But-Unsupported Spectroscopic Capabilities
- • Glossary