Contents

• Revision History
• 1. Introduction
• 2. Getting Started
  • 2.1 Proposing Observations for the Spitzer Space Telescope
  • 2.2 Preliminaries
    • 2.2.1 Are the targets available for observations with Spitzer?
    • 2.2.2 What is the IR background?
    • 2.2.3 What is the instrument sensitivity?
    • 2.2.4 What is the required exposure time?
  • 2.3 Obtaining Spot
  • 2.4 Designing the Observations with Spot
    • 2.4.1 Start Spot
    • 2.4.2 Enter Target Information
    • 2.4.3 Fill Out an Astronomical Observation Template
    • 2.4.4 Obtain Resource Estimates
    • 2.4.5 Save AORs
  
  
• 3. Common Observation Planning Errors
  • 3.1 Duplications
  • 3.2 Visualization
  • 3.3 Orientation
  • 3.4 IRAC
    • 3.4.1 Use Dithers
    • 3.4.2 Dither Size
  • 3.5 IRS
    • 3.5.1 Saturation of PU arrays with SL
    • 3.5.2 SL both/LL both
    • 3.5.3 Diffraction Pattern of Telescope near Bright Sources
    • 3.5.4 Peaking up on Extended Sources
  • 3.6 MIPS
    • 3.6.1 Scan Map Coverage
    • 3.6.2 Scan Map Offsets
  
  
• 4. Deep Imaging of Five Clusters of Galaxies at 3.6 - 8.0 micron using IRAC
  • 4.1 Overview of the Program
  • 4.2 Target Selection: Massive, Intermediate Redshift, Galaxy Clusters
  • 4.3 Target Entry
  • 4.4 Background Estimate
  • 4.5 Sensitivity and Exposure Time
  • 4.6 Filling out the IRAC AOT
    • 4.6.1 Readout Modes and Frame Times
    • 4.6.2 Field of View
    • 4.6.3 Mapping
    • 4.6.4 Dithering
  • 4.7 Duration
  • 4.8 Visualization
  • 4.9 Duplicating the A2218 AOR to Design the Complete Program
  
  
• 5. Deep Imaging of Five Galaxy Clusters at 24 - 160 microns using MIPS
  • 5.1 Overview of the Program
  • 5.2 Background Estimate
  • 5.3 Exposure Time
  • 5.4 Filling out the MIPS Photometry/Super Resolution Imaging AOT
    • 5.4.1 Field Size and Resolution
    • 5.4.2 Frame Times
  • 5.5 Duration
  • 5.6 Constraining the Observations
  
  
• 6. High Resolution Staring Mode Observations at 10-37 microns with the IRS
  • 6.1 Introduction to the IRS
  • 6.2 Summary of the Observing Program
  • 6.3 Target Selection and Duplication Check
  • 6.4 Target Entry
  • 6.5 Checking Slit Orientation
  • 6.6 Saturation
  • 6.7 Sensitivity and Exposure Time Estimate
  • 6.8 Long-High Sky Background Observations
  • 6.9 Filling Out the IRS Staring Mode AOT
    • 6.9.1 Naming the AOR
    • 6.9.2 Choosing the Best Peak-up Option
    • 6.9.3 IRS Peak-up Array Saturation and Droop Correction
    • 6.9.4 Ramps and Cycles
    • 6.9.5 LH Background
  • 6.10 Completing the Program: Duration Calculation and Proposal Submission
  • 6.11 Reference Material
  
  
• 7. Low Resolution Spectral Mapping at 5-14 microns with the IRS
  • 7.1 Summary of the Observing Program
  • 7.2 Target Selection and Duplication Check
  • 7.3 Target Entry
  • 7.4 Slit Orientation and Timing Constraints
  • 7.5 Saturation
  • 7.6 Sensitivity and Exposure Time Estimate
  • 7.7 Filling Out the IRS Spectral Mapping Mode AOT
    • 7.7.1 Droop Correction Considerations
    • 7.7.2 Peak-up Settings
    • 7.7.3 Instrument Settings
  • 7.8 Completing the Program
    • 7.8.1 Timing Constraints
    • 7.8.2 Duration Calculation
    • 7.8.3 Proposal Submission
  • 7.9 Reference Material
  
  
• 8. 16 Micron Imaging of Five Clusters of Galaxies using IRS
  • 8.1 Overview of the Program
  • 8.2 Target Selection
  • 8.3 Background Estimates
  • 8.4 Exposure Time and Survey Design
  • 8.5 Filling in the AOT using Spot
    • 8.5.1 Mapping Abell 2218
    • 8.5.2 Fixed Cluster Targets
    • 8.5.3 Single Target
  
  
• 9. Large-Area Mapping in the Trapezium at 24 - 160 microns using MIPS
  • 9.1 Overview of the Program
  • 9.2 Target Selection: Orion Nebula Cluster
  • 9.3 Target Entry
  • 9.4 Image Retrieval
    • 9.4.1 ISSA
    • 9.4.2 2MASS
  • 9.5 MIPS Scan Map
    • 9.5.1 Background Estimates
    • 9.5.2 Bright Objects and Instrumental Backgrounds
    • 9.5.3 Exposure Time
    • 9.5.4 Filling in the AOT
    • 9.5.5 Time Estimates
    • 9.5.6 Visualization
  • 9.6 Another MIPS Scan Map Option: Tiling a Larger Region
    • 9.6.1 Constraints
  
  
• 10. Large-Area Mapping in the Trapezium at 3.6 - 8.0 microns with IRAC
  • 10.1 Overview of the Program
  • 10.2 Exposure Time
    • 10.2.1 Saturation Limits
    • 10.2.2 Background Estimates
    • 10.2.3 Source Count Estimates
    • 10.2.4 Sensitivity Estimates
    • 10.2.5 Final Decision on Exposure Time
  • 10.3 Filling in the AOT
    • 10.3.1 Basic Identification
    • 10.3.2 Instrument Settings
  • 10.4 Time Estimates
  • 10.5 Visualization
  
  
• 11. Photometry of Moving Object Centaur 5145 Pholus using MIPS
  • 11.1 Overview of the Observations
  • 11.2 Target Selection and Suitability: Pholus
  • 11.3 Target Entry
  • 11.4 Visualizing Your Target
  • 11.5 MIPS Photometry
    • 11.5.1 Exposure Time & Saturation
    • 11.5.2 Background
    • 11.5.3 Filling in the MIPS Photometry/Super Resolution Imaging AOT
    • 11.5.4 Visualization
  
  
• 12. MIPS Spectral Energy Distribution (SED) Observations of Canopus
  • 12.1 Introduction
  • 12.2 Overview of the Program
  • 12.3 Target Selection and Duplication Check
  • 12.4 Saturation, Sensitivity and Integration Time Estimate
    • 12.4.1 Saturations
    • 12.4.2 Sensitivities
    • 12.4.3 Integration Time Estimate
  • 12.5 Filling in the MIPS SED AOT
    • 12.5.1 Enter the Target
    • 12.5.2 Specify the Observing Parameters
    • 12.5.3 Calculate the Time
  • 12.6 Visualization of the Observation
  • 12.7 Additional Notes for Consideration
    • 12.7.1 Constraining the Slit Orientation
    • 12.7.2 Mapping Observations
    • 12.7.3 Spectroscopic Photometry of Extended Sources
  
  
• 13. Time Series Observations
  • 13.1 Overview of the Observations
  • 13.2 Target Selection and Suitability
  • 13.3 Target Entry
  • 13.4 The IRAC AOR: Exposure Time & Observing Strategy
  • 13.5 Constraints
    • 13.5.1 Timing Constraints
    • 13.5.2 Chaining AORs
    • 13.5.3 Other kinds of constraints
  
  
• 14. Target of Opportunity (ToO) Observations
  • 14.1 Overview of the Observations
  • 14.2 Target Selection and Suitability
  • 14.3 Impact definitions
  • 14.4 Single Instrument, Medium Impact
  • 14.5 Multiple Instrument, High Impact
  • 14.6 Single Instrument, Multiple epoch
    • 14.6.1 Setting Constraints
    • 14.6.2 Special Overhead
  • 14.7 Hints and Tips
  • 14.8 Obtaining the AOR file
  
  
• 15. How to Submit A Spitzer Proposal
  • 15.0.1 Planning Stages
  • 15.0.2 Planning stage Hints and Tips
  • 15.0.3 Proposal Submission
  • 15.0.4 Proposal Submission Hints and Tips
  • 15.0.5 Updating your Submitted Proposal
  • 15.0.6 Proposal Updating Hints and Tips
  • 15.0.7 Checklist Including Common Errors
  
  
• 16. Planning Observations Frequently Asked Questions
• A. Conversion of Units
  • A.1 Conversion Between Flux Densities
  • A.2 Converting Between Flux Density and Magnitudes
  • A.3 Conversion Among Surface Brightness Units
  
  
• B. Deep Imaging AORs
• C. IRS Staring AORs
• D. IRS Mapping AORs
• E. PUI AORs
• F. Survey AORs
• G. IRSKY output for MIPS background near the Trapezium
• H. SSO AORs
• I. SED AORs
• J. Time Series AORs
• K. Target of Opportunity (ToO) AORs
• Index
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