70µm WF Focal Plane Survey, Fine

Principal: Jocelyn Keene
Deputy: Jane Morrison, Bill Wheaton
Data Monkey(s): Jane Morrison and Bill Wheaton
Priority: Critical
Downlink Priority: Normal
Analysis Time: Campaign Q: 2880 minutes, Campaign R: 2880 minutes, combining campaign Q and R: 120 minutes
Last Updated:

Objective

To measure the pixel locations (i.e. array orientation, scale,and distortion) as a function of scan mirror angle for the 70 µm wide field array configuration to an accuracy of 1.1 arcseconds relative to the PCRS.

Description

Use an IER based on the 70 µm photometry compact source AOT to measure the locations on the sky of several positions on the array as a function of scanning mirror angle.
This task is run in campaigns Q and R. The data from each campaign is processed separately by the MIPS and IPF teams. The IPF team then combines the results from both campaigns. The results from the IPF multi-run are used to update Frame Table 14. The frame table updates for all the campaigns can be found in the following table: Frame Table Updates.

Data Collected

The observing strategy is exactly the same as 70 µm coarse, except that the set of observations is repeated for a total of 924 ( 462*2) observations. The IER is set up so data is collected in 3 columns on the array: on the left-side, center and right-side of the array. After moving the telescope in the V direction according to the V offset, the observational patter is repeated 7 more times (with a V offset between each set). The entire process is then repeated a second time.

Calibration Star

For the selected calibration star see the IER for this survey. The requirements on the 70 µm fine focal plane calibration star are as follows:

In CVZ

Mips requirements: stellar brightness corresponding to S/N of 30 (3 sec integrations) 0.212 Jy, K mag 1.25

Observing Strategy

Figure 1. Observing Pattern at 3 locations on the detector. Note size of box is not the total size of the array but a portion of the central region which depends on array and if it is a coarse or fine survey

Definitions:

W axis direction is defined by the Frame Table, and is always within +/- 90 degrees of the TPF z axis as projected on the sky. Motion along this axis corresponds to motion in the spacecraft motion (left/right).

V axis direction is defined by the Frame Table, and is always within +/- 90 degrees of the TPF y axis as projected on the sky. Motion along this axis correspond to motion in the scan mirror direction (up/down).

W offset, the amount of motion in the W direction which results in the spacing between left array, middle array and right array observations

V offset, the amount of motion in the V direction which occurs between a set of observations.

70 µm Coarse FPS observational parameters:

W offset = 120 arc seconds

V offset = 60 arc seconds

W dither = 15 arc seconds

V dither = 15 arc seconds

mirror locations for 1 position shown in figure 1.

position 1 = 0
position 2 = -60
position 3 = 20
position 4 = -40
position 5 = 40
position 6 = -20
position 7 = 65
position 8 = position 1 = 0

Observational Strategy

Step 1

PCRS observation

Step 2 - (total of 11 observations)

Position the telescope so the data falls on the left side of array
Position star at position 1 in figure 1 (left), turn stim on take an observation
Turn stim off
Take 8 DCES at positions shown in figure 1 (left)
Position star at position 1, turn stim on and take observation
With star still at position 1 turn stim off and take observation
dither in V and W
Repeat above 11 observations.

Step 3

Move the space craft according to the W offset (120 arc seconds), image should now be on the center of the array.
Position star at position 1 in figure 1 (middle), turn stim on take an observation
Turn stim off
Take 8 DCES at positions shown in figure 1 (middle)
Position star at position 1, turn stim on and take observation
With star still at position 1 turn stim off and take observation
dither in V and W
Repeat above 11 observations.

Step 4

Move the space craft according to the W offset (138 arc seconds), image should now be on the right side of the array.
Position star at position 1 in figure 1 (right), turn stim on take an observation
Turn stim off
Take 8 DCES at positions shown in figure 1 (right)
Position star at position 1, turn stim on and take observation
With star still at position 1 turn stim off and take observation
dither in V and W
Repeat above 11 observations in step.

Step 5

PCRS observation

Step 6: move telescope according to V offset (60 arc seconds) and repeat steps 1-5

Step 7: move telescope according to V offset (60 arc seconds) and repeat steps 1-5

Step 8: move telescope according to V offset (60 arc seconds) and repeat steps 1-5

Step 9: move telescope according to V offset (60 arc seconds) and repeat steps 1-5

Step 10: move telescope according to V offset (60 arc seconds) and repeat steps 1-5

Step 11: Repeat Steps 1-10 a second time.

Number of observations from step 1-5, 66. Step 1-5 repeated 7 times for a total of (66 * 7) = 462 observations. Repeat entire set for a total of 924 observations

Data Reformatting Requirements

Array Data Desired:

70 µm Wide

Data Reformatting Option:

Normal - One FITS multi-image extension file per AOR. Output from MIPS DATPACK, one DCE in each image extension.

Task Dependencies

MIPS-911 : 70 µm Darks
MIPS-306 : 70 µm illumination correction
MIPS-132: 70 µm Wide Field Focal Plane Survey, Coarse.
IPF run is to occur after FTU# 13 (PAC filer and OET CTA Frame Tool inputs)

Calibration Dependencies

Calibration product needed:

70 µm IC

70 µm darks

Items needed by IPF team for this task to run with the IPF filter software:
- IPF team Labeling convention for files: XXYYYZZZ.m where,
  - XX for type of file (example FF for Offset file, IF for output data, CS for Centroid supplemental file)
  - YYY for the version number, '001' to '499' for Coarse survey, '501' to '999' for Fine Surveys
  - ZZZ for the Frame table number associated with the Prime Frame being calibrated. Use 107 for the 70 µm WF array. .
- CB file: The OET Centroid File and Generation Tool is run to generate a centroid B file (CB file)
- A and As files: SIST generates a A and AS files (attitude history files) and emails them to IPF team.
- FF file: The MIPS team generates an Offset file (match derived frames to prime frames) and ftps to IPF team (this can be done before launch and has been).
- CS file: The MIPS team generated a CS file (Centroid supplemental file) to IPF team. This can be done before launch and has been.
Output and Deliverable Products
Output of MIPS DAT: calibrated data file with appropriated header keywords. The name of this file will be "mips_YYY107.fits", where where "YYY" is 3-digit string denoting run number, and "107" is IPF code for 70 µm WF array. This file is sent to B. Wheaton's centroiding program.
Output from Centroid program: Centroid data file. The calibrated data is centroided and the centroided data filename is CAYYY107.m, where the YYY is the version number. This file is sent to the IPF team.
Output from IPF team which the MIPS team analyzes:
- IF file: output data from a single IPF run.
- MF file: output data from a multi-run IPF run
The FF file (offset file) and CS file (centroid supplemental file) have been generated and sent to the IPF team. Unless the results from the coarse survey result in significant changes to these files, these files will not be changed for the fine survey.
Data Analysis
- Process data for Campaign Q:
  1. JPL MIPL transfers downlink data to SSC.
  2. SSC downlink ops processes data and places results in sandbox.
  3. SSC MIPS IST uses FTZ to transfer AOR data from sandbox to SSCIST21.
  4. Data is repackaged with MIPS DATPACK
  5. The data are calibrated using the MIPS DAT using the following options
    1. Run mips_sloper : with following options:
      
      mips_sloper filename
      IF we do not use the default directory for the calibration files. Then use the -j option.
      -j dirname : directory below $MIPS_DIR/Cal to find calibration files.
    2. Run mips_caler : with following options:
      
      mips_caler -I illumination_correction_filename -D dark_filename-C pathname
      -C path is the path to where the calibration files live. If you do not use the -C then the default will be used.
      -D dark filename.
      -I illumnation correction filename
    3. The calibrated data file mipsfps_YYY107.fits (YYY a 3-digit integer string, identifying the run number) is a FITS multi-extension image file, one extension per DCE.
    4. Run Xsloper_view and check to make sure data seems reasonable:
  6. The calibrated data file mipsfps_YYY107.fits is placed on sscist21: /mipsdata/fps/inpdat. File is linked to processing subdirectory (currently sscist21: /home/sscmip/users/waw/fps).
  7. The MIPS IDL Centroid File Generation tool, mipspos.pro, is run according to detailed instructions in sscist21: /home/sscmip/users/waw/fps/fps.doc.
  8. The output files CAYYY107.m (and CSYYY107.m - just passed along) are placed on the TFS at SSC and transfered to DOM at JPL.
  9. IPF team retrieves previously approved spreadsheet and SSC's CA/CS files from DOM.
  10. IPF filter is run using input files: CB,A,AS,O, CA, CS files and the previously approved spreadsheet.
  11. The IPF output files (IF files) are placed on the DOM for MIPS team to analyze.
  12. End of Campaign Q.
- The entire process above is repeated for Campaign R.
- Results from the IPF filter for Campaign Q and Campaign R are analyzed by the MIPS team and compared to one another for consistency.
- On approval of consistency, the IPF team runs the IPF multi-run tool and produces an output file, MF, that is placed on the DOM.
Software Requirements
- STINYTIM for PSF generation.
- SSC downlink system.
- MIPS DAT
- IDL for IDL program mipspos.pro for star centroiding.
- At JPL, IPF Filter program.
Actions Following Analysis
- After each run 133-Q and 133-R the MIPS team recieves the results from the IPF team and reviews then.
- The MIPS team reviews the IF file from the IPF tool and approves or disapproves.
- When approved, SSC generates mini-spreadsheet for review and approval by MCCB, followed by handoff to JPL OET, and uplink of FTU #14.
Failure Modes and Responses
1. Failure of one campaign (Q or R) to produce useful data
  - If one of the runs looks bad, then go back and analyze the data better. We may need to plot the data to look for bad data, we may need to edit the CA file and resend it to the IPF team.
  - We might need to ask the IPF team to look closer at their analysis.
  - If one set is bad and can not be fixed, then use data from other campaign, if data appear reasonable and change is not large.
2. Results of Q & R inconsistent, neither obviously bad, then average the results.
3. Both results are bad - then reschedule observations.
Additional Notes

70µm WF Focal Plane Survey, Fine

Objective

Description

Data Collected

Calibration Star

Observing Strategy

Definitions:

70 µm Coarse FPS observational parameters:

Observational Strategy

Data Reformatting Requirements

Task Dependencies

Calibration Dependencies

Output and Deliverable Products

Data Analysis

Software Requirements

Actions Following Analysis

Failure Modes and Responses

Additional Notes