Principal: Alberto
Deputy: Chad et al.
Data Processors(s): Dave Frayer and/or Stefani Wachter
Priority: Normal
Downlink Priority: Normal
Analysis Time: 6hrs
Last Updated: July 7, 2003

Objective

Confirm basic functionality of small field 70um photometry. This is a short preliminary test.

Description

This is a standard AOT photometry observation and should be treated as such, using either SSC science pipeline or DAT MIPS caler. The target is a 70um calibrator/standard star (Chad's list) HD 183439 M0III, with 0.60Jy flux at 70um. For an August 23 launch this task taskes place in early October, the star is visible from Sep11-Nov10 (60 days). One cyle is performed for both Default and Narrow Field (Fine) scales using 3 and 10secs. Like in any standard photometric observation we will get 16 DCEs per pointing or 7 star images per pointing [see MIPS Handbook for details].

Data Collected

  • One cyle is performed for both Default and Narrow Field (Fine) scales using 3sec
 and 10secs. Like in any standard photometric observation we will get 16 DCEs per 
pointing. 

    

    

    Data Reformatting Requirements
    



    Array Data Desired:
    

    
     70 µm 

    


    Data Reformatting Option:
    

    


    Special Instructions:
    


    

  none

    

    Task Dependencies
    




    

    Calibration Dependencies
    

 MIPS Standard Photometry  calibration: Electronic Linearity Correction, Dark Current image and
 Illumination correction, and perhaps image distorsion (SSC Pipeline).



    

    Output and Deliverable Products
    

  
  •  The AOR will generate 16 DCEs per pointing at 70um, so a total of 64 DCEs.
       So 14 images of the standard star.
  
  •  simple mosaic of stellar images.
  
  •  flux converson (DN/s --> Jy or Jy/sq arcsec) factor.
  
  •  comparison of pipeline and DAT results.



    Data Analysis
    

 Analysis of BCDs products, using standard IRAF/IDP3 IDL software tools.

The main goal is to test the functionality of the AOT prior to be full tested and comissioned.
Like in MIPS-922, the data will be processed with both the SSC pipeline and the MIPS DAT. 
The derived flux conversion factors, for Defult and Narrow Field, will be compared
to check for problems in the data processing. To derive the flux conversion factor, photometry will 
be performed on the mosaicked image.  This must be done in such a way that corrects for
distortion. The errors will be derived using the error images that accompany the BCDs. 
The assumed flux of the star (from the tables on the MIPS IST web page) will be divided by 
the measured counts (corrected from the measured aperture to the total star counts using an
aperture correction) to compute the flux conversion factor [borrow this from Chad, but it should be
the standard procedure for calibration stars]. 

A mosaic of the stellar images will be generated. 
This image will be examined visually for any obvious problems, such as poor matching of
background levels between DCEs, missing data, asteroids in the field, etc. 
The mosaic may need to be regenerated if inappropriate data were used in the initial mosaic 
generation [as above].
    

    Software Requirements
    


    

    Actions Following Analysis
    

This a key step for the full commissioning of this observing mode.
The results should be internally consistent, independent of the flux consverion factor,
since the same star is observed in a slighlty different way (integration time and FOV).



    


    Failure Modes and Responses
    
Contingency plan:  

Revise AOT logic if necessary. Await for full AOT confirmation.


    

    Additional Notes