Principal: alberto
Deputy: cengelbracht et al.
Data Processer(s): Dave Frayer and/or Setafani Wachter
Priority: Normal
Downlink Priority: Normal
Analysis Time: 6hrs
Last Updated: July 8, 2003

Objective

Confirm basic functionality of MIPS 160um small field photometry

Description

A standard small field 160um Photometry is used for this task, and as such the new defaults values are 4 cycles, this for integration times of 3 and 10sec. The target is Gamma Draconis, a well studied FIR standard.

Data Collected

  • 52 DCEs per integration time.

    Data Reformatting Requirements

    Array Data Desired:

    160 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 13 DCEs at 160um per integration time, so FOUR cycles will provide 52 DCES.
  • 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-322, the data will be processed with both the SSC pipeline and the MIPS DAT. The derived flux conversion factors to check for problems in the data processing. To obtain 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 at 3 and 10secs.

    Failure Modes and Responses

    Revise AOT logic. Await to full confirmation.

    Additional Notes