Principal: alberto
Deputy: SStolovy
Data Analyst(s): Dave Frayer and/or Stefani Wachter
Priority: Normal
Downlink Priority: Normal
Analysis Time: 12hrs
Last Updated:

Objective

Verify that the baseline slew state for MIPS works and does what is planned. And to check the state of the detectors after slewing through a bright source.

Description

*During slews (long ones, between AORs) the CSMM is placed in the neutral position (all three arrays see sky). When not exposing the array reset intervals alternate between 0.5 and 1.5 seconds. In general we do not know the slew paths that will be taken between AORs prior to final scheduling. Question - Is this adequated enough or we need to set the FOV to a different position (e.g. a "dark") Does the possibility of slewing over very bright sources have a potential of impacting the following AORs with residual images? Of particular concern to the 24 micron data. Task - Do PH/SR AOR of known source in all three bands. A calibration source would work great, but might be hard to find one that meets that needs. Chain another PH/SR AOR of a source or region that is relatively nearby, and will force the slew between AORs to go over a region of very bright IR sources (Orion for example). Repeat. If there appear no ill effects on the following AORs, then there is no need to change the instrument state for slewing. If we do bad things, then it is possible we will need to consider putting the 24 micron array in the dark for slewing. This is a standard AOT photometry observation and should be treated as such, using either SSC science pipeline or DAT MIPS caler.

Data Collected

  • 16 DCEs per AOR (2 AORs)

    Data Reformatting Requirements

    Array Data Desired:

    Primary, 24 µm (check 70 & 160µm as well)

    Data Reformatting Option:

    Special Instructions:
    none

    Task Dependencies

    Calibration Dependencies

    Output and Deliverable Products

  • Two standard AORs are taken for this test.
  • The AOR will generate 16 DCEs per pointing at 24um. So 14 images of the standard star.
  • simple mosaic of stellar images.

    Data Analysis

    Analysis of BCDs products, using standard IRAF/IDP3 IDL software tools. Check the data before, during and after slewing through a bright region. Noise in the data, non-linearities, saturation and latency in the 3 arrays should be analyzed, but 24um could be the array more affected by this observing strategy. The health of the raw ramps is a strong diagnostic of what the final products will look like.

    Software Requirements

    Actions Following Analysis

  • If there appear no ill effects on the following AORs, then there is no need to change the instrument state for slewing.
  • make data available to IT/IST

    Failure Modes and Responses

    Revisit instrument state during slews. Consider different reset rates, or other options. One possibility is to place the 24um array in the dark while slewing. The disadvantage is the increased uplink command load, that is already too large, for reconfiguring the CSMM.

    Additional Notes