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Principal: Almudena Alonso
Deputy: David Frayer
Data Monkey(s): Almudena Alonso, Eiichi Egami, David Frayer
Priority:
Downlink Priority: Normal
Analysis Time: 2-5 days
Last Updated:

Objective

To carry out a detailed comparison of 70micron ICs as a function of the scan mirror position.

Description

We will acquire the data needed to produce IC frames at 70micron in scan mode with enough DCEs taken at 33 scan-mirror positions. This will allow us to produce an IC for each scan-mirror position. If these individual ICs are judged to be indistinguishable they can be combined to create a single IC. We will perform the necessary data reduction (median-filtering) needed to create the IC frames. This activity is a companion to the ROUTINE Photometry and ROUTINE Scan AOR IC activity (MIPS-918 and MIPS-915). These activities will allow us to determine the relative efficiency and quality of ICs created using scan and photometry AORs.

This task is executed in MIPS Campaign Q.

Data Collected

A 5-degree long x 3 legs scan map is taken using the fast-scan AOT in a region of sky chosen to avoid bright point-sources. The map will require about 65.5 minutes of observing time. In each calibration cycle 33 scan mirror positions are observed. In a 5degree long scan map observed in fast mode. For a given leg each will observe 10DCEs per scan mirror position, so a total of ~30DCE per scan mirror position will be available when the task is executed.

 
#  Please edit this file with care to maintain the
#  correct format so that SPOT can still read it.
#  Generated by SPOT on:  10/3/2002     13:42:16

HEADER: FILE_VERSION=6.2, STATUS = PROPOSAL

      AOT_TYPE:  MIPS Scan Map
     AOR_LABEL:  MIPS-305-Feb25-Apr10
    AOR_STATUS:  new

 MOVING_TARGET:  NO
   TARGET_TYPE:  FIXED SINGLE
   TARGET_NAME:  MIPS-305-Feb25-Apr10
  COORD_SYSTEM:  Equatorial  J2000
      POSITION:  RA_LON=6h40m18.6381s,  DEC_LAT=+43d09m59.7558s
OBJECT_AVOIDANCE:  EARTH = YES, OTHERS = YES

    REQUIRE_160: YES
      SCAN_RATE: fast
 FAST_RESET_160: NO
      STEP_SIZE: TURNAROUND=302", FORWARD=302"
    N_SCAN_LEGS: 3
   N_MAP_CYCLES: 1
SCAN_LEG_LENGTH: 5.0
MAP_CENTER_OFFSET: CROSS_SCAN = 0, IN_SCAN = 0
SPECIAL: IMPACT = none, LATE_EPHEMERIS = NO,SECOND_LOOK = NO
RESOURCE_EST: TOTAL_DURATION=3927.325, SLEW_TIME=37.2, SETTLE_TIME=68.625, SLEW_
OVERHEAD=180.0, SPECIAL_OVERHEAD=0.0, UPLINK_VOLUME=749, DOWNLINK_VOLUME=8247770
4, VERSION=S6.2.7
INTEGRATION_TIME: MIPS_24=15.7,MIPS_70=15.7,MIPS_160=3.1

COMMENT_START: 

COMMENT_END:

Data Reformatting Requirements

Array Data Desired:

All Arrays

Data Reformatting Option:

NORMAL

1 FITS file per AOR per array.

Special Instructions:

Task Dependencies

MIPS-326: 24 um Scan AOT Validation - preliminary
etc.

Calibration Dependencies

Dark

Output and Deliverable Products

Mosaic of observed field at all three wavelegths. The 24micron mosaic may be useful for IRS to select their own flatfield regions, since they will need to avoid bright sources.

Comparison of IC accuracy as a function of the scan mirror position.

Data Analysis

Standard Pipeline reduction using the DAT and/or SSC Pipeline. If using the DAT, we will run MIPS_SLOPER to do electronic linearity correction, cosmic ray rejection, etc, and MIPS_CALER to do the dark subtraction.
Use MIPS_ENHANCER to produce a mosaic of the observed field corrected for geometrical distorsions (useful for screening of possible bright sources present in the FOV).
Obtain the scan mirror position from header of images (e.g., using the IRAF 'hselect' task). The keyword we need is called: CSM_PRED.
Median combine images obtained at 70micron (with some rejection algorithm) using the IRAF "imcombine" task to create the ICs as a function of the scan mirror position. If S/N of individual flatfields is not high enough, we could bin the scan mirror positions as needed to obtained the desired S/N (this may be the case for 160micron data). Alternatively we can use MIPS_ENHANCER to median combine the images.
For each scan mirror position IC:

Perform illumination correction to 70 micron star observations at different positions across the array. For instance we can use the Focal Plane Survey observations: MIPS-137 and MIPS-138.
Aperture photometry on star using the IRAF "phot" task to measure star flux. We will use the tasks: photpars, fitskypars to set up the photometry parameters (aperture, sky/background estimate).
Comparison of star aperture photometry at different positions across the array to determine IC accuracy, and comparison as a function of the scan mirror position
Or alternatively, ratio all different ICs (for different scan mirror position) to a reference IC (or a combination of all ICs), and look for possible variations as a function of scan mirror position.

This will done for all three wavelengths as long as images are not saturated.

Software Requirements

DAT
IRAF
IDL

Actions Following Analysis

Depending on the output of this task, we will have to determine whether we need to use different flatfield frames for different scan mirror positons.