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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: 24-48 hours
Last Updated:

Objective

To obtain 24, 70 and 160 micron Routine SLOW rate Scan Flats and ICs

Description

We will obtain IOC acceptable routine 24, 70 and 160um SLOW SCAN mode flats and ICs (this task is repeated a number of times in different IOC campaigns) to be used on a regular basis. This activity is a companion to the routine PHOTOMETRY tasks and the routine SCAN (fast and medium rate) tasks. These activities will allow us to determine the relative efficiency and quality of flats/ICs created using scan and photometry AORs.

Since this task is repeated a number of times during IOC, we will observe different regions of the sky each time. The task will check for possible variations of quality of the flat/IC or saturation. This task will also be useful for screening regions of the sky to obtain flats/ICs in SIRTF routine operations.

This task is executed in:

    MIPS Campaign V
    MIPS Campaign X3
    MIPS Campaign M001

Data Collected

A 0.5 degree long (2 legs) scan map will be obtained using the slow scan AOT in a region of the sky chosen to avoid bright point sources. The images to be median combined to produce a 24 um flat and 70 and 160 um ICs. The map will require about 46 minutes of observing time.

HEADER: FILE_VERSION=7.0, STATUS = PROPOSAL




      AOT_TYPE:  MIPS Scan Map

     AOR_LABEL:  MIPS-942-Nov13-Dec24-leading

    AOR_STATUS:  new



 MOVING_TARGET:  NO

   TARGET_TYPE:  FIXED SINGLE

   TARGET_NAME:  zodi_30b-offset1

  COORD_SYSTEM:  Equatorial  J2000

      POSITION:  RA_LON=23h03m15.74s,  DEC_LAT=+4d27m58.7s

OBJECT_AVOIDANCE:  EARTH = YES, OTHERS = YES



    REQUIRE_160: YES

      SCAN_RATE: slow

 FAST_RESET_160: NO

      STEP_SIZE: TURNAROUND=302", FORWARD=0"

    N_SCAN_LEGS: 2

   N_MAP_CYCLES: 1

SCAN_LEG_LENGTH: 0.5

MAP_CENTER_OFFSET: CROSS_SCAN = 0, IN_SCAN = 0

SPECIAL: IMPACT = none, LATE_EPHEMERIS = NO,SECOND_LOOK = NO

RESOURCE_EST: TOTAL_DURATION=2741.55, SLEW_TIME=16.2, SETTLE_TIME=45.75, SLEW_OVERHEAD=180.0, SPECIAL_OVERHEAD=0.0, UPLINK_VOLUME=691, DOWNLINK_VOLUME=45333370,

 VERSION=S8.9.0

INTEGRATION_TIME: MIPS_24=104.9,MIPS_70=104.9,MIPS_160=10.5

Data Reformatting Requirements

Array Data Desired:

All Arrays

Data Reformatting Option:

NORMAL

1 FITS file per AOR per array.

Special Instructions:

Task Dependencies

etc.

Calibration Dependencies

Dark

Output and Deliverable Products

Mosaics at all three wavelengths of the observed region.

24 micron flat, and 70 and 160 micron ICs obtained in SLOW SCAN mode.

We will apply the flat/IC to a star observed at a grid of positions across the array to check the quality of the flat/IC. We will provide an array map showing the location dependences -if any- of the photometric sensitivity.

We will provide a detailed comparison between ICs obtained in Photometry and Scan modes at all three wavelengths.

Data Analysis

Standard Pipeline reduction using the DAT and/or SSC Pipeline. If using the DAT, we will run MIPS_SLOPER and MIPS_CALER.
Produce a mosaic of the observed region using MIPS_ENHANCER.
Median combine the images obtained at 24, 70 and 160 micron (with some rejection algorithm) using the IRAF "imcombine" task to create an IC. Alternatively, once IC DCEs are screened for possible saturation, etc, we can use the MIPS_ENHANCER to create the flatfield/IC frame using an appropriate rejection algorithm.
Apply the IC to star observations at different positions across the array.
Aperture photometry on star using the IRAF "phot" task to measure 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 flat/IC accuracy.
Once the task is executed more than once:

we can look for possible IC variations with time/region of sky used
we can determine the number of DCEs necessary to construct a 'super' flat/IC (see A. Alonso's report on flatfield/IC simulations; NEED TO ADD LINK TO FLATFIELD MODEL WEBPAGE).

We will carry out a detailed comparison between flats/ICs created in photometry and scan modes.
We will analyze the 24 and 160micron images in a similar fashion to determine if the observed region of the sky is suitable to create flatfield/ICs at all three wavelengths.

Software Requirements

DAT
IRAF
IDL

Actions Following Analysis

If the flat/IC S/N and quality requirements are met, then the flatfield/IC frame will be put in the calibration data archive.

Failure Modes and Responses

If region of the sky used is saturated at one or more wavelengths, this region will be removed from the list of flatfield regions (Jeonghee Rho's list of flatfield regions), as ideally we would like to use the same region of the sky to obtain flatfields and ICs at all three wavelengths.