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Principal: Almudena Alonso
Deputy: David Frayer
Data Monkey(s): Almudena Alonso, David Frayer, Eiichi Egami
Priority:
Downlink Priority: Normal
Analysis Time: 24-48 hours
Last Updated:

Objective

To obtain a 70micron Routine Photometry IC

Description

We will obtain IOC acceptable routine 70um PHOTOMETRY mode 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 70 um routine SCAN IC task (MIPS-915). The pair of activities will allow us to determine the relative efficiency and quality of 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 IC or saturation. This task will also be useful for screening regions of the sky to obtain ICs in SIRTF routine operations. This task together with MIPS-915 will determine whether routine ICs will be obtained in photometry or scan mode.

This task is executed in:

    MIPS Campaign G
    MIPS Campaign H
    MIPS Campaign I
    MIPS Campaing K

Data Collected

A 3x3 square dither map (1 cycle) will be obtained at 70microns with 3 second DCEs in a region of the sky chosen to avoid bright point sources. The offsets are 300 arcseconds. At each position there will be 12 images, so a total of 108 images will be produced each time this task is excecuted. The map will require about 21.0 minutes of observing time. This is the AOR file overlaid on the sky:


#  Please edit this file with care to maintain the
#  correct format so that SPOT can still read it.
#  Generated by SPOT on:  8/15/2002     11:26:55

HEADER: FILE_VERSION=6.1, STATUS = PROPOSAL

      AOT_TYPE:  MIPS Photometry
     AOR_LABEL:  MIPS-918-Feb07-Mar22
    AOR_STATUS:  new

 MOVING_TARGET:  NO
   TARGET_TYPE:  FIXED CLUSTER - OFFSETS
   TARGET_NAME:  MIPS-918-Feb07-Mar22
  COORD_SYSTEM:  Equatorial  J2000
     POSITION1:  RA_LON=5h19m37.90s,  DEC_LAT=+3d54m01.5s
     OFFSET_P2:  EAST_ARRAY_V=300.0",   NORTH_ARRAY_W=0.0"
     OFFSET_P3:  EAST_ARRAY_V=300.0",   NORTH_ARRAY_W=300.0"
     OFFSET_P4:  EAST_ARRAY_V=0.0",     NORTH_ARRAY_W=300.0"
     OFFSET_P5:  EAST_ARRAY_V=-300.0",  NORTH_ARRAY_W=300.0"
     OFFSET_P6:  EAST_ARRAY_V=-300.0",  NORTH_ARRAY_W=0.0"
     OFFSET_P7:  EAST_ARRAY_V=-300.0",  NORTH_ARRAY_W=-300.0"
     OFFSET_P8:  EAST_ARRAY_V=0.0",     NORTH_ARRAY_W=-300.0"
     OFFSET_P9:  EAST_ARRAY_V=300.0",   NORTH_ARRAY_W=-300.0"
OFFSETS_IN_ARRAY:  NO
OBSERVE_OFFSETS_ONLY:  NO
OBJECT_AVOIDANCE:  EARTH = YES, OTHERS = YES

    MICRON_70: IMAGE_SCALE = DEFAULT, FIELD_SIZE = SMALL, EXPOSURE_TIME = 3, N_C
YCLES = 1
SPECIAL_OVERHEAD: IMPACT = none, LATE_EPHEMERIS = NO
RESOURCE_EST: TOTAL_DURATION=1306.4854, SLEW_TIME=121.4, SETTLE_TIME=117.98532, 
SLEW_OVERHEAD=180.0, SPECIAL_OVERHEAD=0.0, UPLINK_VOLUME=4756, DOWNLINK_VOLUME=9
370224, VERSION=S6.1.2
INTEGRATION_TIME: MIPS_24=0.0,MIPS_70=37.748737,MIPS_160=0.0

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-322: 70 um first light and Ph/SR AOT Validation - preliminary
etc.

Calibration Dependencies

Dark

Output and Deliverable Products

Mosaic of the observed field.

70micron IC obtained in PHOTOMETRY mode.

An IC will be applied to a star observed at different positions across the array to check the quality of the IC. We will provide an array map showing the location dependences -if any- of the photometric sensitivity.

Once the MIPS-915 task (Routine Scan IC at 70micron) is executed, we will provide a detailed comparison between ICs obtained in Photometry and Scan modes at 70micron.

Data Analysis

Standard Pipeline reduction using the DAT and/or SSC Pipeline. If using the DAT, we will run MIPS_SLOPER and then we will do the dark subtraction with MIPS_CALER.
Produce a mosaic of the observed region using MIPS_ENHANCER.
Median combine 108 images (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 frame using an appropriate rejection algorithm.
Apply IC to star observations at different positions across the array. We will use for instance observations of the Focal Plane Survey: MIPS-132 and MIPS-133.
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.
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' IC (see A. Alonso's report on flatfield/IC simulations; NEED TO ADD LINK TO FLATFIELD MODEL WEBPAGE). NOTE: According to our simulations we will need between 100 and 200 DCEs (depending on zodi brightness and Galactic column density) at 70microns to get an IC with an accuracy of 0.5% (rms, over the whole array).

metry and scan modes.

Software Requirements

DAT
IRAF
IDL

Actions Following Analysis

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

Failure Modes and Responses

If region of the sky used is saturated, this region will be removed from the list of flatfield/IC regions (Jeonghee Rho's list of flatfield/IC regions). This task is repeated a number of times with different regions of the sky, so it should be possible to obtain 70micron ICs. If regions used are all saturated, we will look for different regions of the sky.