MIPS- IOC Task Cookbook:
Super Resolution of a Proto-stellar Region

Principal: Karl Stapelfeldt
Deputy: Alberto Noriega-Crespo
Data Monkey(s):
Priority: Desired
Downlink Priority: Normal
Analysis Time:
Last Updated:

Objective

Verify that MIPS can spatially resolve sources near the Rayleigh limit

Description

We will observe the young stellar object binary CV Cha / CW Cha, which has a separation of 11" at PA 105 degrees. The photometry AOT will be used to observe the target at 24 and 70 µm [the sky background at 160 µm is saturated in the region of this source]. We will resolve the flux densities contribution of each star to the spatially unresolved IRAS measurements.

Data Collected

24 µm, 70 µm coarse, and 70 µm fine measurements are made using a four point cluster target. At each band, the cluster is formed from pointings at offset positions of 0,0; 3.5,0; 3.5,3.5; and 0,3.5 pixels. Three AORs will be used with standard pipeline data products. 



#  Please edit this file with care to maintain the
#  correct format so that SPOT can still read it.
#  Generated by SPOT on:  10/29/2002     16:50:4

HEADER: FILE_VERSION=6.2, STATUS = PROPOSAL

      AOT_TYPE:  MIPS Photometry
     AOR_LABEL:  MIPSIOC-134-1
    AOR_STATUS:  new

 MOVING_TARGET:  NO
   TARGET_TYPE:  FIXED CLUSTER - OFFSETS
   TARGET_NAME:  cv cha
  COORD_SYSTEM:  Equatorial  J2000
     POSITION1:  RA_LON=11h12m27.76s,  DEC_LAT=-76d44m22.3s, PM_RA=-0.01", PM_DEC=-0.034"
     OFFSET_P2:  EAST_ROW_PERP=0.0",	NORTH_COL_PARA=17.47"
     OFFSET_P3:  EAST_ROW_PERP=17.47",	NORTH_COL_PARA=0.0"
     OFFSET_P4:  EAST_ROW_PERP=17.47",	NORTH_COL_PARA=17.47"
OFFSETS_IN_ARRAY:  YES
OBSERVE_OFFSETS_ONLY:  NO
OBJECT_AVOIDANCE:  EARTH = YES, OTHERS = YES

    MICRON_70: IMAGE_SCALE = FINE, FIELD_SIZE = SMALL, EXPOSURE_TIME = 3, N_CYCLES = 2
SPECIAL: IMPACT = none, LATE_EPHEMERIS = NO,SECOND_LOOK = NO
RESOURCE_EST: TOTAL_DURATION=1320.025, SLEW_TIME=54.6, SETTLE_TIME=88.625, SLEW_OVERHEAD=180.0, SPECIAL_OVERHEAD=0.0, UPLINK_VOLUME=3086, DOWNLINK_VOLUME=13534784, VERSION=S6.2.7
INTEGRATION_TIME: MIPS_24=0.0,MIPS_70=50.33165,MIPS_160=0.0





      AOT_TYPE:  MIPS Photometry
     AOR_LABEL:  MIPSIOC-134-2
    AOR_STATUS:  new

 MOVING_TARGET:  NO
   TARGET_TYPE:  FIXED CLUSTER - OFFSETS
   TARGET_NAME:  cv cha
  COORD_SYSTEM:  Equatorial  J2000
     POSITION1:  RA_LON=11h12m27.76s,  DEC_LAT=-76d44m22.3s, PM_RA=-0.01", PM_DEC=-0.034"
     OFFSET_P2:  EAST_ROW_PERP=0.0",	NORTH_COL_PARA=8.93"
     OFFSET_P3:  EAST_ROW_PERP=8.93",	NORTH_COL_PARA=0.0"
     OFFSET_P4:  EAST_ROW_PERP=8.93",	NORTH_COL_PARA=8.93"
OFFSETS_IN_ARRAY:  YES
OBSERVE_OFFSETS_ONLY:  NO
OBJECT_AVOIDANCE:  EARTH = YES, OTHERS = YES

    MICRON_24: FIELD_SIZE = SMALL, EXPOSURE_TIME = 3, N_CYCLES = 1
SPECIAL: IMPACT = none, LATE_EPHEMERIS = NO,SECOND_LOOK = NO
RESOURCE_EST: TOTAL_DURATION=657.425, SLEW_TIME=37.6, SETTLE_TIME=88.625, SLEW_OVERHEAD=180.0, SPECIAL_OVERHEAD=0.0, UPLINK_VOLUME=1209, DOWNLINK_VOLUME=5413920, VERSION=S6.2.7
INTEGRATION_TIME: MIPS_24=48.234497,MIPS_70=0.0,MIPS_160=0.0





      AOT_TYPE:  MIPS Photometry
     AOR_LABEL:  MIPSP-0000
    AOR_STATUS:  new

 MOVING_TARGET:  NO
   TARGET_TYPE:  FIXED CLUSTER - OFFSETS
   TARGET_NAME:  cv cha
  COORD_SYSTEM:  Equatorial  J2000
     POSITION1:  RA_LON=11h12m27.76s,  DEC_LAT=-76d44m22.3s, PM_RA=-0.01", PM_DEC=-0.034"
     OFFSET_P2:  EAST_ROW_PERP=0.0",	NORTH_COL_PARA=34.44"
     OFFSET_P3:  EAST_ROW_PERP=34.44",	NORTH_COL_PARA=0.0"
     OFFSET_P4:  EAST_ROW_PERP=34.44",	NORTH_COL_PARA=34.44"
OFFSETS_IN_ARRAY:  YES
OBSERVE_OFFSETS_ONLY:  NO
OBJECT_AVOIDANCE:  EARTH = YES, OTHERS = YES

    MICRON_70: IMAGE_SCALE = DEFAULT, FIELD_SIZE = SMALL, EXPOSURE_TIME = 3, N_CYCLES = 1
SPECIAL: IMPACT = none, LATE_EPHEMERIS = NO,SECOND_LOOK = NO
RESOURCE_EST: TOTAL_DURATION=711.925, SLEW_TIME=37.2, SETTLE_TIME=88.625, SLEW_OVERHEAD=180.0, SPECIAL_OVERHEAD=0.0, UPLINK_VOLUME=1560, DOWNLINK_VOLUME=5413912, VERSION=S6.2.7
INTEGRATION_TIME: MIPS_24=0.0,MIPS_70=37.748737,MIPS_160=0.0

Data Reformatting Requirements

Array Data Desired:

24 µm, 70 µm

Data Reformatting Option:

Ideally, one fits file per cluster position per AOR. Each such fits file would contain all the DCEs for that cluster position.
Special Instructions:

Task Dependencies

Calibration Dependencies

Output and Deliverable Products

The output will be resolved measurements of the 24 micron and 70 micron flux densities of CV Cha and CW Cha. Potentially, a science paper will be written on the results, if the unexpected result is obtained that one star dominates the infrared excess of the pair.

Data Analysis

Reduced, coadded, and subsampled images will be produced using the pipeline data products and some variation of the HST drizzle algorithm. Non-linear least-squares fitting will then be used to determine the x,y position and flux density of each component, using Tiny Tim PSFs to describe the SIRTF beamshape.

Software Requirements

Actions Following Analysis

Results posted to SSC MIPS web pages as demonstration of what can be done using MIPS 70 µm fine scale imaging. Possible science paper.

Failure Modes and Responses

Image smearing would prevent a useful result. If smearing is seen, the cause must be determined (telescope pointing or scan mirror instablility), corrected, and the program repeated.

Additional Notes