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Combination of ASM or AF11 windows for the imaging of structured objects

Combination of ASM or AF11 windows for the imaging of structured objects. Claire Dollet DMS meeting, Brussels 19-20 december 2003. ASM WA0T48. ASM WA0T25. AF11 WA11T26. 10+6+10 rows. G 16-20. G 12-16. G 16-20. complementarity of the windows at the end of the mission. Situation.

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Combination of ASM or AF11 windows for the imaging of structured objects

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  1. Combination of ASM or AF11 windows for the imaging of structured objects Claire Dollet DMS meeting, Brussels 19-20 december 2003

  2. ASM WA0T48 ASM WA0T25 AF11 WA11T26 10+6+10 rows G 16-20 G 12-16 G 16-20 complementarity of the windows at the end of the mission Situation Transmission of a window for each on board detected object definition according to the magnitude and the rows of CCDs DMS 19/12/2003

  3. Restored F Relation of dependence Relation between the patches F 1, al1, ac1 3, al3, ac3 n, aln, acn DMS 19/12/2003 2, al2, ac2

  4. Relation • Ill-conditioned system Wi=Hi (i, ali, aci) F p x m n x m n x p • Around N=100 observations during the 5-years mission DMS 19/12/2003

  5. Least mean square Smooth constraint Tikhonov algorithm DMS 19/12/2003

  6. Binary systems small angular separation 0.2” & small magnitude difference mag= 0.94 =0.196” mag=0.66 = 0.173” mag=0.22 =0.184” mag= 0.34 =0.151” DMS 19/12/2003

  7. Binary systems 0.2” < angular separation < 0.3” & small magnitude difference mag= 1.55 =0.254” mag=0.72 =0.270” mag= 0.54 =0.295” mag= 1.38 =0.225” mag= 0.34 =0.210” mag= 0.71 =0.212” DMS 19/12/2003

  8. Combination of 100 ASM windows mag increases with a step of 0.5 magnitude Combination of 100 AF11 windows mag = 0 / 1.5 / 2 / 2.5 / 3 / 3.5 Magnitude difference Angular separation 0.19 arcsec Primary G mag =18.5 Variable secondary G mag DMS 19/12/2003

  9. Combination of 100 ASM windows mag increases with a step of 0.5 magnitude Combination of 100 AF11 windows mag = 0 / 1.5 / 2 / 2.5 / 3 / 3.5 Magnitude difference Angular separation 0.24 arcsec Primary G mag =18.2 Variable secondary G mag DMS 19/12/2003

  10. 94 observations & not uniform Position angle distribution 100 observations & uniform DMS 19/12/2003

  11. Working process… Comparison Automatic estimation Tests carried out with an algorithm of CLEAN type => reveal the secondary star by subtraction the brightest star. currently not satisfying due to the lack of pixels representing the components • Method allowing no assumption on the contents of the fields. • Once the binary is identified, a parametric method will be more efficient for the estimation of the flux and the angular separation of the components. DMS 19/12/2003

  12. Complex environment How will the structured objects be restored from the different patches? M100 galaxy Positions of ASM Windows DMS 19/12/2003

  13. ASM AF11 M100 DMS 19/12/2003

  14. ASM AF11 M100 DMS 19/12/2003

  15. Synthesis • No hypothesis on the contents of the field But assumption of stability for the magnitude and the position during the mission. • Method less efficient than parametric ones for binaries But useful for studies of complex environments • Gathering all the windows of a same field: ASM & AF11 together, BBP windows… DMS 19/12/2003

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