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Title: ETC and per<strong>for</strong>mance analysis Reference: MUSE-MEM-SCI-051 Issue: 1.3 Date: 28/01/04 Page: 29/14 10.2 MUSE spatial PSF in HR mode 10.2.1 AO Gen II, good seeing conditions TabEEgenII good := 0 1 2 3 4 5 6 0 1 2 3 4 5 6 7 8 9 0.025 0.0735 0.1362 0.2195 0.3019 0.1954 0.2321 0.05 0.1848 0.2586 0.3131 0.4066 0.4835 0.4297 0.075 0.2183 0.3111 0.4008 0.4611 0.5327 0.5782 0.1 0.2468 0.3357 0.4319 0.505 0.557 0.6007 0.125 0.2628 0.3537 0.4422 0.5169 0.5721 0.6152 0.15 0.2787 0.3699 0.4597 0.5356 0.5931 0.6263 0.175 0.3032 0.3858 0.4753 0.5436 0.6014 0.6355 0.2 0.3201 0.4018 0.4902 0.5581 0.6089 0.6508 0.225 0.3375 0.4182 0.4976 0.565 0.6224 0.6574 0.25 0.3642 0.4349 0.5126 0.5786 0.6288 0.6636 i := 0.. 18 j := 1.. 6 EE := sousmatrice TabEEgenII i good , i , i , 1, 6 ⎛ ⎜ ⎜ ⎜ ⎜ ⎜ ⎝ ⎞ 0.465 0.55 ⎟ ⎜ 0.65 ⎟ λ EE := ⎜ ⎟⋅µm 0.75 ⎟ 0.85 ⎟ 0.93 D EEi := TabEEgenII goodi , 0 k := 0.. 5 T := k ⎠ cspline( λ EE , EE k ) Note that MUSE IQE is now included in ensquared energy ( ) T ( ) EEgenII good ( λ , k) := interp T , λ k−1 EE , EE , λ k−1
Title: ETC and per<strong>for</strong>mance analysis Reference: MUSE-MEM-SCI-051 Issue: 1.3 Date: 28/01/04 Page: 30/14 10.3 Number of spatial pixels In the case of unresolved objects and in good seeing conditions we will sum up 3x3 spatial pixels to recover a fraction of the object flux, this correspond to 0.6x0.6 arcsec² in WF mode and 0.075x0.075 arcsec² in HR mode k spa_good := 3 EEnoao good ( λ V , k spa_good ) 0.446 EEgenI good ( λ V , k spa_good ) 0.583 EEgenII good ( λ V , k spa_good ) 0.311 ( ) = 0.496 = EEnoao good λ I , k spa_good ( ) = 0.655 = EEgenI good λ I , k spa_good ( ) = 0.489 = EEgenII good λ I , k spa_good In the case of unresolved objects and in poor seeing conditions we will sum up 4x4 spatial pixels to recover a fraction of the object flux, this correspond to 0.8x0.8 arcsec² in WF mode and 0.1x0.1 arcsec² in HR mode k spa_poor := 4 EEnoao poor ( λ V , k spa_poor ) 0.373 EEgenI poor ( λ V , k spa_poor ) 0.49 ( ) = 0.417 = EEnoao poor λ I , k spa_poor ( ) = 0.563 = EEgenI poor λ I , k spa_poor Note that this choice is somewhat arbitrary. It is a trade between S/N and spatial resolution. Optimum summation should allow increase of the S/N while keeping the spatial resolution.
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SCIENCE DOCUMENTS SECTION Title Ver
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The median descendant mass of galax
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with the slicer development for NIR
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Science Case Coordinator : R. Bacon
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Title: Science Case Reference: MUSE
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Keck Telescope (Rhoads et al. 2000)
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Assuming that most of the black hol
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Page 96 and 97: 5. Solar system Title: Science Case
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Page 120 and 121: ANNEX - ETC mathcad sheet Roland Ba
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Title: Science preparation and key
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Reference: MUSE-MEM-SCI-054 Issue:
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