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Title: ETC and performance analysis Reference: MUSE-MEM-SCI-051 Issue: 1.3 Date: 28/01/04 Page: 33/14 Signal to Noise SN Main ETC Formula ( ) := n⋅K O SN F O , n, t, F S , RN , DC , K O , K S , K RN , K DC ⋅F O ⋅ t⋅ ⎛ ⎜ ⎜ ⎝ K O ⋅F O ⋅ t + K S ⋅F S ⋅ t ... + K RN ⋅RN 2 + K DC ⋅DC⋅ t ⎞ ⎠ − 1 2 Object Flux F O ( ) := a ← n F O SN, n, t, F S , RN , DC , K O , K S , K RN , K DC b ← ⎛ ⎜ ⎝ K O ⋅ t K O ⋅ t SN ⎞ ⎠ 2 c ← K S ⋅F S ⋅ t + K DC ⋅DC⋅ t + K RN ⋅RN 2 Integration time t ( ) := a ← n tSNn , , F O , F S , RN , DC , K O , K S , K RN , K DC b + b 2 + 4⋅a⋅c 2⋅a b ← ⎛ ⎜ ⎝ K O ⋅F O SN K O ⋅F O c ← K RN ⋅RN 2 ⎞ ⎠ 2 + K S ⋅F S + K DC ⋅DC b + b 2 + 4⋅a⋅c 2⋅a Where F O is the Object Flux ( erg s − 1 ⋅ ⋅ cm − 2 ) if it is a surface brightness, flux should be in arcsec − 2 if it is a continuum source, flux should be in A − 1 and F S is the Sky Flux ( erg⋅s − 1 ⋅cm − 2 ⋅A − 1 ⋅ arcsec − 2 ) and n is the number of exposures and t is the integration time in sec of one exposure and RN is the readout noise in electron per pixel and DC is the dark current in electron per pixel and per hour The coefficient K O transform the object flux in photons per second the coefficients K O , K S , K RN , K DC are defined below ( ) f s ⋅∆ s K O f s , f a , ∆ s , ∆ a , λ, A m := 2 ⋅f a ⋅∆ a ⋅T MUSE ( λ) ⋅Area VLT ⋅ ( ) Extinct λ , A m λ ⋅ hc ⋅
Title: ETC and performance analysis Reference: MUSE-MEM-SCI-051 Issue: 1.3 Date: 28/01/04 Page: 34/14 Where f s is the fraction of total flux enclosed in a spectral bin and f a is the fraction of total flux enclosed in a spatial bin and ∆ s is the size of a spectral bin and ∆ a is the linear size of a spatial bin in arcsec and λ is the wavelength and A m is the airmass and T MUSE is the MUSE+VLT total throughput and Area VLT is the effective collective area of VLT primary mirror and Extinc is the extinction absorption coefficient at Paranal Note that when the flux is a flat continuum source (flux per A) f s must be set to 1 and ∆ s to the size of the spectral bin and when the flux is an emission source (flux not per A) f s must be set to the flux fraction enclosed in the bin and ∆ s to 1 Note that when the flux is a surface brightness source (flux per arcsec²) f a must be set to 1 and ∆ a to the size of the spectral bin and when the flux is a total flux (flux not per arcsec²) f a must be set to the flux fraction enclosed in the bin and ∆ a to 1 The coefficient K S transform the sky flux in photons per second 2 ( ) := ∆ s ⋅∆ a K S ∆ s , ∆ a , λ λ ⋅T MUSE ( λ) ⋅Area VLT ⋅ hc ⋅ The coefficient K RN is the number of summed bin The coefficient K DC is the number of summed pixels back
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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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Title: Science preparation and key
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Reference: MUSE-MEM-SCI-054 Issue:
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