deletions | additions       diff --git a/section_Experimental_Setup_An_optimal__.tex b/section_Experimental_Setup_An_optimal__.tex  index d0f9229..ea647fb 100644  --- a/section_Experimental_Setup_An_optimal__.tex  +++ b/section_Experimental_Setup_An_optimal__.tex 
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940-nm photons are detected by a Si APD (Perkin-Elmer) to herald the presence of $1283$-nm photons and generate a synchronization signal that is used trigger the pulse generator.  The marginal bandwidth of the signal photons is larger than $10$ nm, and to match it to the acceptance bandwith of BS-FWM, centered at $1284.45$ nm with $\delta\omega_{BS} = 0.5$ nm FWHM), both heralding and signal photons are spectrally filtered, the former with an holographic .5 nm filter (??), the latter with the free space tunable grating setup.  We monitor the noise at one of the outputs while the fiber is changing temperature. If we collect the full signal setup, where contributions come over $12$ nm bandwidth of the WDM, we can observe the temperature dependency (fig 5). (fig. \ref{fig:raman}).  The reduction of noise is limited to 2 orders of magnitude, which is expected because of the amount of fiber not placed in the cryostat (about $1$ meter over $100$ m of fiber in the cooler). Taking losses into account, we calculate the probability of generating a photon of noise is, while being already extremely low compared with other BS demonstrations, about 1 photon of noise per gate in highest efficiency reported \cite{Clark_2013}), can be additionally filtered both temporally and spectrally to match the acceptance bandwidth.