deletions | additions       diff --git a/section_Experimental_Setup_An_optimal__.tex b/section_Experimental_Setup_An_optimal__.tex  index 46a7b1c..fedf4ce 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 $0.3$ nm filter (OptiGrate), the latter with the free space tunable grating setup.  \textit{Superseeded}  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. \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.