Attendees: Guang Yang (GY), Ciro Riccio (CR), Chang Kee Jung (CKJ), Abraham Teklu (AT), Alex Ramirez (AR), Andriaseta Sitraka (AS), Eric Chong (EC), Ki-Young Jung (KYJ), Shih-Kai Lin (SL), Sunwoo Gwon (SG), Cesar Jusus Valls (CJV), Martini Tzanov (MT), Mikhail Danilov (MD), Nataliya Skrobova (NS), Perri Zilberman (PZ), Ki-Young Jung (KYJ), Christopher Mauger (CM)
Ciro Riccio - Updated on xsec fitter
Abraham Teklu - Update on the neutron energy scale systematics
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CM: The width of the gamma peak? AT: 20-30 tick
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CM: It would be useful to look at the time structure from the beamline, the gamma flash may contain pi0 The gamma flash should essentially be peaked and provide us a time-resolution. The smearing effects are from detector.
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CKJ: Do we have enough statistics in high energy? AT: Yes.
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MD: What we know about the time calibration of different channel? GY: We didn't correct by the fiber length.
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CKJ: Many effect can contribute. GY: Fiber length is the major error. CKJ: But we know it very well. CM: We should decouple the effects. GY: We can use cosmics.
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MT: Resolution is very important, but also the bias. If you have a bias in time you bias the energy. How do you define the T0? GY: T0 is fixed for every channel.
Eric Chong - Status of efficiency correction
Guang Yang - Update on invisible scattering scaling
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CKJ: Slide 6: What do you mean with weight 0? GY: I remove all the event with elastic scattering. CKJ: Why does it grow as it goes it in the detector?GY: It could be a detector effect. CKJ: You need to figure this out.
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MD: Why invisible scattering is so important? GY: We have 20 PE threshold.
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CKJ: You can allineare your detector. GY: We know the detector is not straight. CKJ: You can measure it and take it out.