Minutes of the E00-102 Meeting
Tuesday, July 9 2002

Fissum

KF/SG/DH/WH/BR/AS/LW

o We began with a discussion of the current status of 
  the data analysis.  Wendy summarized.  Earlier this 
  year, using the ESPACE version which referred to the 
  HRS as 'electron' and 'hadron', the detector 
  optimization was more-or-less finished, but looked a 
  bit strange.  The y_target optimization was the next 
  step.  It was then discovered that the y_target 
  optimization could only be performed with the ESPACE 
  version that referred to the spectrometers as 'right' 
  and 'left'.  Thus, the work with the 'eh' ESPACE 
  version stopped, and everything was redone with the 
  'lr' ESPACE version (which occured after redoing all 
  the modifications Wendy did for our detector stack 
  configuration).  The waterfall target had to be built 
  in to the 'lr' version from scratch.

o this was done, and now all the spectra, particularly 
  t_corr, look *much* better.  Unexplained quirks in 
  the data are largely gone.  The beta optimizations 
  look good.  Coincidence timing vs. (x_fp or theta) 
  for example still have structure as a function of 
  scintillator paddle that needs to be taken out by 
  hand.  S0 vs. S0 coincidence timing spectra seem a 
  little broader than expected.  The thought is that 
  time-walk corrections have not yet been done.  Wendy 
  will check to see if this is the case.  If they have 
  not been done, she will implement them and 
  investigate the results.  We hope that including S0 
  in the timing optimization will improve the S/N 
  ratios in the coincidence timing.  If they have in 
  fact already been done, we will stop fooling around 
  with S0 timing, and use the S0 information only to 
  quantify the S1 and S2 detection efficiencies.

o at this point, the detector data base optimization 
  will be considered finished, and it will be time to 
  investigate the optics.  Rumour has it that Nilanga 
  has some software that can be used to investigate 
  just how well our present optics databases are doing, 
  and if and where there is room for improvement. We 
  anticipate the HRSr is OK (at nominal 1 GeV/c), but 
  that the HRSl (at nominal 4 GeV/c) could possibly be 
  improved.  We are hoping that the diagnostics will 
  reveal that the 4 GeV/c data base is good enough for 
  the first pass analysis, in which case we will wait 
  for RCS to evaluate their extended y_target 4.3 GeV/c 
  databases and 'copy' them for the second pass.  This
  will allow us to get going on the physics analysis 
  and really develop an idea of what we have on disk.  
  If the diagnostics indicate the databases are worse 
  than we believe, we will have to stop and evaluate 
  just how bad things are.

o We feel it is also time to start building the 
  experiment in pseudo space.  Kevin will use Mattias' 
  SQL databases for the needed information to create a 
  shell-driven version of the experiment in MCEEP.  In 
  this case, setting up the shells and the automation 
  is more important than which version of MCEEP is 
  being used.  Simultaneously, he (or Jose/Javier) 
  will build into the MCEEP code itself the latest 
  version of the Udias code (so we don't have to rely 
  on spectral functions).  Further, Wendy has been 
  developing a version of MCEEP which uses a SIMC-style 
  trace through the spectrometers which agrees (at 
  present) to the upstream face of the dipole with the 
  SIMCish model of the HRS2.  She will also pursue this.  
  When all the modifications are finished, we can swap 
  in the new executable, and create a very detailed 
  pseudo experiment for comparison to data. 

o We then moved on to other subjects.  Arun pointed 
  out that we are not doing ourselves any favours by 
  providing people improperly documented transparencies.  
  We agreed that in the future, all transparencies will 
  be properly labelled, and will read: (Preliminary, 
  E00-102, Hall A) at least! Further, we will do our 
  best to circulate transparencies within the core 
  group prior to releasing them to the requestor.

o We then went through a design for a Gordon Conference 
  poster. The design will include:
  - abstract as per the proposal
  - electron kinematics, QE
  - general (e,e'p)
  - how we fold the cross sections to get Alt and Rlt
  - spectrometer figure
  - waterfall target figure/photo
  - figure/table with hadron angles and pmiss
  - 'online' spectrum showing Pmiss vs. Emiss, 
    projected onto Emiss, coincidence timing and the 
    like (as per PRC fig)
  - anticipated data as per the proposal with fewer 
    curves
  - plot of Juncai's PRL cross sections and then 
    linearized 
  Kevin will bring a set of draft poster figures to 
  the next meeting for everyone to review and we'll cut 
  and paste and scribble something together.

o finally, we discussed the PRC article that is now well
  underway.  The experiment and data analysis sections 
  are finished.  The p-shell data is more-or-less 
  archived.  We haved decided to include Kelly's 
  calculation suite which examines the behaviour of the 
  SFs as a function of Q^2 'for now'.  We will also 
  include all the figures and discussions from Juncai's 
  PRL.  The Udias calculation suite is in place.  
  Nilanga has provided his continuum data in files for 
  tabulation.  We will also include all the figures and 
  discussions from Nilanga's PRL.  Further, Kevin will 
  contact Ryckebusch to see if he would like to contribute 
  anything new in exchange for coauthorship.  We may 
  include the dip results in an Appendix.  Kevin will 
  try to have a distributable draft ready by mid-August.
  
o next meeting 020716 (next Tuesday) at 14:00 in B101 
  (the same room).  Preliminary agenda is to go over the 
  draft GRC poster...