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The Fill Pattern for 2006

The Fill Pattern for 2006. 4/12/2007. Tai Sakuma. The spin dependent yields and the relative luminosity should use the same set of the bunches for the spin asymmetries. Unfilled Bunches are in the abort gaps kicked bunches bunches which are lost before they enter RHIC

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The Fill Pattern for 2006

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  1. The Fill Pattern for 2006 4/12/2007 Tai Sakuma • The spin dependent yields and the relative luminosity should use the same set of the bunches for the spin asymmetries. • Unfilled Bunches are • in the abort gaps • kicked bunches • bunches which are lost • before they enter RHIC • after they enter RHIC Tai Sakuma

  2. How to determine fill pattern • 127 RHIC fills • Fills for which there are both CDEV files and scaler files and during which STAR took physics data • One fill pattern for one RHIC fill • For a bunch to be counted as filled, this bunch needs to be filled the entire period of the RHIC fill • For example, if a bunch was lost during a RHC fill, this bunch is not counted as filled. • Determine from CDEV files • CDEV was recorded every 4 minutes. • Tag <measuredFillPatternM> • If <measuredFillPatternM> changed during a RHIC fill, take logical AND. • If one CDEV file says unfilled, the bunch is unfilled. • Bunch 20 and 60 are fixed to be unfilled, since these are kicked bunches • Confirm with the BBC coincidence rates • Compare with what was observed at STAR IR. Tai Sakuma

  3. Result: Fill Pattern http://deltag5.lns.mit.edu/~sakuma/protected/star/scaler/2006/data/fillPatternBxRun6_070412.txt • I stored the result in a text file which looks like the image on the right • and uploaded to the above URL • The username and password are the same as the protected website at RCF. Tai Sakuma

  4. Comparison with BBC coincidence rates • Use the board 11 bit16 and the board 6 timebin • Primarily, the board 11. Board 6 for the fills during which the Board 11 was not running. • Quantitative comparison requires one number for each bunch that quantify the degree to which the bunch is filled • If this quantity can reproduce the fill pattern, the fill pattern will be confirmed by the BBC coincidence rates. • The minimum BBC coincidence rates for each bunch for each fill can be such a quantity • The next slide has sample plots. • The plot shows the BBC coincidence rate for the bunch 76 and 22 for the fill 7722. • While the bunch 76 is filled, the bunch 22 is unfilled. • The number of the entry for each plot is equal to the number scaler files from the board 11 for this fill. • For these bunches, the minimum coincidence rates are the rates from the last scaler file. Tai Sakuma

  5. Tai Sakuma

  6. The fill pattern is consistent with the BBC coincidence rates. The thresholds are 200 counts/sec for 200 GeV 6 counts/sec for 62 GeV The unfilled bunches and the filled bunches are well separated for the transverse runs and 2nd longitudinal runs. The result of the comparison • The kicked bunches are sometimes above the threshold • The next slide has a bigger plot Tai Sakuma

  7. Tai Sakuma

  8. I plotted the fill patterns with the BBC coincidence rates for every bunch for all 127 fills. • PDF file (127 pages) http://deltag5.lns.mit.edu/~sakuma/protected/star/scaler/2006/images/UnfilledBx.pdf Tai Sakuma

  9. Proposal on the fill pattern • I propose to use this fill pattern for the spin analyses in the spin PWG. • The fill pattern can be found at this URL. http://deltag5.lns.mit.edu/~sakuma/protected/star/scaler/2006/data/fillPatternBxRun6_070412.txt Tai Sakuma

  10. Summary • The same fill pattern should be used for the spin dependent yields and the relative luminosities for the spin asymmetries • The fill pattern was uniquely determined for every bunch from the CDEV files • The fill pattern was consistent with what was observed at the STAR IR with BBC • I proposed to use the fill pattern for the spin analyses in the spin PWG Tai Sakuma

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