1. The Fill Pattern for 2006 Tai Sakuma
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
4/12/2007
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.
4/12/2007
Tai Sakuma

3. and uploaded to the above URL
Result: Fill Pattern
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.
4/12/2007
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.
4/12/2007
Tai Sakuma

5. 4/12/2007
Tai Sakuma

6. The result of the comparison
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 kicked bunches are sometimes above the threshold
The next slide has a bigger plot
4/12/2007
Tai Sakuma

7. 4/12/2007
Tai Sakuma

8. I plotted the fill patterns with the BBC coincidence rates for every bunch for all 127 fills.
PDF file (127 pages)
4/12/2007
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.
4/12/2007
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
4/12/2007
Tai Sakuma

11. End