Thank you Joanna, I will ask Yuji or Takahiro for producing similar information from Phenix. The specific luminosity from STAR is fairly stable, and there are a few bunches which are apparently wrong. So I do not think we need the text file for the specific luminosity. We can count them from the plots. As far as I scan with my eyes and my MicroSoft mouse, following anomaly bunches are found (here I have ignored the default wrong bunches 1st,11th, and two groups of 5-bunches) fill | bxing of specific lumi | consistency with CNI ------------------------------------------------------------- 2207 46 missing blue 26 missing 2222 41 missing or enhanced blue 21 missing 2233 51 reduced no correlation with CNI 2235 51 55 enhanced no correlation with CNI 2246 12,13, 32,33, 52,55 reduced reduced in both blue and yellow 2269 10 reduced or enhanced yellow 10 missing 2281 25 reduced yellow 25 missing ------------------------------------------------------------- As you know, following is the bunch # correlation at STAR and PHENIX. K: kicked bunch A: Abort gap 0: every 10 bunches *: bunch (STAR) 1 11 21 31 41 51 Y 0*********K*********0*********0*********0*********0****AAAAA B 0*********0****AAAAA0*********K*********0*********0********* 41 51 1 11 21 31 C 0*********K****AAAAA0*********K*********0*********0****AAAAA (PHENIX) 1 11 21 31 41 51 Y 0*********K*********0*********0*********0*********0****AAAAA B 0*********0*********0*********0****AAAAA0*********K********* 21 31 41 51 1 11 C 0*********K*********0*********0****AAAAA0*********K****AAAAA The 3rd line "C" is the product of the two rings (observed at each experiment). Then if we know a certain bunch in blue is wrong, we need to discard the corresponding two bunches in yellow to keep the consistency between the STAR and PHENIX (since I do now think it is a good idea to make different bunch selection sets for PHENIX and STAR). Vise versa for the bad bunch in yellow. As a result from input from Joanna, this is the list of bunches which will be thrown away. fill origin bunch selection as a result ------------------------------------------------------------- 2207 blue 26 missing discard B:26 Y:6,46 2222 blue 21 missing discard B:21 Y:1,21 2246 12,13, 32,33, 52,55 reduced discard 12,13,32,33,52,55 both rings 2269 yellow 10 missing discard B:50,30 Y:10 2281 yellow 25 missing discard B:5,45 Y:25 ------------------------------------------------------------- -- Osamu p.s. For the fill 2233 and 2235, the apparent correlation between CNI and STAR was not confirmed. We should postpone the decision til the input from PHENIX is available. From: Joanna Kiryluk Subject: Re: notes on RHIC polarimeter meeting Date: Tue, 13 Aug 2002 15:38:41 -0700 (PDT) > > > Hello Osamu, > > > Who should I ask for the specific luminosity info from experiments? Could > > anybody nominate the persons for STAR and PHENIX? > > STAR specific luminosity plots: > www.physics.ucla.edu/~joanna/WCM_Data > > This is done run by run (STAR), fill number is included in > the title of each plot. STAR run number is 30XXYYY where XX=day, > YYY-run number. So to look at plot from e.g. 18January, look at > any of Run30180**_WCM.ps > This is done for runs where we have reliable luminosity information > from the scalers (11- 23January) > > I can prepare this specific luminosity info in any format you like > (text file instead of ps), just let me know. > > Regards, Joanna > >