STAR Flow, Chirality and Vorticity PWG

[rishabh <rishabh AT rcf.rhic.bnl.gov>]

Dear ShinIchi,

Thank you so much for your email. I tried recentering the Q-vector 
event-wise but still could not see a significant flattening of the event 
plane angle. However, trackwise phi-weight correction was able to 
visibly flatten the event plane distribution. Please find attached the 
slides comparing the two methods of flattening the event plane 
distribution in Au+Au collisions at √sNN = 54.4 GeV.
So for my analysis, I am going ahead with the phi-weight correction.

Thanks and regards,
Rishabh Sharma



On 2022-03-16 15:20, ShinIchi Esumi via Star-fcv-l wrote:
> Dear Rishabh
> I’m questioning the same thing to everyone yesterday in the special
> pwg session,
> it looks like you also have the similar problem in your re-centering
> calibration, as we
> still see about a half of the 1st moment of the non-flatness even
> after the re-centering
> calibration in your page 8, which tells me there is some problem in
> the method. You
> could look at the Priyanshi’s slide page 7, where we only see the
> higher order contributions
> than 1st order moments in a remaining non-flatness after the
> re-centering calibration,
> that is what is supposed to be, although the formula in the page 6 has
> some issues.
> So please make sure your re-centering correction is OK or not. It is
> flat after the final
> Fourier shift correction, so that the final results might still be OK,
> but it would be better
> to do it right. In stead of re-centering the q-vector, which should be
> done in event-wise,
> one can do an inverse weighting factor correction (track-wise) with
> measured azimuthal
> distribution. You can go back to the famous "flow bible" from Sergei
> and Art in '96.
> Best regards, ShinIchi
>
> > 2022/03/14 3:16、subhash via Star-fcv-l <star-fcv-l AT lists.bnl.gov>のメール:
> >
> > Dear All,
> >
> > We will hold an additional FCV meeting this Tuesday, March 15, at 9:30 
> > am EST. This is a special meeting to accommodate some QM talk/posters 
> > for which we have not received the request for preliminary. We would 
> > request you to make a short presentation following:
> > https://drupal.star.bnl.gov/STAR/system/files/Prelim_Request_template.pdf
> >
> > Since the QM is in a few weeks from now, it will be too late for us to 
> > review and sign off your analysis if you can't present. Thanks for 
> > your understanding.
> >
> > Best regards,
> > Jiangyong, Prithwish and Subhash
> >
> >
> > The tentative agenda can be found below:
> > https://drupal.star.bnl.gov/STAR/blog/jjiastar/bulkcorr
> >
> > (Special Meeting for QM-approval) March 15, 2022:
> > 1. Joey Adams -- lambda polarization
> > 2. Gavin Wilks -- phi spin alignment
> > 3. Shuai Zhou -- PID v2 BES
> > 4. Diyu Shen -- charge dependent v1
> > 5. Aditya Prasad -- charge dependent v1
> > 6. Eddie Duckworth -- net proton v1
> > 7. Niseem Magdy -- flow momentum correlation
> >
> > We shall use the FCV zoom link:
> > https://urldefense.com/v3/__https://stonybrook.zoom.us/j/95735410810?pwd=M2JRZDBDSng4MG5SYmx6dlppYXhLZz09__;!!P4SdNyxKAPE!UXhP_DS8ys-TdWPw0_Vm4ATdCQdbWUfil5xQC2X14Niv1NnkB5575iHyZ29jG4Z4AVeuU8wc$
> > Meeting ID: 957 3541 0810
> > Passcode: 486227
> >
> >
> > _______________________________________________
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> > Star-fcv-l AT lists.bnl.gov
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>
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Attachment: Recentering vs phi-weight.pdf
Description: Adobe PDF document