STAR Flow, Chirality and Vorticity PWG

["Zuowen Liu" <liuzw AT mails.ccnu.edu.cn>]

Dear Subhash,

Thanks a lot for your nice suggestions.

I have implemented all of them into the proceeding.

For the typos, I checked again and fixed them.

Kindly find the updated proceeding by the link:

https://drupal.star.bnl.gov/STAR/system/files/qm23proceeding_Zuowen.pdf

Thanks again for your great help.

Best regards,

Zuowen

 

 

------------------ Original ------------------

From:  "subhash"<subhash AT rcf.rhic.bnl.gov>;

Date:  Wed, Nov 29, 2023 04:47 PM

To:  "Zuowen Liu"<liuzw AT mails.ccnu.edu.cn>;

Cc:  "star-fcv-l"<star-fcv-l AT lists.bnl.gov>;

Subject:  Re: [Star-fcv-l] STAR presentation by Zuowen Liu for Quark Matter 2023 submitted for review

 

Dear Zuowen,

Nice proceedings. Please consider running a latex spell checker to spot
the typos. In general, at several places sentences are not formatted
properly. I tried to correct. Please get it proof read by a colleague in
your group to check if my interpretations are proper. The followings are
a few suggestions for your consideration:


l#1: you may consider adding "at RHIC" for completeness

l#5: In this proceeding, --> In these proceedings,

l#5,6: may be: transverse momentum dependence of the rapidity slope of
directed flow (dv1/dy|y=0) for π+ and K0S in Au+Au ... and 3.9 GeV.

l#7: Both π+ and K0S show negative

l#8: "spectator shadowing could result in anti-flow at low pT "
--> spectator shadowing may lead to anti-flow at low pT.

"Furthermore, Number of Constitute Quark (NCQ) scaling of v2 at √ sNN =
3.2 GeV was observed which is completely broken"
--->
Furthermore, we observe a complete breaking of Number of Constitute
Quark (NCQ) scaling of elliptic flow (v2) at √sNN = 3.2 GeV.
It implies that the dominance of hadronic degrees of freedom occurs at
√sNN = 3.2 GeV and below.

l#12: At last, --> Finally,

"and physical implications are discussed."
--> and the implications in the context of highly dense baryonic matter
are discussed.

l#16: In this contribution, we present the most recent measurements ...
in Au + Au collisions at √sNN = 3.0 - 3.9 GeV in STAR Fixed Target mode

l#18:  For identification of π±, K±, and p, a combination of Time
Projection Chamber (TPC) and Time of Flight (TOF) is used

l#20-23: Suggest:
The left panel of Fig. 1 illustrates the rigidity (p/q: particle
momentum divided by charge) dependence of ionization energy loss (dE/dx)
in the TPC. The dashed line represents the theoretical ionization energy
loss curve for particles passing through the TPC. Particle
identification by TOF is based on the particle mass square (m^2)
distribution, which can be obtained from the particle velocity (β).

l#24-26: suggestion:
Moreover, the Kalman Filter (KF) particle package [3], where the
covariance matrix of reconstructed tracks is taken into account, is
employed to reconstruct weak decay particles (KS0 and Lambda).

l#26-28: suggestion:
An example of reconstructing the invariant mass using the KF particle
package is demonstrated with the KS0 meson in the right panel of Fig. 1.

l#30:  kaon --> Kaon

l#31-33:
The anti-flow of kaons was first observed  .....  6 A GeV. It was
attributed to the repulsive potential associated with the strange quark
in K0S.

l#33-36: suggestion:
We have observed anti-flow behavior in kaons and pions for pT < 0.6
GeV/c in mid-central Au + Au collisions at 3.0, 3.2, 3.5, and 3.9 GeV
using the fixed target data from STAR.

l#37-43: suggestion:
The hadronic transport model JAM [5] calculations are compared with
experimental data at 3.9 GeV. The JAM model in hadronic cascade mode
(blue band) can successfully capture the anti-flow pattern at low pT for
π+ and K0S, even without the inclusion of a kaon potential [4]. However,
the JAM model with baryonic mean field (red band) tends to overestimate
the v1 slope for π+ and K0S. Additionally, the JAM mean field without
spectator contribution (black band) exhibits a larger v1 slope compared
to the one with spectators. The data-model comparisons above suggest
that the shadowing effect [6] from the spectator may also play a
significant role in generating anti-flow at low pT.


l#45-48: suggestion
The left and right panels of Fig. 3 illustrate the number of constituent
quarks (nq) scaled elliptic flow (v2/nq) as a function of transverse
kinetic energy ((mT − m0)/nq) for particles (π+, K+, K0S, p, and Λ) and
antiparticles (π−, K−, and K0S), respectively.

l#48-52: please re-format to clarify the sentence.



Thanks and regards,
Subhash


On 2023-11-25 12:05 PM, Zuowen Liu wrote:
> Dear Subhash,
>
> Kindly find the updated proceeding by the link:
> https://drupal.star.bnl.gov/STAR/node/65884
> Thank you.
>
> Best regards,
> Zuowen
>
> ------------------ Original ------------------
>
> From:  "Zuowen Liu"<liuzw AT mails.ccnu.edu.cn>;
> Date:  Fri, Nov 24, 2023 04:41 PM
> To:  "star-fcv-l"<star-fcv-l AT lists.bnl.gov>;
> Cc:  "subhash"<subhash AT rcf.rhic.bnl.gov>;
> Subject:  Re: [Star-fcv-l] STAR presentation by Zuowen Liu for Quark
> Matter 2023 submitted for review
>
> Dear Subhash,
>
> Thank you for the kind reminder.
> I would short it to four.
>
> Best regards,
> Zuowen
>
> ------------------ Original ------------------
>
> From:  "subhash via Star-fcv-l"<star-fcv-l AT lists.bnl.gov>;
> Date:  Wed, Nov 22, 2023 04:15 PM
> To:  "star-fcv-l"<star-fcv-l AT lists.bnl.gov>;
> Cc:  "subhash"<subhash AT rcf.rhic.bnl.gov>;
> Subject:  Re: [Star-fcv-l] STAR presentation by Zuowen Liu for Quark
> Matter 2023 submitted for review
>
> Dear Zuowen,
>
> Thanks for posting your proceedings.
> I guess there are page limits on the proceedings. It supposed to be
> 4-page including references, you have 5-pages now.
> Can you please check and shorten it to fit the limit.
>
> Thanks and regards,
> Subhash
>
> On 2023-11-10 05:14 PM, webmaster--- via Star-fcv-l wrote:
>> Dear star-fcv-l AT lists.bnl.gov members,
>>
>> Zuowen Liu (liuzw AT mails.ccnu.edu.cn) has submitted a material for a
>> review,
>> please have a look:
>> https://drupal.star.bnl.gov/STAR/node/65884
>>
>> ---
>> If you have any problems with the review process, please contact
>> webmaster AT www.star.bnl.gov
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