STAR Flow, Chirality and Vorticity PWG

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Dear star-fcv-l AT lists.bnl.gov members,

Subhash Singha ( connectsubhash AT gmail.com ) has commented on a material  
originally submitted by Junyi Han ( jyhan AT mails.ccnu.edu.cn ) at
https://drupal.star.bnl.gov/STAR/presentations/SQM-2024/Directed-Flow-Lambda-prescript3Lambdarm-H-and-prescript4Lambdarm-H-AuAu-col-0

Comment:
Dear Junyi,


Nice proceedings. I have a few suggestions and comments below  for your  
consideration:
Abstract:"In this presentation" -->Â  In these proceedings,"We will show" --> 
 
we present"energy dependence of the directed flow" --> energy dependence of  
the directed flow (v1)"These hyper-nuclei results will be compared" --> These 
 
hyper-nuclei results are compared"Finally, discussions ... calculations"  
--->Â Finally, these results are compared with a hadronic transport model  
including coalescence after-burner.

l#3: substances --> QCD matter"The extremely .... high density substances"  
--> An extremely high temperature and high density matter is produced  
...delete "are known as "fireball"."
l#4: "The strange particles produced in the “fireball”5 interact with the 
 
surrounding hadron matter and may eventually combine with the nucleon to 6  
form a bound state" --> please rephrase this line.
l#9:Â Could you please explain how Y-N enters into QCD EoS?
l#14: need a reference for thermal model"In secondly phase of RHIC-STAR  
Au+Au..." -->Â In the second phase of the RHIC Beam Energy Scan program, the  
collision energy for fixed-target Au+Au collisions is extended down to 3 GeV.
l#22: in the centar of mass energy s_NN --> at s_NN
l#30: mention the typical value of EP resolution
l#35: "The decay channels used for are:" -->Â The following decay channels  
are used: ....l#38: "by rotation method." --> by rotating one of the  
daughter tracks by XX degree.
l#42: "Due to the collective flow ... for comparison" --> Since collective  
flow depends on pT, we select a similar pT/A range (approximately 0.4 < pT/A  
< 0.8 GeV/c) for comparison for a given particle.
l#45: "to fit. Where the p0 = (v1)s = dv1/dy|y=0 is the mid-rapidity slope." 
 
--> to extract the v1 slope (p0 = (v1)s = dv1/dy|y=0).
l#46: "Due to the statistics is poor" --> Due to poor statistics
l#47: "In all fitting processes, zero48 point (0, 0) is forced going through, 
 
taking the advantage of the symmetry" -->Â Taking the advance of symmetry in  
v1 near mid rapidity, the fit functions are enforced to pass through (0, 0).
l#52: "The top part ... bottom part" --> The top panels present .... and  
bottom panels present ....
l#60: "From the results, we can find with the col61lision energy increases,  
the mid-rapidity v1 slope of light-nuclei and hyper-nuclei decreases"  
-->Â From the results, we observe that as the collision energy increases, the 
 
mid-rapidity v1 slope of light nuclei and hypernuclei decreases.
l#62: "From the comparison, the hadronic transport model with coalescence  
afterburner calculations  are also added, which is consistent with observed 
 
energy denpendence results from data." -->Â In the comparison, hadronic  
transport model calculations with a coalescence afterburner are also  
included, which are consistent with the observed energy dependence in the  
data.
l#65: efficiency --> reconstruction efficiency
l#70: "The results in this analysis imply coalescence procedure 71 dominants 
 
the formation mechanism. And the hadronic transport model calculations  
are 72 consistent with observed mass and energy dependence" --> The results 
 
of this analysis suggest that the coalescence process could be a dominant  
mechanism in the formation of light nuclei and hypernuclei. Additionally, the 
 
hadronic transport model calculations are consistent with the observed mass  
and energy dependence.
l#72: "In the next, STAR has collected 2Â Â billion events for 3.0 GeV Au+Au  
collisions which will help us to constrain coalescence4 parameters for both  
light-nuclei and hyper-nuclei." -->Â billion events from 3.0 GeV Au+Au  
collisions. Analysis of this data will provide improved precision, leading to 
 
stronger constraints on the coalescence parameters for both light nuclei and  
hypernuclei.

ps: please remember to post proceedings at least two weeks before the  
deadline so we have enough time to go through.

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