STAR Flow, Chirality and Vorticity PWG

[韩成栋 <chdhan AT impcas.ac.cn>]

Dear All,

The updated slides and answers to comments and suggestions on the rehearsal talks (Backup) have been uploaded to the STAR drupal page.

Please Kindly find the updated report by the link:https://drupal.star.bnl.gov/STAR/node/64787 

Thank you for your attention.

Best wishes,

Chengdong Han

-----Original Messages-----
From:"韩成栋" <chdhan AT impcas.ac.cn>
Sent Time:2023-08-30 15:44:12 (Wednesday)
To: "STAR Flow, Chirality and Vorticity PWG" <star-fcv-l AT lists.bnl.gov>
Cc: "Sooraj Radhakrishnan" <skradhakrishnan AT lbl.gov>
Subject: Re: Re: Re: [Star-fcv-l] STAR presentation by Xionghong He for Quark Matter 2023 submitted for review

Dear Sooraj,

The plot in the attachment is a supplement to question: “S11, S12: On S11 for light nuclei, both the data and model show good mass scaling (except for He4) separately. On S12, the proton v1 slope is very different between data and model, but for other light nuclei are comparable. Is this consistent?”
Answer S11,12:  The results in the two plots from p11 and p12 are consistent.The plot attached is the dv1/dy distribution in slide11 divided by the mass number A, which shows that they do not follow the A scaling at higher energies.

Thank you for your attention.

Best wishes,

Chengdong Han, Xionghong He

-----Original Messages-----
From:"韩成栋" <chdhan AT impcas.ac.cn>
Sent Time:2023-08-30 12:35:38 (Wednesday)
To: "STAR Flow, Chirality and Vorticity PWG" <star-fcv-l AT lists.bnl.gov>
Cc: "Sooraj Radhakrishnan" <skradhakrishnan AT lbl.gov>
Subject: Re: Re: [Star-fcv-l] STAR presentation by Xionghong He for Quark Matter 2023 submitted for review

Dear Sooraj,

Thank you very much for your review and suggestions, I have revised the draft according to your comments. 

Please Kindly find the updated report by the link:https://drupal.star.bnl.gov/STAR/node/64787

Also find my some reply below:

Question: On the outlook you mention that the high statistics 3 GeV dataset can constrain the coalescence parameters. But in the slides you do not show any attempt in that direction. If you reweight the input distributions to the coalescence afterburner to match the flow of protons and Lambda, would this help you constrain the parameters and test the coalescence picture? Was this tried?

Answer: Our plan is first to analysis the 2B events. Then use transport model plus coalescence afterburner to compare with data and extract coalescence parameters.  We will also compare these results with that of light nuclei.

S3: A caveat here is that for neutron stars what is relevant are the interactions at high densities, but through coalescence the extracted parameters are sensitive to the density at freeze-out 

Answer S3: Good point! Our experimental data will provide a starting to understand Y-N interaction and the inner structure of neutron star.

S4: Title - Light and Hyper Nuclei in BES-II?

Answer S4: The current title is fine.

S5: Left bullet 1) magnitude of v_n. v_n are sensitive quantities for studying EoS

Answer S4: Done, I made modifications based on your and Subhash's suggestions.

S5: Left 2) can be removed 

Answer S5: Yes, we removed the Left 2). 

S6: What do you mean uniform efficiency?

Answer S6: The detection efficiency of TPC is uniform with different theta angles, which means that the acceptance in the phi direction is basically uniform.

S7: Right plot, seems this comes a bit early as you show the reconstruction only in next slides

Answer S7: The reason for putting this plot in this position is to explain why we choose the centrality range 5-40% to analyze the hyper-nuclei directed flow. Namely, in order to balance the event plane resolution and hyper-nuclei yield, we choose 5-40% centrality range to preform hyper-nuclei directed flow analysis.

S11: The He4 slope deviates from the fit, this is likely because of the acceptance. Would it make sense to compare the values at fixed rapidity, say -0.6 to -0.4 for all light nuclei?

Answer S11: For the calculation results from the JAM2 model, we also saw the same phenomenon of deviation from the fitting as the experimental data, and we do not know what the reason is.

S11, S12: On S11 for light nuclei, both the data and model show good mass scaling (except for He4) separately. On S12, the proton v1 slope is very different between data and model, but for other light nuclei are comparable. Is this consistent?

Answer S11,12:  The results in the two plots from p11 and p12 are consistent.The plot attached is the dv1/dy distribution in slide11 divided by the mass number A, which shows that they do not follow the A scaling at higher energies.

Thank you for your attention.

Best wishes,

Chengdong Han, Xionghong He 

-----Original Messages-----
From:"Sooraj Radhakrishnan via Star-fcv-l" <star-fcv-l AT lists.bnl.gov>
Sent Time:2023-08-28 00:02:44 (Monday)
To: "STAR Flow, Chirality and Vorticity PWG" <star-fcv-l AT lists.bnl.gov>
Cc: "Sooraj Radhakrishnan" <skradhakrishnan AT lbl.gov>
Subject: Re: [Star-fcv-l] STAR presentation by Xionghong He for Quark Matter 2023 submitted for review

Dear Chengdong, Xionghong, 

   These are very nice results and nicely prepared slides. On the outlook you mention that the high statistics 3 GeV dataset can constrain the coalescence parameters. But in the slides you dont show any attempt in that direction. If you reweight the input distributions to the coalescence afterburner to match the flow of protons and Lambda, would this help you constrain the parameters and test the coalescence picture? Was this tried?

Please find a few other comments on the slides below

S3: A caveat here is that for neutron stars what is relevant are the interactions at high densities, but through coalescence the extracted parameters are sensitive to the density at freeze-out 

S4: Title - Light and Hyper Nuclei in BES-II?

S5: Title - Collective Flow

S5: Left bullet 1) magnitude of v_n. v_n are sensitive quantities for studying EoS

S5: Left 2) can be removed

S5: Right side top: Collective flow

S5: Why restrict to only v_1 in the last two equations on the right?

S5: What are R, italic R and R_n in the first equation in the step? (N^R(phi - Psi_m) = ...). Also wjy Psi_m instead of Psi_n?

S6: Can you use a new version of the figure without HFT? Also, iTOF? 

S6: What do you mean uniform efficiency?

S7: Right plot, seems this comes a bit early as you show the reconstruction only in next slides

S9: 2) Collective flow (and everywhere); are calculated within the 

S11: The He4 slope deviates from the fit, this is likely because of the acceptance. Would it make sense to compare the values at fixed rapidity, say -0.6 to -0.4 for all light nuclei?

S11, S12: On S11 for light nuclei, both the data and model show good mass scaling (except for He4) separately. On S12, the proton v1 slope is very different between data and model, but for other light nuclei are comparable. Is this consistent?

S15: coalescence is the dominant formation mechanism at mid-rapidity

S15: 2) calculations for v1

Best,

Sooraj

On Mon, Aug 21, 2023 at 3:15 AM hexh--- via Star-fcv-l <star-fcv-l AT lists.bnl.gov> wrote:

Dear All,

This is the slides from Chengdong. He has problem to login the blog webpage.
Thanks.

Best regards,
Xionghong

-----Original Message-----
From: star-fcv-l-bounces AT lists.bnl.gov <star-fcv-l-bounces AT lists.bnl.gov> On
Behalf Of webmaster--- via Star-fcv-l
Sent: Monday, August 21, 2023 5:51 PM
To: star-fcv-l AT lists.bnl.gov
Cc: webmaster AT star.bnl.gov
Subject: [Star-fcv-l] STAR presentation by Xionghong He for Quark Matter
2023 submitted for review

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

Xionghong He (hexh AT impcas.ac.cn) has submitted a material for a review,
please have a look:
https://drupal.star.bnl.gov/STAR/node/64787

Deadline: 2023-09-03
---
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--

Sooraj Radhakrishnan

Research Scientist,

Department of Physics

Kent State University

Kent, OH 44243

Physicist Postdoctoral Affiliate

Nuclear Science Division
Lawrence Berkeley National Lab
MS70R0319, One Cyclotron Road

Berkeley, CA 94720

Ph: 510-495-2473

Email: skradhakrishnan AT lbl.gov