STAR Correlations and Fluctuations PWG

[Dylan Neff <dneffucla AT gmail.com>]

Hi Toshihiro/Hanna,

Thank you both for your very helpful comments. I've tried to implement most of your suggestions and uploaded the modified slides. I've responded to some of your comments below.

Toshihiro:

S3:

- I am not sure if lower right 3 sketches help in this presentation, because the focus of the first half of the presentation is C5 and C6. What is the purpose to show the multiplicity distribution in this slide? In this slide, I think it’s important to explain why we present the ratios C5/C1 and C6/C2, instead of cumulants. This is for direct comparison between theory (susceptibility) and experiment, by canceling out the trivial volume dependence of cumulants, which I think can be presented in s3.

I've removed the figures and tried to emphasize the connection to susceptibilities. I originally included the multiplicity distributions as I thought it may be good to show what was actually measured. Let me know what you think.

S6:

- Are you going to discuss something about C4/C2 in this slide? If not, I suggest to remove the left plot.

It was suggested I include C4 and mention data and models are positive without spending too much time on it. I've added some brief text.

S10:

- What is Npq?

This is the variance of the binomial where here the number of trials N --> number of protons in event, probability of success p --> fraction of the azimuth covered. The probability of failure q=1-p so I've just put it in terms of p.

I've put the relation of p to the width on slide 9 and again on this slide.

S19:

- Is this a toy model calculation? Can you briefly explain about this model?

Yes this was a pure momentum conservation model that we discussed at the last pwg. I had it in there for discussion while going over the slides but it's not solid enough yet for the public so I removed it.

Hanna:

Slide 8:

Can you provide any reference to the statement: possible sign of a first order phase transition?

I don't have an ideal reference for this. Phase coexistence in first order transitions can produce surface tension which can lead to clustering in coordinate space. I'll talk with others and see if I can find a reference to use here but wanted to get the other updates uploaded.

Thanks,

Dylan Neff

On Fri, Aug 25, 2023 at 8:03 AM Hanna Paulina Zbroszczyk via Star-cf-l <star-cf-l AT lists.bnl.gov> wrote:

Hi Dylan,

Please find my comments on your nice slides.

My general comment is that I have the impression you copied some content from Ashish's slides.

I encourage you to substitute these parts with your own (e.g. try to make fonts uniform, etc..).

Slide 1:

I suggest keeping it in one line: Dylan Neff for the STAR Collaboration.

Slide 2:

Can you increase the references for both figures?

Right figure: Please add \sqrt{sNN} when you describe the top-horizontal axis with collision energies. 

Slide 4:

Consider removing + when you mention 0.5 (\eta)

Slide 5:

Here you mention (crossover), before you stated "cross-over" (slide 2). Please make all of them uniform.

Slide 6:

Do you have a better-quality top-right figure?

Please increase the reference to the main figure.

3 GeV -> \sqrt{s_{NN}} = 3 GeV

Slide 7:

3 GeV -> \sqrt{s_{NN}} = 3 GeV

7.7 GeV and 200 GeV -> \sqrt{s_{NN}} = 7.7 GeV and 200 GeV

Slide 8:

Can you provide any reference to the statement: possible sign of a first order phase transition?

Summary:

39 GeV -> \sqrt{s_{NN}} = 39 GeV

7.7 GeV - 200 GeV -> \sqrt{s_{NN}} = 7.7 GeV - 200 GeV

3 GeV -> \sqrt{s_{NN}} = 3 GeV

Thanks,

Hanna

Hanna Paulina Zbroszczyk

PhD DSc Eng, Professor WUT

E-mail: hanna.zbroszczyk AT pw.edu.pl

Tel: +48 22 234 5851 (office)

Address:

Warsaw University of Technology

Faculty of Physics

Nuclear Physics Division

Koszykowa 75

Office: 117b (via 115)

00-662 Warsaw, Poland

Wiadomość napisana przez 野中俊宏 via Star-cf-l <star-cf-l AT lists.bnl.gov> w dniu 25.08.2023, o godz. 15:57:

Dear Dylan,

Nice slides. I have some comments/suggestions for your consideration.

Best regards,

Toshihiro

General:

- Some texts look like a copy from Ashish’s slides. I would suggest to write down by yourself with the font you mainly use through your slides.

S1:

- Higher-Order Cumulants

S2:

- Crossover

S3:

- I think s3 and s5 should be presented in consecutive slides. I would suggest to put current s4 right after s2.

- I am not sure if lower right 3 sketches help in this presentation, because the focus of the first half of the presentation is C5 and C6. What is the purpose to show the multiplicity distribution in this slide? In this slide, I think it’s important to explain why we present the ratios C5/C1 and C6/C2, instead of cumulants. This is for direct comparison between theory (susceptibility) and experiment, by canceling out the trivial volume dependence of cumulants, which I think can be presented in s3.

S6:

- Hyper-Order Cumulant Ratios

- Are you going to discuss something about C4/C2 in this slide? If not, I suggest to remove the left plot.

- The resolution of top right figure needs to be improved.

S10;

- What is Npq?

S9, S11:

- In these slides you explain how the histograms should look like for no-correlation, lack/excess of clustering, while in S10 you’re talking about variance extracted from the histogram. I understand why you employed this ordering, but it might be easier for the audience to follow if current S9 and S11 are presented in consecutive slides first, then you move to the variance.

S12:

- Please add year for top right papers

S15:

- Can the boundary line of the legend box be removed?

S16:

- I see black dotted lines which are not explained in the legend.

S17:

- 1st bullet: Comparison of hyper-order cumulants with lattice calculations favor crossover….

- 4th bullet: Hadronic interactions are dominant

- 5th bullet: Strong signal of proton repulsion observed

S19:

- Is this a toy model calculation? Can you briefly explain about this model?

S21:

- Move “STAR Preliminary” so it does not overlap with the legend box.

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件名: [Star-cf-l] STAR presentation by Dylan Neff for Quark Matter 2023 submitted for review

 

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

Dylan Neff (dneff AT physics.ucla.edu) has submitted a material for a review,  
please have a look:
https://drupal.star.bnl.gov/STAR/node/64847

Deadline: 2023-09-03
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