STAR Correlations and Fluctuations PWG

[Wielanek Daniel <Daniel.Wielanek AT pw.edu.pl>]

Dear All,

I'm sending updated version, the direct link is here: https://drupal.star.bnl.gov/STAR/system/files/star4_on.pdf

Pozdrawiam/Best regards,

Daniel Wielanek

---

Od: star-cf-l-request AT lists.bnl.gov <star-cf-l-request AT lists.bnl.gov> w imieniu użytkownika Hanna Zbroszczyk <star-cf-l AT lists.bnl.gov>
Wysłane: piątek, 30 sierpnia 2024 17:32:18
Do: star-cf-l AT lists.bnl.gov
Temat: Re: [[Star-cf-l] ] Odp.: Odp.: Odp.: STAR presentation by Daniel Wielanek for NTHEP-2024 submitted for review

 

Dear Daniel,

Thanks for incorporating our comments.

I comment on the presentation: https://drupal.star.bnl.gov/STAR/system/files/star4.pdf

Here is is the link to the main repository: https://drupal.star.bnl.gov/STAR/node/68615

Here I hope the last improvements come:

S2: Since you discuss Fluctuations & criticality, I suggest to stress Femtoscopy & interactions

S8: .. system assures. -> system

Remove dots in the end of each bullet (keep it consistent with the rest of your slides)

S14: Working on FXT data -> Analyzing FXT data (the same on S15)

S18: reconstructed  the eccentricity-> estimated (or calculated) eccentricity

Reformulate the 2nd bullet: Reconstructed the energy dependence of the eccentricity in Au+Au collisions at RHIC

Apply the same changes on S19

S22: last 3 bullets replace with one: It is observed that Kaons R_inv do not follow the power-law distributions extracted from pions at the same collisions implying lack of equilibrium among different species in such collisions

S24: List please 4 papers with 4 parametrization of SI (including masses, you may take them from one of Diana’s presentation)

S26: Add somewhere the physics message: For the first time, we extracted the the spin dependent scattering parameters from the d-\Lambda correlation functions from the  3.0 GeV Au+Au collisions. For p-\Lambda CF, only spin-averaged parameters are extracted

I hope it helps,

Kind regards,

Hanna

prof. dr hab. inż. Hanna Zbroszczyk
E-mail: hanna.zbroszczyk AT pw.edu.pl
Tel: +48 22 234 5851 (biuro)

Adres:
Poltechnika Warszawska

Wydział Fizyki
Zakład Fizyki Jądrowej
ul. Koszykowa 75
Biuro: 117b (via 115)
00-662 Warszawa

Wiadomość napisana przez Wielanek Daniel (via star-cf-l Mailing List) <star-cf-l AT lists.bnl.gov> w dniu 30.08.2024, o godz. 11:28:

Dear Hanna, Nu, All

I uploaded newer version. I removed few slides, moved few equations to the backup and sligthly changed the descriptions (as suggested by Nu and Hanna).

Pozdrawiam/Best regards,

Daniel Wielanek

---

Od: star-cf-l-request AT lists.bnl.gov <star-cf-l-request AT lists.bnl.gov> w imieniu użytkownika Nu Xu <nxu AT lbl.gov>
Wysłane: piątek, 30 sierpnia 2024 02:17:13
Do: STAR Correlations and Fluctuations PWG
DW: Nu Xu
Temat: Re: [[Star-cf-l] ] Odp.: Odp.: STAR presentation by Daniel Wielanek for NTHEP-2024 submitted for review

 

Hi Daniel and All,

I have few comments regarding your presentation "STAR3-1.pdf":

1) I share Hanna’s concern that the draft is too long, 39 slides, too dense for a 15 minutes presentation. I would suggest to reduce the number of slides to around 25;

2) The physics messages could be more precise. For example, in slide 39 - Summary:

(i) Fluctuations: ’There is visible a deviation from non-CP models around 20 GeV’ ==> “There is a visible deviation from non-CP models around 20 GeV”

                                  Plans: ==> Here, in my view, "The most important issue is to complete the FXT data set include 3.0, 3.2, 3.5 GeV Au+Au collisions”;

    (ii) Correlations: Kaons-HBT: the results here are from the FXT energies, this is important. The statement could be: “It is observed that Kaons R_inv do not follow the power-law distributions extracted from pions at the same collisions implying lack of equilibrium among different species in such collisions.” That is enough. 

      p-L and d-L correlations: (a) "For the first time, we extracted the the spin dependent scattering parameters from the d-L correlation functions from the  3.0 GeV Au+Au collisions. For p-L CF, only spin-averaged parameters are extracted."

3) I suggest remove the following slides in order to make the presentation more concise and more focused: slides 9, 10, 11, 12, 13 and add an arrow to indicate the target location for the FXT program in slide 8.

4) slide 14 - last bullet: add at the end “extends the mu_B coverage to about 750 MeV!” and remove slide 15;

5) slide 19: (i) before this slide, it is necessary to show an energy dependence of net-proton C4/C2. You may find the slide 49 in the presentation;

     (ii) I am not sure what do you  mean by ‘Further studies required!’. I would suggest replace by “FXT data from 3 - 7.7 GeV, is needed to understand the deviation!”; (iii) Remove the last bullet starts with ‘BES I statistics too small …’;

6) slide 22: The most important message from the figure is: "Reconstructed the energy dependence of the eccentricity in Au+Au collisions at RHIC”;

7) slides 23, 24, 25: I am not sure what are the main messages you have in mind with the multi-panel energy depend figure. I am not sure we can claim the EOS sensitivity in slide 25.

8) slide 26: I am not sure what is the physics message. If no clear physics message, I suggest remove the slide. I understand there is a push to show the slide. However, the real push should be focused on the publish the data;

9) slide 27: I suggest remove the slide. I understand that baryon correlation function, especially the hyperon-nucleon correlations could lead to the interaction parameters. These parameters are extracted at very diluted environment when the system is after freeze-out. How much they are related to the inner structure of compact stars is unknown.  

10) slide 31: I suggest remove this slide as it is too detailed and not time to make audience to understand!

11) slide 33: I suggest remove this slide as it is not related to the main physics focus of the talk;

12) remove slides 34 and 35 as the info is NOT used in later discussions;

I hope these are helpful. 

Best regards,

Nu 

On Aug 29, 2024, at 2:19 PM, Hanna Zbroszczyk (via star-cf-l Mailing List) <star-cf-l AT lists.bnl.gov> wrote:

Dear Daniel,

Your presentation is becoming quite dense. With only 15 minutes, I’m concerned you might struggle to fit everything in. I suggest compressing your talk a bit. Please do not add any new content. 
S9-13: Consider moving these slides to your backup section. They contain a lot of detailed information about the STAR detector, which isn’t essential for following the physics discussion. Additionally, since there will be a second STAR talk in the session, I believe Slide 8 is sufficient, allowing you to proceed directly to Slide 14.
S26: Change "expected" to "suggested" and include the relevant reference.
S27: I recommend showing a general overview of the neutron star and mentioning how femtoscopy aids in determining the EoS. Be cautious about claiming the precision of femtoscopy in exploring the inner structure of neutron stars. Instead, you might mention that understanding hyperons and N-Y, Y-Y interactions is crucial, as their presence relate to stiffer EoS, which better accounts for the correct mass of a neutron star.
S:30-33: I suggest starting with the kaon results at 200 GeV, as they highlight the strong interaction needed to determine whether a_0 is a diquark or tetraquark. Then, proceed with the 3 GeV results. My proposal is to move Slide 30 after Slide 32.
S32: Conclude that a_
0​ is observed as a tetraquark, but clarify that this conclusion arises from a different parametrization of the strong interaction, which better describes neutral kaon data when assuming a_0 as a tetraquark. Be sure to include references here.
S34-35: Consider combining these into a single slide. The figure on Slide 34 doesn’t seem relevant to your talk. Also, remove the word "Generally" from Slide 34. On Slide 35, ensure consistency in how you write fractions (e.g., 1/4, 1/3, etc.).
S37: Make sure to use consistent terminology when describing systems, such as d-\Lambda or deuteron-lambda. Also, ensure that you consistently use thesis names in your presentation.

Kind regards,
Hanna

prof. dr hab. inż. Hanna Zbroszczyk
E-mail: hanna.zbroszczyk AT pw.edu.pl
Tel: +48 22 234 5851 (biuro)

Adres:
Poltechnika Warszawska
Wydział Fizyki
Zakład Fizyki Jądrowej
ul. Koszykowa 75
Biuro: 117b (via 115)
00-662 Warszawa

Wiadomość napisana przez Wielanek Daniel (via star-cf-l Mailing List) <star-cf-l AT lists.bnl.gov> w dniu 29.08.2024, o godz. 21:25:


Dear Hanna, Mate,
I uploaded never version.
I modified part with vHLLE+UrQMD model. The point is that model have some free parameters, and those parameters were tuned only for crossover EoS. It is therefore possible that another parametrization give oposite results (1PT will better describe the data).
That I want to avoid a statement that this model favors crossover EoS.

Pozdrawiam/Best regards,
Daniel Wielanek
Od: star-cf-l-request AT lists.bnl.gov <star-cf-l-request AT lists.bnl.gov> w imieniu użytkownika Mate Csanad <csanad AT bnl.gov>
Wysłane: czwartek, 29 sierpnia 2024 17:16:17
Do: star-cf-l AT lists.bnl.gov
Temat: Re: [[Star-cf-l] ] Odp.: STAR presentation by Daniel Wielanek for NTHEP-2024 submitted for review
 Dear Hanna,

For the slide Daniel kindly included (S26), let me send some thoughts.

- I guess Daniel meant by "nontrivial" nonmonotonic, as the (naive) expectation 
would be a nonmonotonic change in alpha(sqrt(sNN)), more specifically, a 
minimum. I would actually write: "Minimum predicted in alpha(sqrt(sNN)), not 
visible in the data". A reference could be:
https://arxiv.org/abs/nucl-th/0512060

- I think what can be stated (verbally) very quickly and clearly is the following:
  * With collision energy, not just the source size (R) but also the shape may 
change, and this latter is characterized by alpha
  * According to the measurements, calculations based on a Lévy-shaped source 
describe the data well, and alpha can be extracted for each energy
  * It was predicted that there would be a strong decrease of alpha near the 
critical point, not visible in the data so far
  [* While alpha changes monotonically and smoothly with sqrt(sNN), the size and 
shape are entangled if alpha=2 is assumed, hence this observed alpha(sqrt(sNN)) 
trend indicates that the source size with Lévy assumption has a different trend 
with collision energy as compared to the source size with Gaussian assumption] 
This last point may or may not be included, depending on time. Otherwise these 
things can be told quickly, clearly and efficiently, I think.

Best regards,
Mate

2024. 08. 29. 14:35 keltezéssel, Hanna Zbroszczyk (via star-cf-l Mailing List) írta:
> Dear Daniel,
> 
> Thank you for incorporating my comments.
> 
> General comments:
> Check please page numbering, some slides have missing slides numer, please add 
> where necessary.
> You use different fonts at different slides (e.g, S19, S22), please make fonts 
> at you presentation consistent
> 
> S4. Page number missing.
> Remove = at Low /sqrt{…}
> 
> S15: add EPD as detector improvement
> 
> S19: 20 GeV should be in one line
> 
> S22: add please definitions of variable used (\sigma, radii, etc..)
> 
> S22/23: add a reference to the STAR paper
> 
> S25: I don’t really get what you mean that model parameters were tuned only to 
> this EoS, I suggest to remove this statement as it may confuse the audience
> 
> S26: I am very confused here.
> As your motivation you mentioned at the beginning of your presentation studies 
> of the QCD phase diagram.
> The content discussed here should be consistent with the physics motivation.
> Nontrivial behavior of \alfa - this statement is very puzzling. Can you be more 
> precise?
> Please mention, what do we expect as a signature of critical behavior?
> You don't mention any reference which is needed here.
> Moreover, I am afraid you will not have much time to go into too many details, 
> so planning of this slide is crucial.
> Mate, can you suggest the content fitting to this context?
> The leading topic of this talk is exploration of the structure of the QCD phase 
> diagram and the content should be consists with the physics motivation.
> 
> S29: please change the figure, as an example: S2 
> https://drupal.star.bnl.gov/STAR/system/files/KKCF20240829PWG.pdf
> <https://drupal.star.bnl.gov/STAR/system/files/KKCF20240829PWG.pdf%3E
> 
> I hope it helps,
> Thanks,
> Hanna
> 
> Prof.*Hanna Zbroszczyk*,PhD, DSc, Eng.
> *E-mail*: hanna.zbroszczyk AT pw.edu.pl <mailto: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 Wielanek Daniel (via star-cf-l Mailing List) 
>> <star-cf-l AT lists.bnl.gov> w dniu 29.08.2024, o godz. 13:49:
>>
>> Dear All,
>> I've uploaded never version of my presentation.
>>
>> Pozdrawiam/Best regards,
>> Daniel Wielanek
>> --------------------------------------------------------------------------------
>> *Od:*star-cf-l-request AT lists.bnl.gov 
>> <mailto:star-cf-l-request AT lists.bnl.gov><star-cf-l-request AT lists.bnl.gov 
>> <mailto:star-cf-l-request AT lists.bnl.gov>> w imieniu użytkownika Mate Csanad 
>> <csanad AT bnl.gov <mailto:csanad AT bnl.gov>>
>> *Wysłane:*środa, 28 sierpnia 2024 10:04:57
>> *Do:*star-cf-l AT lists.bnl.gov <mailto:star-cf-l AT lists.bnl.gov>
>> *Temat:*Re: [[Star-cf-l] ] STAR presentation by Daniel Wielanek for NTHEP-2024 
>> submitted for review
>> Dear Daniel,
>>
>> Since this is a centrally invited overview talk, may I ask to include a slide
>> about the collision energy (and centrality) dependent Lévy femtoscopy analyses?
>> I believe the CPOD talk of Daniel Kincses contains the necessary materials:
>> https://conferences.lbl.gov/event/1376/contributions/8829/attachments/5136/4936/kincsesd_CPOD2024_talk_v6.pdf%3Chttps://conferences.lbl.gov/event/1376/contributions/8829/attachments/5136/4936/kincsesd_CPOD2024_talk_v6.pdf%3E
>> maybe just slide 18 of that talk would be good, showing Figure 8 of this blogpost:
>> https://drupal.star.bnl.gov/STAR/blog/kincses/Pion-interferometry-Levy-stable-sources-STAR-FXT-energies%3Chttps://drupal.star.bnl.gov/STAR/blog/kincses/Pion-interferometry-Levy-stable-sources-STAR-FXT-energies%3E
>> https://drupal.star.bnl.gov/STAR/system/files/alpha0_sqrts_fxt.pdf
>> <https://drupal.star.bnl.gov/STAR/system/files/alpha0_sqrts_fxt.pdf%3E
>> with an inset showing Figure 6 of this blogpost:
>> https://drupal.star.bnl.gov/STAR/blog/kincses/Two-particle-interferometry-Levy-stable-sources-sqrtsNN-200-GeV-AuAu-collisions%3Chttps://drupal.star.bnl.gov/STAR/blog/kincses/Two-particle-interferometry-Levy-stable-sources-sqrtsNN-200-GeV-AuAu-collisions%3E
>> https://drupal.star.bnl.gov/STAR/system/files/alpha0_npart.pdf
>> <https://drupal.star.bnl.gov/STAR/system/files/alpha0_npart.pdf%3E
>> I know you have to make a selection, but maybe this could still have a place in
>> your talk.
>>
>> Thanks, best regards,
>> Mate
>>
>> 2024. 08. 27. 17:28 keltezéssel, Hanna Zbroszczyk (via star-cf-l Mailing List) 
>> írta:
>> > Dear Daniel,
>> >
>> > Thank you for submitting your presentation in time.
>> > Please find below my comments for you:
>> >
>> > S1: I suggest adding a one paragraph break between the tittle of your
>> > presentation and your name and another one between your name and the name of
>> > conference
>> >
>> > S2: I suggest to increase the size of your fonts and to add some content to the
>> > right size (figure / graphic / whatever you find as useful)
>> >
>> > S4: I suggest to change = to /rightarrow in all, four places
>> >
>> > Lattice QCD works -> Lattice QCD calculations available
>> > You may add a bullet that we have cross-over transition here  (high
>> > \sqrt{s_{NN}}, low \mu_B)
>> > Critical Point -> Critical Point? (As it’s not obvious whether it exists)
>> >
>> > S5: I suggest to add that this is the motivation of Au-Au heavy-ion collision
>> > programs
>> > First stage -> High collision energies program: QGP properties
>> > Second stage -> Beam Energy Scan program I, II (including FXT):
>> > - onset on deconfinemet,
>> > - 1st order phase transition
>> > - Critical Point
>> >
>> > S14: Star Detector -> BES program
>> > You can show also here the QCD phase diagram from S5 (as it nicely illustrates
>> > the coverage of the collision energies)
>> >
>> > S18: I suggest to remove the last bullet, but putting a reference that this
>> > figure is taken from CPOD’23
>> > Increase font size of text please
>> >
>> > S19: as here you have only 2 bullets, I suggest to add them to the previous slide
>> >
>> > S22: define \epsilon_F with a formula
>> > It will be good to add a conclusion from this slide, e.g. that no phase
>> > transition indicated, and that these results are consistent with the scenario of
>> > cross-over transition
>> > Increase the font size please
>> >
>> > S23: CP?-> critical behavior? (Since the location of the CP here is questionable)
>> >
>> > S24: add reference to the figure and add references to EoS included in these
>> > calculations
>> > Except sensitivity to the EoS, please mention that all results are closer to the
>> > cross-over EoS.
>> > This figure is usually shown for identical particles that you can not
>> > distinguish, I suggest you can use any other future that is applicable for all
>> > particles species.
>> >
>> > S29: not contaminated -> less contaminated
>> > I suggest to remove the last bullet, instead to keep a reference to the figure:
>> > CPOD’23 (as you did)
>> > Please separate a bit the text and the figure, they overall each other
>> >
>> > S30: plays -> play
>> > Pleae define all symbols mentioned here
>> > Instead of mentioning of properties  of resonances, you can mention that this
>> > analysis helps to disctiguise whether a_0 is a tetraquark ro not (but here you
>> > need to add title bit more details regarding extracting parameters from Diana)
>> > Add a reference to LL model
>> >
>> > S32, instead of the last sentence, please add a reference to the SQM’24 conference
>> >
>> > S33: Title: Femtoscopy - baryons -> Baryon femtoscopy
>> > Remove the repetition: Baryon femtoscopy
>> > Remove „generally"
>> > By measuring the CF’s with knows sources we can probe the interactions: ->
>> > Assuming known source function, possible to probe interactions:
>> > Are they repel or attract themselves? -> Do the particle attract or repeal each
>> > other?
>> >
>> > S34: Title: Femtoscopy - baryons -> Baryon femtoscopy
>> >
>> > S33, 34: you may consider adding some graphics
>> >
>> > S34: d_0,f_0 -> d_0, f_0 (add a space)
>> >
>> > S35: deuteron lambda -> deuteron-lambda
>> > General comment: if you use greek symbols, do this in your all slides, so lambda
>> > -> \Lambda, etc..
>> > Rewrite the numerical values in the math mode, eg. 2.32^{+0.12}_{-0.11} fm
>> >
>> > S38:
>> > Chosen results… -> STAR highlights on fluctuations and correlations were shown
>> >
>> > I hope this helps, I will go through your slides once more when you implement my
>> > comments,
>> >
>> > Thanks,
>> > Hanna
>> >
>> >
>> > Prof.*Hanna Zbroszczyk*,PhD, DSc, Eng.
>> > *E-mail*:hanna.zbroszczyk AT pw.edu.pl 
>> <mailto:hanna.zbroszczyk AT pw.edu.pl><mailto:hanna.zbroszczyk AT pw.edu.pl 
>> <mailto: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 przezwebmaster AT star.bnl.gov <mailto:webmaster AT star.bnl.gov>w dniu 20.08.2024, o 
>> godz. 21:13:
>> >>
>> >> Dearstar-cf-l AT lists.bnl.gov <mailto:star-cf-l AT lists.bnl.gov>members,
>> >>
>> >> Daniel Wielanek (daniel.wielanek AT pw.edu.pl <mailto:daniel.wielanek AT pw.edu.pl>) has submitted a 
>> material for a
>> >> review, please have a look:
>> >>https://drupal.star.bnl.gov/STAR/node/68615
>> <https://drupal.star.bnl.gov/STAR/node/68615%3E
>> >>
>> >> Deadline: 2024-09-02
>> >> ---
>> >> If you have any problems with the review process, please contact
>> >>webmaster AT www.star.bnl.gov <mailto:webmaster AT www.star.bnl.gov>
>> >>
>> >
>