STAR HardProbes PWG

[Yi Yang <yiyang0429 AT gmail.com>]

Hi Veronika,

Just for the record... 

Thanks a lot for the updated version and I am fine with your decision. Sorry, I was on vacation last week and the internet connection was pretty bad. 

Cheers,

Yi

On Wed, Apr 3, 2024 at 4:17 AM Veronika Prozorova via Star-hp-l <star-hp-l AT lists.bnl.gov> wrote:

Hi Yi, Isaac,

Thank you very much for your comments. I have implemented most of them. I have also implemented the comments I got today after the rehearsal.  Please, take a look at the new version https://drupal.star.bnl.gov/STAR/system/files/DIS2024_ver4.pdf

Below are my answers to some of your comments. Let me know if you have any further suggestions.

Best regards,

Veronika

Yi:

1. Unfortunately, I do not have time to include cross-section and polarization results (at today's rehearsal I run out of the time limit)
2. I decided to keep the last two quarkonium slides in order 1)Upsilon 2)psi(2s) as I want to tell mention first the upsilon sequential suppression that was already observed in AuAu and then go to the new results for psi(2s)

Isaac: It was decided to remove some bullets in order to not confuse people. I also kept the right plot on page 11, because I forgot to add the bullet discussing the AuAu results. This is now changed.

Thank you.

Virus-free.www.avast.com

пн, 1 апр. 2024 г. в 21:15, Mooney, Isaac <isaac.mooney AT yale.edu>:

Hi Veronika,

I have some small comments on your nice slides. Please see below. With these addressed, I sign off.

Thanks,

Isaac

8. You give some outlook at the beginning of this slide, but it isn't picked back up in the concluding bullets for the slide after we've seen the results. You could add to the last bullet a point on what this says about the energy density dependence for example. Also, I would say "similar suppression in isobar and Au+Au collisions despite different <Npart> at a given centrality" (this seems especially worth highlighting given that on s. 12 we conclude that the suppression is "driven by collision energy density").

10. Bullets two and three seem like they can be combined (the third is a bit redundant currently). And I'm not sure what you mean in bullet 4 by "theoretical model calculations". Do you mean models e.g. an update/retune of Pythia? Or do you mean a first principles calculation? Or something else?

11. Since you're not talking about the AuAu data on this slide, I'm not sure why you have the plot on the right included as well. It seems like it would lead to more distraction than anything else, especially since the colors of the makers change going from left to right for the same data.

In general, the slides in about the first half of the talk are fairly busy. I would recommend animating in some transitions as you're going through each one rather than having all the text shown all at once. 

On Mar 31, 2024, at 17:57, Yi Yang via Star-hp-l <star-hp-l AT lists.bnl.gov> wrote:

Dear Veronika,

Thanks a lot for the updated version. I have some very minor comments on ver 3 for your consideration. 

 - p2: You have plenty of room, so you can use "heavy flavor" and "heavy flavor electron" instead of "HF" and "HFE" here. 

 - Suggestion: I would change the order in quarkonium part: 

        1. J/psi with jet in p+p  (this is for production mechanism, it would be good to mention the cross section and polarization results if you have time). 

        2. J/psi RpA in p+A

        3. J/psi RAA in different energy and sizes

        4. J/psi v2 in isobar      

        5. Psi(2S) RAA in isobar

        6. Upsilon RAA in isobar

In this order, you will cover all chromionium first, then talk about bottomonium, but it is up to you, you probably have a thought of presenting the results.

Cheers,

Yi

On Fri, Mar 29, 2024 at 11:36 PM Veronika Prozorova <v.d.prozorova AT gmail.com> wrote:

Dear Yi,

Thank you very much for your comments! I tried to implement most of them. Please, let me know if you have any further comments.

Comments:

Upsilon result in Au+Au 200 GeV - I decided to put it to backup slides

Elliptic flow (v2) and RAA/RCP - This is planned to be explained a bit later during the presentation (There are definitions on the next slides).

The updated version of the presentation can be found here: https://drupal.star.bnl.gov/STAR/system/files/DIS2024_ver3.pdf

Best wishes,

Veronika

ср, 27 мар. 2024 г. в 06:35, Yi Yang <yiyang0429 AT gmail.com>:

Hi Veronika,

Thanks a lot for the nice slides. I have some suggestions/comments on version 2. 

 - General:

     - the topic is "Recent heavy-flavor measurements from STAR", but you showed many published results on heavy-flavor electrons. Two nature categories should be "Open Heavy Flavor" (heavy-flavor electrons results are part of it) and "Quarkonia". 

     - You can consider also include "D0 production in isobar" (Preliminary) in open heavy flavor part

     - CNN from Jpsi pAu 200 GeV is a bit old (2022), but you can add Ziyue's preliminary result (dielectron channel) in that part 

     - I would suggest also add Upsilon result in Au+Au 200 GeV (published last year) 

     - Regarding the J/psi (and HFE, also) elliptic flow, I am not sure how important to the audiences, I would change to J/psi polarization in isobar (or J/psi RAA in isobar), or Jpsi with jet in pp (also old), but something more related to the production mechanism. 

     - Psi(2S) in isobar is also a very important result from RHIC. 

     - Collision energy dependency of J/psi RAA is also important since you are mentioning many RAA results. 

 

 - p3: It would be good to add the eta coverages for each sub detector 

 - p4: Before this slide, it would be good to have a page to talk about what is the current understanding of heavy flavors, production, polariation, and what is QGP (you kind of directly jump to QGP, it might be too fast for some audiences.)   

 - p4: Elliptic flow (v2) and RAA/RCP probably are not clear to some audiences. 

 - p8: is this n = 8.99 +/- 0.26 important? What does this mean (I probably forgot it)? 

 - p14: I would also show Upsilon in Au+Au 200 GeV (published) results for comparison here. 

 

I understand you have a short talk, but it would be good to show more "new" results (it is okay to have some old ones) in the conference. 

 

Cheers,

Yi

On Tue, Mar 26, 2024 at 5:28 PM Veronika Prozorova via Star-hp-l <star-hp-l AT lists.bnl.gov> wrote:

Hi Yuanjing,

Thank you very much for your valuable feedback! An updated version can be found here: https://drupal.star.bnl.gov/STAR/system/files/DIS2024_ver2.pdf

Best regards,

Veronika

пн, 25 мар. 2024 г. в 22:12, Yuanjing Ji via Star-hp-l <star-hp-l AT lists.bnl.gov>:

Hi Veronika,

Nice slides!

For slide 6-7 reference: the paper has been published on PLB:
Phys.Lett.B 844 (2023) 138071 (also in slide 2). And for the figure,
could you use the final published version:
https://drupal.star.bnl.gov/STAR/system/files/NPEv2_27_54_model_0.pdf
(the only difference is the tiny changes on the style).

Also in slide 6-7, we should be careful here when talking about 27 GeV
heavy flavor electron v2 since uncertainties are large thus hard to make
solid conclusion. So probably
"𝑣2 is consistent with 0" -> "𝑣2 is consistent with 0 within
uncertainties"
"Deviation of c quarks from local thermal equilibrium?" -> "Hints of
deviation of c quarks from local thermal equilibrium? "

Best
Yuanjing

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