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Subject: STAR Flow, Chirality and Vorticity PWG
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Re: [Star-fcv-l] STAR presentation by Rishabh Sharma for Quark Matter 2023 submitted for review
- From: Sooraj Radhakrishnan <skradhakrishnan AT lbl.gov>
- To: "STAR Flow, Chirality and Vorticity PWG" <star-fcv-l AT lists.bnl.gov>
- Cc: rishabh <rishabh AT rcf.rhic.bnl.gov>, webmaster AT star.bnl.gov
- Subject: Re: [Star-fcv-l] STAR presentation by Rishabh Sharma for Quark Matter 2023 submitted for review
- Date: Mon, 28 Aug 2023 14:08:05 -0700
Hi Rishabh,
Thanks for preparing the nice presentation and the interesting results. Please find a few comments from me below
It is somewhat surprising that v3 shows good mass scaling, while v2 doesn't. Is there an explanation for this?
From BES-I results, we had claimed that mass number scaling holds for v2 within pT/A < 1.5 GeV (PRC 94, 034908 (2016)). With BES-II we see deviations. Do you have a comparison of the BES-I and BES-II results for the different particle species?
S4: What is the equation about?
S4: Why is the fluctuating initial conditions relevant here?
S5: Please include EPD and ETOF also under BES-II upgrades
S5: track momentum and event plane?
S6: What is track resolution?
S9: What is the low pT you refer to here? Please indicate the range
S12: seems to be --> is in
S15: Can you quantify the extend of scaling? May be fit a constant to your lower plots and evaluate the value and uncertainty. This should tell you to within what percentage you can claim v3 scaling
S16: seems to be --> is in
S17: You could also point to other light nuclei flow results from STAR (Chengdong's talks for eg). In th outlook, you can indicate the remaining energies to be measured and their relevance
Best,
Sooraj
On Mon, Aug 28, 2023 at 7:09 AM rishabh via Star-fcv-l <star-fcv-l AT lists.bnl.gov> wrote:
Dear Subhash,
Thank you for your comments. Please find the revised version of slides
here: https://drupal.star.bnl.gov/STAR/node/64854.
> s#4: This is for my understanding, how light nuclei v3 of has better
> sensitivity to initial fluctuation, if they are formed at later stage?
Nucleons will propagate the initial state fluctuations if the light
nuclei are formed by the coalescence mechanism.
> s#9: Could you indicate the fraction of reduction in error in BES-II
> relative to BES-I?
The improvement in statistical uncertainty varies from particle to
particle and with the pT bin. On average, we observe a 30–40%
improvement in BES-II energies compared to BES-I energies.
Instead of writing it down on the slide, I was hoping, just like in my
SQM talk, that I could tell the fraction while delivering the talk.
Please let me know if that is okay.
> s#14: At the lowest pT, I see v3 of p and d are consistent. It might be
> better if you specify the pt-range for which mass dependence is
> observed.
Implemented.
> s#15: You can indicate fit to proton data beside the function in the
> legend. The Y-axis scale of the bottom panels is very large, can you
> try reducing them, so the level of scaling would be clearly visible.
Implemented.
Please let me know if you have any further suggestions for me.
Thanks and regards,
Rishabh
On 2023-08-28 13:14, subhash via Star-fcv-l wrote:
> Dear Rishabh,
>
> Nice slides. I have a few suggestions for your consideration:
>
> s#4: This is for my understanding, how light nuclei v3 of has better
> sensitivity to initial fluctuation, if they are formed at later stage?
>
> s#9: Could you indicate the fraction of reduction in error in BES-II
> relative to BES-I?
>
> s#14: At the lowest pT, I see v3 of p and d are consistent. It might
> be better if you specify the pt-range for which mass dependence is
> observed.
>
> s#15: You can indicate fit to proton data beside the function in the
> legend.
> The Y-axis scale of the bottom panels is very large, can you try
> reducing them, so the level of scaling would be clearly visible.
>
>
> Thanks and regsrds,
> Subhash
>
>
> On 2023-08-24 10:01 PM, webmaster--- via Star-fcv-l wrote:
>> Dear star-fcv-l AT lists.bnl.gov members,
>>
>> Rishabh Sharma (rishabhsharma AT students.iisertirupati.ac.in) has
>> submitted a
>> material for a review, please have a look:
>> https://drupal.star.bnl.gov/STAR/node/64854
>>
>> Deadline: 2023-09-03
>> ---
>> If you have any problems with the review process, please contact
>> webmaster AT www.star.bnl.gov
>> _______________________________________________
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_______________________________________________
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Sooraj Radhakrishnan
Research Scientist,
Department of Physics
Kent State University
Kent, OH 44243
Physicist Postdoctoral Affiliate
Lawrence Berkeley National Lab
MS70R0319, One Cyclotron Road
Email: skradhakrishnan AT lbl.gov
-
[Star-fcv-l] STAR presentation by Rishabh Sharma for Quark Matter 2023 submitted for review,
webmaster, 08/24/2023
-
Re: [Star-fcv-l] STAR presentation by Rishabh Sharma for Quark Matter 2023 submitted for review,
subhash, 08/28/2023
-
Re: [Star-fcv-l] STAR presentation by Rishabh Sharma for Quark Matter 2023 submitted for review,
rishabh, 08/28/2023
-
Re: [Star-fcv-l] STAR presentation by Rishabh Sharma for Quark Matter 2023 submitted for review,
Sooraj Radhakrishnan, 08/28/2023
- Re: [Star-fcv-l] STAR presentation by Rishabh Sharma for Quark Matter 2023 submitted for review, Md. Nasim, 08/29/2023
-
Re: [Star-fcv-l] STAR presentation by Rishabh Sharma for Quark Matter 2023 submitted for review,
rishabh, 08/29/2023
- Re: [Star-fcv-l] STAR presentation by Rishabh Sharma for Quark Matter 2023 submitted for review, Sooraj Radhakrishnan, 08/30/2023
-
Re: [Star-fcv-l] STAR presentation by Rishabh Sharma for Quark Matter 2023 submitted for review,
Sooraj Radhakrishnan, 08/28/2023
-
Re: [Star-fcv-l] STAR presentation by Rishabh Sharma for Quark Matter 2023 submitted for review,
rishabh, 08/28/2023
-
Re: [Star-fcv-l] STAR presentation by Rishabh Sharma for Quark Matter 2023 submitted for review,
subhash, 08/28/2023
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