STAR Flow, Chirality and Vorticity PWG

[ASHIK IKBAL <ashikhep AT gmail.com>]

Dear Subhash,

First of all, sorry for my late reply. Somehow I had issues getting the emails from this group and therefore missed your email. Prithwish helped me to find this email. Thanks to him. 

Thanks for your nice set of comments. I have addressed them in the next version: https://drupal.star.bnl.gov/STAR/system/files/proc_icnfp21_ashik_2.pdf

Here are my answers to your questions:

line 31: Do you mean scattering in the hadronic phase?

A. Here, I meant hadronic scattering cross-section of multi-strange particles (omega, cascade) is low.

line 127: phi is a strong decay. How do you use V0 cuts for phi
reconstruction?

A. Phi-meson is reconstructed in K+K- channel using standard (conventional) method (invariant mass technique) - pairing the K+ and K- in each event. And the cuts used are the standard topological cuts. The same method has been used before in STAR (Phys. Rev. Lett. 120, 062301 (2018)).

Q. What is the dominant source of syst uncertainty of Omega+ at
y=0.1, which is relatively large compared to other data points?

A. The dominant source of syst uncertainty of Omega+ at

y=0.1 is kaon mass^2 cut variation. We noticed this before and looked here -- found nothing suspicious. 

Q.Figure 4: Right and bottom panel, you may consider changing the Y-axis

range, so data trends are clearly visible with errors and you may scale the
AMPT

A. I have kept the y-scale for the right and bottom panel the same as the left panel. This is because the left panel is for an identical quark case where we expect minimum deviation from zero. Whereas the right and bottom panel are the non-identical quark cases and here we expect more deviation from zero. So, I thought if I zoom these two plots then the comparison would not be at the same scale. 

Figure 5: This is not for this proceedings, but I am wondering what is
the expected trend for PHSD W/O EMF. Is it similar to AMPT?

A. Actually we got help from PHSD authors to get the calculations with EMF. The model has a huge computation cost and is very much time consuming. They did not provide us calculations w/o EMF. So, we don't know the expected trend of w/o EMF.
line 239: Do you mean larger v1-slope for Omega-? Also the hint for
larger v1-slope is only for 27 GeV, not so apparent for 200 GeV.

A. Yes! This is observed for Omega- at 27 GeV. For 200 GeV, the measurements have huge uncertainties. So apparently it is difficult to conclude at 200 GeV.

Thanks,

Ashik

--

Ashik Ikbal

Research Associate

Kent State University

Department Of Physics

Kent, OH 44242, USA

Contact no.s: +1 631-504-7647 (USA)

                      +91 8250216234 (India)

Alternate e-mails: asheikh2 AT kent.edu

                             ashik AT rcf.rhic.bnl.gov

                             ashik.ikbal.sheikh AT cern.ch