Weekly phone meeting:
Monday 3-4PM (EDT)
https://bluejeans.com/333205157
April 4, meeting agenda:
Drupal Calendar
latest version of current BUR:
Version 12, 05/21/2016
Last-year's BUR and CAD projections
Lambda/Lambdabar polariation at 27GeV
Subsequent meeting with Berndt after the NSAC meeting in March 23 about
Run17: Berndt said that after discussion with DOE and BNL management,
it is likely that 19 cryo-weeks of RHIC operation should be taken as baseline,
this should include two weeks of CeC commissioning.
That means effectively 17 cryo-weeks for run 17.
Executive Summary:
The STAR Collaboration makes the following two-year beam-use proposal, in order to achieve its spin and relativistic heavy ion physics goals on a timescale consistent with intense international interest and competition in these areas, as well as to utilize RHIC beams effectively, taking full advantage of recent improvements in machine and detector capability.
|
Run |
Energy |
Duration |
System |
Goals |
priority |
Sequence |
|
17 |
ÖsNN=510 GeV
|
13-wk
1-wk
2-wk |
Transverse
p+p
CeC |
AN of W±, g, Drell-Yan,
RHICf |
1
|
1
2 |
|
18 |
ÖsNN =200 GeV
ÖsNN=200 GeV
ÖsNN=27 GeV |
3.5-wk
3.5-wk
2-wk |
Ru+Ru
Zr+Zr
Au+Au |
1.2billion MB
1.2billion MB
500M MB |
2
2
3 |
4
3
5 |
Table STYLEREF 1 \s 1‑ SEQ Table \* ARABIC \s 1 1: Scenario I: 19 cryoweeks for Run 17 and 13 cryo-weeks for run 18. We assume most of the TPC bandwidth (1800Hz) is for the minbias event rate for isobar data-taking with 90 hours per week of DAQ time. All luminosities requested are actual sampled luminosity. See text for details of HFT and pp510 run conditions and optimizations.
STAR’s highest scientific priority is the first significant measurement of the sign change of the Sivers’ function, when compared to the value measured in SIDIS, and evolution effects in transverse momentum distributions through measurements of single spin asymmetries in W+/-, Z, direct photon and Drell-Yan production in transversely polarized √s = 500 GeV p+p collisions. The sign change measurement is a fundamental test of QCD and is being pursued by other experiments, making a timely measurement imperative.
STAR’s second scientific priority is to clarify the interpretation of the observed signatures of the chiral magnetic effect, chiral magnetic wave and chiral vortical effect by making measurements that disentangle signal from background v2 effects. We request a 3.5 week run each for Ruthenium-96 (Ru+Ru) and Zirconium-96 (Zr+Zr) collisions in run 18. This choice of nuclei is ideal as it allows for a variation in magnetic field at a maximum of 10%, while keeping nearly all other parameters the same. This decisive measurement of the ratio of charge separation in the isobar reduces the flow background dramatically, and will greatly advance our understanding of the chiral magnetic effect, which has fundamental impact beyond the field of high-temperature QCD.
|
Run |
Energy |
Duration |
System |
Goals |
priority |
Sequence |
|
17 |
ÖsNN=510 GeV
ÖsNN=62.4 GeV |
13-wk
1-wk
2-wk
4-wk |
Transverse
p+p
CeC
Au+Au |
AN of W±, g, Drell-Yan,
RHICf
Jets, dileptons, NPE 1.5B MB |
1
4
5 |
1
2
3 |
|
18 |
ÖsNN =200 GeV
ÖsNN=200 GeV
ÖsNN=27 GeV |
3.5-wk
3.5-wk
2-wk |
Ru+Ru
Zr+Zr
Au+Au |
1.2billion MB
1.2billion MB
500M MB |
2
2
5 |
5
4
6 |
Table STYLEREF 1 \s 1‑ SEQ Table \* ARABIC \s 1 2: Scenario 2: 24 cryoweeks for Run 17 and 13 cryo-weeks for run18
Our next scientific priority is to take data at beam energies that are lower than the nominal energies, but are not part of STAR’s proposed Beam-Energy-Scan Phase-II program. There are two programs in our requests in this category:
a) Au+Au collisions at 62 GeV for measurements of inclusive jets and charm spectrum at low energy. With newly developed analysis techniques, inclusive jet measurements are possible with minimum-bias data in Au+Au collisions. We have recently extended the measurement to Au+Au at 62 GeV with limited statistics from run 10. We request 4 weeks of Au+Au collisions at this energy for an inclusive jet RCP measurement. This will also provide a measurement of Non-photonic electrons from charm semileptonic decays. In addition, with the significant reduction of material from run 16 to run 17 and run 18, dilepton measurements with good statistics are possible in 4 weeks of data-taking.
b) STAR has observed an exciting new effect, the global polarization of hyperons in noncentral Au+Au collisions. Theorists are excited and BES-II (2019-2020) will provide opportunities for higher precision explorations of the effect. There is also a possibility of observing a difference in Lambda and anti-Lambda polarization if the global polarization effect connected to the Chiral magnetic effect. We propose to extract important information from this effect at beam energy above the nominal BES-II energies through a high-statistics dataset at 27 GeV. It will be even better if we are able to collect this dataset in run17 with sufficient beam time, which allows us to analyze the effect with high statistics and guide our future direction in this subject ahead of the BES-II program.
The STAR Collaboration presents in this BUR five compelling and prioritized scientific programs for the 2017 and 2018 RHIC runs, prior to the start of BES-II [[i]]. In this BUR we furthermore discuss the highlights from the scientific publications, on-going analyses and detector performance from recent runs. We also outline the planned upgrades in the next few years in preparation for Run 17 and the Beam Energy Scan II.
[i] STAR Beam Energy Scan II: Studying the Phase Diagram of QCD Matter at RHIC
https://drupal.star.bnl.gov/STAR/starnotes/public/sn0598
1) Spin publications and analyses from run15
2) HFT preliminary results and other open charm results (Xin Dong and Zhenyu et al.)
3) MTD preliminary and other quarkonium results (Lijuan et al.))
4) chiral magnetic effect (Paul and Gang)
5) Lambda Global Polarization (Mike)
Anything else?
on May 24, add one para in Section 4.8 for MTD in run17.
Update on May 16th:
seperate run 16 performance and projection from section 2.5.
on May 6.
1) include recent results and status in the current write up.
2) for another section 3.1 under Run 16 performance report: The HFT and MTD data performance and projections,
there is not much to say for the MTD. Information in terms of sampled luminosity is included in Section 2.5.
PAC talks:
1) run14/15 experimental results and status (Frank)
2) BUR (Zhangbu)
3) BES-II and iTPC upgrade (Helen+Flemming)
It will be good if we can have a preview of the RHICf (Sako, Itaru), Spin (Carl) and CME (Paul) talks.
Producing the requested data for physics will involve significant use of data stores, considerable processing time, and time spent understanding and completing calibrations. When a dataset is a continuation of a collision species and energy from a previous year (with STAR's detector similarly set up), first-physics calibrations for the highest priority dataset typically require on the order of two months after the conclusion of data-taking for that year. Subsequent dataset calibrations for a given year need another month each. The proposed 500 GeV p+p and 27 GeV (and potentially 62 GeV) Au+Au datasets will be such continuations, adding to what were acquired in 2013 and 2011 (2010) respectively (repeating the environment of no HFT and no iTPC). Understanding features of new running conditions could extend calibrations of the isotope datasets to take a few months more, and it is important to keep in mind that unforeseen peculiarities of any given data set can further delay delivery.
Table X presents estimates of the DAQ and data summary ("MuDst") dataset sizes of the proposed colliding species, along with projected single-pass production times on 100% of STAR's 2016 allocation of the RACF computing farm. It is critical to emphasize that these numbers are tied to the proposed event goals, and would scale with the actual events acquired. These productions will need to balance computing resource usage with prior-year datasets as well as ongoing calibrations and run support. STAR may choose, as an imaginable example, to produce Run 16 200 GeV Au+Au concurrently with the Run 17 500 GeV p+p in a 60%-40% apportionment, which would elongate the latter production to a year or more.
For the 500 GeV pp dataset, we expect 360 pb^-1 to require approximately 3.3 billion events recorded for processing.
Data set Events DAQ size [PB] MuDst size [PB] Production time [months]
500 GeV p+p 3.3B 3.20 1.75 5.0
62 GeV Au+Au 1.5B 0.81 0.54 1.0
27 GeV Au+Au 0.5B 0.24 0.12 0.5
200 GeV Ru+Ru 1.2B 0.88 0.65 1.0
200 GeV Zr+Zr 1.2B 0.88 0.65 1.0
Totals 6.01 3.71
Caption: Table X: Computing resource estimates for production of the proposed Runs 17 and 18 datasets (see text for details)
similar to last BUR with updates from Spin Plan and also detector
section structure same as last BUR
proposal and Projection for 62GeV (Helen et al.)
proposal and projection for 2 weeks of 27GeV Au+Au
proposal and projects for Isobar (Zr+Zr and Ru+Ru)
3+3 weeks
Discuss possible Isobar BES?
The isobar (CME search) part of the BUR has been prepared by Gang, Paul and Sergei:
http://www.star.bnl.gov/protected/bulkcorr/rexwg/service/BUR1718/CME.pdf
The tex and eps files are in the same directory,
while the pdf file is also attached below.