State of STAR

John Harris

Outline:• Data - Physics

• Detector Update

• Collaboration Update• Physics• Open Physics Issues• Collaboration Issues• Long Term Future

STAR Collaboration MeetingBNL

7 February 2002

STARSTAR

Data Summer 2000 snn = 130 GeV Au + Au 2.0 M total trigger events taken

844 K central (top 15%) 331 K (top 5%) central trigger events 458 K good minimum bias trigger events

Data Fall 2001 snn = 200 GeV Au + Au ~ 14 M total trigger events taken

3.6 M (top 10%) central trigger events 4.7 M minimum bias trigger events

Data-TakenData-Taken

Data Fall 2001 (1-day) snn = 20 GeV Au + Au ~ 250 K total trigger events taken 30 K central trigger events 200 K minimum bias events

Data Winter 2001-2 s = 200 GeV p + p ~ 20 M total trigger events taken 17 M minimum bias trigger events for RHI reference data subset with forward pi-zero trigger (single spin asymmetry)

What Physics to Expect from 2001 Au + Au RunWhat Physics to Expect from 2001 Au + Au Run• Data on tape

– Min Bias events = 10x more than last year

– Central events = 7x more than last year

• Physics Reach

– High-pt

• h spectra and anisotropy out to 12 GeV/c

• ratios at high-pt (RICH)

– Strangeness , (width, mass-shifts), higher reach in pT for (multi-) strange

baryons, (1520), K*(1430), (1385)

– HBT

• 3D K-K, K- w/ greater resolution,

• K-p, -p, K0s-K0

s, pt dependence of R()

– Spectra , He4, particle ratio

– EbyE , K* flow, K/

– … and much more … (also p + p reference data and spin surprises)

STARSTAR

“Large acceptance hadronic detector”

New Detectors 2001 Run: SVT, FTPCs, ToF patch, partial EMC, FPD, BBC

Detector Installation 2002: SSD, PMD, 1/2 EMC,

move RICH, EEMC (?)

Status of the Detector at RHICStatus of the Detector at RHICSTARSTAR

Ring Imaging Cerenkov Detector

Coils MagnetSilicon Vertex Tracker + Silicon Strip Detector

EM Cal Barrel + End Cap EMC

Trigger Barrel + Time of Flight Patch

Time Projection Chamber

Forward Time Projection Chamber

Electronics Platforms

Detectors Run 2000 TPC, Trigger Barrel, RICH

Status of the Status of the

CollaborationCollaborationSTARSTAR

Brazil RussiaUniversidade de Sao Paolo MEPHI – Moscow

LPP/LHE JINR - DubnaChina IHEP-Protvino IHEP - BeijingUSTC - Hefei IMP - LanzhouSINR - ShanghaiTsinghua UniversityIPP - Wuhan U.S. Labs

Argonne National LaboratoryEngland Brookhaven National LaboratoryUniversity of Birmingham Lawrence Berkeley National Laboratory

France U.S. Universities IReS Strasbourg UC Berkeley / SSLSUBATECH - Nantes UC Davis

UC Los AngelesGermany Carnegie Mellon UniversityMPI – Munich Creighton UniversityUniversity of Frankfurt Indiana University

Kent State UniversityIndia Michigan State UniversityIOP - Bhubaneswar City College of New YorkVECC - Calcutta Ohio State UniversityPanjab University Penn. State UniversityUniversity of Rajasthan Purdue UniversityJammu University Rice UniversityIIT - Bombay University of Texas - Austin

Texas A&M UniversityPoland University of Washington Warsaw University of Technology Wayne State University

Yale University

419 collaborators 44 institutions 9 countries

Physics Progress: Conclusions So FarPhysics Progress: Conclusions So Far

low net baryon density approaches early Universe

particle ratios consistent with quark coalescence

strong radial and elliptic flow large pressure gradients

simple models of radial flow “fit” spectra [ definitely too naïve? ]

Kinetic parameters: ßr (RHIC) = 0.6c , Tfo (RHIC) = 100-120 MeV

Do not yet understand details of flow or expansion!!

simple chemical model “fits” ratios [ fundamental or too naïve? ]

Chemical parameters: Tch (RHIC) = 175 MeV , B (RHIC) = 51 MeV

Need multiply strange baryon data for hard test!!

source sizes similar to SPS inconsistent with hydrodynamical models

Do not yet understand spacetime evolution!!

variables wrt flow plane! further constrain dynamical models

single particle distributions and elliptic flow at high Pt

most exciting data at QM parton energy loss in-medium?Need pp and pA reference data to understand mechanisms!!

STARSTAR

Physics Progress: STAR Journal Publications/SubmissionsSTAR Journal Publications/Submissions

Midrapidity -meson Production in Au+Au at snn = 130 GeVsubmitted to Phys. Rev. C

Measurement of Inclusive Anti-Protons from Au+Au at snn = 130 GeV C. Adler et al. Phys. Rev. Lett. 87, 262302-1 (2001).

Anti-deuteron and Anti-helium3 Production in Au+Au at snn = 130 GeV C. Adler et al. Phys. Rev. Lett. 87, 262301-1 (2001).

Identified Particle Elliptic Flow in Au+Au at snn = 130 GeVC. Adler et al. Phys. Rev. Lett. 87, 182301 (2001).

Multiplicity Distribution and Spectra of Negatively Charged Hadrons in Au+Au at snn = 130 GeV C. Adler et al. Phys. Rev. Lett. 87, 112303 (2001).

Pion Interferometry of snn = 130 GeV Au+Au at RHICC. Adler et al. Phys. Rev. Lett. 87, 082301 (2001).

Midrapidity Antiproton-to-Proton Ratio from Au+Au snn = 130 GeV

C. Adler et al. Phys. Rev. Lett. 86, 4778 (2001).

Elliptic Flow in Au+Au at snn = 130 GeV

K.H. Ackermann et al. Phys. Rev. Lett. 86, 402 (2001).

STARSTAR

Physics in ProgressPhysics in Progress

• SpectraMidrapidity Inclusive p and pbar*

Particle Production Summary Paper (PRC)

Pi-zero Paper (PRC)

StrangenessCascade Paper

Mixed Hadron Ratio Paper (PRC)

High pt

Inclusive High Pt Spectra and V2 Paper(s)

Event-by-EventMultiplicity Fluctuations Paper* (PRC)Balance Functions* (PRL) +Pt Fluctuations Paper (2) in Special Committee4-Particle Correlation Paper* (PRC) +

HBT

3-pion Correlations* (PRL) +

K-pi Correlations* (PRL) +

Phase Space Density

Azimuthally Sensitive HBT* (PRL)

STARSTARSTAR Physics Papers in Preparation from 130 GeV Au + Au

• Ultra-Peripheral CollisionsProduction of the -meson in UPC

• In Godfather Committee:Ratios Paper (PRL)

K* Paper (PRL)

Strange Particle Flow (PRL)

Kaon Paper

~ ready for submission:

Lambda Paper

* = completed preview

PWG Convenor Group Paper Preview ProcessPWG Convenor Group Paper Preview Process

• PWG Convenor (PWGC) Group agreed to meet:- bi-weekly meetings by telephone. - in-person 1 day/month to discuss PWGC business. - Physics Analysis Coordinator (PAC) will chair these meetings.

In order to:1) allow early examination of "papers" by a group with a broad physics perspective and a range of individual physics interests in STAR. This could include the merging of different types of analyses, specific figures, and possibly papers. This will rapidly become important for STAR as we attempt to correlate our results and better understand the physics from our data. We also anticipate that more "interpretive" papers, including a range of data and analyses from STAR, will become increasingly important. Such an early overview of proposals will help STAR prepare and publish better papers.

2) provide guidance on the journal for which each paper is targeted, and

3) provide feedback and guidance to the PA's and PWG Convenors before the text and format of papers have been determined. Early examination is important to allow direction changes prior to any large investment of time and effort on the text of papers.

STARSTAR

PWG Convenor Group Paper Preview ProcessPWG Convenor Group Paper Preview Process

Spokesman & Physics Working Group Convenor Group decided unanimously:

- to institute practice of Principal Authors submitting proposals for papers to the Spokesman, once the analysis has been discussed in the PWG and agreed to be sound, but prior to agreement on the text.

- proposal to include

abstract

primary physics points of the paper

proposed figures and tables

other supporting or explanatory info

journal to which paper is intended for submission.

Physics Analysis Coordinator and the PWGC Group are charged to discuss each proposal and make recommendations on proposal to the Spokesman.

Spokesman shall provide PA's and PWG Convenors with relevant PWGC Group's guidance on proposal.

This is intended to be a fast process.

Presented to Council (Dec. 7) / will be discussed tomorrow also.

STARSTAR

Physics - “accomplished a lot, much more to do, Physics - “accomplished a lot, much more to do, so little beam time!”so little beam time!”

What are the open questions? Deconfinement? Chiral restoration? Understand Dynamics (early, expansion, late stages) & kinetic properties Parton Propagation (systematics, Cronin, propagation in hadronic matter)

• What must we still measure? When (next slide)?• Multiply-strange baryon spectra (s and A dependences)• J/ e+e-

• Open Charm (D-mesons) future• Disoriented chiral condensates? low Pt spectra, charge/neutral ratios• e+e-

• Particle production systematics• Evolution (and systematics) of colliding systems• High Pt hadrons (at least to 10 - 12 GeV/c, other systems inc. p/d + Au)

also p, p out to 5 GeV/c• High Pt correlations future

• Still Room for New Ideas!

• Photon-Pomeron Physics!

• Entire Spin Physics Program!

STARSTAR

RHI Physics Program 2001 - 2005RHI Physics Program 2001 - 2005

Relativistic Heavy Ion Physics (AA plus reference data using pp, pA)

Soft (pt < 2 GeV/c) Physics (2000 - 2004)• identified particle spectra (K, p, anti-particles, strange particles, resonances)• light anti-nuclei yields• flow• particle correlations• multiply-strange baryon () spectra• transverse energy production• event-by-event fluctuations (inc: charge, DCC, pt , ...; P, CP violations)• studies of event classes

High pt Physics (2000 - 2004)• parton energy loss

– charged single particles– identified particles (inc. o) to ~ 5 GeV/c

• high pt particle correlations, photons, jets*“electrons” (2002/3 )

• e+e-• J/ e+e-

p/d + A physics (2002 )• nuclear structure functions/shadowing (-jet)• jets, direct photons• J/ e+e-

STARSTAR

Photon/Pomeron Physics (ultra-peripheral AA)Two-photon and photon-pomeron physics (2000 - 2003)

• states with mass < 2 GeV (2-prong final states)• multiple vector meson production (4-prong final states)• J/ e+e-

Higher mass states (2002/3 )• electron decays of higher charm states• final states containing photons• particle identification to identify higher mass strange and charm decays• trigger on semi-leptonic decays of charm states• ….

Spin physics (2001 2005)

2001 AN (with transverse spin)

2002 start (?) to measure ALL via inclusive jet production sensitive to G

2003 measure ALL via direct photons and jets sensitive to G

G(x) and q(x) from dijet production

Higher energy - tests of parity-violating asymmetries in W production

2004 ALL from -jet coincidences

ALL from Drell-Yan production of e+e-

Initial studies of parity-violating asymmetries in W production

2005 Measurement of parity-violating asymmetries in W production

(quark and anti-quark contribution to proton spin)

Photon/Pomeron Physics and Photon/Pomeron Physics and Spin Physics Programs 2001 - 2005Spin Physics Programs 2001 - 2005STARSTAR

STAR Installation for 2001 Run

• Silicon Vertex Tracker

• Barrel Electromagnetic Calorimeter modules (complete 24 of 120 modules)

• Level 3 Processors

• 2 Forward Time Projection Chambers

• Time-of-Flight Patch

Summary Detector Additions 2001 - 2004Summary Detector Additions 2001 - 2004STARSTAR

STAR Installation for 2002 Run

• Silicon Strip Detector

• Barrel Electromagnetic Calorimeter modules (complete 60 of 120)

• Endcap Electromagnetic Calorimeter (lower half installed)

• Data Rate Increase

• Level 1,2,3 Processors

STAR Installation for 2003 Run

• Barrel Electromagnetic Calorimeter modules (complete 88 of 120)

• Endcap Electromagnetic Calorimeter (complete, 1 < < 2, = 2))

• Photon Multiplicity Detector

• start Time-of-Flight Barrel?

STAR Installation for 2004 Run

• Barrel Electromagnetic Calorimeter modules (complete 120 of 120. I.e. -1 < < 1, = 2)

• Time-of-Flight Barrel (completed in 2005)?

• start Micro-vertex Detector?

Issues in STARIssues in STAR

• “Physics First!”detectors data-taking recon analysis papers“complex” convergence

STARSTAR

• Physics, physics directions, and futureopen discussioncommon goals guidance (Spokesperson, Council, Collaboration)

• Sociologyindividuals working toward common goalsrepresentation and voicediversify committees (Talks, PWGC Group, GFCs,…)service workinclusive

Future of STARFuture of STAR

• Finish papers for snn = 130 GeV Au + Auesp. High Pt, Strange baryons, …………………

• Start snn = 200 GeV Au + Au, p + p production, and analyse for physicsphysics for Quark Matter………beyond

• Must increase data (for-physics) ratescontinue to increase

trigger capabilities (to select physics of interest)(Trigger Board is in place)

DAQ ratescpu/disk for recon/analysis

install and commission new detectors EMC, SSD, PMD, TOF-RPC patch, …TOF-barrel……

vtx…..)test, install and commission new software

Integrated Tracking• R&D and Detector Plans (see afternoon session)

• STAR Future Physics Workshop in April (details in Ludlam’s talk)• Decide STAR Physics Goals & Priorities (this summer)• Determine R&D Funding Requests (this summer)

• Must finally get STAR Detector Trailer at STAR Hall!• Long Term Major Upgrade Proposal (end of year)

STARSTAR

The EndThe End