STAR Detector Overview

K.H. Ackermannp, N. Adamsx, C. Adlerk, Z. Ahammedw,S. Ahmadx, C. Allgower, J. Amonettn, J. Amsbaughad,

B.D. Andersonn, M. Andersone, E. Andersseno, H. Arnesenb,L. Arnold n, G.S. Averichevi, A. Baldwinn, J. Balewski,

O. Barannikovai,w, L.S. Barnbyn, J. Baudotm, M. Beddoa,S. Bekelet, V.V. Belagai, R. Bellwiedae, S. Bennettae,

J. Bercovitzo, J. Bergerk, W. Bettsb, H. Bichselad, F. Biesero,L.C. Blandb, M. Bloomero, C.O. Blythc, J. Boehmo, B.E. Bonnerx,

D. Bonnetm, R. Bossinghamo, M. Botlob, A. Bouchamz,N. Bouillo z, S. Bouvierz, K. Bradleyo, F.P. Bradye, A. Brandinr,

R. L. Brownb, G. Brugalettead, M. Burkeso, R.V. Cadmana,H. Cainesag, M. Calderon de la Barca Sanchezb, A. Cardenasw,

L. Carrad, J. Carrollo, J. Castilloz, M. Castroae, D. Cebrae,S. Chattopadhyayae, M.L. Chenb, W. Chenb, Y. Chenf ,

S.P. Chernenkoi, M. Cherneyh, A. Chikanianag, B. Choiab,J. Chrinh, W. Christieb, J.P. Coffinm, L. Coninz, C. Consigliob,T.M. Cormierae, J.G. Cramerad, H.J. Crawfordd, I. Danilovi,

D. Daytonb, M. DeMellox, W.S. Dengb, A.A. Derevschikovv,M. Dialinasz, H. Diazb, P.A. DeYoungg, L. Didenkob,

D. Dimassimob, J. Dioguardib, C. Drancourtz, T. Dietelk,J.E. Drapere, V.B. Dunini, J.C. Dunlopag, V. Eckardtp,

W.R. Edwardso, L.G. Efimovi, T. Eggertp, V. Emelianovr,J. Engelaged, G. Eppleyx, B. Erazmusz, A. Etkinb, P. Fachinib,

V. Faineb, C. Felicianob, D. Ference, M.I. Fergusonf , H. Fesslerp,K. Filimonovo, E. Finchag, Y. Fisyakb, D. Flierl k, I. Floresd,

K.J. Foleyb, D. Fritzo, J. Fuo, C.A. Gagliardiaa, N. Gagunashvilii,J. Gansag, L. Gaudichetz, M. Gazdzicki, M. Germainm,F. Geurtsx, V. Ghazikhanianf , C. Gojakm, J. Grabskiac,

O. Grachovae, M. Graub, D. Greinero, L. Greinerd, V. Grigorievr,D. Grosnicka, J. Grossh, M. Guedonm, G. Guillouxz, E. Gushinr,J. Hallae, T.J. Hallmanb, D. Hardtkeo, G. Harperad, J.W. Harrisag,

M. Heffnere, S. Heppelmannu, T. Herstonw, D. Hill a,

Preprint submitted to Elsevier Science 18 November 2002

B. Hippolytem, A. Hirschw, E. Hjorto, G.W. Hoffmannab,M. Horsleyag, M. Howead, H.Z. Huangf , T.J. Humanict,

H. Hummlerp, W. Hunt, J. Huntero, G. Igof , A. Ishiharaab,Yu.I. Ivanshinj, P. Jacobso, W.W. Jacobs, S. Jacobsono,

M. Janikac, R. Jaredo, P. Jensenab, I. Johnsono, P.G. Jonesc,E.G. Juddd, M. Kanetao, M. Kaplang, D. Keanen, A. Khodinovr,

J. Kiryluk f , A. Kisiel ac, J. Klayo, S.R. Kleino, A. Klyachko,G. Koehlero, A.S. Konstantinovv, I. Kotov t, M. Kopytinen,L. Kotchendar, A.D. Kovalenkoi, M. Kramers, P. Kravtsovr,

K. Kruegera, T. Krupienb, P. Kuczewskib, C. Kuhnm,A.I. Kulikov i, G.J. Kundeag, C.L. Kunzg, R. Kh. Kutuevj,

A.A. Kuznetsovi, L. Lakehal-Ayatz, M.A.C. Lamontc,J.M. Landgrafb, S. Langek, C.P. Lansdellab, B. Lasiukag, F. Laueb,

A. Lebedevb, T. LeComptea, R. Lednicky i, W.J. Leonhardtb,V.M. Leontievv, M.J. LeVineb, Q. Li ae, C.-J. Liawb, J. Linh,

S.J. Lindenbaums, V. Lindenstrutho, P.J. Lindstromd, M.A. Lisa t,F. Liu af, L. Liu af, Z. Liu af , Q.J. Liuad, T. Ljubicicb, W.J. Llopex,

G. LoCurtop, H. Longf , R.S. Longacreb, M. Lopez-Noriegat,W.A. Loveb, D. Lynnb, R. Maierp, R. Majkaag, S. Margetisn,

C. Markertag, L. Martin z, J. Marxo, H.S. Matiso,Yu.A. Matulenkov, C. McParlando, T.S. McShaneh, J. Meierh,

F. Meissnero, Yu. Melnickv, A. Meschaninv, M. Messerb,P. Middlekampb, B. Miller b, M.L. Miller ag, Z. Milosevichg,

N.G. Minaevv, B. Minor o, J. Mitchellx E. Mogaverob,V.A. Moiseenkoj, D. Moltz o, C.F. Mooreab, V. Morozovo,

M.M. de Mouraae, M.G. Munhozy, G.S. Mutchlerx, J.M. Nelsonc,P. Nevskib, M. Nguyenb, T. Nguyenb, V.A. Nikitin j, L.V. Nogachv,

T. Noggleo, B. Normann, S.B. Nurushevv, T. Nussbaumx,J. Nystrando, G. Odynieco, A. Ogawau, C.A. Ogilvie1,

V. Okorokovr, K. Olchanskib, M. Oldenburgp, D. Olsono, G. Ottab,D. Padrazob, G. Paict, S.U. Pandeyb, Y. Panebratsevi,

S.Y. Panitkinb, A.I. Pavlinovae, T. Pawlakac, V. Perevoztchikovb,W. Perytac, V.A Petrovj, W. Pinganaudz, S. Pirogovf , E. Platnerx,

J. Plutaac, I. Polkb, N. Porilew, J. Porterb, A.M. Poskanzero,E. Potrebenikovai, D. Prindlead, C. Pruneauae, J. Puskar-Pasewicz,

2

G. Raio, J. Rassono, O. Ravelz, R.L. Rayab, S.V. Razini,,D. Reichholdh, J.G. Reidad, R.E. Renfordtk, F. Retiereo,

A. Ridigerr, J. Risoae, H.G. Rittero, J.B. Robertsx, D. Roehrichk,O.V. Rogachevskii, J.L. Romeroe, C. Royz, D. Russg, V. Rykovae,I. Sakrejdao, R. Sanchezf , Z. Sandlerf , S. Salurag, J. Sandweissag,

A.C. Saulysb, I. Savinj, J. Schambachab, R.P. Scharenbergw,J. Scheblienb, R. Scheetzb, R. Schluetero, N. Schmitzp,

L.S. Schroedero, M. Schulzb, A. Schuttaufp, K. Schwedao,J. Sedlmeirb, J. Segerh, D. Seliverstovr, P. Seybothp,R. Seymourad, E. Shahalievi, K.E. Shestermanovv,

S.S. Shimanskiii, D. Shumano, V.S. Shvetcovj, G. Skoroi,N. Smirnovag, L.P. Smykovi, R. Snellingso, K. Solberg,P. Sorensenf , J. Sowinski, H.M. Spinkaa, B. Srivastavaw,E.J. Stephenson, R. Stockk, A. Stolpovskyae, N. Stoneb,

M. Strikhanovr, B. Stringfelloww, H. Stroebelek, C. Struckk,A.A.P. Suaideae, E. Sugarbakert, C. Suirem, M. Sumberat,

T.J.M. Symonso, A. Szanto de Toledoy, P. Szarwasac, A. Tai f ,J. Takahashiy, A.H. Tangn, A. Tarchinim, J. Tarziano,

J.H. Thomaso, M. Thompsonc, V. Tikhomirovr, M. Tokarevi,M.B. Tonjesq, S. Tonseo, T.A. Trainorad, S. Trentalangef ,

R.E. Tribbleaa, V. Trofimovr, O. Tsaif , K. Turnerb, T. Ullrich b,D.G. Underwooda, I. Vakulaf , G. Van Burenb,

A.M. VanderMolenq, A. Vanyashino, I.M. Vasilevskij,A.N. Vasilievv, S.E. Vigdor, G. Visserd, S.A. Voloshinae, C. Vuo,

F. Wangw, H. Wardab, J.W. Watsonn, D. Weerasundaraad,R. Weidenbacho, R. Wellst, T. Wenausb, G.D. Westfallq,

J.P. Whitfieldg, C. Whitten Jr.f , H. Wiemano, R. Willsont,K.Wilsonae, J. Wirtho, J. Wisdomf , S.W. Wissink, R. Witt ag,

J. Wolfo, J. Woodf , N. Xu o, Z. Xub, A.E. Yakutinv,E. Yamamotoo, J. Yangf , P. Yepesx, A. Yokosawaa, V.I. Yurevichi,

Y.V. Zanevskii, I. Zborovsky i, H. Zhangag, W.M. Zhangn,D. Zimmermano, R. Zoulkarneevj, A.N. Zubarevi

(STAR Collaboration)aArgonne National Laboratory, Argonne, Illinois 60439

bBrookhaven National Laboratory, Upton, New York 11973

3

cUniversity of Birmingham, Birmingham, United KingdomdUniversity of California, Berkeley, California 94720

eUniversity of California, Davis, California 95616fUniversity of California, Los Angeles, California 90095

gCarnegie Mellon University, Pittsburgh, Pennsylvania 15213hCreighton University, Omaha, Nebraska 68178

iLaboratory for High Energy (JINR), Dubna, RussiajParticle Physics Laboratory (JINR), Dubna, Russia

kUniversity of Frankfurt, Frankfurt, GermanyIndiana University, Bloomington, Indiana 47408

mInstitut de Recherches Subatomiques, Strasbourg, FrancenKent State University, Kent, Ohio 44242

oLawrence Berkeley National Laboratory, Berkeley, California 94720pMax-Planck-Institut fuer Physik, Munich, Germany

qMichigan State University, East Lansing, Michigan 48824rMoscow Engineering Physics Institute, Moscow Russia

sCity College of New York, New York City, New York 10031tOhio State University, Columbus, Ohio 43210

uPennsylvania State University, University Park, Pennsylvania 16802vInstitute of High Energy Physics, Protvino, RussiawPurdue University, West Lafayette, Indiana 47907

xRice University, Houston, Texas 77251yUniversidade de Sao Paulo, Sao Paulo, Brazil

zSUBATECH, Nantes, FranceaaTexas A & M, College Station, Texas 77843

abUniversity of Texas, Austin, Texas 78712acWarsaw University of Technology, Warsaw, Poland

adUniversity of Washington, Seattle, Washington 98195aeWayne State University, Detroit, Michigan 48201

af Institute of Particle Physics, Wuhan, Hubei 430079 ChinaagYale University, New Haven, Connecticut 06520

Abstract

An introduction to the STAR detector and a brief overview of the physics goals of theexperiment are presented.

4

1 Introduction

The Solenoidal Tracker at RHIC (STAR) is one of two large detector systems con-structed at the Relativistic Heavy Ion Collider (RHIC) at Brookhaven National Lab-oratory.

There are eighteen articles in this volume that describe the STAR detector. Theyare:

• STAR Detector Overview (This article)• The STAR Detector Magnet System• The STAR Silicon Vertex Tracker• The STAR Silicon Strip Detector• The STAR Time Projection Chamber• The Readout System for the STAR Time Projection Chamber• The Laser System for the STAR Time Projection Chamber• The STAR TPC Gas System• The Forward Time Projection Chamber in STAR• Identification of Highpt Particles with the STAR-RICH Detector• The STAR Barrel Electromagnetic Calorimeter• The STAR Endcap Electromagnetic Calorimeter• The STAR Photon Multiplicity Detector• An Overview of the STAR DAQ System• The STAR Trigger• The STAR Level-3 Trigger System• Hardware Controls for the STAR Experiment at RHIC• Integration and Conventional Systems at STAR

STAR was constructed to investigate the behavior of strongly interacting matterat high energy density and to search for signatures of quark-gluon plasma (QGP)formation. Key features of the nuclear environment at RHIC are a large numberof produced particles (up to approximately one thousand per unit pseudo-rapidity)and high momentum particles from hard parton-parton scattering. STAR will mea-sure many observables simultaneously to study signatures of a possible QGP phasetransition and to understand the space-time evolution of the collision process inultra-relativistic heavy ion collisions. The goal is to obtain a fundamental under-standing of the microscopic structure of these hadronic interactions at high energydensities.

1 Presently at Iowa State University, Ames, Iowa 50011

5

Fig.

1.P

erspectiveview

ofthe

STA

Rdetector,

with

acutaw

ayfor

viewing

innerdetector

systems.

2D

etectorO

verview

Inorder

toaccom

plishthis,

STA

Rw

asdesigned

primarily

form

easurements

ofhadron

productionovera

largesolid

angle,featuringdetector

systems

forhigh

pre-cision

tracking,mom

entumanalysis,and

particleidentification

atthecenterofm

ass(c.m

.)rapidity.T

helarge

acceptanceofS

TAR

makes

itparticularlyw

ellsuitedfor

event-by-eventcharacterizations

ofheavy

ioncollisions

andfor

thedetection

ofhadron

jets.

The

layoutoftheS

TAR

experiment[1]is

shown

inF

igure1.A

cutaway

sideview

ofthe

STA

Rdetector

asconfigured

forthe

RH

IC2001

runis

displayedin

Fig-

ure2.

Aroom

temperature

solenoidalmagnet[2]

with

am

aximum

magnetic

fieldof0.5

Tprovides

auniform

magnetic

fieldforcharged

particlem

omentum

analysis.C

hargedparticle

trackingclose

tothe

interactionregion

isaccom

plishedby

aS

il-icon

VertexT

racker[3](S

VT

)consisting

of216

silicondrift

detectors(equivalent

toa

totalof13

million

pixels)arranged

inthree

cylindricallayersat

distancesof

approximately

7,11and

15cm

fromthe

beamaxis.In

thenearfuture,a

4thlayerof

Silicon

DriftD

etectors[4](SD

D)

willbe

addedto

theinner

tracker.The

siliconde-

tectorscover

apseudo-rapidity

range|η|≤

1w

ithcom

pleteazim

uthalsymm

etry(∆

φ=

2π).S

ilicontracking

closeto

theinteraction

allows

precisionlocalization

ofthe

primary

interactionvertex

andidentification

ofsecondary

verticesfrom

weak

decaysof,for

example,Λ,Ξ

,andΩ

s.Alarge

volume

Tim

eP

rojectionC

hamber[5]

(TP

C)

forcharged

particletracking

andparticle

identificationis

locatedata

radialdistance

from50

to200

cmfrom

thebeam

axis.T

heT

PC

is4

meters

longand

itcovers

apseudo-rapidity

range|η|≤

1.8for

trackingw

ithcom

pleteazim

uthalsym

metry

(∆φ

=2π

)providing

theequivalent

of70

million

voxelsvia

136,608

6

channels of front end electronics[6] (FEE). Both the SVT and TPC contribute toparticle identification using ionization energy loss, with an anticipated combinedenergy loss resolution (dE/dx) of 7 % (σ). The momentum resolution of the SVTand TPC reach a value ofδp/p = 0.02 for a majority of the tracks in the TPC. Theδp/p resolution improves as the number of hit points along the track increases andas the particle’s momentum decreases, as expected.

Fig. 2. Cutaway side view of the STAR detector as configured in 2001.

To extend the tracking to the forward region, a radial-drift TPC (FTPC)[7] is in-stalled covering2.5 <| η |< 4, also with complete azimuthal coverage and sym-metry. To extend the particle identification in STAR to larger momenta over a smallsolid angle for identified single-particle spectra at mid-rapidity, a ring imagingCherenkov detector [8] covers| η |< 0.3 and∆φ = 0.11π, and a time-of-flight(TOF) patch covers−1 < η < 0 and∆φ = 0.04π (as shown in Figure 2). About10 percent of the full-barrel electromagnetic calorimeter[9] (EMC) shown in Fig-ure 1 was installed for 2001 (see Figure 2). The remaining EMC and an endcapelectromagnetic calorimeter[10] (EEMC) will be installed over the next three yearsto obtain an eventual coverage of−1 < η < 2 and∆φ = 2π. This system willallow measurement of the transverse energy of events, and trigger on and measurehigh transverse momentum photons, electrons, and electromagnetically decayinghadrons. The EMC’s include shower-maximum detectors to distinguish high mo-mentum single photons from photon pairs resulting fromπ andη meson decays.The EMC’s will also provide prompt charged particle signals essential to discrim-inate against pileup tracks in the TPC, arising from other beam crossings fallingwithin the 40µsec drift time of the TPC, which are anticipated to be prevalent atRHIC pp collisions luminosities (≈ 1032cm−2s−1).

7

3 DAQ and Triggering

The STAR data acquisition system[11] (DAQ) is fast and flexible. It receives datafrom multiple detectors and these detectors have a wide range of readout rates. Theevent size is of order 200 MB and the events are processed at input rates up to 100Hz.

The STAR trigger system[12] is a 10 MHz pipelined system which is based oninput from fast detectors to control the event selection for the much slower track-ing detectors. The trigger system is functionally divided into different layers withlevel 0 being the fastest while level 1 and level 2 are slower but they apply moresophisticated constraints on the event selection.

STAR has a third level trigger[13] which performs complete online reconstructionof the events in a dedicated CPU farm. The level 3 trigger can process central Au-Au collisions at a rate of 50 Hz including simple analysis of physics observablessuch as particle momentum and rate of energy loss. The level 3 trigger systemincludes an online display so that individual events can be visually inspected inreal time. See Fig. 3 for an end view of an event in the TPC.

Fig. 3. Beam’s eye view of a central event in the STAR Time Projection Chamber. Thisevent was drawn by the STAR level-3 online display.

The fast detectors that provide input to the trigger system are a central trigger bar-rel (CTB) at| η |< 1 and zero-degree calorimeters (ZDC) located in the forwarddirection atθ < 2 mrad. (In the future, additional detectors will be used as in-put to the trigger system.) The CTB surrounds the outer cylinder of the TPC, and

8

triggers on the flux of charged-particles in the midrapidity region. The ZDCs areused for determining the energy in neutral particles remaining in the forward di-rections. Each experiment at RHIC has a complement of ZDC’s for triggering andcross-calibrating the centrality triggering between experiments [14]. Displayed inFigure 4 is the correlation between the summed ZDC pulse height and that of theCTB for events with a primary collision vertex successfully reconstructed fromtracks in the TPC. The largest number of events occurs for large ZDC values andsmall CTB values (gray region of the plot). From simulations these correspond tocollisions at large impact parameters, which occur most frequently and which char-acteristically leave a large amount of energy in the forward direction (into the ZDC)and a small amount of energy and particles sideward (into the CTB). Collisions atprogressively smaller impact parameters occur less frequently and result in less en-ergy in the forward direction (smaller pulse heights in ZDC) and more energy inthe sideward direction (larger pulse heights in CTB). Thus, the correlation betweenthe ZDC and CTB is a monotonic function that is used in the experiment to providea trigger for centrality of the collision. The ZDC is double-valued since collisionsat either small or large impact parameter can result in a small amount of energy inthe forward ZDC direction.

Central Trigger Barrel (arb. units) 0 5000 10000 15000 20000 25000

Zer

o D

egre

e C

alo

rim

eter

(ar

b. u

nit

s)

0

20

40

60

80

100

120

140

160

180

200

Fig. 4. Correlation between the summed pulse heights from the Zero Degree Calorime-ters and the Central Trigger Barrel for events with a primary collision vertex successfullyreconstructed from tracks in the Time Projection Chamber.

A minimum bias trigger was obtained by selecting events with a pulse height largerthan that of one neutron in each of the forward ZDC’s, which corresponds to 95percent of the geometrical cross section. Triggers corresponding to smaller impact

9

parameter were implemented by selecting events with less energy in the forwardZDCs, but with sufficient CTB signal to eliminate the second branch at low CTBvalues shown in Figure 4.

4 Physics Overview

The STAR physics program at RHIC can be divided into three main categories: astudy of high density QCD, measurement of the spin structure function of the pro-ton, and a study of photon and pomeron interactions from electromagnetic fields ofthe passing ions at RHIC. RHIC and STAR were built initially to study high den-sity QCD and to search for the QGP using ultra-relativistic heavy ion collisions.STAR will also study proton-proton interactions and proton-nucleus interactionsin order to understand the initial parton distribution functions of the incident nu-clei and for reference data for the heavy ion studies. By studying interactions ofpolarized protons at RHIC, STAR will determine the contributions from the prefer-ential orientation of gluon spins to the overall spin of the proton, and we will mapthe flavor-dependence of antiquark polarizations in a polarized proton. Through theuse of ultra-peripheral heavy ion interactions STAR will study photon and pomeroninteractions resulting from the intense electromagnetic fields of the colliding ionsand colorless strong interactions, respectively.

Inclusive pt andη distributions of charged particles will be measured in STAR toinvestigate the degree of thermalization, contribution of collective flow, possibleeffects of disoriented chiral condensates, at low pt, and nuclear effects and partonenergy loss at high pt. The pt spectra of baryons and anti-baryons at mid-rapidityhelp determine the nuclear stopping power, baryon number transport, and estab-lishes the baryo-chemical potential of the particle-emitting source at mid-rapidity.Global thermodynamic variables such as entropy, baryon and strangeness chemi-cal potentials, temperature, energy density, and pressure can be associated with themultiparticle final state observables of pion multiplicity, net baryon distributionsand strange particle abundance, mean transverse momentum, transverse energy andparticle flow, respectively.

As a consequence of the large particle multiplicities in central collisions and thelarge acceptance of STAR, STAR will investigate nonstatistical (dynamical) fluctu-ations, deviations from global thermodynamic variables, and other significant de-partures from conventional hadronic physics. Color fluctuations in the early par-tonic stages of collision may result in significant dynamical variation in the pro-duced particle spectra. Chiral symmetry restoration and nonequilibrium evolutionof the collision system may produce chirally-disoriented domains in which theneutral-to-charged ratio of low-pt pions deviates significantly from its nominalvalue.

10

Correlations between identical and non-identical pairs of particles will provide in-formation on the freezeout geometry, the expansion dynamics and possibly the ex-istence of a QGP. The dependence of the pion-emitting and kaon-emitting sourceparameters on the transverse momentum components of the particle pairs, and as afunction of the various types of particle pairs will be measured with high statistics.

The hard scattering component becomes prominent at RHIC energies and is calcu-lable in perturbative quantum chromodynamics (pQCD). This allows, for the firsttime in relativistic heavy ion collisions, the use of high transverse momentum pro-cesses (such as hard scattering of partons) in the form of high pt jets, mini-jets andsingle particles to probe the properties of the medium through which they propa-gate.

In addition to the heavy ion program, STAR will utilize polarized proton-protoncollisions to accumulate detailed information on the contribution of gluons to thespin of the proton. Recent results from polarized deep-inelastic scattering experi-ments indicate that the intrinsic spins of all the quarks and antiquarks combined canonly account for a fraction (≈ 30 percent) of the overall spin of the nucleon. TheSTAR experiment is uniquely suited to measure the contribution due to gluons viathe detection of photon-jet coincidence events at pt ≥ 10 GeV/c. If the quark andgluon spins together do not account for the nucleon spin, the only remaining sourcewould be the relative orbital motion of the quarks and gluons. Thus, measurementsof the spin substructure of the proton may lead beyond our current, still rudimentaryunderstanding of the quark motion inside a nucleon. In addition to probing gluonpolarization, STAR will study Wpm production in

√s = 500 GeV polarized proton

collisions to determine the flavor-dependence of antiquark polarization which isexpected to be sensitive to the mechanism for dynamical chiral symmetry breakingin the proton.

STAR will also study ultra-peripheral collisions, where the nuclei physically misseach other, but interact via longer ranged forces that couple coherently to the nucle-ons[15]. The best known example of this is two-photon collisions, studied at e+e−

colliders. Photon-Pomeron interactions will also be studied.

At the time of submission of this article the first physics results from RHIC havestarted to emerge. Initial results from STAR have been reported in [16–22], with theanticipation of many new physics results to come. In the remainder of this volume,the STAR detector subsystems will be described in detail in individual articles.

Acknowledgements

We wish to thank the RHIC Operations Group and the RHIC Computing Facilityat Brookhaven National Laboratory, and the National Energy Research Scientific

11

Computing Center at Lawrence Berkeley National Laboratory for their support.This work was supported by the Division of Nuclear Physics and the Division ofHigh Energy Physics of the Office of Science of the U.S.Department of Energy, theUnited States National Science Foundation, the Bundesministerium fuer Bildungund Forschung of Germany, the Institut National de la Physique Nucleaire et de laPhysique des Particules of France, the United Kingdom Engineering and PhysicalSciences Research Council, Fundacao de Amparo a Pesquisa do Estado de SaoPaulo, Brazil, the Russian Ministry of Science and Technology and the Ministry ofEducation of China and the National Science Foundation of China.

References

[1] ‘Conceptual Design Report for the Solenoidal Tracker At RHIC’, The STARCollaboration, PUB-5347 (1992); J.W. Harris et al, Nucl. Phys. A 566, 277c (1994).

[2] R.L. Brown et al., Proc. 1997 IEEE Particle Accelerator Conf., 3230 (1998)and F. Bergsma et al., ‘The STAR Detector Magenet Subsystem’, (this volume).

[3] D. Lynn et al., Nucl. Instrum. Meth. A447, 264 (2000)and R. Bellwied et al., ‘The STAR Silicon Vertex Tracker’, (this volume).

[4] L. Arnold et al., ‘The STAR Silicon Strip Detector’, (this volume).

[5] H. Wieman et al., IEEE Trans. Nucl. Sci. 44, 671 (1997)and M. Anderson et al., ‘The STAR Time Projection Chamber’, (this volume).

[6] S. Klein et al., IEEE Trans. Nucl. Sci. 43, 1768 (1996)and M. Anderson et al., ‘A Readout System for the STAR Time Projection Chamber’,(this volume).

[7] A. Schuttauf et al., Nuc. Phys. A661, 677c (1999)and K.H. Ackerman et al., ‘The Forward Time Projection Chamber in STAR’, (thisvolume).

[8] ‘A Ring Imaging Cherenkov Detector for STAR’, STARnote 349, STAR/ALICE RICHCollaboration (1998); ALICE Collaboration, Technical Design and Report, Detectorfor High Momentum PID, CERN/LHCC 98-19.

[9] M. Beddo et al., ‘The STAR Barrell Electromagnetic Calorimeter’, (this volume).

[10] C.E. Allgower et al., ‘The STAR Endcap Electromagnetic Calorimeter’, (this volume).

[11] A. Ljubicic et al., IEEE Trans. Nucl. Sci. 47, 99 (2000)and J.M. Landgraf et al., ‘An Overview of the STAR DAQ System’, (this volume).

[12] F.S. Beiser et al., ‘The STAR Trigger’, (this volume).

[13] J.S. Lange et al., IEEE Trans. Nucl. Sci. 48, 3 (2000)and C. Adler et al., ‘The STAR Level-3 Trigger System’, (this volume).

12

[14] ‘The RHIC Zero Degree Calorimeter’, C. Adler, A. Denisov, E. Garcia, M. Murray,H. Strobele, and S. White, Nucl. Instrum. Meth. A470, 488 (2001).

[15] S. R. Klein and J. Nystrand, Phys. Rev. C 60, 014903 (1999).

[16] ‘Elliptic Flow in Au+Au Collisions at√

snn = 130 GeV’, K.H. Ackermann et al.(STAR Collaboration), Phys. Rev. Lett. 86, 402-407 (2001).

[17] ‘Midrapidity Antiproton-to-Proton Ratio from Au+Au at√

snn = 130 GeV’, C. Adleret al. (STAR Collaboration), Phys. Rev. Lett. 86, 4778-4782 (2001).

[18] ‘Pion Interferometry of√

snn = 130 GeV Au+Au Collisions at RHIC’, C. Adler et al.(STAR Collaboration), Phys. Rev. Lett. 87, 082301 (2001).

[19] ‘Multiplicity Distribution and Spectra of Negatively Charged Hadrons in Au+AuCollisions at

√snn = 130 GeV’, C. Adler et al. (STAR Collaboration), Phys. Rev.

Lett. 87, 112303 (2001).

[20] ‘Identified Particle Elliptic Flow in Au+Au Collisions at√

snn = 130 GeV’, C. Adleret al. (STAR Collaboration), Phys. Rev. Lett. 87, 182301 (2001).

[21] ‘Antideuteron and Antihelium Production in Au+Au Collisions at√

snn = 130 GeV’,C. Adler et al. (STAR Collaboration), Phys. Rev. Lett. 87, 262301-1 (2001).

[22] ‘Measurement of Inclusive Antiprotons from Au+Au Collisions at√

snn = 130 GeV’,C. Adler et al. (STAR Collaboration), Phys. Rev. Lett. 87, 262302-1 (2001).

13