The hottest matter on earth: a look at the Relativistic Heavy Ion Collider

1. The hottest matter on earth: a look at the Relativistic Heavy Ion Collider Barbara V. Jacak Stony Brook March 7, 2002

2. outline • Science questions which define our goals • Structure of nuclear matter and theoretical tools we use • Making super-dense matter in the laboratory • the Relativistic Heavy Ion Collider • experimental observables & • what have we learned already? • Next steps…

3. Studying super-dense matter by creating a little bang! Structure of atoms, nuclei, and nucleons At very high energy shatter nucleons into a cloud of quarks and gluons Expect a phase transition to a quark gluon plasma does this really happen??? Such matter existed just after the Big Bang how does this stuff “work”?

4. At high temperature/density • Quarks no longer bound into nucleons ( qqq ) and mesons (qq ) • Phase transition  quarks move freely within the volume • they become a plasma*  • Early universe was a quark-gluon plasma • for a few microseconds after Big Bang • Probably also in the core of neutron stars • Plasma: conducting material, but charges • shield each other, making it ~ neutral • usually has a high temperature/density

5. Phase Transition • we don’t really understand • how process of quark confinement works • how symmetries are broken by nature  massive particles from ~ massless quarks • transition affects evolution of early universe • latent heat & surface tension  • matter inhomogeneity in evolving universe? • why more matter than antimatter today? • equation of state of nuclear matter compression in stellar explosions

6. + +… Quantum ChromoDynamics • Field theory • for strong interaction • among colored quarks • by exchange of gluons • Works pretty well... • Quantum Electrodynamics (QED) • for electromagnetic interactions • exchanged particles are photons • electrically uncharged • QCD: exchanged gluons have “color”charge •  a curious property: they interact among themselves This makes interactions difficult to calculate!

7. Transition temperature? QCD “simplified”: a 3d grid of quark positions & summing the interactions predicts a phase transition: Karsch, Laermann, Peikert ‘99 e/T4 T/Tc Tc ~ 170 ± 10 MeV (1012 °K) e ~ 3 GeV/fm3

8. So, we need to create a little bang in the lab! Use accelerators to reach highest energy vBEAM = 0.99995 x speed of light at RHIC center of mass energy s = 200 GeV/nucleon SPS (at CERN) has s  18 GeV/nucleon AGS (at BNL) s  5 GeV/nucleon Use heaviest beams possible maximum volume of plasma ~ 10,000 quarks & gluon in fireball

9. Experimental method Look at region between the two nuclei for T/density maximum Collide two nuclei RHIC is first dedicated heavy ion collider 10 times the energy previously available!

10. RHIC at Brookhaven National Laboratory Relativistic Heavy Ion Collider started operations in summer 2000

11. STAR 4 complementary experiments

12. Uncovering nature’s secrets is not easy! Large collaborations PHENIX has ~500 incl. Stony Brook many countries! “small” experiments have > 50 people! • Use connected computing around the world! • transfer data over the internet • centrally located software libraries • meetings span 3 continents • post slides on the web • circulate agendas, questions by email • everyone phones in

13. Collect the Data! Collect the Data! Collect the Data! Complex events require selections All 4 experiments have fast, custom electronics + multiple layers of computing inside • RHIC makes many collisions per second • can’t afford to write them all to tape • tape bandwidth is ~ 20 MB/sec • (would fill 20 GB disk in < 20 min) • select the interesting ones - in real time! • use the electronics + computing to collect, collate, calculate & trigger • take THIS one! PHENIX trigger coordinator: J. Nagle

14. In Heavy Ion Collisions When nuclei collide at near the speed of light, a cascade of quark & gluon scattering results…. 104 gluons, q, q’s

15. What do we want to knowabout the plasma? • Temperature • early in the collision, just after nuclei collide • Density • also early in the collision, when it is at its maximum • Are the quarks really free or still confined? • Properties of the quark gluon plasma: • equation of state (energy vs. pressure) • how is energy transported in the plasma?

16. pR2 2ct0 Is energy density high enough? PRL87, 052301 (2001) Colliding system expands: Energy  to beam direction per unit velocity || to beam e 4.6 GeV/fm3 YES - well above predicted transition! 50% higher than seen before

17. Density: a first look Central Au+Au collisions (~ longitudinal velocity) Adding all particles under the curve, find ~ 5000 charged particles These all started in a volume ~ that of a nucleus!

18. schematic view of jet production hadrons leading particle q q hadrons leading particle Observables IIDensity - use a unique probe Probe: Jets from scattered quarks Observed via fast leading particles or azimuthal correlations between the leading particles But, before they create jets, the scattered quarks radiate energy (~ GeV/fm) in the colored medium  decreases their momentum  fewer high momentum particles  beam  “jet quenching”

19. nucleons Something new at RHIC? From Federica Messer • Compare to a baseline, or control • use nucleon-nucleon collision at same energy • Au + Au collisions • are a superposition • of N-N reactions • (modulo effect of • nuclear binding or • collective motions) • Hard scattering processes scale as • number of N-N binary collisions <Nbinary> • so expect: YieldA-A = YieldN-N. <Nbinary>

20. Compare momentum spectra Compiled by A. Drees N-N collision at sNN = 130 GeV Phys. Rev. Lett. 88, 022301 (2002) Au+Au Nbinary = 905 central Nbinary = 20 peripheral

21. Deficit observed in central collisions Phys. Rev. Lett. 88, 022301 (2002) charged is from analysis by F. Messer of Stony Brook charged p0 transverse momentum (GeV/c) Charged deficit seen by both STAR & PHENIX STAR preliminary

22. u, d, s u, d, s c c Observables IIIConfinement • J/Y (cc bound state) • produced early, traverses the medium • if medium is deconfined (i.e. colored) • other quarks “get in the way” • J/Y screened by quark gluon plasma • binding dissolves  2 D mesons

23. J/Y suppression observed at CERN NA50 J/Y yield Fewer J/Y in Pb+Pb than expected! But other processes affect J/Y too so interpretation is still debated...

24. How about at RHIC? • PHENIX looks for J/Y  e+e- and m+m- A needle in a haystack must find electronwithout mistaking a pion for an electron at the level of one in 10,000 There is the electron. We use special detector to tag the electrons “RICH” Prof. Tom Hemmick of Stony Brook

25. g conversion All tracks Electron enriched sample (using RICH) We do find the electrons Energy/Momentum PHENIX sees some “extra” electrons they come from charm quarks c  D meson  e + K + n J/Y analysis is underway now

26. Observables IV: Propertieselliptic flow “barometer” Origin: spatial anisotropy of the system when created followed by multiple scattering of particles in evolving system spatial anisotropy  momentum anisotropy v2: 2nd harmonic Fourier coefficient in azimuthal distribution of particles with respect to the reaction plane Almond shape overlap region in coordinate space

27. Large v2: the matter can be modeled by hydrodynamics v2= 6%: larger than at CERN or AGS! Hydro. Calculations Huovinen, P. Kolb and U. Heinz STAR PRL 86 (2001) 402 pressure buildup  explosion pressure generated early!  early equilibration !? first hydrodynamic behavior seen

28. q e-, m- g * Thermal dilepton radiation e+, m+ q q Thermal photon radiation g q, g Observables VTemperature Look for “thermal” radiation processes producing thermal radiation: Rate, energy of the radiated particles determined by temperature NB: g, e, m interact only electromagnetically  they exit the collision without further interaction

29. At RHIC we don’t know yet But it should be higher since the energy density is larger At CERN, photon and lepton spectra consistent with T ~ 200 MeV Temperature achieved? NA50 WA98 photons m+ m- pairs

30. What have we learned? • unprecedented energy density at RHIC! • high density, probably high temperature • very explosive collisions  matter has a stiff equation of state • new features: hints of quark gluon plasma? • large elliptic flow, suppression of high pT, • J/Y suppression at CERN? • but we aren’t sure yet… What’s next?? To rule out conventional explanations • extend reach of Au+Au data • compare p+p, p+Au to check effect of cold nuclei on observables • study volume & energy dependence • are jets quenched & J/Y suppressed???

31. Mysteries... How come hydrodynamics does so well on elliptic flow and momentum spectra of mesons & nucleons emitted D. Teaney & J. Burward-Hoy … but FAILS to explain correlations between meson PAIRS? pT (GeV) Hydrodynamics is not explosive enough!

32. Mysteries II  If jets from light quarks are quenched, shouldn’t charmed quarks be suppressed too? nucl-ex/0202002

33. PHENIX at RHIC 2 Central spectrometers 2 Forward spectrometers 3 Global detectors Philosophy: optimize for signals / sample soft physics

34. vacuum matter box QGP Did something new happen? • Study collision dynamics • Probe the early (hot) phase Do the particles equilibrate? Collective behavior i.e. pressure and expansion? Particles created early in predictable quantity interact differently with QGP and normal matter fast quarks, bound cc pairs, s quarks, ... + thermal radiation!

35. Thermal Properties measuring the thermal history g, g* e+e-, m+m- p, K, p, n, f, L, D, X, W, d, Real and virtual photons from quark scattering is most sensitive to the early stages. (Run II measurement) Hadrons reflect thermal properties when inelastic collisions stop (chemical freeze-out). Hydrodynamic flow is sensitive to the entire thermal history, in particular the early high pressure stages.