The HBT excitation function in relativistic heavy ion collisions Mike Lisa Ohio State University
Jan 20, 2016
The HBT excitation functionin relativistic heavy ion collisions
Mike LisaOhio State University
Plan
)s(HBT T 1 2 sysˆHBT( ;p , y, b ,b,ms ,m ,A )
y
I will discuss a set of zero measure in this rich parameter space
• what do we think we can learn from systematics in X (=y, pT, |b|…)?
• what do we think we have learned from systematics in X (=y, pT, |b|…)?• how does this change with s ?
Also, upon request: comments on technical issues (event-mixing, Coulomb, non-Gaussianness, RP resolution correction…)
|b|
pT
Brief “summary” (intro to discussion)
qout
qside
qlong
Reminder
Rsi
de
R long
Rout
x1
x2
12 ppq
p1
p2
q
12 pp2
1k
• Two-particle interferometry: p-space separation space-time separation
• HBT: Quantum interference between identical particles
pairsevent mixed
pairsevent real
)(P)(P
),(P),(
21
2121
pp
ppppC
2long
2long
2side
2side
2out
2out)(1),(
RqRqRqekkqC
q (GeV/c)q (GeV/c)
C (
q)C
(q)
11
22R
1~
• Final-state effects (Coulomb, strong) also can cause correlations, need to be accounted for
Gaussian model (3-d):
qout
qside
qlong
Reminder
Rsi
de
R long
Rout
x1
x2
12 ppq
p1
p2
q
12 pp2
1k
• Two-particle interferometry: p-space separation space-time separation
RRsideside
RRoutout
Pratt-Bertsch (“out-side-long”) decomposition designed to help disentangle space & time
ˆT 1b ys2 sHBT( ;p , y, ,b ,m ,m ,A )s
E802 PRC66 054906 (2002)
14.6 AGeV Si+Al 14.6 AGeV Si+Au11.6 AGeV Au+Au
AGS: sNN 2-5 GeV
• Expected “geometric” scaling of transverse radii with |b|, Npart
• RL: trend (and expectation) less clear
ˆT 1b ys2 sHBT( ;p , y, ,b ,m ,m ,A )s
158 AGeV Pb+Pb
200 AGeV S+S
158 AGeV p+p
RQMD
NA49 NPA661 448c (1999)
“initial” Rside
SPS: sNN 17-20 GeV
• Expected “geometric” scaling of transverse radii with |b|, Npart
• RL: trend (and expectation) less clear
• apparent ~2x expansion
AGS: sNN 2-5 GeV
• Expected “geometric” scaling of transverse radii with |b|, Npart
• RL: trend (and expectation) less clear
ˆT 1b ys2 sHBT( ;p , y, ,b ,m ,m ,A )s
SPS: sNN 17-20 GeV
• Expected “geometric” scaling of transverse radii with |b|, Npart
• RL: trend (and expectation) less clear
• apparent ~2x expansion
AGS: sNN 2-5 GeV
• Expected “geometric” scaling of transverse radii with |b|, Npart
• RL: trend (and expectation) less clear
NA44, Eur Phys J C18 317 (2000)
ˆT 1b ys2 sHBT( ;p , y, ,b ,m ,m ,A )s
SPS: sNN 17-20 GeV
• Expected “geometric” scaling of transverse radii with |b|, Npart
• RL: trend (and expectation) less clear
• apparent ~2x expansion
AGS: sNN 2-5 GeV
• Expected “geometric” scaling of transverse radii with |b|, Npart
• RL: trend (and expectation) less clear
RHIC: sNN = 130-200 GeV
• Expected “geometric” scaling of transverse radii with |b|, Npart
• RL trend very similar (expected?)
• apparent ~2x expansion
PHENIX nucl-ex/0401003
STAR nucl-ex/0312009accepted to PRL
32-72% 12-32% 0-12%
STAR PRL87 082301 (2001)
So far…
ˆT 1b ys2 sHBT( ;p , y, ,b ,m ,m ,A )s
• can learn: how does FO system size track with initial size?• did learn: transverse expansion ~2x
• HBT radii appear to follow expected increases with (initial) system size(comforting to remember in present age of uncertainty)
• Rlong(Npart) with s ?
However, recall: HBT radii do not measure entire source, but “homogeneity regions” *
* [Sinyukov, “Hot Hadronic Matter: Theory and Experiment,” NATO ASI Series B 346:309 (1995)]
ˆ 1 2 sysbTHBT( ; , y, b , ,m ,m ,A )ps
Kolb & Heinz, QGP3 nucl-th/0305084
Decreasing R(pT)
• usually attributed to collective flow
• flow integral to our understanding of R.H.I.C.; taken for granted
• femtoscopy the only way to confirm x-p correlations – impt check
ˆ 1 2 sysbTHBT( ; , y, b , ,m ,m ,A )ps
Decreasing R(pT)
• usually attributed to collective flow
• flow integral to our understanding of R.H.I.C.; taken for granted
• femtoscopy the only way to confirm x-p correlations – impt check
Non-flow possibilities• cooling, thermally (not collectively)
expanding source
• combo of x-t and t-p correlationsearly times: small, hot source
late times: large, cool source
ˆ 1 2 sysbTHBT( ; , y, b , ,m ,m ,A )ps
Decreasing R(pT)
• usually attributed to collective flow
• flow integral to our understanding of R.H.I.C.; taken for granted
• femtoscopy the only way to confirm x-p correlations – impt check
Non-flow possibilities• cooling, thermally (not collectively)
expanding source
• combo of x-t and t-p correlations
MAL et al, PRC49 2788 (1994)
1500 fm/c (!)
ˆ 1 2 sysbTHBT( ; , y, b , ,m ,m ,A )ps
Decreasing R(pT)
• usually attributed to collective flow
• flow integral to our understanding of R.H.I.C.; taken for granted
• femtoscopy the only way to confirm x-p correlations – impt check
Non-flow possibilities• cooling, thermally (not collectively)
expanding source
• combo of x-t and t-p correlations
• hot core surrounded by cool shell
• important ingredient of Buda-Lund hydro picturee.g. Csörgő & LörstadPRC54 1390 (1996)
ˆ 1 2 sysbTHBT( ; , y, b , ,m ,m ,A )ps
Decreasing R(pT)
• usually attributed to collective flow
• flow integral to our understanding of R.H.I.C.; taken for granted
• femtoscopy the only way to confirm x-p correlations – impt check
Non-flow possibilities• cooling, thermally (not collectively)
expanding source
• combo of x-t and t-p correlations
• hot core surrounded by cool shell
• important ingredient of Buda-Lund hydro picturee.g. Csörgő & LörstadPRC54 1390 (1996)
t
Each scenario generatesx-p correlations but…
x2-p correlation: yesx-p correlation: yes
x2-p correlation: yesx-p correlation: no
x2-p correlation: yesx-p correlation: no
80 AMeV Ar+Sc(pp,X)
MAL et al, PRL70 3709 (1993)
ˆ 1 2 sysbTHBT( ; , y, b , ,m ,m ,A )ps
decreasing HBT R(p) present at all energies• sub-AGS energies (protons, IMFs)
• cooling significant• AGS (and upward) – flow dominated
•signs of trouble in s dep…(models OK @ one s but…)
x (fm)
y (f
m)
E895 PRL84 2798 (2000).
RQMD: Sorge PRC52 3291 (1995)
ˆ 1 2 sysbTHBT( ; , y, b , ,m ,m ,A )ps
decreasing HBT R(p) present at all energies• sub-AGS energies (protons, IMFs)
• cooling significant• AGS (and upward) – flow dominated
•signs of trouble in s dep…(models OK @ one s but…)
• SPS: smooth, almost (!) featureless transition AGS RHIC• can the models do that??!
E895 PRL84 2798 (2000)CERES, NPA714 124 (2003)STAR, PRL87 082301 (2001)
NB: error in CERES paper
E895 PRL84 2798 (2000).At fixed s, a chance to
understand system• higher energy AGS: hadronic flow• @ lower s
• could tune RQMD to give less flow…• model source too small and (maybe)
emits too slowly?
• SPS energy:• source too large?•model could be tuned…
• already pre-RHIC: doubts of a complete understanding•but RQMD (nor hydro) did not get p-space perfectly, so…
ˆ 1 2 sysbTHBT( ; , y, b , ,m ,m ,A )ps
NA44 RQMD
Rout 4.88 0.21 6.96 0.14
Rside 4.45 0.32 6.23 0.20
Rlong 6.03 0.35 7.94 0.21
NA44) PRC58, 1656 (1998)D. Hardtke, Ph.D. thesis (1997)
• already pre-RHIC: doubts of a complete understanding•but RQMD (nor hydro) did not get p-space perfectly, so…
ˆ 1 2 sysbTHBT( ; , y, b , ,m ,m ,A )ps
RHIC: new hope!• hydro reproduces p-space very well
with no/minimal tuning• details!
• But alas!• hydro nor hydro+RQMD
nor AMPT simultaneously gets p- and x-space
Hydro: P.Huovinen et al.(’01)PHENIX, PRL91(’03)182301.
Kolb &Heinz, hep-ph/0204061
QM01Heinz & Kolb, hep-ph/0204061
time
dN/dt
PCM & clust. hadronization
NFD
NFD & hadronic TM
PCM & hadronic TM
CYM & LGT
string & hadronic TM
• p-space observables well-understood within hydrodynamic framework
• x-space observables not well-reproduced• correct dynamical signatures with
incorrect dynamic evolution?
• Too-large timescales modeled?• emission/freezeout duration (RO/RS)• evolution duration (RL)
ˆ 1 2 sysbTHBT( ; , y, b , ,m ,m ,A )ps
Heinz & Kolb, hep-ph/0204061
ˆ 1 2 sysbTHBT( ; , y, b , ,m ,m ,A )ps
T=106 ± 1 MeV<InPlane> = 0.571 ± 0.004 c<OutOfPlane> = 0.540 ± 0.004 cRInPlane = 11.1 ± 0.2 fmROutOfPlane = 12.1 ± 0.2 fm
Life time () = 8.4 ± 0.2 fm/cEmission duration = 1.9 ± 0.2 fm/c2/dof = 120 / 86
BW: F. Retiere & MAL, nucl-th/0312024
• Poor experimentalist’s exploratory tool: BW• tunable parameters (T, , timescales..)
• p-space observables well-understood within hydrodynamic framework
• x-space observables not well-reproduced• correct dynamical signatures with
incorrect dynamic evolution?
• Too-large timescales modeled?• emission/freezeout duration (RO/RS)• evolution duration (RL)
Retiere QM04
ˆ 1 2 sysbTHBT( ; , y, b , ,m ,m ,A )ps
T=106 ± 1 MeV<InPlane> = 0.571 ± 0.004 c<OutOfPlane> = 0.540 ± 0.004 cRInPlane = 11.1 ± 0.2 fmROutOfPlane = 12.1 ± 0.2 fm
Life time () = 8.4 ± 0.2 fm/cEmission duration = 1.9 ± 0.2 fm/c2/dof = 120 / 86
• Poor experimentalist’s exploratory tool: BW• tunable parameters (T, , timescales..)
• Similar results from similar hydro-inspired models (e.g. Buda-Lund)
Csanád, Csörgő, Lörstad nucl-th/0311102 and nucl-th/0310040
ˆ 1 2 sysbTHBT( ; , y, b , ,m ,m ,A )ps
• flow-dominated “models” can reproduce soft-sector x-space observables
• imply short timescales
• however, are we on the right track? [flow]• puzzles? check your assumptions!
Csanád, Csörgő, Lörstad nucl-th/0311102 and nucl-th/0310040
ˆ 1 2 sysbTHBT( ; , y, b , ,m ,m ,A )ps
Decreasing R(pT)
• usually attributed to collective flow
• flow integral to our understanding of R.H.I.C.; taken for granted
• femtoscopy the only way to confirm x-p correlations – impt check
Non-flow possibilities• cooling, thermally (not collectively)
expanding source
• combo of x-t and t-p correlations
• hot core surrounded by cool shell
• important ingredient of Buda-Lund hydro picturee.g. Csörgő & LörstadPRC54 1390 (1996)
t
Each scenario generatesx-p correlations but…
x2-p correlation: yesx-p correlation: yes
x2-p correlation: yesx-p correlation: no
x2-p correlation: yesx-p correlation: no
ˆ 1 2 sysbTHBT( ; , y, b , ,m ,m ,A )ps
• flow-dominated “models” can reproduce soft-sector x-space observables
• imply short timescales
• however, are we on the right track? [flow]• puzzles? check your assumptions!• look for flow’s “special signature”
x-p correlation
• In flow pictures, low-pT particles emitted closer to source’s center (along “out”)
• non-identical particle correlations(FSI at low v) probe:
(x1-x2)2 (as does HBT)
x1-x2
Csanád, Csörgő, Lörstad nucl-th/0311102 and nucl-th/0310040
[click for more details on non-id correlations]
F. Retiere & MAL, nucl-th/0312024
pT
T
K
p
ˆT 2 sysb 1HBT( ;p , y, b , m ,m, ,A )s
• In flow pictures, low-pT particles emitted closer to source’s center (along “out”)
• non-identical particle correlations(FSI at low v) probe:
(x1-x2)2 (as does HBT)
x1-x2
• extracted shift in emission point x1-x2 consistent w/ flow-dominated blastwave
A. Kisiel (STAR) QM04
x
(fm
)
x (
fm)
T T
T s1b y2 sˆHBT( ; , y, b , ,m ,m , )p As
• latest “puzzle” in HBT?
• HBT radii from pp fall with pT
(as observed previously, usually attributed to string kT kick)…
• …but as much (proportionally) as dAu and AuAu ??• coincidence…?• something deeper…?
Rout
Rside
Rlong
p+p+X
pT
0.25 0.5
2
1
STAR, QM04
Rout / Rout(pp) Rside / Rside(pp)
Rlong / Rlong(pp)
Au+AuCollective expansion
p+pstring fragmentation
transverse plane
T s1b y2 sˆHBT( ; , y, b , ,m ,m , )p As
• latest “puzzle” in HBT?
• HBT radii from pp fall with pT
(as observed previously, usually attributed to string kT kick)…
• …but as much (proportionally) as dAu and AuAu ??• coincidence…?• something deeper…?
• What it does NOT mean:• AA=N*(strings)• AA=N*(“little blastwaves”)
• AA: global x-p correlations
localx-p corr.
NB: p-space observables identical in the two cases
So far…ˆT 1b ys2 sHBT( ;p , y, ,b ,m ,m ,A )s
• HBT radii appear to follow expected increases with (initial) system size• comforting to remember in present age of uncertainty
• Rlong(Npart)(s) less clear
ˆ sT 1 2 ysbHBT( ; , y, b , , ,A )p m ,ms
• can learn• what is nature of dynamic x-p correlations?• how strong is the flow?• what are the timescales involved?
• did learn• emitting source dominated by (global) collective flow
• HBT (and non-id) correlations described consistently with p-space• short evolution and emission timescales indicated
• HBT “puzzle”
puzzle? Get more information!
• generically: breaking azimuthal symmetry (b0) more differential detailed picture
• HBT(): as v2, sensitive to interplay b/t anisotropic geometry & dynamics/evolution
• another handle on dynamical timescales – likely impt in HBT puzzle
P. Kolb and U. Heinz, hep-ph/0204061P. Kolb, nucl-th/0306081
“radial flow”
“elliptic flow”
Obtaining more detailed information in p-space…
Strongly-interacting 6Li released from an asymmetric trapO’Hara, et al, Science 298 2179 (2002)
T ˆ 1 ysb 2 sHBT( ;p , y, b , ,m ,m ,A )s
What can we learn?
in-plane-extended
out-of-plane-extended
Teaney, Lauret, & Shuryak nucl-th/0110037
transverse FO shape+ collective velocity evolution time estimate
check independent of RL(pT)
?
T ˆ 1 ysb 2 sHBT( ;p , y, b , ,m ,m ,A )s
• observe the source from all angles with respect to RP
• expect oscillations in HBT radii (including “new” cross-terms)
big RS
small RS
T ˆ 1 ysb 2 sHBT( ;p , y, b , ,m ,m ,A )s
• observe the source from all angles with respect to RP
• expect oscillations in HBT radii (including “new” cross-terms)
• At AGS: observed at2, 4, 6 AGeV Au+Au• including first-order
oscillations at y=0• elliptical transverse shapes• strongly tilted w.r.t. beam
• physics of directed flow
p (°) 0 180
0
0 180 0 180
10
-10
20
40
R2 (
fm2 ) out side long
ol os sl
Au+Au 2 AGeV; E895, PLB 496 1 (2000)
(Beam)
Coordinate space!
x
y
z
s
b
2y~
2x~
x
y
Images of --emitting sources (scaled ~ x1014)
Mike Lisa:
1 fm = 1/4”
Mike Lisa:
1 fm = 1/4”
3 fm
x ’
y
2 AGeV
x
zS=47°
x ’
y
4 AGeV
x
zS=37°
x ’
y
6 AGeV
x
zS=33°
Large, positivetilt angles
35.1x~
y~
2
2
similar to naïveoverlap: b~5 fm
E895 – QM01
T ˆ 1 ysb 2 sHBT( ;p , y, b , ,m ,m ,A )s
• observe the source from all angles with respect to RP
• expect oscillations in HBT radii (including “new” cross-terms)
• At AGS: observed at2, 4, 6 AGeV Au+Au• including first-order
oscillations at y=0• elliptical transverse shapes• strongly tilted w.r.t. beam
• physics of directed flow
• At RHIC:• no 1st-order RP no tilt (yet)
(Beam)
Coordinate space!
x
y
z
s
b
2y~
2x~
x
y
1 2 sˆT b ysHBT( ; , y, , ,m ,m ,A )p bs
• observe the source from all angles with respect to RP
• expect oscillations in HBT radii (including “new” cross-terms)
• At AGS: observed at2, 4, 6 AGeV Au+Au• including first-order
oscillations at y=0• elliptical transverse shapes• strongly tilted w.r.t. beam
• physics of directed flow
• At RHIC:• no 1st-order RP no tilt (yet)• oscillations versus centrality• oscillations versus pT
• average values same as “traditional” HBT (sizes)
• oscillations: transverse shape STAR, nucl-ex/0312009, PRL in press
Estimate of initial vs F.O. source shape
2x
2y
2x
2y
RR
RR
20,S
22,S
FO R
R2
• estimate INIT from Glauber
• from asHBT:
FO < INIT → dynamic expansion
FO > 1 → source always OOP-extended
• constraint on evolution time
STAR, nucl-ex/0312009, PRL in press
FO =
init
1 2 sˆT b ysHBT( ; , y, , ,m ,m ,A )p bs
1 2 sˆT b ysHBT( ; , y, , ,m ,m ,A )p bs
2x
2y
2x
2y
RR
RR
sNN (GeV)
(approximately same centrality)
AGS: FO init
RHIC: FO < init
• transverse shape:• non-trivial excitation function• increased flow*time rounder
FO geometry @ RHIC• insufficient [flow]x[time] to
become in-plane
1 2 sˆT b ysHBT( ; , y, , ,m ,m ,A )p bs
(o
)
sNN (GeV)
(Beam)
x
y
z
s
? ?
STAR: this year
• transverse shape:• non-trivial excitation function• increased flow*time rounder
FO geometry @ RHIC• insufficient [flow]x[time] to
become in-plane
• Spatial orientation:• another handle on flow & time• HUGE tilts @ AGS!!• RHIC?• QGP-induced orientation?
AGS
v1 predictions (QGP invoked)
J. Brachmann et al., Phys. Rev. C. 61 024909 (2000)
L.P. Csernai, D. Rohrich: Phys. Lett. B 458 (1999) 454
x-p transverse-longitudinal coupling may be affected in early (v1) stage
1 2 sˆT b ysHBT( ; , y, , ,m ,m ,A )p bs
(o
)
sNN (GeV)
(Beam)
x
y
z
s
? ?
STAR: this year
• transverse shape:• non-trivial excitation function• increased flow*time rounder
FO geometry @ RHIC• insufficient [flow]x[time] to
become in-plane
• Spatial orientation:• another handle on flow & time• HUGE tilts @ AGS!!• RHIC?• QGP-induced orientation?• requires true 3D dynamical
model (explicitly non-B.I.)
AGS
ˆT 1 2 sysbHBT( ;p , y, b , ,m ,m ,A )s
• neglecting dynamics (flow), timescale, etc: is it trivial?• (though much of the interesting stuff is
dynamics and timescales…)
• gross geometrical features dictated by rule of critical mfp ~ 1 fm?
fm 1~
N
V fffMean free path
2sidelong
2/3)2( RRV f rough FO volume
i
NNii NNNN use measured:
Vf
N
CERES, PRL 90 (2003) 022301
Quark Matter 2004 Dan Magestro, Ohio State University
Same universal freeze-out in p+p, Same universal freeze-out in p+p, d+Au ?d+Au ?
Vf
N
CERES, PRL 90 (2003) 022301
10
20
30
40
50
60
70
80
90
10
20
30
40
50
60
70
80
90
Vf (
fm3 )
d+Au
p+p
√s=200 GeV
0
N
(fm
2 ) ff ~ 1 fm seems to hold for light systems as well (!) ~ 1 fm seems to hold for light systems as well (!)
• Why are p+p, d+Au and Au+Au so similar?Why are p+p, d+Au and Au+Au so similar?
• Check CERES’ ansatz using dN/dy’s and HBT radii for p+p and d+AuCheck CERES’ ansatz using dN/dy’s and HBT radii for p+p and d+Au
• dN/dy’s taken from power-law fits to STAR pdN/dy’s taken from power-law fits to STAR pTT spectra (nucl-ex/0309012) spectra (nucl-ex/0309012)
Magestro, QM04
• first order: “R=6 fm” (though this means 2x expansion)• Well… R=(1.2 fm)*A1/3
• Well… R ~ (Npart)1/3
• HBT radii are, indeed, connected with geometry…• but these are easy rules: dynamical models cannot follow them?
• pT, m1-m2 dep:
• strong global collective flow dominates
-dep: freezeout in out-of-plane configuration• non-trivial aspect of excitation function
• IMHO: Soft-sector dynamical observations (x- and p-space) demand faster timescales than present understanding allows.• e.g. maybe essentially no hadronic phase?
• personal most worrisome “puzzle”: pp = “small AA”??
ˆT 1 2 sysbp , y, b , ,m ,HBT( m; ,As )
broad strokes… (shorter than usual)