jet quenching and direct photon production
DESCRIPTION
Jet quenching and direct photon production. F.M. Liu 刘复明 Central China Normal University, China T. Hirano University of Tokyo, Japan K.Werner University of Nantes, France Y. Zhu 朱燕 Central China Normal University, China arXiv: hep-ph/0807.4771v2. - PowerPoint PPT PresentationTRANSCRIPT
Jet quenching and direct photon production
F.M. Liu 刘复明 Central China Normal University, China
T. Hirano University of Tokyo, Japan
K.Werner University of Nantes, France
Y. Zhu 朱燕 Central China Normal University, China
arXiv: hep-ph/0807.4771v2
SQM2008 Beijing Oct 6-10
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Outline
• Motivations• Calculation approach• Results• Conclusion
3
Motivations• Heavy ion collisions at various centralities offer us various bulks of
hot dense matter.
• The interaction between jets ( hard partons) and the bulk has receiv
ed notable interest, i.e. jet quenching is one of the most exciting obs
ervables at RHIC.
• The interaction of partons inside the bulk and the properties of the b
ulk are of great interest, which may offer us some insight to quark c
onfinement.
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direct photons, jets and plasmaPRL94,232301(2005), PRL96,202301(2006)
1. Jet queching gives different effects to direct photons?
2. Direct photons (thermal, jet-photon conversion) are penetrating probes
for the interaction of partons inside the bulk and the interaction betwee
n jet and bulk. We can make cross check of the properties of the medi
um.
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Calculation approachA precise calculation requires careful treatments on
• The space-time evolution of the created hot dense matter
• The propagation of jets in plasma
( interaction between jet + plasma)
• All sources of direct photons
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Space-time evolution of Plasma
),,,,...(,,, zyxBsu
%) ,(d
dn
Described with ideal hydrodynamics in full 3D spaceConstrained with PHOBOS data
Tested with hadrons’ yields, spectra, v2 and particles correlation
For more details, read T. Hirano
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Jets (hard partons)
)ˆˆˆ()(ˆ
ˆ),(),( 2
/2
/AB2
jet
utscdabtd
dsMxGMxGdxdxTK
pdyd
dNbBb
abcdaAaba
t
AB
),()()()( /// AxRxGA
ZxG
A
NxG EKS
apaNaAa
MRST 2001 LO pDIS and EKS98 nuclear modification are employed
)(),2
(),2
(),(30 zy
bxTy
bxT
pd
dNrpf BA
Jet phase space distribution at τ=0:
)(),(),,(),( 00003 Evpptvrpfpdrpfxpf
at τ>0:
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Parton Energy Loss in a Plasma
• Energy loss of parton i=q, g, D: free parameter
• Energy loss per unit distance, by BDMPS
• Every factor depends on the location of jet in plasma , i.e.,
0
))(,())(,,( ),,( 00 rfridrpiE QGP
is EDri / ))(,,( *2
)/8ln()233(
6)(
cfs TTN
T
upE *
)(r
fQGP: fraction of QGP at a given point
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Fix D with pi0 suppression • From pp collisions:
• From AA collisions, parton energy loss is considered
via modified fragmentation function
),(1 20
/2t
2,t
2
0
QzDzpdyd
dNdz
pdyd
dNcc
c
cpp
gqcc
pp
Factorization scale and renormalization scale to be tpQM
functionion fragmentat KKP :),( 20/ QzD cc
),,( 2/ ccc EQzD X.N.Wang’s formula
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Raa(pi0, %) at high pt gives D=1.5
A common Dfor various Centralities!
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Sources of direct photons• Leading Order contr. from primordial NN scatterings
• Thermal contribution
upETExdpdyd
dN
t
**thermal
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thermal
),,(
qqg
gqq
)ˆˆˆ()(ˆ
ˆ),(),( 2
/2
/AB2
)LO(
utscdabtd
dsMxGMxGdxdxT
pdyd
dNbBb
abaAaba
t
AB
2004 al,et Rapp R.
1991 al,et Kapusta:),( *HG TE
AMY/
22
*QGP
1
1
2
)(
9
6),( * C
eT
TTE
TEs
Interactions of thermal partonsare inside the rate!
...effect LPM
qqg
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Sources of direct photons• Jet photon conversion
• Fragmentation contribution: similar to pi0 production
Ignored contributions: Medium induced radiation (mainly at low pt )
radiation from pre-equilibrium phase (short time)
qqg
gqq
C
Tg
TETxpfeTE q
S22
*22
2*
JPC
24ln),(
4),(
),( *JPC
42
TExdpdyd
dN
t
JPC
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Results
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Centrality dependent pt-spectra(1)PHENIX data: PRL 98, 012002 (2007) & arXiv:0801.4020
Our predictions coincide with the precise measurement!
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Centrality dependent pt-spectra(2)PRL94,232302(2005)
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Pt spectrum from pp collisions
The PHENIX fit of pp spectrum is used for Raa of thermal photons.
PRL 98, 012002 (2007)
A good test for contributions from leading order +fragmentation without Elossin AA collisions.
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Raa: energy loss
• Data is reproduced within theory uncertainty.
• E loss makes about 40% decrease of total photon production
• Centrality independent ? central and peripheral results differ
by less than 5% with Eloss
by about 20% at intermediate pt w/o Eloss
PRL94,232302(2005);J.Phys.G34, S1015-1018,2007
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Jet quenching & bulk volume
• E loss does play a important role in fragmentation contribution and
jet photon-conversion contribution.
• This is centrality-dependent, similar to the suppression to pi0 production.
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Competition btw different sources
Thermal and LO dominate low and high pt region respectively.Raa is not sensitive to E loss, because of the centrality dependence of them.
When collisions move to perpherial, JPC becomes less importantwhile fragmentation becomes more important .
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Information from Thermal photonsEnergy density at plasma center
• High Temp. from fitting a pt spectrum A higher Temp. plasma
• More yields (shines) of thermal photons A bigger-size (longer-life) plasma.
Raa due to thermal source
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V2 of thermal photons
Contrary to hadronic v2 (ideal hydro predicted increase monotonically), the elliptic flow of thermal photons decrease at high pt!
( Information for the earlier evolution of the plasma?)
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Time evolution
• At initial time there is no transverse flow, so v2 vanishes.
• A big fraction of energetic thermal photons are emitted at early time: More than 50\% at pt=3GeV/c and more than 70\% at pt=4GeV/c within the first 0.3fm/c, though the whole evolution time is about 20fm/c.
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Discussion and Conclusion• Parton energy loss does make 40% decrease of Raa(γ)
• Raa(γ) is independent of centrality (within 5% accuracy) because of
1) the dominance of leading order contribution
2) strong suppression to JPC and frag. contributions due to E-loss
• Thermal photons can provide information of the temperature and size of
the plasma via the slope of pt spectrum and the yields.
• The elliptic flow of thermal photons is predicted to first increase and then
decrease with pt, contrary to hadronic v2, which does not carry the early i
nformation of the QGP.
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Thank you!
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purely leading order calculation:
Isosping mixture and nuclear shadowing make an evident decrease.
Why RAA decreases at high pt?
),()]()(
)([)( /// AxRxfA
zAxf
A
zxf EKS
aNapaAa
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Thermal fraction