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The STAR Decadal Plan Tim Hallman RHIC Open Planning Meeting December 34, 2003

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Provides a vision of the compelling science STAR ... A Strategic Approach / Scientific Plan for STAR ... First look in STAR at the onium states (J/ , Upsilon, ... – PowerPoint PPT presentation

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Title: The STAR Decadal Plan Tim Hallman RHIC Open Planning Meeting December 34, 2003


1
The STAR Decadal PlanTim Hallman
RHIC Open Planning MeetingDecember 3-4, 2003
2
The STAR Decadal Plan
  • This talk
  • addresses the period now to 2010
  • Provides a vision of the compelling science
    STAR
  • proposes to accomplish (a picture being
    developed)
  • - high Q2 (triggered) probes ?
    high luminosity, good

  • tracking, and vertexing
  • - studies of bulk
    ? fast DAQ, FEE
  • phenomena
  • Identifies important RD and upgrade
    directions
  • that are beginning now to carry out the
    proposed
  • program

3
Three Must do STAR Physics Goals in the next
5 years that drive the planned use of
RHIC
  • Have we produced the quark-gluon plasma
  • pT dependence of suppression
  • Measurement of open charm and charmonium
  • Full flow systematics (mesons, baryons, multiply
    strange baryons, open charm)
  • Evolution versus energy/species
  • Gluon contribution to the nucleon spin
  • ALL for mid-rapidity jet production
  • ALL for direct photon jet
  • Gluon density saturation in cold nuclei at very
    low Bjorken x
  • Inclusive leading hadrons/jets in dAu collisions
  • Search for mono-jets in dAu collisions

With a 27 week standalone run each year
only one of these can be accomplished
With an additional 5 weeks per year, all 3 can be
achieved in the STAR plan
4
A Strategic Approach / Scientific Plan for STAR
Significant results from 1 shift at ?sNN
19.6 GeV ! Why does it work large acceptance
and very high tracking/detector efficiency
STAR Preliminary
The results from one shift of data taken at ?sNN
19.6 GeV !
NA49
STAR
5
A Strategic Approach/ Scientific Plan for STAR
First high pt suppression data at ?sNN 130 GeV
from a relatively short ( ?2 week) period of
actual data taking pointed out the need for more
data at 200 GeV, and finally the need for dAu
leading to
AuAu, ?sNN 130 GeV
? A diverse portfolio of soft physics
studies and measurements of rare probes is
possible within STAR
6
STAR Rare Probes
Di-Jet trigger in dAu collision in STAR EMC
7
Opening a Window in STAR on Onium
First look in STAR at the onium states (J/?,
Upsilon, and excited states) to measure the
thermodynamics of deconfinement through varying
dissociation temperatures
To deeply probe the plasma through studies of
(Debye) screening length l 1 /gT
  • Study vs. pT
  • Study vs. centrality
  • Study in lighter systems
  • Study vs a control (the ?)
  • Upsilon rate 10-3 J/Y
  • Yield in 10 weeks of AuAu
  • running at 32 µb-1 /week
  • will be a start
  • To fully utilize this probe requires
  • high luminosity RHIC running

8
STAR Scientific Approach
STAR has tremendous capability and flexibility
due to its large acceptance and efficient,
complimentary suite of detectors A robust
program of measuring rare probes, as well as soft
physics observables to study the bulk matter
properties is possible STAR believes the way to
achieve maximum scientific impact and full
utilization of the machine is to have a balanced
portfolio soft physics studies of the
properties of the bulk matter triggered
rare probes measurements change of energy
change of system size This will provide
the most leverage in understanding the new matter
produced at RHIC.
9
For the physics that drives the Run IV BUR, the
requirements are Goal
Hours/week ?sNN Dead Time
Weeks Min L0 30M (50M)
Central 45 200
50 6(10) 12 µb-1
/week 50M Min-Bias 45
200 50
6.8 2 µb-1 /week p? to
pT ? 15 GeV/c 45 200
50 6 (10) 33
(20) µb-1 /week 4s ? signal
45 200 50
10 32 µb-1 /week
h to pT ? 8 GeV/c 45 63
100 1
1.8 µb-1 /week
Even for rare probes ? relatively modest running
periods yield significant reach in pt ( 8 GeV/c
at ?sNN 63, which is the full reach of the
reference)
This is reflected in response to request for 5
year, 27 week projection Run/Weeks
Mode 1/Weeks Mode 2/Weeks Mode
3/weeks Mode 4/weeks Run IV, 27
AuAu _at_ 200, 514 pp _at_ 200, 5 Run V,
27 AuAu _at_ 20, 2 AuAu _at_ 40, 3
AuAu _at_ 63, 5 4 pp _at_ 200, 55 Run
VI, 27 dAu _at_ 200, 59 pp_at_200, 55
Run VII, 27 AuAu_at_200, 55
pp_at_200, 59 Run VIII, 27 AuAu_at_200,
510 pp_at_500, 55
But STARs conclusion is that scenario
is unworkable to achieve the goals of both the
heavy ion and spin physics programs
10

? ?
?u , ?d determination via ALPV in p p ? W
X _at_ ? s 500 GeV
To get into the game
  • ? s 200 GeV, P 4?L ? eff dt ? 100 pb 1
  • ? s 500 GeV, P 4?L ? eff dt ? 250 pb 1

11
The Nature of the Problem
Spin Physics Machine Development that has to
happen Test effectiveness of NEG
coated beam pipe Commissioning of
polarized gas jet target Commissioning
of warm-bore helical dipole Commissioning
of RHIC AC dipole Establish new RHIC
working point (WP) (2 IRs ?) Luminosity
in Roser model somewhat better than Run III ( 1
pb-1/week) at this point Testing of RHIC
working point First calibration of
gas-jet target Luminosity development
Commission cold bore helical dipole (P?
70) Complete calibration of gas-jet
target Luminosity in Roser model
something like ? 2 pb-1/week at this point
Annual access for key developments is
inconsistent with long runs to develop
luminosity and polarization required ( 10
pb-1/week, ? 60-70 ) A 27 week standalone
run will not work for both the heavy ion and spin
programs
5 0 weeks in Run IV?
Run V 55?
12
Some important strategic considerations for STAR
There is excellent, high impact science waiting
to be done, near and long term !
pp ? p x
Possible for Run IV
A number of Institutions have or will invest in
junior faculty appointments in the area of RHIC
Spin SUNY Stony Brook Indiana
University Massachusetts Institute of
Technology U.C. Riverside
University of Illinois The period 2005 -2006 is
a natural time frame to try to achieve several of
the main spin physics Goals Analysis of
the large data set from Run IV will take a
significant amount of time After this
period, new upgrades for the ion program will
start to come on the horizon and there
will be a strong interest in continued ion
measurements to utilize the new capability
The evolution in this area has consequences for
the future of both the heavy ion and spin programs
13
A Possible Path Forward
Within STAR, in the context of the planning group
discussions, alternative scenarios have been
discussed, including the constant effort scenario
(2) shown by Tom Ludlam. With 5 weeks of
additional running there is a qualitative change
in the robustness of the program. This allows
an energy scan a species change
high statistics AuAu running a
second dAu run robust, timely spin
physics (?G(x) and commissioning for Ws at ?s
500) In preliminary discussions STARs preferred
32 week scenario
Run/Weeks Mode 1/Weeks Mode
2/Weeks
Run IV, 32 AuAu _at_ 200, 514 pp _at_
200, 50
Run V, 32 AuAu _at_ 63, ?,68 pp _at_ 200,
510 Run
VI, 32 CuCu _at_ 200, 58 pp_at_200, 511
Run VII, 32
AuAu_at_200, 510 dAu_at_200, 59
Run VIII, 32
AuAu_at_200, 510 pp_at_500, 59
14
RHIC II Physics in STAR
  • QCD studies of unprecedented breadth
    and depth
  • Detailed studies of the fundamental properties of
    matter by heating the QCD vacuum
  • Studying the accompanying phase transitions, and
    the hot, superdense states preceding the
    formation of a plasma of quarks and gluons to
    understand e.g.
  • the nature of chiral symmetry breaking and
    how is it related to the masses of
  • the hadrons
  • the quark mass dependence of partonic
    energy loss
  • collective behavior in partonic systems
  • the nature of a possible saturated gluon
    state in cold nuclei at low Bjorken x
  • The helicity preference of gluons inside a
    proton the origin of the proton sea
  • the transversity distribution for quarks
    in a proton

15
RHIC II STAR Physics Probes
  • In the heavy ion program, to test and extend
    QCD theory and its predictions regarding the
    behavior of bulk color-deconfined matter, STAR
    will
  • use hard probes such as
  • Inclusive jets and direct photons
  • back to back jets (correlation of leading
    particles)
  • direct gamma leading hadron from jet
  • flavor tagged jets
  • measurement of spectra and yields for the
    Upsilon family of states
  • to measure the differential energy loss for
    gluon, light quark,
  • and heavy quark probes which couple
    differently to the medium
  • measure very large samples of soft physics
    events to unfold the bulk properties of the
    produced matter, studying e.g.
  • heavy quark thermalization
  • heavy baryon / meson (open charm) elliptic flow
  • spectrum of extended hadronic matter (resonances)

16
High pT hadrons in coincidence with g
High Luminosity STAR Physics
Quantitative measurements of partonic
energy loss
Measurement of the gluon density via direct ?
jet and flavor-tagged jets to study the quark
mass dependence of energy loss
AuAu (b 0), s1/2 200 GeV
  • Leading hadrons are very rare only
  • 0.1 of jets fragment hard enough
  • that hadrons are above incoherent
  • background
  • cross section for ? jet coincidences
  • (central AuAu)
  • Eg10 GeV 6 nb/GeV
  • Eg15 GeV 0.6 nb/GeV
  • 50 weeks of AuAu _at_ RHIC I design
  • 10 nb-1 !! ? luminosity upgrade
  • needed to access this physics!

dN/dyd2pT (y0) (GeV-2c-3)
PT (GeV/ c)
17
STAR Future Physics and Planned Upgrades
  • The next step? -- Trying to be quantitative and
    understand
  • quark mass dependence of partonic (?)
    energy loss.
  • A possible approach
  • differential energy loss of gluon, light
    quark, and heavy quark jets
  • Statistical, kinematic separation of gluon
    and light quark jets based
  • on underlying PDFs and reconstructed
    parton- parton cms
  • flavor tagging of heavy quark jets
  • D/ ?, B / ? ratio versus pT

Dokshitzer and Kharzeev (hep-ph/0106202)
0.8
1
dV
qsea
1.4
Q2 100 GeV2
uV
10
g(x)
Suppression of co-linear gluon radiation
Q2 10 GeV2
10-3
XBJ
10-3
10-1
10-1
Further theoretical and experimental development
needed !
18
Pressing the search with heavy flavor first
direct observation at RHIC of open charm in
dAu and min-bias AuAu collisions

Open charm a probe of initial conditions, and
possible equilibration at early times
For high statistics measurements
and event-by-event open charm, MRPC TOF
and silicon µvtx essential (This buys a factor
of 100 reduction in event sample required)
D ? K??, dAu
D0 ? K?, dAu
Star Preliminary
STAR Preliminary
y
y
Do c quarks thermalize? If yes, ratio of
charm hadrons yield changes from p-p to Au-Au
Ds most sensitive.
D ? K??, AuAu
A.Andronic, P.Braun-Munzinger,
K.Redlich, J.Stachel (nucl-th/0209035)
STAR Preliminary
19
With regard to flavor tagging, e.g.
STAR Future Physics and Planned Upgrades
Ramona Vogt, hep-ph/0111271
pp
  • pT 15 GeV/c s (pp)5x10-4 mb/Gev ? s
    (AuAu) 20mb/Gev
  • centrally produced
  • 5 years of AuAu 10 nb-1 ? 200K b-bar pairs

The yield is there! Can they be pulled out?
20
STAR Future Physics and Planned Upgrades
A First look - Using a proposed STAR ?VTX
Detector
B - Jet Tagging - Heavy Quark Energy Loss B ?
e/- hadron X
EMC triggers e/- from B, mVertex cleans the
sample
  • High pt e/- triggered by EMC
  • Enhance yield some h /- mis-idd as e/-
  • Remove hadronic background
  • Associate e/- with h /- at a displaced vtx
  • DCA sign positive if displaced vertex and Pe
    point in the same direction

- Pe 4 GeV/c, Ph 0.7 GeV/c - DCA between
e and h
misidentification
CDF Data
STAR ? vtx simulation
The first look is encouraging!
distance
21
Probing Rescattering Resonances
STAR Future Physics and Planned Upgrades
?, ?, ?(892), ?(1385), ?(1520) ?, D
pp
AuAu 40 to 80
STAR Preliminary
pp
STAR Preliminary
0.2 ? pT ? 0.8 GeV/c y ? 0.5
0.2 ? pT ? 0.9 GeV/c y ? 0.5
?0 f0 K0S ? K0
  • Short-lived resonances probe the medium and map
    the history wrt rescattering after chemical
    freezeout
  • Destruction of signal in hadronic channel
  • Regeneration in elastic scattering stage
  • Large data samples necessary
  • PID from TOF essential to extend pT reach

K/K
pp
Statistical error only
Au Au
22
To carry out its future program STAR needs
  • A Barrel MRPC TOF PID
    information for 95 of kaons

  • and protons in the STAR acceptance

  • extended scientific reach for

  • key observables
  • A micro-vertex detector precise (3
    ?m) hit position close to the

  • primary vtx ? Ds ,flavor- tagged jets
  • A DAQ/ TPC FEE Upgrade new architecture /
    FEE ? 1 khz of

  • events sampled at L3 effective

  • integration of 10 x more data
  • Development of GEM tech. Preparation for a
    compact, fast, next

  • generation TPC needed for 40 x L
  • Forward Tracking Upgrade W charge sign
    identification
  • High Luminosity 10 - 50 times the
    luminosity (10 nb-1)

23
STAR Future Physics and Planned Upgrades
  • The STAR MRPC TOF Barrel will
  • allow STAR to provide PID for an additional 60
    of the particle in the hadronic final state
  • Cut the time (events) needed to measure the open
    charm yield by a factor of 5 (12.6M ? 2.6M) (TPC
    SVT versus TPC SVT TOF)
  • Cut the time (events) needed for bulk measures
    (e.g. heavy baryon elliptic flow) which may
    distinguish between hadronic/ partonic degrees of
    freedom by a factor of 10 (200M ? 20M)
  • allow the detailed unfolding of large and small
    scale correlations fluctuations to map the
    dynamics/evolution of the produced matter
  • extend the pt reach to for measuring resonances
    to 1-2 GeV/c
  • affording a precision tool for model
    comparison and a definitive determination of the
    importance of re-scattering versus regeneration
  • (calibration of an important set of standard
    candles)

24
The STAR Barrel TOF MRPC Prototype
Prototype Tray Construction at Rice University
MRPC design developed at CERN, built in
China
28 MRPC Detectors 24 made at USTC
FEE
Neighbor CTB Tray
EMC Rails
? ? 70 ps, 2 meter path Strong team including
6 Chinese Institutions in place
Completed Prototype 28 module MRPC TOF Tray
installed in STAR Oct. 02 in place of existing
central trigger barrel tray
25
The STAR Barrel TOF MRPC Prototype
Prototype modules met all performance specs in
the STAR environment and produced important
physics on PIDd Cronin Effect
Proposal reviewed and approved by STAR
and submitted to BNL Management
26
Important new data from the MPRC TOF Prototype
Results will be key to help understand the
processes underlying particle
production in the intermediate pT region
Entirely new capability for measuring open
charm opened up as well !
27
Physics provided by the STAR mVertex detector
STAR Future Physics and Planned Upgrades
  • Open charm
  • Charm quark yield
  • Reconstructing D0
  • Charm hadron chemistry
  • Reconstructing D, Ds,
  • Charm hadron flow
  • Constructing D0 spectra
  • Open beauty
  • Identifying B mesons
  • Identifying heavy quark jets

Thin silicon ladders under tension
28
STAR Future Physics and Planned Upgrades
  • Key features of the proposed STAR ?vtx detector
  • ultra-thin 50 ?m silicon (APS) chips
  • excellent position resolution (5 ?m), 20 ?m x
    20 ?m pixels
  • minimal coulomb scattering, beam pipe wall 600 ?m
  • state of the art mechanical support allowing
    easy
  • insertion/removal and eventual replacement
    with
  • faster APS chips
  • 10-20 ms readout initially storage of all
    events in
  • 20 ms bucket per pixel probability of hit
    0.5 at 4 x L
  • per pixel probability of pile up in 20 ms,
    10-5
  • data matching offline

29
STAR Future Physics and Planned Upgrades
  • The DAQ and Front End Electronics
    Upgrades
  • The DAQ and FEE upgrades will allow STAR to
    acquire large data
  • samples, increasing the luminosity
    effectively integrated by STAR
  • by a factor of 10
  • This upgrade will increase the number of
    events sampled to 1000/sec
  • minimum bias, 200 Hz central. The baseline
    plan is to present
  • these to level III and write out 100/sec.
  • The upgrade will address the present
    bottlenecks throughout the
  • DAQ/FEE chain
  • DAQ FEE
  • DAQ CPU
    Chip Speed
  • VME Bandwidth
    Analog Processing
  • Event Builder
    Zero Suppression
  • LIII CPU
    Noise

30
STAR Future Physics and Planned Upgrades
The Scope Scientific Merit of Proposed RD /
Upgrade Plan System RD
Constr/Cost Benefit to STAR
  • Barrel MRPC 04 ? 05
    05 ? 06 PID information for 95
  • TOF 260k
    4.3M of kaons and
    protons in acc

  • 2.5M in- kind extended pT for
    resonances

  • ?
    v2 Ds ebe correlations


  • anti-nuclei inclusive


  • electrons
  • Inner ?vtx 04 ? 06
    06 ? 07 Ds , flavor- tagged jets
  • (Forward Tracker) 965K
    4M (TBD) (Charge sign for W )
  • DAQ Upgrade 04 ? 06
    06 ? 08 1 kz ? L3 Ds ? D,
  • 1.77M
    5M v2, cp, D
    thermalization

  • FEE Upgrade 04 ? 05
    05 ? 06 1 kz ? L3 Ds ?, D,
  • 250k
    2.5M v2, cp, D
    thermalization

  • GEM DeV 04 ? 06
    08 - 10 Compact, fast TPCrobust
  • 900k
    ? tracking
    for high Q2 physics

  • at
    40 x L

Serious RD on these projects has begun
31
STAR Future Physics and Planned Upgrades
This projection for the TPC assumes the following
RHIC Luminosity Upgrade Plan
  • Enhancements possible with existing machine
  • Double the number of bunches to 112
  • Decrease b from 2 m to 1m

4x increase in ave. L Still limited by I.B.S.
Electron beam cooling at full RHIC energy will
eliminate intra-beam scattering effects and
reduce beam emittance 10x increase in average
luminosity
Evolution of Au Au parameters Luminosity in
units of 1026 cm-2sec-1 Current in units of 1010
ions/beam
32
STAR Future Physics and Planned Upgrades
  • The GEM Development essential for STAR
    tracking
  • in the High Luminosity Era
    at RHIC
  • In 2010
  • the STAR TPC will be 15 years old
  • large space charge distortions and pile-up
    may be problematic
  • for the high luminosity, high pt program
    STAR intends to carry out
  • The proposed GEM development will
  • lay the foundation for a possible future high
    rate, compact TPC with
  • shorter drift and additional trigger
    capability
  • develop important technology which may also
    be needed elsewhere
  • in STAR (e.g. forward tracking)

33
STAR Future Physics and Planned Upgrades
What about the STAR Spin Program
?u , ?d determination via ALPV in p p ? W
X _at_ ? s 500 GeV
?G (x) from)
pp ??? X
  • The baseline physics
  • will take until 2010
  • A forward (GEM ?)
  • tracking detector
  • will be needed for
  • W/- sign

34
STAR Decadal Plan Conclusions
STAR proposes a future program of QCD
studies of unprecedented breadth and depth to
study the nature of chiral symmetry
breaking and how is it related to the masses of
the hadrons the quark mass dependence of
partonic energy loss collective behavior
in partonic systems the nature of a
possible saturated gluon state in cold nuclei at
low Bjorken x the helicity preference of
gluons inside a proton the origin of the proton
sea the transversity distribution for
quarks in a proton
This physics program requires a Barrel
MRPC TOF detector to extend STARs scientific
reach a micro vertex detector to enable
measurement of Ds and flavor-tagged jets
a DAQ / FEE upgrade to allow 1 khz to L3 to
integrate needed event samples a
tracking upgrade to afford good forward charge
sign determination Development of GEM
technology to insure the possibility of robust
tracking for the 40 x L era STAR has
embarked on this plan work is beginning
35
The Feasibility of the Future STAR program
21 scientific papers published (16 PRL, 4 PRC,
1 PLB), and 9 submitted (8 PRL, 1 PRC) 18
technical papers published 1060
Citations 28 Ph.Ds granted STAR is
a vibrant, strong collaboration which can
successfully carry out the proposed program
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