NEWAGE -- A direction-sensitive dark matter search

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K. Miuchi NEWAGE -- A direction-sensitive dark matter search Kentaro Miuchi Kyoto University) H. Nishimura T. Tanimori, H. Kubo, S. Kabuki, K. Tsuchiya, A. Takada, Y. Okada, K. Hattori, K. Ueno, S. Kurosawa A. Takeda (ICRR), H. Sekiya (ICRR) (New generation WIMP search with an advanced gaseous tracker experiment)

description

NEWAGE -- A direction-sensitive dark matter search. ( Ne w generation W IMP search with an a dvanced g aseous tracker e xperiment). Kentaro Miuchi ( Kyoto University) H. Nishimura T. Tanimori, H. Kubo, S. Kabuki, K. Tsuchiya, A. Takada, Y. Okada, K. Hattori, K. Ueno, S. Kurosawa - PowerPoint PPT Presentation

Transcript of NEWAGE -- A direction-sensitive dark matter search

Page 1: NEWAGE  -- A direction-sensitive dark matter search

K. Miuchi

NEWAGE -- A direction-sensitive dark matter search

Kentaro Miuchi

( Kyoto University)H. Nishimura

T. Tanimori, H. Kubo,

S. Kabuki, K. Tsuchiya,

A. Takada, Y. Okada,

K. Hattori, K. Ueno, S. Kurosawa

A. Takeda (ICRR), H. Sekiya (ICRR)

(New generation WIMP search with an advanced gaseous tracker   experiment)

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OUTLINE

Introduction

Detector

NEWAGE surface run

FUTURE PLANS & SUMMARY

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Introduction: Direct DM search in 2010’s

What happened in 2000’s…

<1> DAMA (~100kg) : 7 years’ result <3> LIBRA (post DAMA):

<2> “challenge DAMA” (~10kg):CDMS, EDELWEISS, XENON10

YESsearch **GeV ! atLCH, GLAST

NONO NO

Please for SUSY

What will happen in 2010’s

YES

NO

<4> “challenge SUSY” (~100kg): SUPER**, **0

BACK to <1>

YES, but not conclusive…

<5> use various nuclei, and

or, MAYBE

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1 .   Direction sensitive DM search    “ WIMP-wind” detection

The WIMP-wind

WIMPV0 =230 km/s

SOLAR SYSTEM220 km/s

PLB 578 (2004) 241

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WHY “Direction-sensitive” ?Large mass for exclusion ( and indication )

BUT Annual modulation is not enough…

Direction-sensitive for detection

WIMPWIMP WIND WIND γ γ

FF

Annualmodulation

direction

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Sensitivities Goal: Detect the WIMP-wind  ( 2010~ )

• underground ・ low pressure ( CF4 0.05 bar ) ・large volume ( 1m3 × N )

CURRENT: • surface ・ CF4 0.2 atm ・ 30cm cube

sensitivity

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2. DETECTOR

June 22, 2007   SUSY in 2010’s

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2 micro-TPC (3D tracking device)

Feb. 20, 2007   APPEAL07

Position Encoder

PIC (×5000)

GEM(×10)

TPC

Particle tracks

e

Preprints: physics/0701085 K.Miuchi et.al

40cm

TPC

X readout ( 768ch ) Y

readout ( 768ch )

FAGA position encoder( 1536ch )

23×28×31cm3

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Readout electronics• 768 anode + 768 cathode• Digital (LVDS) signals at ASD• (X,Y,T) at the position encoder

31cm

gas volume

TPC system

Gas volume• DRIFT length 31cm• CF4 0.2bar gas

100MHz, pipeline

2D imaging device: -PIC (gas gain 5000)

• 400mm pitch• 589824 pixels• 768+768 readout

30cm μPIC(Toshiba)

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CF4+C4H10 (9:1) 0.2 atm

n -> p forward scattering (emulation of WIMP -> F scatterings)

Jan 27, 2007   3rd MPGD workshopRecoil direction  image

252Cf( NE45°  zenith35° )

10

Cos

n

p

CF4+C4H10

252Cf run

Proton tracks

n252Cf

YX-15cm

15cm

15cm

-15cm

30cm

Z(drift)

0cm

TPC performance 1:           nuclear tracks, imagingPreprints: physics/0701118 K.Miuchi et.al

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TPC performance 2:   gamma-ray rejection

energy   length   correlation

gamma-rays from 137Cs

neutron ( BG )

neutron ( BG )

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  gamma-ray rejection ( continued )spectrum, BG subtrucction

• gamma rejection <  2e-4  ( statistics limited )

neutron ( BG )

Subtracted energy spectrumEnergy spectrum

thick: 137Cs run

hatched: no source

consistent with 0 ( >100keV )

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3. SURFACE RUN

June 22, 2007   SUSY in 2010’s

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Surface run①2006 Nov.1st ~ Nov.27th

exposure 0.15 kg days (=0.0089kg ×16.7days)

@Kyoto university (N35.03   E135.783 ) Energy spectrum ( conventional method )

Energy spectrum

3 Surface run

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Surface run ②The sky map (by nuclear recoil tracks)

flat neutron background is seen

North sky view seen by C and F nuclei(100-400keV)

DM direction

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Jan 27, 2007   3rd MPGD workshop

Surface run ③Cosθ distribution

consistent with a flat distribution

Cosθ 分布

(100-400keV)

DM limit

First step to theNEWAGE

WE ARE   HERE

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KAMIOKA LAB-B

Underground run @ KAMIOKAData taking since January 2007.

low background material selection

background neutron measurement

4 Next step…

TPC improvements @ KYOTOlarger TPC (30cm cube -> 60cm cube)

lower threshold (100keV -> 30keV)

readout ASIC (with KEK)

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SUMMARYμTPC : 30cm cube in operation

direction-sensitive method works!

NEWAGE : underground run just started

AcknowledgementThis work was partially supported by Grand-in-Aid for Scientific Research on Priority Areas: "Discoveries of Higgs Particles and Supersymmetry to Pioneer the Particle Physics in the 21st Century"

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20062006 年年 1111 月月 1717 日日

TPC performance ②  stability

Drift velocity: fast drop

⇒ slow decrease after 1 day

gain, energy resolution :  stable within   the systematic error

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TPC performance: nuclear track efficiencyneutrons from 252Cf

• 0.4 @ 100keV

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エネルギー校正• ガラスに蒸着した 10B   ( 厚さ 0.6μm )• ドリフトケージ内部にセット、外から 252Cf の中性子を減速して照射• 10B(n,a)7Li 反応  (Q=2.70MeV 1.8MeV for )• 原子核による校正、低エネルギーへの線形性は別途確認示す必要あり• 現状では、校正には 6 時間程度、見せれる絵には 12 時間程度かかって

いる

XY イメージ

keV

スペクトル

エネルギー vs 飛跡長

keV

Li

2000

スペクトル(GEANT4 )

検出器応答

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位置分解能から角度分解能• アルファ線の飛跡を直線フィット、残差を求める: 0.8mm• BG run の C,F recoil での 飛跡長 / (nhit-1) = 1mm   ( サンプリング密

度 )

• 上記二つのパラメータをもちいてsimulation 振る。

• NHIT=3  で直線 FIT すると左の様になる。

• ローレンツィアンで FIT して、 γ=25°(=HWHM)

検出器応答

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エネルギー分解能• 高エネルギー( 5-8MeV )ではラドンのピークを使ってモニタ• 40 % FWHM• これは検出器固有の数字(ゲインのばらつきが効いている)

• 低エネルギーでは、以前の Ar での実測 60 % FWHM@60keV• これが電子数統計とすると、

W 値、エネルギーで外挿すると、 60×sqrt((54/26)×(60/100))   =   70 % FWHM   @100keV

60%@59.5keV

検出器応答

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Gas gains • operation gain for MIPs ~50,000

Gain curves

Gain map

Gain uniformity • Maximum / minimum = 2.2

TPC   performance (with Ar+C2H6 gas)

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TPC performance①   tracking400m digital “HIT” ( for tracking) + summed analog ( for energy)

F 500keV 5~6mm    in 0.2atm CF4

F,C tracks

n

252Cf

YX-15cm15cm

15cm

-15cm

30cm

Z(drift)

0cm

X,Y image Z projection

Fidutial   24×21.5×31cm3

(CF4 8.9g)FLAT response

trigger

Trigger :z=0

cm 30

Preprints: physics/070118 K.Miuchi et.al

• gamma rejection <  2e-4  ( statistics limited )

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データ シミュレーション

クロスセクション

検出器の方向依存感度マップ

測定値

「 DM の風」

測定値

×

sim

=

sim

Expected 「 DM の風」

sim

Expected cosθ 分布( DM )

Input: エネルギー分解能、角度分解能、

WIMP 質量、エネルギー BIN

Input: エネルギー BIN 、絶対検出効率

For given   WIMP 質量、

反跳エネルギー

WIMP 質量、エネルギーBIN

ごとに用意

比較

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Jan 27, 2007   3rd MPGD workshop

SpectraSpectra• Energy spectra from the whole volume

   (with energy corrections)

109Cd

linearity

Energy resolution

133Ba

241Am

Ag-KCu-K

Cs-KCu-K

Cu-K

59.5keV

60%@59.5keV

22.2+24.9keV

31keV

8keV

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Jan 27, 2007   3rd MPGD workshop

Particle TrackingParticle Tracking muons

Electrons (~100keV)

Protons (~2MeV)

30cm

Neutrons( 252Cf )

511keV   ‘ s( 22Na )

Cosmic ray muons

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Jan 27, 2007   3rd MPGD workshop

3D Spatial resolution3D Spatial resolution• Fit muon tracks with straight lines• plot the residuals

Residual muon tracks

dataFitted line

data

residual

Residual (short drift)

Residual (long drift)

)2

exp(2

222 rr

22222 )( lDdetectordiffusiondetector

Drif

t le

ngth

-PIC

mm1

mm2

mm51.0detector

cmmm/37.0D

)2

exp(2

222 rr

dependence on drift length

r [cm] 

r [cm] 

l [cm]