R. BernabeiUniv. Roma - Tor Vergataand INFN-Roma2

LNGS21th July 2003

Further results onthe WIMP annual modulation

signature by DAMA/NaI

Roma2, Roma, LNGS, IHEP/BeijingDAMA site @ www.lngs.infn.it

R&

DL

Xe

low

bck

g G

e fo

r sa

mpl

ing

mea

s.

NaI

(Tl)

LIB

RA

üPr

opos

alby

R. Be

rnab

ei, P.

Belli,

C. B

acci,

A.

Incicc

hitt

i, R

. M

arco

vald

ian

d D. Pr

ospe

rion

larg

e mas

s NaI

(Tl)

and

liquid

Xen

on e

xper

imen

ts f

or D

ark

Mat

ter

sear

chan

d firs

t fu

nding

on 1

990.

üThe

chine

seco

lleag

ues

joined

the

pro

ject

in

1992

üSev

eral r

esults

since

the

beg

inning

and

var

ious

tes

t/pr

elim

inar

yse

t-up

s

üth

e ~

100

kg N

aI(T

l) se

t-up

:

-First

exp

erim

enta

l re

sult p

ublis

hed

on 1

996

(DAM

A c

oll.,

PLB3

89(1

996)

757)

. -Fi

rst

resu

lt o

n W

IMP

annu

al m

odulat

ion

sign

atur

e pr

esen

ted

at T

AUP9

7-Dat

a fr

om 4

ann

ual cy

cles

relea

sed

and

publ

ishe

d-Sev

eral o

ther

rar

e pr

oces

ses

inve

stigat

ed.

-New

elect

ronics

and

DAQ

in

summer

200

0.

-Out

of

oper

ation

in J

uly

2002

.-to

day:

relea

se o

f th

e cu

mulat

ive

7 an

nual c

ycles

expo

sure

P. B

elli,

R.B

erna

bei, A

. Bu

ssolot

ti*,

F.

Capp

ella,

R. C

erulli+

, P.

Delfini*,

F.

Mon

tecc

hia%

,F.

Noz

zoli

Dip.

diFi

sica

, Unive

rsita'

diRo

ma

''Tor

Verg

ata”

and

INFN

, se

z. R

oma2

, I-

0013

3 Ro

me,

Ita

ly

A.

Incicc

hitt

i, A

. M

atte

i*,

D.

Pros

peri

Dip.

diFi

sica

, Unive

rsita'

diRo

ma

''La

Sap

ienz

a” a

nd I

NFN

, se

z. R

oma,

I-0

0185

Rom

e, I

taly

C.J.

Dai,

H.H

. Ku

ang,

J.M

. M

a, Z

.P.

Ye$

IHEP

, Ch

ines

e Aca

demy,

P.O

. Bo

x 91

8/3,

Beijing

100

039,

Chi

na

Past

mem

bers

wh

o ga

ve ve

ry va

luab

le co

ntribu

tion

s: M

. Amat

o, C.

Ba

cci, V.

Bi

doli*

, F.

Br

onzini*,

D.B

. Ch

en,

L.K.

Ding,

W.

Di

Nicolan

tonio,

H.L

. He,

G.

Ign

esti,

V. L

ando

ni,

G.

Rane

lli*,

X.D

. She

ng,

G.X.

Sun

and

Z.G

. Ya

o

+ in

the

neut

ron

mea

sure

men

ts a

t EN

EA-F

rasc

ati:

M.

Ang

elon

e, P

. Ba

tist

onian

d M

. Pillo

n

unde

rlined

the

coll. lea

der

* te

chnica

l st

aff

+ no

w: I

NFN

-LNGS

, Ass

ergi

(Aq),

Italy

%

also

: U

nive

rsita'

"Ca

mpu

s Bi

omed

ico"

diRo

ma,

001

55,

Rome,

Ita

ly$

also

: Unive

rsity

of Z

hao

Qing,

Gua

ngDon

g, C

hina

Ack

nowl

edge

men

ts t

o th

e:ü

INFN

Scien

tific

Committe

e II

for

eff

ective

sup

port

and

con

trol

üRe

fere

es o

f th

e ex

perimen

t in t

hat

Committe

e, w

ho a

llowe

d se

vera

l tim

es t

o im

prov

e th

e qu

ality

of t

he

effo

rts

üDirec

tors

and

coo

rdinat

ors

of t

he I

NFN

invo

lved

units

-du

ring

mor

e th

an o

ne d

ecad

e -

for

supp

ort

üIN

FN-R

oma2

, IN

FN-R

oma,

INFN

-LNGS

and

IHEP

/Beijin

g fo

r co

ntinuo

us a

ssista

nce

üDr.

C. Arp

esella, In

g.M

. Ba

lata

, Dr.

M. La

uben

stein,

Mr.

M. De

Deo

, Pr

of. A. Sc

acco

and

Prof

. L.

Tr

inch

erini, f

or c

ontr

ibut

ions

to

sample

mea

sure

men

ts a

nd r

elat

ed d

iscu

ssions

ü

Prof

. I.

R. Ba

raba

novan

d Pr

of. G.

Heu

sser

for

man

y us

eful s

ugge

stions

on

the

feat

ures

of

low

radioa

ctive

dete

ctor

s ü

Dr.

R. M

cAlpine

and

Dr.

T. W

righ

t, f

rom E

MI-

THORN

/Elect

ron-

Tu-b

es, fo

r co

mpe

tent

ass

ista

nce

üCr

ismat

ecco

. fo

r de

vote

d ef

fort

s in r

ealiz

ing

of t

he lo

w ba

ckgr

ound

NaI

(TI)

ü

LNGS

, IN

FN-R

oma

and

INFN

-Rom

a2 m

echa

nica

l and

elect

ronica

lsta

ffs

for

supp

ort

üACF

, GT

S, S

EGEA

sta

ffs

for

effe

ctive

supp

ort

in h

ardw

are

work

s an

d as

sist

ance

. ü

Prof

. A. Bo

ttino,

Dr.

F. Don

ato,

Dr.

N. Fo

rnen

goan

d Dr.

S. Sco

pelf

or u

sefu

l discu

ssions

on

theo

retica

l as

pect

s

R.B.

wishe

s to

ded

icat

e th

is t

alk

to t

he m

emor

y of

Pro

f. L

. Pa

oluz

i, w

ho w

as a

ble

as D

irec

tor

of I

NFN

Ro

ma2

to

unde

rsta

nd t

he p

ossibilit

y of

this

field

when

mos

t of

the

peo

ple

igno

red

it a

nd t

o of

fer

the

need

ed

supp

ort

The

Milk

y W

ay

The

dyna

mic

al e

volu

tion

of t

he U

nive

rse

depe

nds

on t

he

quan

tity

and

kind

of

mas

s an

d en

ergy

den

sitie

s pr

esen

t. Th

e cu

rvat

ure

radi

us o

f the

Uni

vers

e is

rela

ted

to th

e de

nsity

para

met

er Ω

= ρ/

ρ c(ρ

= pr

esen

t den

sity

of m

ass

and

ener

gy

in t

he U

nive

rse

and

ρ c=

3H02 /8

πG).

Ωis

a k

ey p

aram

eter

.

~ 70

yea

rs lat

er t

han

the

firs

t ev

iden

ce f

or D

ark

Mat

ter

by Z

wick

y

•In

ther

mal

equ

ilibr

ium

inth

eea

rly

stag

eof

Uni

vers

e•

Non

rel

ativ

istic

atde

coup

ling

time

•<σ

ann. v

>~

10-2

6 /ΩW

IMPh2

cm3 s

-1→

σor

dina

ry m

atte

r~

σw

eak

•E

xpec

ted

flux:

Φ~

107

.(G

eV/M

W) c

m-2

s-1(0

.2<ρ

halo<0

.7 G

eV c

m-3

)•

For

ma

diss

ipat

ionl

essg

as tr

appe

din

the

grav

itatio

nal f

ield

of th

eG

alax

y(v

~10

-3c)

•ne

utra

l •

stab

le(o

rwith

τ~

age

ofU

nive

rse)

•

mas

sive

•R

-par

ity c

onse

rved

→LS

P is

sta

ble

•LS

P (n

eutra

lino,

sne

utrin

o, g

ravi

tino,

axi

no)

The

WIM

PsTh

e W

IMPs

relic

CDM

part

icles

from

primor

dial

Unive

rse

Sear

ching

for

Sear

ching

for

a ca

ndidat

ea

cand

idat

e

SUSY

•an

hea

vy ν

of th

e 4-

th fa

mily

•th

e sn

eutri

no in

the

Sm

ith a

nd W

eine

r sc

enar

io

•ev

en a

par

ticle

not

yet

fore

seen

by

theo

ries

Ann

ual m

odul

atio

n of

the

rate

•v s

un=

232

km/s

(Sun

vel

ocit

y in

the

halo

)•

v orb

= 30

km

/s (E

arth

vel

ocit

y ar

ound

the

Sun)

•γ

= π

/3•

ω=

2π/T

T =

1 y

ear

•t 0

= 2nd

Jun

e (w

hen

v ⊕is

max

imum

)

Exp

ecte

d ra

te in

giv

en e

nerg

y bi

n ch

ange

s be

caus

e th

e an

nual

m

otio

n of

the

Ear

th a

roun

d th

e S

un m

ovin

g in

the

Gal

axy

Sun

Ear

th

30 k

m/s

232

km/s60

°

4)W

ith

pro

per

ph

ase

(ab

ou

t 2

Jun

e)

5)F

or

sin

gle

hit

in a

mu

lti-d

etec

tor

set-

up

6)W

ith

mo

du

late

d a

mp

litu

de

in t

he

reg

ion

of

max

imal

sen

siti

vity

< 7

%

Req

uire

men

ts o

f the

ann

ual m

odul

atio

n1)

Mo

du

late

d r

ate

acco

rdin

g c

osi

ne

2)In

a d

efin

ite

low

en

erg

y ra

ng

e

3)W

ith

a p

rop

er p

erio

d (

1 ye

ar)

To

mim

ic th

is s

igna

ture

, the

spu

riou

s ef

fect

s an

d si

de r

eact

ions

To

mim

ic th

is s

igna

ture

, the

spu

riou

s ef

fect

s an

d si

de r

eact

ions

mus

t sa

tisfy

con

tem

pora

neou

sly

all t

hese

6 r

equi

rem

ents

mus

t sa

tisfy

con

tem

pora

neou

sly

all t

hese

6 r

equi

rem

ents

Dru

kier

,Fre

ese,

Sper

gelP

RD

86Fr

eese

et a

l. PR

D88

Iden

tify

ing

sign

al f

rom

Iden

tify

ing

sign

al f

rom t

he W

IMP

the

WIM

P wi

ndwi

nd

v ⊕(t

) = v

sun

+ v or

bco

sγco

s[ω

(t-t

0)]

S k[η(

t)]=

dR dER

dER

≅S 0

,k+

∆E k∫

S m,k

cos[

ω(t

−t 0

)]

NaI(Tl) well suitable to NaI(Tl) well suitable to investigate the WIMP annual investigate the WIMP annual

modulation signaturemodulation signature

• Well known technology

• Large mass possible

• Technology for radiopurification feasible

• Full control of running conditions feasible

• High duty cycle

• Cost/Mass relatively low

• Sensitive to purely SI, purely SD and mixed SI&SD coupled WIMP + preferred sensitivity in several scenarios

(+ Statistical discrimination of recoil nuclei feasible in suitable conditions at reasonable level )

Resu

lts

on W

I M

PS:

•P

SD

: P

LB

389(

1996

)757

•In

vest

igat

ion

on d

iurn

al e

ffect

:N

.Cim

.A11

2(19

99)1

541

•A

nnua

l Mod

ulat

ion

Sig

natu

re:

PL

B42

4(19

98)1

95, P

LB

450(

1999

)448

, PR

D61

(199

9)02

3512

, P

LB

480(

2000

)23,

PL

B50

9(20

01)1

97, E

PJ

C18

(200

0)28

3,

EP

J C

23 (2

002)

61, P

RD

66(2

002)

0435

03

~100

kg

~100

kg

NaI

NaI

(( Tl

Tl) DAM

A s

et) DAM

A s

et-- u

p:

up:

data

da

ta t

aking

complet

ed

taking

com

plet

ed o

n on J

uly

July 2

002

2002

NaI(Tl) detectors

Perf

orm

ance

s:

N

.Cim

.A11

2(19

99)5

45Re

sult

s on

rar

e pr

oces

ses:

Riv

. N. C

im. 2

6 n

. 1 (

2003

) 1-

73

•Po

ssib

le P

auli

excl

usio

n pr

inci

ple

viol

atio

n PL

B40

8(19

97)4

39•

Nuc

lear

leve

l exc

itatio

n of

127 I

and

23N

a du

ring

CN

C p

roce

sses

PRC

60(1

999)

0655

01•

Elec

tron

stab

ility

and

non

-pau

lian

trans

ition

s in

Iodi

ne a

tom

s (b

y L-

shel

l)

PLB

460(

1999

)235

•Ex

otic

Dar

k M

atte

r sea

rch

PRL8

3(19

99)4

918

•Se

arch

for s

olar

axi

ons

by P

rimak

off e

ffec

t in

NaI

(Tl)

crys

tals

PL

B51

5(20

01)6

•Ex

otic

Mat

ter s

earc

h EP

Jdire

ct C

14(2

002)

1

tod

ay:

incl

ud

ing

oth

er 4

9745

kg

⋅d (

3 cy

cles

) f

or

a to

tal e

xpo

sure

of:

1077

31 k

g⋅d

(up

to 5

7986

kg

⋅d -

4 cy

cles

)

The

inst

alla

tion

The

det

ecto

rs

Glo

ve b

ox fo

rca

libra

tion

N. C

im.A

112(

1999

)545

The

˜10

0kg

NaI

(Tl)

set-u

p

Full

subs

titut

ion

of e

lect

roni

cs a

nd D

AQ

in 2

000

End

of d

ata

taki

ng 2

002

•Reduced standard contaminants (e.g. U/Th of order of ppt) by material selection and growth/handling protocols.

•Each detector coupled - through 10cm long tetrasil-B light guides acting as optical windows - to 2 low background EMI9265B53/FL (special development) 3” diameter PMTs working in coincidence.

•Detectors inside a sealed Cu box maintained in HP Nitrogen atmosphere in slight overpressure

•Very low radioactive shields: 10 cm of copper, 15 cm of lead, 1.5 mm Cd foil+ polyethylene/paraffin for neutron shield + around about the whole shield ~ 1 m concrete outside the barrack

•A plexiglass box encloses the whole shield and is also maintained in HP Nitrogen atmosphere in slight overpressure

• Installation in air conditioning + huge heat capacity of shield

•Walls, floor etc. of inner installation sealed by Supronyl (2×10-11

cm2/s permeability).•Calibration using the upper glove-box (equipped with compensation chamber) in HP Nitrogen atmosphere in slight overpressure calibration → in the same running conditions as the production runs.

•Each PMT works at single photoelectron level. Considered software energy threshold: 2 keV.

•Pulse shape recorded over 3250 ns by Transient Digitizers.•Monitoring and alarm system continuously operating by self-controlled computer processes.

•Data collected from low energy up to MeV region, despite the hardware optimization was done for the low energy.

+ electronics and DAQ fully renewed in summer 2000

Main Features of DAMA/Main Features of DAMA/NaINaI(Il Nuovo Cim. A112 (1999) 545)

New DAQ and electronic chain New DAQ and electronic chain after August 2000after August 2000

DAQ:

- Computer: Workstation Digital Alpha

- Bus: GPIB

- Mainframe: VXI e CAMAC

VXI

CAMAC

Workstation alpha

PCI-GPIB

I-FGPIB-VXI

I-FGPIB-CAMAC

Electronic Chain:

- Installation of Waveform Analyzer Tektronix TVS641A for bus VXI, 4 channels, Sample rate = 1 Gsample/s, 8 bit, band width 250MHz, 1channel for each crystal

Crystal1

PMT2

PMT1

ADC 1CAMAC

WA 1 VXIIn 1

TFA 2

TFA 1

AND1

Gate 1500us

OR enable 1Line CAMAC

Scaler 1CAMAC

Single Triggercrystal 1

Single Trigger crystal 1

ADC 2CAMAC

Discrim 1

Discrim 2

ADC 3CAMAC

R 1KΩ

Cable lineDelay line

200ns

Delay line

200ns

Delay line

200ns

Cable line

Cable line

PreampGain 10

PreampGain 10

F 1

F 3

F2

Gate

Gate

Gate

Main Triggergate 1

Main Triggergate 2

Main Trigger gate 3

Analog signal

from crystal 1

Light guide

A 1

A 2

In 1IR pattern

recognition

L1

L2

L4

L3

L2

L5

L6

L8

L9

L10

L11

L12

L13

L14

L15

L16

L17

L18

L19

L20

L21

L22

L23

L24

L25

L27

L28

L7

L26

AND14

AND 15

Gate500us

Gateopen

T sing cryst 1T sing cryst 2T sing cryst 3T sing cryst 4T sing cryst 5T sing cryst 6T sing cryst 7T sing cryst 8T sing cryst 9

Gate600ns

Gate50nsD 1us

Scaler

R

Main Trig gate1Main Trig gate2Main Trig gate3

Reset ACQLine CAMAC

OR1

STROBE IRT sing cryst 10T sing cryst 11T sing cryst 12T sing cryst 13

AND 17

AND 18

AND 19

Gate3us

Gate3us

Gate3us

AND 16

1 < E < 90 keVSA

SA

SA

AnalogSUM

from AND15

trigger TD1

trigger TD2

trigger TD3

X 9

DGG

X 9

IR input

New electronic chain after New electronic chain after August 2000August 2000

Advantage of the ~100 kg NaI(Tl) Advantage of the ~100 kg NaI(Tl) exptexpt

• Knowledge of the physical energy threshold(external keV range sources +

low energy Compton electrons)

• Noise identification(high # ph.el./keV + pulse time structures)

• Measurability of the software cut efficiencies(by irradiating the crystal with γ

sources and Compton e-)

• Knowledge of the needed efficiencies

• Knowledge of the sensitive volume

• Quenching factors measured(by irradiating a detector from the same

growth with neutrons, inducing recoils in the whole sensitive volume)

°

data

taki

ng o

f eac

h an

nual

cyc

le s

tart

s fr

om a

utum

n/w

inte

r (w

hen

cosω

(t-t

0)˜0

) tow

ard

sum

mer

(max

imum

exp

ecte

d).

° r

outi

ne c

alib

rati

ons

for

ener

gy s

cale

det

erm

inat

ion,

for

acce

ptan

ce w

indo

ws

effi

cien

cies

, etc

. by

mea

ns o

f rad

ioac

tive

so

urce

s ea

ch ~

10

days

col

lect

ing

typi

cally

~10

5ev

ts/k

eV/d

etec

tor

+ in

trin

sic

calib

rati

on f

rom

210 P

b by

sum

min

g ea

ch ti

me

the

data

ta

ken

duri

ng ~

7 d

ays

+ pe

riod

ical

Com

pton

cal

ibra

tion

s, e

tc.

° co

ntin

uous

on-

line

mon

itor

ing

of a

ll th

e ru

nnin

g pa

ram

eter

s

wit

h au

tom

atic

ala

rm to

ope

rato

r if

any

out

of a

llow

ed r

ange

.

N.C

im.A

112(

1999

)545

, PL

B42

4(19

98)1

95, P

LB

450(

1999

)448

, PR

D61

(199

9)02

3512

, P

LB

480(

2000

)23,

PL

B50

9(20

01)1

97, E

PJ

C18

(200

0)28

3, E

PJ

C23

(200

2)61

,P

RD

66(2

002)

0435

03, R

iv.N

.Cim

. 26

n. 1

(200

3) 1

-73

Mai

n pr

oced

ures

of t

he D

AM

A d

ata

taki

ngM

ain

proc

edur

es o

f the

DA

MA

dat

a ta

king

for

the

WIM

P an

nual

mod

ulat

ion

sign

atur

efo

r th

e W

IMP

annu

al m

odul

atio

n si

gnat

ure

22455 DAMA/NaI-3 ~ middle August PLB480(2000) 23

to end September

DAMA/NaI-0 4123 PLB389(1996) 757(PSD)

16020 DAMA/NaI-4 ~ middle October idem

to second half August

14962 DAMA/NaI-2 ~ November PLB450(1999)440

to end of July PRD61(1999)023512

PERIOD STATISTICS REFERENCES (kg ·day)

3363.8 winterDAMA/NaI-1 + PLB424(1998)195

1185.2 summer

Cumulative 1-4 57986 idem + PLB509(2001) 197+ EPJ C18 (2000)283

EPJ C 23 (2002)61+PRD66(2002)043503

100 kg DAMA/100 kg DAMA/NaINaI data data takingstakings

NEW

DAMA/NaI-5 15911~ August to end of the next July

16608DAMA/NaI-6 ~ November to

end of July17226

DAMA/NaI-7 ~ August to end of the next July

electronics and DAQ fully renewed)

TOTAL EXPOSURE 107731

partiallyoverlapped

Riv. N.Cim. 26 n.1 (2003)1-73

The switching off of the ~100kg NaI(Tl) set-up at end of July 2002

Dismounting the ~100kg NaI(Tl) set-up in August 2002

Opening the shield

DAMA/NaI out of operation

Mile

ston

es o

f thi

s da

ta re

leas

e

•DA

MA

/NaI

-5da

ta ta

king

•Aug

ust 2

000

el

ectr

onic

and

DA

Q fu

lly re

new

ed•D

AM

A/N

aI-6

da

ta ta

king

•Fal

l 200

1de

cisi

on to

pub

lish

the

resu

lts o

nly

at th

e en

d of

the

expt

sinc

e L

IBR

A p

repa

ratio

n w

as a

t goo

d po

int a

nd

com

plet

ion

of D

AM

A/N

aIfo

rese

en fo

r Jul

y 20

02•D

AM

A/N

aI-7

da

ta ta

king

; DA

MA

/NaI

out o

f ope

ratio

n Ju

ly 2

002

Febr

uary

200

3

deci

sion

to w

rite

a s

ingl

e co

mpl

ete

pape

r: R

iv. N

.Cim

chos

en3r

d M

arch

200

3 co

nclu

sion

of t

he o

vera

ll m

odel

inde

pend

ent a

naly

sis

30th

Apr

il 20

03en

d of

the

exam

ined

mod

el d

epen

dent

ana

lyse

s an

d of

th

e w

ritin

g of

the

pape

r6t

h M

ay 2

003

pape

r sen

t to

Riv

. N.C

im.

4th

June

200

3ac

cept

ance

of t

he p

aper

for p

ublic

atio

n

disi

nsta

lling

D

AM

A/N

aI;

inst

allin

g an

d pu

ttin

g in

ope

rati

on

LIBR

A (w

hich

is

runn

ing

sinc

e m

arch

/03)

DA

MA

/D

AM

A/ N

aIN

aI-- 1

to

1 to

-- 77

Res

idua

ls o

f the

rat

evs

time

and

ener

gy

Ann

ual m

odul

atio

n A

nnua

l mod

ulat

ion

of th

e ra

te: t

he m

odel

of

the

rate

: the

mod

el in

depe

nden

t res

ult

inde

pend

ent r

esul

t1077

31 k

g · d

Riv

. N. C

im. 2

6 n.

1. (2

003)

1-7

3

Tim

e (d

ay)

fitte

d (a

ll pa

ram

eter

s fr

ee):

fitte

d (a

ll pa

ram

eter

s fr

ee):

A =

(0.0

200

A =

(0.0

200

±±0.

0032

0.00

32) c

pd/k

g/ke

V

;

) cpd

/kg/

keV

;

tt 00

= (1

40

= (1

40 ±±

22) d

; T

= (1

.00

22) d

; T

= (1

.00

±±0.

01) y

0.01

) y

fitte

d: A

= (0

.023

3 ±

0.00

47) c

pd/k

g/ke

Vfit

ted:

A =

(0.0

210

±0.

0038

) cpd

/kg/

keV

2-4

keV

2-5

keV

2-6

keV

Tim

e (d

ay)

Tim

e (d

ay)

Aco

s[ω(t

-t0)

] ; c

ontin

uous

line

s: t 0

= 15

2.5

d, T

= 1

.00

y

P(A

=0)=

7⋅10

-4

χ2 /dof

=71/

37

The

data

fav

or t

he p

rese

nce

of a

mod

ulat

ed b

ehav

ior

with

pro

per

feat

ures

at

6.3σ

C.L.

Th

e da

ta f

avor

the

pre

senc

e of

a m

odul

ated

beh

avio

r wi

th p

rope

r fe

atur

es a

t 6.

3σC.

L.

fitte

d: A

= (0

.019

2 ±

0.00

31) c

pd/k

g/ke

V

ModelModel--independent residual independent residual rate for single hit eventsrate for single hit events

Results of the fits keeping all parameters free:

(2-4) keV A = (0.0252 ±0.0050) cpd/kg/keVt0 = (125 ± 30) dT = (1.01 ± 0.02) y

(2-5) keV A = (0.0215 ± 0.0039) cpd/kg/keVt0 = (140 ± 30) dT = (1.01 ± 0.02) y

(2-6) keV A = (0.0200 ± 0.0032) cpd/kg/keVt0 = (140 ± 22) dT = (1.00 ± 0.01) y

ModelModel--independent single hit independent single hit residual rate in a single annual cycleresidual rate in a single annual cycle

Total Exposure: 107731 kg · d

for t0 = 152.5 d and T = 1.00 y:A = (0.0195 ± 0.0031) cpd/kg/keV

for t0 = 152.5 d and T = 1.00 y:A = -(0.0009 ± 0.0019) cpd/kg/keV

6.3σ C.L.

A clear modulation is present in the lowestA clear modulation is present in the lowest--energy energy region, while it is absent just aboveregion, while it is absent just above

•Initial time 7th August

2-6 keV

Power Power spectrum spectrum of of residualsresiduals(according to Ap. J. 263(1982) 835; Ap. J. 338 (1989) 277)

Treatment of the experimental errors and time binning included here

Principal mode → 2.737 · 10-3 d-1 ˜ 1 y-1

Total exposure: 107731 kg · d

6-14 keV

Power Power spectrum spectrum of of residualsresiduals(according to Ap. J. 263(1982) 835; Ap. J. 338 (1989) 277)

Treatment of the experimental errors and time binning included here

No modulation effect found(only aliasing peaks present)

Statistical distribution of the Statistical distribution of the modulation amplitudes (modulation amplitudes (SSmm))

a) Sm for each detector, each annual cycle and each considered energy bin (here 0.25 keV)

b) <Sm> = mean values over the detectors and the annual cycles for each energy bin; σ = error associated to the Sm

2-6 keV 2-14 keV

Individual Sm values follow a normal distribution since (Sm-<Sm>)/σ is distributed as a Gaussian with a unitary standard deviation

Sm statistically well distributed in all the crystals, in all the data-taking periods and energy bins

Pressure

Temperature

External Radon

Nitrogen flux

The Stability Parameters: DAMA/NaI-7

Running conditions stable at level < 1%Parameters distribution

Hardware Rate

All amplitude well compatible with zero+ no effect can mimic the annual modulation

The Stability ParametersThe Stability Parameters

Time behaviourTime behaviourmodulation amplitudes obtained by fitting the time behaviours of main running parameters, acquired with the production data, when including a WIMP-like modulation

Running conditions stable at a level better than 1%

All the measured amplitudes wellcompatible with zero

+ no effect can mimic the annual modulation

(for the other annual cycles see ref: PLB424(1998)195, PLB450(1999)448, PLB480(2000)23,EPJC18(2000)283)

(For electronic noise, for Radon release from the rocks and for environmental bckg see later)

An effect from temperature can be excluded + Any possible modulation due to temperature would always fail some of the peculiarities of the signature

Distribution of the root mean square values of the operating T within periods with the same calibration factors (typically ≈7days): mean value ≈ 0.05°C

Considering the slope of the light output ≈ -0.2%/ °C: relative light output variation < 10-4 :

< 0.5% Smobserved

DAMA/NaI-5, 6 and 7

TemperatureTemperature

Distribution of the relative variations of the operating T of the detectors

• underground T largely stable during the year @ installation site• detectors in Cu housings directly in contact with multiton shield

→ huge heat capacity (≈106 cal/0C)• Experimental installation air conditioned• operating T of the detectors continuously controlled

amplitudes for a WIMP-like modulation in the operating T of the detectors well compatible with zero

Radon/1Radon/1•Walls and floor of the inner installation sealed in Supronyl (2 x 10-11 cm2/s permeability).

• Whole shield in plexiglas box maintained in HP Nitrogen atmosphere in slight overpressure with respect to environment

• Detectors in the inner Cu box in HP Nitrogen atmosphere in slight overpressure with respect to environment

Time behaviour of the environmental radon in the inner part of the barrack (from which the detector are excluded !)

measured values at level of sensitivity of the used radonmeter

amplitudes for a WIMP-like modulation of external Radon (from which the detectors are excluded!) well compatible with zero:

+ any possible modulation due to Radon would always fail some of the peculiarities of the signature

An effect from Radon can be excluded

Detectors continuously excluded from environmental air since several years (in HP Nitrogen atmosphere)

Investigation in Cu-box atmosphere

• Study of the double coincidences of γ’s (609&1120 keV) from 214Bi Radon daughter

• Rn concentration in Cu-box atmosphere <4.5 · 10-2 Bq/m3

• By MC: <4 · 10-4 cpd/kg/keV@low energy

• An hypothetical 10% modulation of possible Rn in Cu-box:

<0.2% of Smobserved

NO WIMP-like modulation amplitude in the time behaviour of external Radon (from which the detectors are excluded), of HP Nitrogen flux and of Cu box pressure (see before)

Radon/2Radon/2

<flux> of order of 250 l/h

Over-pressure ˜ 2-3 mbar

Noise/1Noise/1

σ = 0.5%

• Distribution of variations of total hardware rates of the 9 crystals over the single ph.el. threshold (that is from noise to “infinity”) during DAMA/NaI-5, 6, 7 running periods :

Cumulative gaussian behaviour fully accounted by expected statistical spread arising from the sampling time used for the rate evaluation

RHj = hardware rate of j-th detector above single photoelectron

<RHj> = mean of RHj in the corresponding annual cycle ≅ 0.25 Hz

amplitudes for a WIMP-like modulation well compatible with zero:

relative modulated amplitude from noise at low energy< 1.4 10-4

Can noise account for the observed Can noise account for the observed modulation effect?modulation effect?

DAMA/NaI-5 + 6 + 7

From the study of the "Hardware Rate" the modulated amplitude (period and phase as for WIMP) is compatible with zero:

-(0.06±0.11) ·10-2 Hz < 1.3 ·10-3 Hz (90% CL)

Hardware Rate=

noise + bckg [up to ˜ MeV] + signal [up to ˜ 6keV]

• noise/crystal ˜ 0.10 Hz• relative modulated amplitude from noise

< 1.3 10-3/9/0.1˜ 1.4 10-3 (90%CL)

NONO

even in the worst hypothetical case of 10% residual tail of noise in the data

< 1% of the observed annual modulation amplitude

The efficienciesThe efficiencies

Time behaviour:Time behaviour: modulation amplitudes obtained by fitting the time behaviours of the efficiencies including a WIMP-like cosine modulation for DAMA/NaI-5, 6, 7 running periods

Distribution of variations of the efficiency values with respect to their mean values during DAMA/NaI-5,6,7 running periods

Amplitudes well compatible with zero+ cannot mimic the annual modulation

2-8 keV

σ = 0.5 %

Energy Modulation amplitude DAMA/NaI-5+6+7

2-4 keV (0.7±1.0) · 10-3

4-6 keV (0.1±0.8) · 10-3

The calibration factorsThe calibration factorsRelative variations of the energy calibration factors (tdcal) from the 210Pb peak - without applying any correction - for all the 9 detectors during DAMA/NaI-5,6,7 running periods

Uncertainties on tdcal for each detector <1% within each ˜ 7 days period: additional energy spread σcal

Negligible effect considering routine calibrations and energy resolution at low energy

2

2 2 11 ;

2cal

res cal resres

σσ σ σ σ

σ

= + ⋅ +

;2

4/17.5 10

2 / 20cal

res

E EE keV

σσ

− ≤ ⋅

No modulation in the energy scaleNo modulation in the energy scale

Confirmation from MC: maximum relative contribution <1.6 · 10-4 (<1% Sm

obs)

gaussian behaviour with σ = 0.5%

Can a hypothetical background Can a hypothetical background modulation account for the modulation account for the

observed effect?observed effect?Integral rate at higher energy (above 90 keV), R90

• R90 percentage variations with respect to their mean values for single crystal in the DAMA/NaI-5,6,7 running periods

Energy regions closer to that where the effect is observed

Mod. Ampl. (6-10 keV): -(0.0076 ± 0.0065), (0.0012 ± 0.0059) and(0.0035 ± 0.0058) cpd/kg/keV for DAMA/NaI-5, DAMA/NaI-6 and DAMA/NaI-7;

→ they can be considered statistically consistent with zero

→ cumulative gaussian behaviour with σ ≈ 0.9%, fully accounted by statistical considerations

• Fitting the behaviour with time, adding a term modulated according period and phase expected for WIMPs:

→ consistent with zero + if a modulation present in the whole energy spectrum at the level found in the lowest energy region → R90 ∼ tens cpd/kg → ∼ 100 σ far away

Period Mod. Ampl.

DAMA/NaI-5 (0.09±0.32) cpd/kgDAMA/NaI-6 (0.06±0.33) cpd/kgDAMA/NaI-7 -(0.03±0.32) cpd/kg

No modulation in the background:these results also account for the bckg

component due to neutrons

Can a possible thermal neutron modulation Can a possible thermal neutron modulation account for the observed effect?account for the observed effect?

Ex.: 23Na(n,γ)24Na; 23Na(n,γ)24mNacapture rate = Φn σn NT = 0.17 captures/d/kg • Φn/(10-6 n cm-2 s-1)

Thermal neutron flux @ LNGS:Φn = 1.08 10-6 n cm-2 s-1 (N.Cim.A101(1989),959)Φn < 5.9 10-6 n cm-2 s-1 (in the DAMA set-up from delayed

coincidences see N.Cim.A112(1999),545)Assuming - very cautiously - a 10% thermal neutron modulation:

⇓Sm

(thermal n) < 10-5 cpd/kg/keV (< 0.05% Smobserved)

In all the cases of neutron captures (24Na, 128I, ...) a possible thermal n modulation induces a variation in all the energy spectrum

Excluded by R90 analysis

NO

E (MeV)

MC

1.4 x 10-3 cpd/kg/keV

7 x 10-5 cpd/kg/keV

when Φn = 10-6 n cm-2 s-1

Can a possible fast neutron Can a possible fast neutron modulation account for the modulation account for the

observed effect?observed effect?Elastic scatterings: recoil nuclei

capture rate = Φn σn NT

Fast neutron flux @ LNGS:

Φn = 0.9 10-7 n cm-2 s-1 (Astropart.Phys.4 (1995),23)

By MC: differential counting rate above 2 keV ˜ 10-3 cpd/kg/keV

Assuming - very cautiously -a 10% neutron modulation:

Sm(fast n) < 10-4 cpd/kg/keV (< 0.5% Sm

observed)

Moreover, a possible fast n modulation inducesa variation in all the energy spectrum

Excluded by R90 analysis

NONO

Can the Can the µµ modulation measured by modulation measured by MACRO account for the observed effect?MACRO account for the observed effect?

Case of fast neutrons produced by muons

Annual modulation amplitude at low energy due to µ modulation:Sm

(µ) = Rn g ε f∆E fsingle 2% /(Msetup ∆E)

where:g = geometrical factorε = detection efficiency by elastic scatteringf∆E = energy window (E>2keV) efficiencyfsingle = single hit efficiency

Hyp.:Meff = 15 tonsg ˜ ε ˜ f∆E ˜ fsingle ˜ 0.5 (cautiously)

Knowing that: Msetup=100kg and ∆E=4keV

Moreover, this modulation also induces a variation in other parts of the energy spectrum

Excluded by R90 analysis

Φµ @ LNGS ˜ 20 µ m-2 d-1 (±2% modulated)Neutron Yield @ LNGS: Y=1÷7 10-4 n /µ /(g/cm2)

(hep-ex/0006014)Rn = (fast n by µ)/(time unit) = Φµ Y Meff

Sm(µ) < (1÷7) 10-5 cpd/kg/keV (< 0.3% Sm

observed)

NONO

Summary of the results obtained by the Summary of the results obtained by the investigation of possible systematics or side investigation of possible systematics or side

reactions in DAMA/NaIreactions in DAMA/NaI--5, 6, 75, 6, 7Source Main comment Cautious upper

limit (90%C.L.)RADON Sealed Cu box in HP <0.2% Sm

obs

Nitrogen atmosphere

TEMPERATURE The installation is air- <0.5% Smobs

conditioned

NOISE Effective noise <1% Smobs

rejection

ENERGY SCALE Periodical calibrations <1% Smobs

+ continuous monitoringof 210Pb peak

EFFICIENCIES Regularly measured by <1% Smobs

dedicated calibrations

BACKGROUND No modulation observed <0.5% Smobs

above 6 keV; this limitincludes possible effectof thermal and fast neutrons

SIDE REACTIONS Muon flux variation <0.3% Smobs

measured by MACRO

+ even if larger they cannot satisfy all the 6 requirements of annual modulation signature

Thus, they can not mimic the observed annual modulation effect

Summary of theSummary of theDAMA/DAMA/NaINaI Model IndependentModel Independent resultresult::

•Presence of modulation for 7 annual cycles at ~6.3σCL with the proper distinctive features for a WIMP induced effect

•The deep investigation has shown absence of known sources of possible systematics and side processes able to mimic the signature

•All the signature features satisfied by the data over 7 independent experiments of 1 year each one

corollary quests for the nature and coupling with ordinary matter of the candidate particle within given model

frameworks

ρ WW

IMP

vel

ocit

y di

stri

buti

on a

nd

its p

aram

eter

s

coup

ling:

SI,

SD

, mix

ed S

I&SD

,pre

ferr

edin

elas

tic, .

..sc

alin

g la

ws

on c

ross

sec

tions

form

fact

ors

and

rela

ted

para

met

ers

spin

fact

ors

etc.

The

y ca

n af

fect

no

t on

lyth

e co

rolla

ry

esti

mat

ed

regi

ons

follo

win

g a

posi

tive

eff

ect

from

th

e W

IMP

an

nual

m

odul

atio

n si

gnat

ure,

but

als

ore

sult

s gi

ven

as e

xclu

sion

plo

ts

To

inve

stig

ate

the

natu

re a

ndco

uplin

g w

ithor

dina

rym

atte

rof

the

poss

ible

WIM

P ca

ndid

ate,

an

effe

ctiv

e en

ergy

and

time

corr

elat

ion

anal

ysis

of t

he e

vent

s ha

s to

be

perf

orm

ed w

ithin

giv

enm

odel

fram

ewor

ks

THUS

unce

rtai

ntie

s on

mod

els

and

com

paris

ons ex

per

imen

tal p

aram

eter

s (t

ypic

al o

f ea

ch e

xper

imen

t)co

mp

aris

on

wit

hin

par

ticl

e m

od

els

Som

e (o

f the

man

y po

ssib

le) c

orol

lary

que

sts

for

the

cand

idat

e pa

rtic

le

??

Exa

mpl

e ef

fect

on

the

excl

usio

n pl

ot w

hen

chan

ging

the

valu

e of

a p

aram

eter

(ins

ide

its

allo

wed

rang

e) w

ithin

the

sam

e m

odel

fram

ewor

k

Ast

rop.

Phy

s. 2

(199

4) 1

17

Na

F

mW

(GeV

)

σp(pb)

•Top

cur

ves:

v0=

180

km/s

; ves

c=50

0 km

/s•L

ower

cur

ves:

v0=

250

km/s

; ves

c=10

00 k

m/s

•v0

affe

cts

mai

nly

the

over

all r

ate

•ves

caf

fect

s m

ostly

the

low

er m

ass

regi

on

Sim

ilar

effe

ct a

refo

und

for

ever

y nu

cleu

s an

d in

tera

ctio

n ty

pe

chan

ging

ass

umpt

ions

and

/or

expt

/the

oret

ical

para

met

ers

WIMPWIMP--nucleus elastic scatteringnucleus elastic scattering

dσdER

(v,ER) = dσdER

SI

+ dσdER

SD

=

2GF2mN

πv 2 Zgp + (A − Z )gn[ ]2FSI

2 (ER) + 8 J + 1J

ap Sp + an Sn[ ]2FSD

2 (ER )

SI+SD differential cross sections:

F2(ER) nuclear form factors

mWp reduced WIMP-nucleon mass

Generalized SI/SD WIMP-nucleon cross sections:

σSI =4π

GF2mWp

2 g2 σSD =32π

34

GF2 mWp

2 a 2

where: g =gp + gn

2• 1 −

gp − gn

gp + gn

1−2ZA

a = a p2 + an

2 tgθ =an

a p

g: independent on the used target nucleus since Z/A nearly constant for the nuclei typically used in WIMP direct searches

Differential energy distribution:dR

dER

= NT

ρW

mW

dσdER

vmin (E R )

v max

∫ (v, ER )vf (v)dv = NT

ρW mN

2mW mWp2 ⋅ Σ(ER ) ⋅ I (ER)

gp,n(a p,n) effective WIMP-nucleon couplings

<Sp,n> nucleon spin in the nucleus

I(ER) =f (v)vvmin (ER )

vmax

∫ dv

vmin =mN ER

2mWN2

Σ(ER ) = A2σ SI FSI2 (ER) +

43

J +1J

σSD Sp cosθ + Sn sinθ[ ]2 FSD2 (ER )

where:

NT: number of target nuclei

f(v): WIMP velocity distribution in the Earth frame (it depends on ve)

ve=vsun+vorbcosω t

vmax: maximal WIMP velocity in the Earth frame

minimal velocity providing ER recoil energy:

The inelastic WIMP The inelastic WIMP –– nucleus nucleus interaction: W + N interaction: W + N →→ WW** + N+ N

Differential energy distribution for SI interaction:

• WIMP candidate suggested by D. Smith and N. Weiner (PRD64(2001)043502)

• Two mass states χ+ , χ- with δ mass splitting WIMP

• Kinematical constraint for the inelastic scattering of χ- on a nucleus with mass mN becomes increasingly severe for low mN

Ex. mW =100 GeVmN µ70 41130 57

12

µv2 ≥ δ ⇔ v ≥ vthr =2δµ

[ ]2

2222

2

22

* 1)()(vv

qFgZAZgmG

dd thr

SInpWNF −⋅−+=

Ω πσ

Nucleus recoil energy:

2

cos12

12

*2

2

2

2

22 θ⋅−−−⋅= v

vv

v

mvm

E

thrthr

N

WNR

Differential energy distribution:

∫=max

min

)(),(v

vR

RW

WT

R

dvvvfEvdEd

mN

dEdR σρ

+⋅=

RN

WN

WN

RNR Em

mm

EmEv

δ1

2)( 2min

gp,n effective WIMP-nucleon couplings

dΩ* differential solid angle in the WIMP-nucleus c.m. frame

q2 = squared threee-momentum transfer

[ ] )()(2 22

2

2

RSInpNF

R

EFgZAZgvmG

dEd

−+=π

σ

Similar situation for all the target nuclei considered in the field

Examples of different Form Factor profiles Examples of different Form Factor profiles for for 127127I available in literatureI available in literature

• Take into account the structure of target nuclei• In SD form factor: no decoupling between nuclear and WIMP

degrees of freedom; dependence on nuclear potential.• Example on 127I nucleus:

Spin Independent2( ) /5nqre−

2 21 2( ) ( )(1 )n nqr qrAe A eα α− −+ −

Helm

charge spherical distribution

2 21 2( ) ( )(1 )n nqr qrAe A eα α− −+ −

Smith et al.,Astrop.Phys.6(1996) 87

2( ) / 5nqre−

“thin shell” distribution

from Ressell et al.

from Helm

Spin Dependent

The Spin FactorThe Spin Factor

Spin Factors for some target-nuclei calculated in simple different models

Spin factor = Λ2J(J+1)/ax2

(ax= an or ap depending on the unpaired nucleon)

Spin Factors calculated on the basis of Ressell et al. for some of the possible θ values considering some target

nuclei and two different nuclear potentials

Spin factor = Λ2J(J+1)/a2

Quenching factorQuenching factorrecoil/electron response ratio measured with a neutron

source or at a neutron generator

Quenching factors, q, measured by neutron sources or by neutron beams for some detectors and nuclei

none available so far(assumed 1)

Isothermal sphere: the most widely used model only in the WIMP direct search (but not correct)

density profile: gravitational potential:

→ Maxwellian velocity distribution

2( )DM r rρ −∝ 20 log( )rΨ ∝

Halo modelingHalo modeling

2 2 20

2 2 2

3( )

4 ( )c

DMc

v R rr

G R rρ

π+

=+

22 20

0 ( ) log( )2 cv

r R rΨ = − +2

2 22 2( )

( )rot cc

rv r v

R r=

+

2 2

2 2 ( 4 ) / 2

3 (1 )( )

4 ( )a c c

DMc

R R rr

G R r

β

β

β βρ

π +

Ψ + −=

+ 0 2 2 / 2( ) , ( 0)( )

a c

c

Rr

R r

β

β βΨ

Ψ = ≠+

22

2 2 ( 2) /2( )( )

a crot

c

R rv r

R r

β

β

β+

Ψ=

+

( )/

0 00

1 ( / )( )

1 ( / )DM

R R ar

r r a

β γ αγ α

αρ ρ−

+ = +

2

0 21r

v

vφβ = −

Evans’ logarithmic

Evans’ power-law

Spherical ρDM, isotropic velocity dispersion

If Axisymmetric ρDM → q flatness

If spherical ρDM with non-isotropic velocity dispersion →

Others:

2 22 20

0 2( , ) log2 c

v zr z R r

q

Ψ = − + +

Triaxial ρDM → p,q,δ2 2 2

200 2 2( , , ) log

2v y z

x y z xp q

Ψ = − + +

δ = free parameter → in spherical limit (p=q=1) quantifies the anisotropy of the velocity dispersion tensor

2

2

22r

v

vφ δ+

=

Constraining the models

• Needed quantities for Dark Matter direct searches:

→ DM local density ρ0 = ρDM (R0 = 8.5 kpc)→ local velocity v0 = vrot (R0 = 8.5kpc) → velocity distribution ( )f v

r

00

1010

10

2.1)100(8.0106101

)50220(

vkpcrvvMMM

skmv

rot

vis

⋅≤=≤⋅⋅≤≤⋅

⋅±=

⊕⊕

−

Models accounted in the following:

• Isothermal sphere ⇒ very simple but unphysical halo model• Several approaches different from the isothermal sphere model:

Belli et al. PRD61(2000)023512; VergadosPR83(1998)3597, PRD62(2000)023519;Ullio & Kamionkowski JHEP03(2001)049; GreenPRD63(2001) 043005, Vergados & Owen astroph/0203293.

• Large number of self-consistent halo models constrained by astrophysical observations

(for DAMA/NaI-0 to 4 see PRD66(2002)043503)

Consistent Halo ModelsConsistent Halo Models

• Allowed intervals of ρ0 (GeV/cm3) for v0=170,220,270 km/s, for the halo models considered in the model-dependent analyses given in the following

Intervals evaluated considering the density profile and the astrophysical constraints

The allowed local The allowed local density valuesdensity values

00

1010

10

2.1)100(8.0106101

)50220(

vkpcrvvMMM

skmv

rot

vis

⋅≤=≤⋅⋅≤≤⋅

⋅±=

⊕⊕

−

PRD66(2002)043503

Model dependent scenarios investigated Model dependent scenarios investigated here (here (others under investigationothers under investigation))

Case A: FF parameters at fixed values and quenching factors at mean measured values

Case B: i) 23Na and 127I quenching factors from mean values up to +2 times the errors; ii) nuclear radius, r, and nuclear surface thickness parameter, s, in the SI FF from fixed values down to 20%; iii) b parameter in the considered SD FF from fixed value down to 20%.

Case C: one of the possible more extreme cases where the Iodine nucleus parameters are fixed at values of case

B, while for Sodium nucleus one considers: i) 23Na quenching factor at the lowest valueavailable in literature (see Table); ii) nuclear radius, rn, and nuclear surface thickness parameter, s, in the used SI FF from central values up to +20%; iii) b parameter in the considered SD FF from fixed value up to +20%.

For simplicity, the results are given in terms of allowed regions obtained as superposition of the configurations corresponding to likelihood function values distant more than 4σ from the null hypothesis (absence of modulation) in each of the several (but still a limited number of the possible)model frameworks considered here.

Main topics:Main topics:Halo models as in PRD66(2002)043503Helm FF for SI couplingRessel FF (Nijmengen II nuclear potential) calculated

for χ++

PRIORS

• Measured upper limits on the recoil fractions in the DAMA/NaI-0 running period, especially devoted to this investigation

• Model dependent mass limit for supersymmetric candidates by accelerator experiments:

– mW > 30 GeV from lower bound on neutralino mass as derived from LEP data in supersymmetric schemes based on GUT assumptions (from DPP2003)

but other model assumptions are possible and would imply significant variations of the accelerators bounds as shown in literature also recently e.g. for the case when the gaugino-mass unification at GUT scale is released

+ candidates other than neutralino are possible.e.g.: • an heavy neutrino of the 4-th family;

• the sneutrino in the Weiner and Smith scenario;• even whatever suitable particle not yet foreseen

by theory

Gene

ral ca

se:

WIM

P wi

th S

I &

SD c

ouplings

Gene

ral ca

se:

WIM

P wi

th S

I &

SD c

ouplings

(Na

and

I ar

e fu

lly s

ensitive

to

SD int

erac

tion

, on

the

con

trar

y of

e.

g. G

ean

d Si,)

•T

he r

esul

t is

an a

llow

ed v

olum

e in

the

spac

e (ξ

σSI

, σξ S

D, m

W) f

or e

ach

poss

ible

θ (

tgθ

= a n

/ap

, with

0=θ

<π)

•ξ

= ρ W

/ ρ0

, ξ =

1 fr

acti

on o

f am

ount

of l

ocal

WIM

P d

ensi

ty•

Seve

ral c

onsi

sten

t hal

o m

odel

s in

clud

ing

halo

rot

atio

n (s

ee b

efor

e)•

Cas

es A

, B a

nd C

The

use

e.g

of m

ore

favo

urab

le fo

rm fa

ctor

s th

an

thos

e w

e co

nsid

ered

her

e al

one

wou

ld m

ove

the

regi

on to

war

ds lo

wer

cro

ss s

ecti

ons

Exa

mp

le o

f sl

ices

of

the

allo

wed

vo

lum

e fo

r g

iven

mW

and

θva

lues

•θ=

0 (a

n=0,

ap≠

0)•

θ=π/

4 (a

n=a p

)•

θ=π/

2 (a

n≠0,

ap=

0)

•θ=

2.43

5 (a

n/a p

= -0

.85,

Z0

coup

l.)

At p

rese

nt e

ithe

r a

pure

ly S

I or

a p

urel

y SD

or

a m

ixed

SI

&SD

con

figu

rati

ons

are

supp

orte

d by

the

data

+ Se

vera

l oth

er p

ossi

bilit

ies

for

the

SI &

SD m

ixed

m

odel

fram

ewor

k ar

e op

en a

nd to

be

inve

stig

ated

(d

iffer

ent S

D-F

F (a

p&

an)

, gn

= g p

?, d

iffe

rent

hal

o m

odel

s, e

tc.)

incl

udin

g al

l the

exi

stin

g un

cert

aint

ies

muc

h la

rger

reg

ions

(and

vol

umes

) are

obt

aine

d

Exam

ple

of h

ow t

he r

egions

hav

e be

en b

uilt

Exam

ple

of h

ow t

he r

egions

hav

e be

en b

uilt

The

figu

re s

how

s th

e su

perp

ositi

on o

f the

slic

es o

btai

ned

for

each

one

of t

he m

odel

fram

ewor

k co

nsid

ered

in th

e ca

se o

f

m

W=9

0 G

eV a

nd θ

= 2.

435

(pur

e Z

0co

uplin

g)

The

incl

usio

n of

oth

er e

xist

ing

unce

rtain

ties

on p

aram

eter

s an

d m

odel

s w

ould

furth

er e

xten

d th

e re

gion

: e.g

. the

use

of m

ore

favo

urab

le

form

fact

ors

than

thos

e w

e co

nsid

ered

he

re a

lone

wou

ld m

ove

the

regi

on

tow

ards

low

er c

ross

sec

tions

WIM

P wi

th d

ominan

t SI

cou

pling

WIM

P wi

th d

ominan

t SI

cou

pling

•ξ

= ρ W

/ ρ0

, ξ =

1 fr

actio

n of

am

ount

of l

ocal

WIM

P d

ensi

ty•

Seve

ral c

onsi

sten

t hal

o m

odel

s in

clud

ing

halo

rot

atio

n (s

ee b

efor

e)

•C

ases

A, B

and

C +

see

pre

viou

s tr

ansp

aren

cies

Mod

el d

epen

dent

lowe

r bo

und

on n

eutr

alin

o m

ass

as d

eriv

ed f

rom

LEP

dat

a in

sup

ersy

mm

etri

c sc

hem

es b

ased

on

GUT

assu

mpt

ions

(DPP

2003

)

Regi

on p

oten

tial

ly o

f in

tere

st f

or a

neu

tral

ino

in

supe

rsym

met

ric

sche

mes

whe

re a

ssum

ptio

n on

ga

ugin

o-m

ass

unif

icat

ion

at G

UT

is r

elea

sed

and

for

“gen

eric

” W

IMP

high

er m

ass

regi

on a

llowe

d fo

r lo

w v 0

, eve

ry s

et o

f pa

ram

eter

s’ va

lues

and

the

hal

o m

odel

s: E

vans

’ lo

gari

thm

ic C

1 an

d C2

co-

rota

ting

, tri

axia

lD2

and

D4

non-

rota

ting

, Eva

ns p

ower

-law

B3

in s

et A

Bes

t-fit

val

ues

of c

ross

sec

tion

and

WIM

P

mas

s sp

an o

ver

a la

rge

rang

e de

pend

ing

on

the

mod

el fr

amew

ork.

Ju

st a

s an

exa

mpl

e: t

riax

ial

D2,

max

ρ0,

low

v0

and

para

met

ers

case

C:

mW

=(74

+17 -1

2)

GeV

and

ξσ

SI=(

2.6±

0.4)

10-6

pb

DA

MA

/NaI

-0to

7

The

incl

usio

n of

oth

er e

xist

ing

unce

rtai

ntie

s on

pa

ram

eter

s an

d m

odel

s w

ould

furt

her

exte

nd

the

regi

on: e

.g. t

he u

se o

f mor

e fa

vour

able

FF

th

an th

ose

cons

ider

ed h

ere

alon

e w

ould

mov

e th

e re

gion

tow

ards

low

er c

ross

sec

tions

An

exam

ple

of t

he e

ffec

t indu

ced

by a

non

An

exam

ple

of t

he e

ffec

t indu

ced

by a

non

-- zer

o ze

ro

SD c

ompo

nent

on

the

allowe

d SI

region

sSD c

ompo

nent

on

the

allowe

d SI

region

s•E

xam

ple

obta

ined

con

side

ring

Eva

ns’ l

ogar

ithm

ic a

xisy

mm

etri

c C2

hal

o m

odel

wit

h v 0

= 17

0 km

/s, ρ

0m

ax a

nd p

aram

eter

s of

set

A•T

he d

iffe

rent

reg

ions

ref

er t

o di

ffer

ent

SD c

ontr

ibut

ions

wit

h θ=

0

a) σ

SD=

0 pb

; b)

σSD

= 0.

02 p

b;c)

σSD

= 0.

04 p

b;

d) σ

SD=

0.05

pb;

e) σ

SD=

0.06

pb;

f)

σSD

= 0.

08 p

b;

•Th

ere

is n

o m

eani

ng in

bar

e co

mpa

rison

be

twee

n re

gion

s al

low

ed in

exp

erim

ents

se

nsiti

ve to

SD

cou

plin

g an

d ex

clus

ion

plot

s ac

hiev

ed b

y ex

peri

men

ts th

at a

re n

ot.

•T

he s

ame

is w

hen

com

parin

g re

gion

s al

low

ed

by e

xper

imen

ts w

hose

targ

et-n

ucle

i hav

e un

pair

ed p

roto

n w

ith e

xclu

sion

plo

ts q

uote

d by

exp

erim

ents

usi

ng ta

rget

-nuc

lei w

ith

unpa

ired

neu

tron

whe

re θ

≈0

or θ

≈π.

A s

mal

l SD

con

trib

utio

n ⇒

dras

tical

ly m

oves

the

allo

wed

reg

ion

in

the

plan

e (m

W, ξ

σSI

) tow

ards

low

er S

I cr

oss

sect

ions

(ξσ

SI<

10-6

pb)

Supersymmetric expectations in MSSM

- purely SI coupling -(mass below 50 GeV obtained when releasing the gaugino

mass unification at GUT scale)

scatter plot of theoretical configurations from hep-ph/0304080

WIM

P wi

th d

ominan

t SD

cou

plings

WIM

P wi

th d

ominan

t SD

cou

plings

•Re

gion

allo

wed

in t

he s

pace

(mW

, ξσ

SD, θ

)•

Her

e ex

ampl

e of

slic

es f

or o

nly

4 (θ

=0, π

/4, π

/2, 2

.435

) val

ues

of θ

(whi

ch c

an r

ange

fro

m0

toπ)

•S

ever

al c

onsi

sten

t ha

lo m

odel

s in

clud

ing

halo

rot

atio

n (s

ee b

efor

e)

•Ca

ses

A, B

and

C +

see

pre

viou

s tr

ansp

aren

cies

Regi

ons

abov

e 20

0 Ge

V al

lowe

d fo

r lo

w v 0

, for

eve

ry s

et o

f pa

ram

eter

s’ va

lues

and

for

Eva

ns’ l

ogar

ithm

ic C

2 co

-rot

atin

g ha

lo m

odel

s

Bes

t-fit

val

ues

of c

ross

sec

tion

and

WIM

P m

ass

span

ove

r a

larg

e ra

nge

depe

ndin

g on

the

mod

el fr

amew

ork

DA

MA

/NaI

-0to

7

The

incl

usio

n of

oth

er e

xist

ing

unce

rtai

ntie

s on

par

amet

ers

and

mod

els

wou

ld f

urth

er

exte

nd t

he r

egio

n: e

.g.

the

use

of m

ore

favo

urab

le F

F t

han

thos

e w

e co

nsid

ered

he

re a

lone

wou

ld m

ove

the

regi

on t

owar

ds

low

er c

ross

sec

tions

An

exam

ple

of t

he e

ffec

t indu

ced

by a

non

An

exam

ple

of t

he e

ffec

t indu

ced

by a

non

-- zer

o ze

ro

SI

compo

nent

on

the

allowe

d SD r

egions

SI

compo

nent

on

the

allowe

d SD r

egions

•Exa

mpl

e ob

tain

ed c

onsi

deri

ng E

vans

’ log

arit

hmic

axi

sym

met

ric

C2 h

alo

mod

el w

ith

v 0=

170

km/s

, ρ0

max

and

par

amet

ers

of s

et A

for

θ=0

.•T

he d

iffe

rent

reg

ions

ref

er t

o di

ffer

ent

SI c

ontr

ibut

ions

a) σ

SI=

0 pb

; b)

σSI

= 2⋅

10-7

pb;

c) σ

SI=

4⋅10

-7 p

b;

d) σ

SI=

6⋅10

-7 p

b;e)

σSI

= 8⋅

10-7

pb;

f)

σSI

= 10

-6 p

b;

The

acco

unti

ng f

or t

he u

ncer

tain

ties

, e.

g., o

n th

e sp

in f

acto

rs, d

iffe

rent

SD

fo

rm f

acto

rs w

ould

ext

end

the

regi

on

allo

wed

and

mov

e it

tow

ards

lowe

r ξσ

SDva

luesA s

mal

l SI

cont

ribu

tion

⇒dr

astic

ally

mov

es th

e al

low

ed r

egio

n in

the

plan

e (m

W, ξ

σSD

) tow

ards

low

er

SD c

ross

sec

tions

(ξσ

SD<

0.1

pb)

WIM

P wi

th p

refe

rred

SI

inelas

tic

inte

ract

ion:

W

IMP

with

pre

ferr

ed S

I inelas

tic

inte

ract

ion:

W

+ N

W

+ N

→→WW

**+

N+

N

v esc

fixe

d bu

t it

s un

cert

aint

ies

can

play

an

impo

rtan

t ro

le, e

xten

ding

the

allo

wed

regi

ons

The

incl

usio

n of

oth

er e

xist

ing

unce

rtai

ntie

s on

pa

ram

eter

s an

d m

odel

s wo

uld

furt

her

exte

nd t

he r

egio

n:e.

g. t

he u

se o

f a

mor

e fa

vour

able

SI

form

fac

tor

for

iodi

ne

woul

d m

ove

the

regi

ons

towa

rds

lowe

r cr

oss-

sect

ions

•Re

gion

allo

wed

in t

he s

pace

(m

W ,

ξσp,δ

)•

ξ=

ρ W/ ρ

0, ξ

=1

frac

tion

of

amou

nt o

f lo

cal W

IMP

dens

ity

•H

ere

exam

ples

of

slic

es f

or s

ome

mW

valu

es•

Sev

eral

con

sist

ent

halo

mod

els

incl

udin

g ha

lo r

otat

ion

(see

bef

ore)

•

Case

s A

, B a

nd C

+ s

ee p

revi

ous

tran

spar

enci

es

Bes

t-fi

t val

ues

of c

ross

sec

tion

and

d fo

r gi

ven

mW

span

ove

r a

larg

e ra

nge

depe

ndin

g on

the

mod

el fr

amew

ork.

Just

as

an e

xam

ple:

mW

= 7

0 G

eV in

NF

W B

5 ha

lo m

odel

wit

h lo

w v

0, m

ax r

0an

d pa

ram

eter

s as

in c

ase

B: δ

=(86

+6-8

) keV

, ξσ

p=(1

.2±

0.2)

10-5

pb

regi

on la

rgel

y lie

s in

δre

gion

s w

here

e.g

. Ge

is d

isfa

vour

ed

HE

AT

dat

a as

ana

lyse

din

P

RD

65(2

002)

0577

01

Som

e po

siti

ve h

ints

fro

m i

ndir

ect

sear

ches

no

t in

co

nflic

t w

ith

DA

MA

(Not

e th

at t

he i

nter

pret

atio

n of

the

se h

ints

an

d th

e de

rive

d W

IMP

m

ass

and

cros

s se

ctio

n de

pend

on

bc

kgm

odel

ing,

on

sp

atia

l/vel

ocity

W

IMP

di

stri

butio

n in

th

e ga

lact

ic h

alo,

etc

.)

A. M

orse

lliet

al.,

as

tro-

ph/0

2112

86

As

a re

sult o

f a

new

R&D f

or r

adiopu

rer

NaI

(Tl)

by

exploiting

new

che

mical/p

hysica

l ra

diop

urificat

ion

tech

niqu

es(a

ll op

erat

ions

invo

lvin

g cr

ysta

ls a

nd P

MTs

-in

clud

ing

phot

os -

in H

P N

itro

gen

atm

osph

ere)

The

new

LIB

RA

set-

up~2

50 k

g N

aI(T

l)(L

arge

sodi

umIo

dide

Bul

k fo

rR

Are

proc

esse

s)in

the

DA

MA

expe

rim

ent

The

new

LIB

RA

LIB

RA

set-

up~2

50 k

g ~2

50 k

g N

aI(T

lN

aI(T

l ))(L

arge

sodi

umIo

dide

Bul

k fo

rR

Are

proc

esse

s)in

the

DA

MA

expe

rim

ent

Impr

ovin

g in

stal

latio

net

chin

gst

aff

at w

ork

PMT

+HV

divi

der

stor

ing

new

cry

stal

s

Inst

allin

gL

IBR

Ade

tect

ors

Sum

mar

y

→→The

mod

el ind

epen

dent

The

mod

el ind

epen

dent

res

ult:

resu

lt:

pres

ence

of

a W

IMP

compo

nent

in

the

galact

ic h

alo

supp

orte

d at

6.3

σC.

L.by

the

WIM

P an

nual m

odulat

ion

sign

atur

e. N

o kn

own

syst

emat

ics

nor

side

rea

ctions

able t

o mim

ic t

he

sign

atur

efo

und

-no

r su

gges

ted

by a

nyon

e.

→Co

rolla

ry m

odel d

epen

dent

que

st f

or a

can

dida

te:W

IMPs

with

mix

ed S

I/SD

or

pure

SI

or

pure

SD c

oupling

as w

ell as

WIM

Pswi

th p

refe

rred

ine

last

ic s

catt

ering

in

some

of t

he m

any

poss

ible m

odel f

ramew

orks

.

ØSu

cces

sfully r

unning

the

~10

0kg

NaI

(Tl)

set-

up o

ver

7 an

nual c

ycles

(~ 1

.1 x

105

kg d

ay)

now

runn

ing

DAM

A/L

IBRA

no

w ru

nning

DAM

A/L

IBRA

(~2

50 k

g (~

250

kg N

aI(T

lNaI

(Tl ))

since

mar

ch 2

003

)) s

ince

mar

ch 2

003

& a

new

R&D f

or f

urth

er N

aI(T

l) ra

diop

urificat

ions

towa

rd 1

ton

set

-up

prop

osed

in

1996

not

exha

usti

ve -

othe

r sc

enar

ios

poss

ible

and

un

der

inve

stig

atio

ns