Arnow

itt: H

UN

T FO

R

DA

RK

M

ATTER

Teru

ki Ka

mo

n1

),2)

1) M

itch

ell In

stitute

for F

un

da

me

nta

l Ph

ysics a

nd

Astro

no

my, Te

xas A

&M

Un

iversity

2) K

yun

gp

oo

k Na

tion

al U

nive

rsity

Arn

ow

itt Sym

po

sium

M

ay 1

8, 2

01

5

1

[Credits] �

Images of Baryon Acoustic

Bscillations with Cosmic

Microwave Background by E.M. Huff, the SDSS-III team

, and the South Pole Telescope team

. Graphic by Zosia Rostom

ian (Lawrence Berkeley National Laboratory)

�Im

age of Neutrino Astrophysics, taken from

https://astro.desy.de/ �

Image of the LHC by CERN Photo

�Im

age of Bullet Cluster by NASA/ Chandra X-ray Center

Sum

mary

ARR

NO

WIT

T-L

INE

3

1)PH

ENO Projects

2)PPC

3)Chasing D

M Signals

Prologue It has been 13.8 B years, since the LH

C m

achine was set up. The LHC started taking

data from

proton-proton

collisions at

a center-of-m

ass energyof 7 TeV on M

arch 30, 2010 and becam

e the energy frontier m

achine to lead to discoveries such as 125-GeV H

iggs boson in July 4, 2012). The Standard M

odel is currently well tested up to ~100 GeV, but is expected to break down in the TeV dom

ain where new physics should occur. This is precisely the dom

ain that we will study at the LH

C.

PPC Cube

Teru

ki Ka

mo

n

2

Hu

nt fo

r Da

rk M

atte

r

PPCCu

Our PH

ENO projects have begun with his sim

ple questions: (a)how

well m

SUGRA

m

odels can

be tested

experimentally;

(b)how cosmologically-consistent collider signals can

be determined.

[1] P

HE

NO

Pro

jects

TTeru

ki Ka

mo

n

3

Hu

nt fo

r Da

rk M

atte

r

This also

helps us

shaping up

ideas of

accelerator upgrades in the U

.S. The choice of PH

ENO project topics has been evolving as

major scientific events occurred:

i)SSC was cancelled in 1993

ii)W

MAP results were out in 2002.

iii)The H

iggs boson was discovered in 2012.

TTeru

ki Ka

mo

n

4

Hu

nt fo

r Da

rk M

atte

r

TTeru

ki Ka

mo

n

5

Hu

nt fo

r Da

rk M

atte

r

TTeru

ki Ka

mo

n

6

Hu

nt fo

r Da

rk M

atte

r

PHEN

O projects continue…

1. SSC was cancelled in 1993

2 paper, 2 WG Reports, 1 Pre-print

2. W

MAP results were out in

2002 8 papers

3. The H

iggs boson was discovered in 2012

10 papers

4. 13-TeV LH

C Run in 2015 C

ounting …

He wanted to listen to m

ost recent results from

both sides at the same conference. This is how

we started

International W

orkshop on

the Interconnection

between Particle

Physics and

Cosmology (PPC).

[2] In

tercon

nectio

n b

etween

…

TTeru

ki Ka

mo

n

7

Hu

nt fo

r Da

rk M

atte

r

“Interconnection” between particles and dark matter

“Num

ber” density (nDM ) ��

�DM

Cross section (�)

SUSY M

asses (at the LHC)

Cosm

olo

gical C

on

nectio

n: �

�� �

�D

M

Teru

ki Ka

mo

n

8

Hu

nt fo

r Da

rk M

atte

r 8

���

��

� � 27%

Interco

nn

ection

betw

een P

article P

hysics a

nd C

osm

olo

gy

PPC 2011 at CERN, June 14-18

PPC 2012 at KIAS, Korea, N

ov. 5-9 PPC 2013 at CETU

P*, SD, U

SA, July 8-13

PPC 2014 at Univ. de Guanajuato, M

exico, June 23-27 PPC 2015 at CETU

P*, SD, U

SA, June 28 - July 3

PPC 2016 at Brazil PPC 2017 at ???

ennrticl

ar

hle

PP

Cs

PPC Cube

TTeru

ki Ka

mo

n

9

Hu

nt fo

r Da

rk M

atte

r

C Cubeeee

CB

S comedy “B

ig Bang T

heory” (Season 1 E

pisode 15)

Ou

treach

: Big B

an

g Th

eory

Teru

ki Ka

mo

n

10

H

un

t for D

ark

Ma

tter

The poster was designed during lunch m

eetings with him…

He was always chasing the signals of m

odels. The story

began with

the Tevatron.

However,

the LH

C changed a landscape of how to search new physics. It is a BIG thinking m

achine.

[3] D

M S

ignals &

ET

Colla

bora

tion

TTeru

ki Ka

mo

n

11

H

un

t for D

ark

Ma

tter

Experimentalist-Theorist (ET) collaboration

helps to solve the “dark matter” puzzle.

Even my daughter was influenced,

and drawing “Texas-style SUSY

hunting” in 2007.

My advisor, Kunitaka Kondo, was sm

iling and exciting, by saying

“Kamon-kun,

there is

an interesting

theory.” It

was “Supersym

metry”.

But I

didn’t pay

attention much

until 1990’s.

1980’s

�Supersym

mtery at Snowm

ass workshop (1982) �

A.H

. Cham

seddine, R.

Arnowitt,

and P.

Nath,

PRL 49

(1982) 970;

R. Arnowitt,

A.H

. Cham

seddine, P.

Nath,

"The Developm

ent of Supergravity Grand Unification: Circa

1982-85", Int. J. Mod. Phys. A

27 (2012) 1230028 �

October 1986: First p-pbar collisions at 1.6 TeV

Teru

ki Ka

mo

n

12

H

un

t for D

ark

Ma

tter

1198

3 ~

198

4

CE

RN

Co

urie

r (Ju

ly/Au

gu

st 20

09

)

19

83

… D

isco

very o

f W’s

19

84

… N

ob

el p

rize to

Ca

rlo R

ub

bia

an

d S

imo

n va

n d

er M

ee

r

13

Te

ruki K

am

on

H

un

t for D

ark

Ma

tter

“… put forward the bold idea to collide beam

s of protons and antiprotons …”

R. Arnowitt and D

. Nanopoulos suggested to search for

“tri-lepton” events as a SUSY signature at the Tevatron.

H. Baer and X

. Tata strongly suggested to look for large tan�� scenarios.

1990’s

�Possible indication of grand unification with M

SSM based on LEP

data: �

The LEP Collaborations, "Electroweak Parameters of the Z Resonance

and the Standard Model, PLB 276 (1992) 247.

�Ugo A

maldi, W

im de Boer, H

ermann Furstenau, "Com

parison of grand unified

theories with

electroweak and

strong coupling

constants measured at LEP," Phys. Lett. B 260 (1991) 447.

�M

y first SUSY analysis (e’s, �’s) at CD

F �

SSC was cancelled (‘93) � D

iTevatron (PRD 50 (1994)

5676) �

Tripler (PLB 505 (2001) 161) �

March 1995: D

iscovery of top quark �

SUGRA

WG at SU

SY+Higgs workshops (’98) �

FERMILA

B-PUB-

00-386-T, hep-ph/0003154) � Letron+Track trigger to enhance

tau-rich final states.

Teru

ki Ka

mo

n

14

H

un

t for D

ark

Ma

tter

TTeru

ki Ka

mo

n

15

H

un

t for D

ark

Ma

tter

Phys. Rev. D

50 (1994) 5676 Lum

inosity vs. Energy

US Rep.(D

-IL 11th D

istrict)

R. Arnowitt and

B. Dutta suggested (i) B

s �� search at

the Tevatron

(2002); (ii)

stau-neutralino coannihilation

search at the LHC (2004).

2000’s

�W

MAP results (2002) �

�DM = 23%

�

Pheno papers (2002, 2006, …)

�M

y first B physics paper at CDF (2004)

�

Decem

ber 2005: Joined CMS

�

June 2007: International Workshop on the

Interconnection between Particle Physics and Cosm

ology (PPC).

�Septem

ber 2008: First Beams in the LH

C �

Novem

ber 2009: LHC’s First 900-GeV pp

Collisions �

My first stau-neutralino paper at CM

S (2013) Te

ruki K

am

on

1

6

Hu

nt fo

r Da

rk M

atte

r

A S

tory o

f Rare B

s Meso

n D

ecay

b �� t

s � t

PLB 538 (2002) 121

Teru

ki Ka

mo

n

17

H

un

t for D

ark

Ma

tter

1st Round Analysis PRL 93 (2004) 032001

First 2-side 90%CL Lim

it

SM Expectation

PRL 93 (2004) 032001 PRL 95 (2005) 221805 PRL 100 (2008) 101802 PRL 107 (2011) 191801 PRD

87 (2013) 072003

PLB 538 (2002) 121

170 pb1 ~ 8.5 x 10

12 collisions

)032001

PLLB538

LB53

2002 �

2013

Teru

ki Ka

mo

n

18

H

un

t for D

ark

Ma

tter

2011.0

7.1

3

PRL 107 (2011) 191802

PRL 107 (2011) 191801

TTeru

ki Ka

mo

n

19

H

un

t for D

ark

Ma

tter

CDF

CMS (7 TeV)

2013.0

9.0

5

TTeru

ki Ka

mo

n

20

H

un

t for D

ark

Ma

tter

Hu

nt

fofoffofr

Da

rkkkkMMMM

atttttttttte

re

r

No H

int of SUSY- I Cry.

PRL 111 (2013) 101804

No hints of SU

SY. SUSY (gluino and 1

st/2nd gen. squarks)

seems to be heavier than ~1.5 TeV.

sts

2010-2

014

A0

�M

arch 2010: First 7-TeV pp collisions

�Decem

ber 2011: 3-sigma evidence for

Higgs boson; no hint of SU

SY �

July 2012: 5-sigma observation; still no

hint of SUSY

�

Sep. 2013: Strong evidence for Bs�����

�

Lightest (?) scalar top quark (stop) �

Compressed chargino/neutralino m

ass spectra

�SU

SY Higgs bosons

�

Connection to the dark matter

Teru

ki Ka

mo

n

21

H

un

t for D

ark

Ma

tter

MMilesto

nes in

200

9-1

0

√

√

Nov 7 (Sat)

Nov 20 (Fri)

Nov 23 (Mon)

√

Nov 30 (Mon)

00:44 am

WR: 1.18 TeV beam

√

��LHC restarts in the middle Feb 2010.

��Start of the long run!

LHC operation ends on Dec 16.

Dec 14 (Sun)

Teru

ki Ka

mo

n

22

H

un

t for D

ark

Ma

tter

7:46 7:46

7:15 7:50

9:11 10:08

12:46 12:33

12:48

12:58

10:13

2010.0

3.3

0: 7

TeV

SSu

ng

hyu

n C

ha

ng

Be

am

1(c.w

.) Be

am

2(c.c.w

.)

33

29

Ge

V

35

00

Ge

V

Teru

ki Ka

mo

n

23

H

un

t for D

ark

Ma

tter

He asked m

e one thing in 2006: “Teruki, how soon ATLA

S and CM

S can publish their first papers after the LHC

turns on?”. I answered: “It will take 2 years”. I was dam

n wrong.

Race to

Disco

ver SU

SY

at 7

TeV

TTeru

ki Ka

mo

n

24

H

un

t for D

ark

Ma

tter

LHC/A

TLAS/CM

STim

eline2008.09.10

First beamcirculations

2009.11.23 First pp collisions at 900 GeV

2010.03.30 First pp collisions at 7 TeV

7-TeV pp program

ended on Oct 29 (Fri)

2011.03.28 PRL 106 (2011) 131802

ATLA

S M

SUGRA

/CMSSM

2011.04.06

PLB 698 (2011) 196 CM

S CM

SSM

2011.06.01 PLB 701 (2011) 186

ATLA

S M

SUGRA

/CMSSM

2011.08.31

JHEP 08 (2011) 155

CMS

CMSSM

Rise of the particle density at (2.36) 7 TeV steeper than in model

predictions. Careful tuning effort of the MC generators is ongoing.

“Transverse Mom

entum and Pseudorapidity D

istributions of Charged H

adrons in pp Collisions at √s = 7TeV”

2010.0

6.1

8 - F

irst 7 T

eV P

RL

TTeru

ki Ka

mo

n

25

H

un

t for D

ark

Ma

tter

Race to

Disco

ver SU

SY

at 7

TeV

TTeru

ki Ka

mo

n

26

H

un

t for D

ark

Ma

tter

LHC/A

TLAS/CM

STim

eline2008.09.10

First beamcirculations

2009.11.23 First pp collisions at 900 GeV

2010.03.30 First pp collisions at 7 TeV

7-TeV pp program

ended on Oct 29 (Fri)

2011.03.28 PRL 106 (2011) 131802

ATLA

S M

SUGRA

/CMSSM

2011.04.06

PLB 698 (2011) 196 CM

S CM

SSM

2011.06.01 PLB 701 (2011) 186

ATLA

S M

SUGRA

/CMSSM

2011.08.31

JHEP 08 (2011) 155

CMS

CMSSM

PRL 106 (2011) 131802 PLB 698 (2011) 196

A S

tory o

f Coan

nih

ilatio

n

TTeru

ki Ka

mo

n

27

H

un

t for D

ark

Ma

tter

March 2004: W

hen the ILC coannihilation "2tau" analysis (last presented at ICH

EP2004; published in PLB 618 (2005) 182) was near complete, we (R. A

rnowitt, B.

Dutta,

T. Kam

on) started

thinking of

a possibility

of detecting

the coannihilation signal in "3tau" at the LH

C. The idea was to capture two �2 0's in the

final state. � PLB 639 (2006) 46; PLB. 649 (2007) 73; PRL 100 (2008) 231802

2004 �

2013

TTeru

ki Ka

mo

n

28

H

un

t for D

ark

Ma

tter

Hu

nt

fofoffofr

Daa

rkkM

er

tea

ttM

No H

int of SUSY- I Cry. But…

CMS: EPJC 73 (2013) 2283

PHEN

O papers:

PLB 639 (2006) 46; PLB. 649 (2007) 73; PRL 100 (2008) 231802

2011.1

2.1

3: P

relimin

ary R

esults

�DD

elive

red

by L

HC

: 5.7

2 fb

1

�R

ec

ord

ed

by C

MS

: 5.2

0 fb

1

(ab

ou

t 92

%)

�H

igh

qu

ality d

ata : 4

.7 fb

1

(~

35

0 trillio

n c

ollisio

ns)

29

Keep in mind they are prelim

inary results; Keep in m

ind they are small num

bers; Keep in m

ind we will run in the next year.

Hu

nt fo

r Da

rk M

atte

r Te

ruki K

am

on

2012.0

7.0

4: A

fter 48

Yea

rs of …

After 48 years of postulate, …

TTeru

ki Ka

mo

n

30

H

un

t for D

ark

Ma

tter

WWh

ere

will m

ore

ne

w p

article

s be

disc

ove

red

?

Ho

w a

bo

ut th

e d

ark

matte

r pa

rticles ?

World

“Disco

very” Map

Sp

in-1

/2 Fe

rmio

ns

qu

ark, c, ��

c, ��

b, to

p,

��

glu

on

W, Z

, h

Sp

in-0

,1 B

oso

ns

m(

� ) � 0

Teru

ki Ka

mo

n

31

H

un

t for D

ark

Ma

tter

�Long-term

Planning

�Now

oVector Boson Fusion [PRD

87 (2013) 035029] o

MonoX

in Nontherm

al DM

Model [PRD

89 (2014) 096009]

�Connection to the dark m

atter?

I hope we see any sign of SUSY before m

y retirement…

2015 a

nd B

eyon

d

Teru

ki Ka

mo

n

32

H

un

t for D

ark

Ma

tter

EEn

ergy Fro

ntier C

hallen

ge

Teru

ki Ka

mo

n

Future Collider

E Tevatron

Precision

LHC

C

llid

Hadron Collider

(�s ) Gluino/Squark M

ass Reach (M)

M/�s

Tevatron (2 TeV) ~400 GeV

0.20 LH

C (8 TeV) ~1.7 TeV

0.21 LH

C (14 TeV) ~2.8 TeV*

0.20* FCC (100 TeV)

~20 TeV* 0.20*

Peter has been putting forward ideas of energy upgrade of the accelerator. Dick was always enjoying with physics

discussion: [1994] 4 TeV p-pbar Collider [2001] 6 TeV p-pbar Collider [2014] The history repeated. H

e is now proposing 100-300 TeV pp Collider. �

Understanding the lim

itations at the LH

C14 will be an important

step for FCC100pp

A 100-TeV collider is

powerful in producing heavy objects.

(*) just use a naïve scaling 33

H

un

t for D

ark

Ma

tter

270 km x $3000/m

= $810M

http://arxiv.org/abs/1402.5973 http://ahttphtt

arxivorg

arxivg//abs/1402

5973/abs//abs

100-3

00 T

eV p

p C

ollid

er

334

P. McIntyre

Hu

nt fo

r Da

rk M

atte

r Te

ruki K

am

on

Peter originally proposed 100-km

collider and seek inputs from B. D

utta, R. Eusebi, TK, and A

. Safonov. We

simply responded “W

hat is the difference?” Peter replied “H

mm

, I was not thinking big enough.”

“Su

persym

metrists, B

eware!”

(submitted to P

hys. Lett. B)

Experim

ental Observation of E

vents with Large M

issing Transverse E

nergy Accom

panied By a Jet or P

hoton(s) in ppbar C

ollisions at /s = 540 GeV

CER

N-EP

/84

-42 29 M

arch 1984

IS S

UP

ER

SYM

ME

TRY FO

UN

D?

CER

N-TH

.3968/84

J. Ellis, SUSY07 H

un

t for D

ark

Ma

tter

Teru

ki Ka

mo

n

35

ME

NUU

~

SP

EC

IAL

S~

*D

ark Energy Pow

er Drink .. $68

-Chef’s choice

-(m

ajor puzzle)

*Dark M

atter Sandwich …

… $27

-N

eutral, long-lived

*Atomic Soup …

……

……

…. $5

- All elements in one

No, S

ir. Bu

t with

n

eutralin

o?

ME

NUU

I am h

un

gry. Can

you m

ake th

e D

M

sand

wich

w

ith

any

Stan

dard

Mod

el particle?

EEpilo

gue: H

un

t for D

M�

Hin

t of D

M

27

$

Teru

ki Ka

mo

n

36

H

un

t for D

ark

Ma

tter

Dk

Mtt

63

6

Discovery of D

ark Matter in 20**?