Dark Matter Searches Dark Matter Searches

8/6/2019 Dark Matter Searches Dark Matter Searches
1/74
Dark Matter SearchesDark Matter Searches
Katherine FreeseMichigan Center for Theoretical Physics
University of Michigan

2/74

3/74
Vera RubinVera Rubin
Studied rotation curves
of galaxies, and found
that they are FLAT

4/74
95% of the matter in galaxies is95% of the matter in galaxies is
unknown dark matterunknown dark matter Rotation Curves of Galaxies:Rotation Curves of Galaxies:
EXPECTED
FROM STARS
OBSERVED:FLAT ROTATION
CURVE

5/74
Good news: cosmologists
don't need to "invent" newparticle:
Weakly Interacting
Massive Particles
(WIMPS). e.g.,neutralinos
Axions
ma~10-(3-6) eV
arises in Peccei-Quinn
solution to strong-CP
problem

6/74
THE BEGINNINGS OF
DARK MATTERPARTICLE
PHENOMENOLOGY

7/74
Axion detector
(axion to photon conversion)
Pierre Sikivie
PRL 51 (1983) p. 1415

8/74
Axion masses

9/74
Overall status of axion bounds

10/74
The WIMP Miracle
Weakly Interacting Massive Particles are the bestmotivated dark matter candidates, e.g.: LightestSupersymmetric Particles (such as neutralino) are theirown antipartners. Annihilation rate in the early universe
determines the density today. The annihilation rate comes purely from particle physicsand automatically gives the right answer for the relicdensity!
This is the mass fraction of WIMPs today, and givesthe right answer (23%) if the dark matter is weakly
interacting
h2
=
31027
cm3/sec
ann
WIMP mass: GeV 10 TeV

11/74
WIMP Dark Matter
Phenomenology: History Looking for neutrinos (Drukier and Stodolsky)
First paper suggesting direct detection: Goodman and
Witten 1986 Second paper on direct detection: we
(I) took into account WIMP distribution in galaxy and (ii)suggested annual modulation (Drukier, Freese, and
Spergel 1986). A followup paper (Freese, Frieman, Gould 1988)
suggested using annual modulation to pull out signalfrom background. This is how the only current claimfor direct detection was done (DAMA experiment).

12/74
Drukier and Stodolsky
(1984)proposed MeV neutrino detection via elasticscattering off nuclei with 100 eV recoil energy
Andrzej
Drukier
Leo Stodolsky

13/74
GOODMAN AND WITTEN (1986)
turned same approach to DMdetection

14/74
Drukier, Freese, & Spergel (1986)
i) included model for galactic halo,
ii) proposed annual modulation, iii)
SI/SD for various detector elements

15/74

16/74
EXCITING TIMES
We made WIMP proposals twenty years
ago:
It is coming to fruition!
My personal prediction: one of the
anomalous results is right and we will
know very soon.

17/74
LHC-Making DM
Coming Soon(We hope)

18/74
Supersymmetric Particles in LHC Signature: missing energy when SUSY particle is
created and some energy leaves the detector
Problem with identification: degeneracy ofinterpretation
SUSY can be found, but, you still dont know howlong the particle lives: fractions of a second to leavedetector or the age of the universe if it is dark matter
Proof that the dark matter has been found requiresastrophysical particles to be found

19/74
Direct Detection of WIMP dark
matterA WIMP in the Galaxy
travels through our
detectors. It hits a
nucleus, and depositsa tiny amount of
energy. The nucleus
recoils, and we detect
this energy deposit.
Expected Rate: less than one count/kg/day!

20/74
Event rate
dR
dE
=
NT
MT
d
dE
nv f(v, t)d3v
(number of events)/(kg of detector)/(keV of recoil energy)
=
0F2 (q)
2m2
f(v, t)
vd
3v
v> ME/ 22
Spin-independent
Spin-dependent
0=A22
p2
p
0=4
2
Sp
Gp + Sn Gn
2

21/74
From DM Tools Website

22/74
Many claims/hints of WIMPdark matter detection: how
can we be sure?
1) The DAMA annual modulation
2) The HEAT, PAMELA, and ATIC positronexcess
3) Gamma-rays from Galactic Center 4) WMAP Haze
HAS DARK MATTER BEENDISCOVERED?

23/74
The DAMA
AnnualModulation

24/74
DAMA annual modulationDrukier, Freese, and Spergel (PRD 1986);Freese, Frieman, and Gould (PRD 1988)
Data do show a 8 modulation
WIMP interpretation???
Bernabei et al 2003

25/74
DAMA/LIBRA
(April 17,2008)
8 sigma

26/74
Can the positive signal in DAMA
be compatible with null resultsfrom other experiments?
Savage, Gelmini, Gondolo, and Freese, arxiv:0808:3607(see also papers by Hooper and Zurek; Fairbairn and Schwetz;
Chang, Pierce and Weiner 2008)

27/74
Small remaining region at 10 GeV WIMP mass
DAMA: spin independent?
DAMA
XENON
CDMS

28/74
DAMA and
Spin-
dependent
cross sections
Savage, Gelmini,
Gondolo, Freese
0808:3607
Remaining window
around 10 GeV.
Removing SuperK:
WIMP mass
up to 20 GeV
allowed
DAMA
SUPER-K
XENON
CDMS
Hooper and Zurek extended Super-K bounds

29/74
New measurements of Suns
velocity relative to Halo:250 km/sec (not 220 km/sec)
All curves movethe left:
Remaining
window moves to
7-8 GeV at 3
sigma (5-15 for
SD)
CRESST
Savage, Freese, Gondolo, Spolyar 2009

30/74
Low mass window: COUPP,KIMS,
COGENT, PICASSO, CRESST
COUPP

31/74
COUPP bounds (2007)COUPP bounds (2007)

32/74
Preview of UC talks:Preview of UC talks:
COUPP (Eric Dahl, Friday) CoGeNT (Juan Collar, Friday)
Demonstration of acoustic discrimination.
Elimination of wall events. Commissioning of COUPP-60 kg.Commissioning of COUPP-60 kg. New spin-dependent limits (4 kg chamber).New spin-dependent limits (4 kg chamber).
Demonstration of surface event rejection.
First results from runs in Soudan. Prospects forProspects for PPCsPPCs in DM detection and beyond.in DM detection and beyond.

33/74
To reconcile DAMA with null
results from other experiements: Popular theory:

34/74
To reconcile DAMA with null
results of other experiments: Popular theory:

35/74
Direct Detection
In past two years, two orders of magnitudeincrease in sensitivity (the following results not
included in our compatibility study):
(i) CDMS
(ii) XENON-10
(iii) ZEPLIN III
New technology: liquid noble gases
XENON, LUX, XMASS
WARP (argon)
DEAPCLEAN (argon and neon)

36/74
ZEPLIN III (in Boulby mine)
Pink: XENON 10
Black: Zeplin IIIBlue: CDMS II
See talk of N. Smith
Future: ZEPLIN and LUX will join forces in DUSEL
(August 2009
First science run)
Second science
Run to begin
soon weeks

37/74

38/74
Electron recoils
Nuclear Recoils

Dark Matter Searches Dark Matter Searches

Documents

Transcript of Dark Matter Searches Dark Matter Searches

Cryodetector Readout for Dark Matter Searches

Optimized dark matter searches in deep observations of - arXiv

Antimatter and Dark Matter Searches in Space: the PAMELA Space Mission Antimatter and Dark Matter Searches in Space: the PAMELA Space Mission Piergiorgio

1 Dark Matter: Indirect Detection & LHC searches

Novel Searches for Dark Matter with Neutrino Telescopes

Searches for Connections Between Dark Matter and Neutrinos

Searches for Dark Matter with GLAST

Properties for liquid argon scintillation for dark matter searches 1 Properties for liquid argon scintillation for dark matter searches Akira Hitachi* Research Institute for Science

High-Energy Phenomena and Dark Matter Searches in Galaxy ... · PDF file High-Energy Phenomena and Dark Matter Searches in Galaxy Clusters Christoph Pfrommer1 in collaboration with

CRESST to EURECA – Progress with cryogenic dark matter searches

Dark Matter Searches in Space Xin Wu

Univ. Tübingen Present and future Dark Matter searches by HESS · PDF file 2015. 12. 2. · Present and future Dark Matter searches by HESS experiment Hunt for Dark Matter Symposium

COSINUS - Cryogenic Dark Matter searches with NaI · PDF fileCOSINUS - Cryogenic Dark Matter searches with NaI crystals Jochen Schieck Institute of High Energy Physics (HEPHY) of the

Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010

Comparing A ccelerator and direct Dark Matter searches

17 November 2008Carsten Rott - Novel Searches for Dark Matter 1 Novel Searches for Dark Matter Wishlist & Goals

A. Lindner, · PDF file A. Lindner, DESY Dark Matter Searches DESY Summer Student Lecture, 22 July 2011 Axel Lindner | DESY Summer Students 2011 | Dark Stuff | Page 2 Dark Matter Searches

Simultaneous Searches for WIMP Dark Matter and 0- at the

Searches for Particle Dark Matter

Paul Brink- SuperCDMS and GEODM Dark Matter Searches