The Simplest Higgs Portal Dark Matter Model and Its Extensions

The Simplest Higgs Portal
Dark Matter Model and Its Extensions
Xiao-Gang He
NCTS/SJTU
Work with Jusak Tandean
arXiv:1304.6058, PRD88, 013020(2013)
Higgs Portal Workshop
Umass, 05/01/2014
Dark Matter Properties
! Neutral (electric charge =0 and colorless)
! Very weakly interacting, no EM interaction
! Very long lived or absolutely stable
! Hot or warm or cold, prefer cold dark matter (CMD)
! Mass, spin not known
This talk will concentrate on WIMP CMD
Inward Bound
Standard Model of Particles
SU(3) x SU(2) x U(1) None of the SM particles can play the role of DM The discovery of Higgs in 2012
mass is about 126 GeV
The Higgs fit SM very well
The LHC Higgs cannot have invisible
branching ratio larger than 20 ~ 30%!
Constrain Higgs portal Dark Matter models.
The simplest: SM + a real scalar!
The Darkon Model
Thermal production of DM
DM relic density, detection
and DM production at colliders
Status of Direct DM detection
10!39
1
DAMA
!40
10
1
CRESST
CoGeNT
1
SIMPLE
CRESST
CDMS II
10!42
SuperCDMS
1
N
CDMS Si
N
Σel !cm2 "
10!41
Σel !cm2 "
XENON10
TEXONO
EDELWEISS
XENON100
!43
10
10!44
1
CDMS Ge
LUX
10
1
15
mWIMP
20
!GeV"
30
50
There are several indications of light DM of order
10 GeV, DAMA, CoGENT, CRESST, CDSMII…
It is often claimed that Xenon and Lux experiments
rule out these possibilities.
But, the detection is target dependent. If interaction
of DM with proton and neutron are different, Isopin
Violating DM, it may happen that the nuclei-DM
cross section for Xenon is small, but not for other
nuclei.
Low mass DM of order 10 GeV mass is not
completely ruled out!
The Darkon Model SM+D, the simplest Higgs portal model, as a realis8c realiza8on
SM+D: SM3 + a real SM singlet D darkon ﬁeld (plays the role of dark maAer). Sileira&Zee, PLB (1985) D is stable due to a D-‐> -‐ D Z2 symmetry. ASer H develops VEV, there is a term: v DD h. This term is important for annihila8on of D D -‐> h -‐> SM par8cle This term also induce h -‐> DD if DM mass is less than half of the Higgs mass increasing the invisible decay width and make the LHC detec8on harder! $D$is$stable,$but$$can$annihila
$D$is$stable,$but$$can$annihilate$throu
$D$is$stable,$but$$can
$D$is$stable,$but$$can$annihilate$through$h$ex
D is stable, but c
an a
nnihilate t
hrough h exchange
$D$is$stable,$but$$can$annihilate$through
Direct Search
10!39
10!39
DAMA
10!40
DAMA
10!40
CRESST
XENON10
CoGeNT
XENON10
10!41
10!41
SIMPLE
Σel !cm2 "
10!42
SIMPLE
150
10!42
EDELWEISS
300
200
CDMS Si
SuperCDMS
XENON100
EDELWEISS
XENON100
10!43
10!43
CDMS Ge
LUX
10!44
CRESST
CDMS II
N
CDMS Si
SuperCDMS
TEXONO
CoGeNT
CRESST
CDMS II
N
Σel !cm2 "
CRESST
TEXONO
CDMS Ge
LUX
10!44
Tong Li et al, MPLA (2007), PRD(2009); PLB(2010). 10
15
mWIMP
20
30
50
10
15
mD
!GeV"
20
30
50
!GeV"
If dark maAer mass is heavy mD > 300 GeV or around mh/2 no problem for both relic density and direct detec8on. But is small than mh/2, there are problems with direct detec8on and also invisible Higgs decay!
Isospin-conserving DM: data only
Isospin-conserving DM: data & THDM+D
10!37
10!37
CDMS Ge
CDMS Ge
XENON10
CDMS Si
DAMA
CRESST
10!39
Σel !cm2 "
10!38
SIMPLE
CoGeNT
TEXONO
DAMA
CRESST
10!39
SIMPLE
p
N
Σel !cm2 "
10!38
CoGeNT
XENON10
CDMS Si
TEXONO
EDELWEISS
EDELWEISS
CRESST
10!40
CRESST
10!40
SuperCDMS
SuperCDMS
CDMS II
CDMS II
XENON100
XENON100
LUX
10!41
10
15
mWIMP
LUX
20
!GeV"
30
50
10!41
10
15
mD
!GeV"
20
30
50
Dark maAer relic density and direct detec8on allow solu8ons with dark maAer mass less than half of Higgs mass. H -‐> DD allowed. Too large an invisible branching ra8o. This model is out! If the DM mass is indeed small, the model has to be extended!!
To have low DM mass (mD < mh/2), one
must overcome two problems:
1.  Reconcile various DM derect search
constraints? Xeno and Lux exclude all
indications of low DM mass from Dama,
CoGENT, CRESST and CDMSII: Isospin
Violating DM. (Fegn etal, PLB2011)
2.  Avoid too large an invisible decay of
Higgs boson.
More than one Higgs boson.(Cai, Ren &He
PRD2011, Tandean & He, 2011, 2012)
Isospin Violating Dark Matter
Feng etal arxiv:1307.1758
10!39
10!39
DAMA
10!40
XENON10
TEXONO
CoGeNT
XENON10
10!41
CoGeN
10!41
SIMPLE
CDMS II
Σel !cm2 "
CRESST
!42
10
SuperCDMS
10!42
N
CDMS Si
N
Σel !cm2 "
Isospin symmetric
10!40
CRESST
EDELWEISS
XENON100
10!43
10!43
CDMS Ge
LUX
10!44
10!44
10
15
mWIMP
20
30
50
!GeV"
Isospin-conserving DM: data only
Isospin-con
10!37
10!37
CDMS Ge
CD
XENON10
CDMS Si
CoGeNT
DAMA
CRESST
10!39
Σel !cm2 "
10!38
SIMPLE
CoGeN
10!39
p
N
fn/fp = -0.7
Σel !cm2 "
10!38
CDMS Si
TEXONO
EDELWEISS
CRESST
!40
10
10!40
SuperCDMS
CDMS II
XENON100
LUX
10!41
10
15
mWIMP
20
30
50
10!41
!GeV"
IVDM: data only
IVDM
ACFI-T13-05
CP3-Origins-2013-047 DNRF90
LA-UR-13-27904
ining LUX on Isospin-Violating Dark Matter Beyond Leading Ord
NLO
corrections
for
nucleon
couplings
Shining LUX on Isospin-Violating Dark Matter Beyond Leading Order
a
a
a,b
a,c
Vincenzo Cirigliano
,
Michael
L.
Graesser
,
Grigory
Ovanesyan
,
Ian
M.
Shoemaker
Vincenzo Cirigliano , Michael L. Graesser , Grigory Ovanesyan , Ian M. Shoemaker
a
a Theoretical
a Theoretical
a
a,b
a,c
arXiv:1311.5886
Division, Los Alamos National Laboratory, Los Alamos, NM 87545, USA
Division,
Los University
Alamos
National
Laboratory,
Los
Physics Department,
of Massachusetts
Amherst,
Amherst, MA 01003,
USA Alamos, NM 87545, USA
CP
-Origins
and
the
Danish
Institute
for
Advanced
Study,
University
of
Southern
Denmark,
Campusvej
55,
DK-5230 Odense M, Denmark
b Physics Department, University of Massachusetts Amherst,
Amherst, MA 01003, USA
ins and the Danish Institute for Advanced Study, University of Southern Denmark, Campusvej 55, DK-5230 Odense M,
Abstract
Isospin-violating dark matter (IVDM) has been proposed as a viable scenario to reconcile conflicting positive and null
Xe, mX =10
GeV; position
of the minimum of DNLO
GeV;
ls experiments.
=0
results fromXe,
directmdetection
matter
We show that the Benchmark
lowest-order
dark
matter-nucleus
scattering
X =10 dark
E: fnê f p=-1.45, ls=0, lq =-0.1
3 D: fnê f p=0.15, ls=0, lq=-0.025 10Benchmark
-37
rate can receive large and nucleus-dependent corrections at next-to-leading
10-37order (NLO) in the chiral expansion. The
size of these corrections depends on the specific couplings of dark matter to quark flavors and gluons. In general the
LO
-38
10-38
full NLO dark-matter-nucleus cross-section is not adequately described10by
just the zero-energy proton and neutron
NLO:
l
=0
q
couplings. These statements are concretely illustrated in a scenario where the dark matter couples to quarks through
2
-39
-39
=0.1
scalar operators. We find the canonical NLO:
IVDMlqscenario
can reconcile 10the
null XENON and LUX results and 10
the
NLO: lqto
=-0.1
recent CDMS-Si findings provided its couplings
second and third generation quarks either lie on a special line or
-40
10-40
are suppressed. Equally good fits with newNLO:
values
of the neutron-to-proton
coupling ratio are found in the presence10of
lq =-0.025
nonzero heavy quark couplings. CDMS-Si remains in tension with LUX and1XENON10/100 but is not excluded.
s pHcm2L
10
3
s pHcm2L
arXiv:1311.5886v1 [hep-ph] 22 Nov 2013
c
b
10-41
rmin
10-42
5
7 8 9 10
15
20
10-42
5
30
6
X
10-37
n
p
s
q
15
n
10-37
10-38
10-38
10-39
10-39
10-40
7 8 9 10
20
30
X
s pHcm2L
n
6
NLO
10-41
s pHcm2L
DHNL LO
lating dark matter (IVDM) has been proposed as a viable scenario to reconcile conflicting positiv
m direct1detection dark matter experiments. We show that the lowest-order dark matter-nucleus
ceive large and
nucleus-dependent corrections at next-to-leading order (NLO) in the chiral expan
1. Introduction
D
0.1
0
m HGeVL to quark flavors and
m HGeVL
se corrections
depends
on
the
specific
couplings
of
dark
matter
gluons. In g
To date, the dominant component of the matter in the Milky Way has only
been detected
through
Benchmark G: f ê f =-1, l = l =1
Benchmark
F: f ê f =-1,
l =0,itsl gravitational
=0.1
interactions. However, a number of experiments around the world are currently seeking to directly detect this Dark
dark-matter-nucleus
cross-section is not adequately described
just the
an
B particle as itby
A zero-energy proton
C
Matter (DM). The aim is detect the recoil energy deposited by an incident DM
scatters on a nuclear
-1
F quark
target, producing
characteristic spectrum
[1].
These0.01
statements
are aconcretely
illustrated
in a scenario
where the dark matter couples to
At present, the field of DM direct detection is in an uncertain and exciting state with a number of experiments
Esame signals with null observations
finding the
evidence
of such a signal [2,
3], and others
seeming to exclude
these
ators. We find
canonical
IVDM
scenario
can
reconcile
the
null
XENON
and LUX result
[4,
5,
6,
7].
An
apparent
reconciliation
however
may
be
achieved
by
allowing
the
coupling
of
the
DM
to
protons,
f
,
0.001
to di↵er
from its coupling
neutrons, f . Whileto
suchsecond
isospin-violating
Dark
Matter (IVDM)
has been studied
by
MS-Si
findings
provided
itsto couplings
and-2
third
generation
quarks
either lie on a spec
many authors [8, 9, 10], it has become especially intriguing given the latest results from CDMS-Si [11], which are
na¨good
ıvley at odds
withwith
the limits
from XENON100
LUXneutron-to-proton
[7]. For example, the authors of [12]
surveyed many
ssed. Equally
fits
new
values[6]ofandthe
coupling
ratio are found in the pr
di↵erent possible astrophysical and microphysical possibilities for DM and
concluded
that
only
IVDM
or
inelastic
10-4
-3
avy quark
CDMS-Si
remains
tension
with
and
XENON10/100
not exc
down-scattering
the
tension between
and XENON100.
After LUX,
similar
conclusions
-0.10 LUX
-0.05
0.00
0.05 but is 0.10
-2.0couplings.
-1.5 significantly
-1.0 reduce
-0.5
0.0 inCDMS-Si
p
s
q
p
10-40
10-41
10-41
-42
-42
spN = 60 MeV
5 6 a
7 reconciliation
8 9 10
15 of20
30 results, 5
are found in Refs. [13, 14], with “Xenophobic” WIMP couplings still providing
existing
m
HGeVL
X
albeit under increasing pressure.
q
In this paper we study the phenomenological implications of chiral NLO corrections to IVDM in light of the recent
10
r
10
l
6
mX HGeVL
7 8 9 10
15
20
30
10-37
Benchmark A: fnê f p=-0.7, ls= lq =0
Benchmark B: fnê f p=-0.7, ls=0, lq =-0.1
Benchmark C: fnê f p=-0.7, ls=0, lq =0.1
10-37
10-38
10-38
10-39
10-39
10-40
CDMS-Ge
10-39
XEN
10-40
CDMS-Si
10-41
10-42
5
ON
100
s pHcm2L
s pHcm2L
10-38
mX HGeVL
7 8 9 10
15
20
10-40
30
10-42
5
10-41
10-42
10-41
LU
X
6
s pHcm2L
XENON10
6
mX HGeVL
7 8 9 10
15
20
30
10-43
5
6
mX HGeVL
7 8 9 10
15
20
30
Figure 4: Best-fit CDMS-Si (contours at 68% and 90% CL) and XENON/CDMS-Ge/LUX exclusions (at 90 % CL) under di↵ering assumptions
labelled on the top of each panel. In all cases, we have set s = 0 and used central values of the hadronic matrix elements. The left-hand panel
shows the ”conventional” IVDM point, reproducing results found in [13]. The middle and right panel show the same r = 0.7 point with small
amounts of ✓ turned on. Note that for both points the region allowed in the left panel is now excluded.
one of their Ge detectors - T1Z5 - that apparently has the best quality data. We use the efficiencies and total exposure
provided by the supplemental information to [40]. The total exposure of this detector was 35 kg–days. To account for
the finite energy resolution
of the detector, the energy of the nuclear recoil is smeared according to [42] with an energy
p
resolution E = 0.2 E/keV keV [35]. This experiment saw 36 events in their signal region whose origin remains
Two Higgs doublets + Darkon Model
If H is the Higgs mediating DM interacctions, whose
couplings to up and down quarks are different and can lead
to IVDM interaction. ( the role of H and h can be switched)
h is the SM like Higgs. If λh = 0 h does not interacts with
DM, no problem with invisible Higgs decay width. H does
the job fo DM physics!
10!37
CDMS Ge
CoGeNT
DAMA
CRESST
10!39
SIMPLE
p
Σel !cm2 "
10!38
TEXONO
XENON10
CDMS Si
ELWEISS
EDELWEISS
CRESST
!40
10
SuperCDMS
0
SuperCDMS
CDMS II
XENON100
LUX
50
10!41
10
15
mD
20
!GeV"
IVDM: data & THDM+D
30
50
Conclusions
! Dark Matter exists, properties are not known completely.
! There are constraints from direct detections of DM. There are
indications that DM has low mass of order 10 GeV, but
excluded naively by Xenon experiments. One can reconcile
the Xenon data with some of the low mass DM indications, via
Isospin Violating DM.
! The properties of the Higgs boson discovered at the LHC can
put stringent constraints on DM models.
! Possible to construct model to explain the low mass of DM
indicated by the recent CDSMII and consistent with Xenon
data, example: TypeIII 2HDM.

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