Seminar slides presenting work on dark matter annihilation into light mediators which subsequently decay in to Standard Model particles. This is motivated by indirect detection signals in gamma rays, such as the recent excess seen in the Fermi Large Area Telescope.

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Flip Tanedo
1
O N - S H E L L
M E D I A T O R S
16 May 2015
arXiv:1404.6528 (PRD), 1503.05919
& W o r k i n P r o g r e s s w i t h C o l l a b o r a t o r s
I N D I R E C T D E T E C T I O N O F D A R K M A T T E R

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2
ANNIHIL
ATION
COLLIDER
DI
RECT DETECTIO
N
Outline0
B
B
B
B
B
B
B
B
@
on shell
1
C
C
C
C
C
C
C
C
A
⇠
3
dm
p
4⇡
0
B
B
B
B
B
@
ave also inserted an explicit factor of
p
4⇡ for the additional phase sp
section of a three- versus two-body final state.
oth (2.5) and (2.6) impose the limit sm ⌧ 1 to suppress the s-channel
fixed (for given masses) to give the correct galactic center photon yi
s addressed in Sec. 4. The limit of a very small coupling to the Sta
vated by the dearth of observational evidence for dark matter intera
t detection experiments. This limit also occurs naturally in models
ng or compositeness. In our scenario, parametrically suppressing this
me of the mediator. This has little phenomenological consequence
Experiments
Simplified Models
Nature
Michelangelo Buonarroti,
“Creation of Adam” (1510)
UV Models

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3
Conventional View of DM Interactions
Exceptions: SIMP Miracle (1402.5143), DMdm (1312.2618), Boosted Dark Matter (1405.7370), …
How Dark Matter talks to the Standard Model
..
χ
.
χ
.
sm
.
sm
..
χ
.
sm
.
χ
.
sm
..
sm
.
sm
.
χ
.
χ
ANNIHIL
ATION
DI
RECT DETECTIO
N
COLLIDER
Ωχh2
Exceptions: e.g. SIMP Miracle (1402.5143); DMdm (1312.2618);
Agashe, Cui, et al. (1405.7370). See talk by Yanou Cui.
Flip Tanedo flip.tanedo@uci.edu Heavy Hidden Hooperon 1404.6528 4/47
4/47
How Dark Matter talks to the Standard Model
..
χ
.
χ
.
sm
.
sm
..
χ
.
sm
.
χ
.
sm
..
sm
.
sm
.
χ
.
χ
ANNIHIL
ATION
DI
RECT DETECTIO
N
COLLIDER
Ωχh2
DirectIndirect Collider

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4
Conventional View of DM Interactions
How Dark Matter talks to the Standard Model
..
χ
.
χ
.
sm
.
sm
..
χ
.
sm
.
χ
.
sm
..
sm
.
sm
.
χ
.
χ
ANNIHIL
ATION
DI
RECT DETECTIO
N
COLLIDER
Ωχh2
Exceptions: e.g. SIMP Miracle (1402.5143); DMdm (1312.2618);
Agashe, Cui, et al. (1405.7370). See talk by Yanou Cui.
Flip Tanedo flip.tanedo@uci.edu Heavy Hidden Hooperon 1404.6528 4/47
4/47
DirectIndirect Collider
CMS HEFTL
XENON100
Ic gm
g5
cM Iq gm g5
qM
L2
1 10 100 1000
10-41
10-40
10-39
10-38
10-37
10-36
10-35
mDM @GeVD
DM-neutroncrosssection@cm2
D
XENON100 limit
stronger
CMS limit
stronger
Region I
Region II
Region III
10 100 1000
10
100
1000
mDM @GeVD
mmed@GeVD
SSO
10-36
10-35
on@cm2
D
CMS limit
Region IBuchmueller et al. 1308.6799; see also Shepherd 1111.2359, etc…
Mono-SM
Mediators
Important

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5
Simplified Models
How Dark Matter talks to the Standard Model
..
χ
.
χ
.
sm
.
sm
..
χ
.
sm
.
χ
.
sm
..
sm
.
sm
.
χ
.
χ
ANNIHIL
ATION
DI
RECT DETECTION COLLIDER
Ωχh2
1 Work inA
ThisiscollectionofusefulsampleFeynman
1WorkinProgress
rather than this… … use this
See, for example: Shepherd et al. (1111.2359), Busoni et al. (1402.1275, 1405.3101),
Buchmueller et al (1308.6799, 1407.8257), Harris et al. (1411.0535), Abdullah et al. (1409.2893), …
sm
smmediator
g
gSM

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Case Study: Fermi 𝝲-ray excess
• Possible indirect detection signal
• There are reasons to be skeptical
We’ll address these soon.
• Framework to play with new ideas
… that can be applied more broadly than any specific signal
Fermi-LAT Collaboration, S. Murgia; 2014 Fermi Symposium
Goodenough & Hooper (0910.2998, 1010.2752), Hooper & Linden (1110.0006),
Abazajian et al. (1011.4275, 1207.6047, 1402.4090), Boyarsky et al. (1012.5839);
Gordon & Macias (1306.5725); Daylan et al. (1402.6703); Calore et al. (1411.4647,
1502.02805); Agrawal et al. (1411.2592); Fermi-LAT collaboration (2014 Symposium)

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COLLIDER
DI
RECT DETECTIO
N
Outline0
B
B
B
B
B
B
B
B
@
on shell
1
C
C
C
C
C
C
C
C
A
⇠
3
dm
p
4⇡
0
B
B
B
B
B
@
ave also inserted an explicit factor of
p
4⇡ for the additional phase sp
section of a three- versus two-body final state.
oth (2.5) and (2.6) impose the limit sm ⌧ 1 to suppress the s-channel
fixed (for given masses) to give the correct galactic center photon yi
s addressed in Sec. 4. The limit of a very small coupling to the Sta
vated by the dearth of observational evidence for dark matter intera
t detection experiments. This limit also occurs naturally in models
ng or compositeness. In our scenario, parametrically suppressing this
me of the mediator. This has little phenomenological consequence
Experiments
Simplified Models
Nature
Michelangelo Buonarroti,
“Creation of Adam” (1510)
ANNIHIL
ATION
UV Models

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Light from Dark Matter
Adapted from D. Zeppenfeld PITP05

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9
Light from Dark Matter
Extracted from Pythia via PPPC4DMID, Cirelli et al. 1012.4515
0.5 1.0 5.0 10.0
10-2
10-1
10-0
Eg @GeVD
µEg
2
dNgêdEg
b
t
m
W
g
40 GeV DM annihilating into SM pairs
spectrum

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Where to look
NASA/JPL-Caltech/ESO/R.Hurt
FERM
I
Lots of DM
~ 8.5 kpc
Also: dwarfs (later); Third Sources (3FGL) Bertoni et al. 1504.02087

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15º
15º
Dark Matter
Galactic Plane
J-factor (astrophysics)
Subtract
J ⇠
Z
dV
1
4⇡r
⇢2
(x)
11
The FERMI Region
FERM
I
Morphology
.
The “Hooperon”
mχ = 40 GeV ..
χ
.
¯χ
.
b
.
¯b
Eb = 40 GeV
fits γ spectrum
10 GeV τ also fits
Overall normalization set by present annihilation rate
⟨σb¯bv⟩ = ..5 ..(1.5) × 10−26
cm3
s−1
..γ =1.12 (1402.4090) ..γ =1.26 (1402.6703) ρ ∼ r−γ
(1 + rα
)
γ−β
α

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Galactic Center Excess, circa 2014
Daylan et al. 1402.6703; Abazajian et al. 1402.4090
Goodenough & Hooper (0910.2998, 1010.2752), Hooper & Linden (1110.0006), Abazajian
et al. (1011.4275, 1207.6047, 1402.4090), Boyarsky et al. (1012.5839); Gordon & Macias
(1306.5725); Daylan et al. (1402.6703) …
FERMI Diffuse BG
FERM
I-m
oleculargasm
ap
(1402.6703) (1402.4090)
All based on Fermi Pass-7 point source background

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Galactic Center Excess today
Fermi-LAT Collaboration, S. Murgia; 2015 Fermi Symposium
Integrated flux in 15ox15o ROI, NFW component
Peaked profiles with long tails (NFW, NFW contracted) yield the most significant improvements in the data-
model agreement for the four variants of the foreground/background models. IC ring 1 contribution ~2-3x
smaller than without additional component and HI ring 1 contribution is ~2-5x larger
➡ The predicted spectrum depends on the foreground/background models.
Calore et al. (1411.4647, 1502.02805); Agrawal et al. (1411.2592); Fermi-LAT
Collaboration (in progress, see Fermi Symposium 2015)
more quantification of systematic uncertainties

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Other Fits
Agrawal et al. 1411.2592 w/ uncertainties from Calore et al. 1409.0042.
hh
W+
W-
tt
bb
ZZ
Xsv=2.2¥10-26
cm3
ês
0 50 100 150 200 250
0
2
4
6
8
10
mc@GeVD
XsvJ@10-26
cm3
êsD
c2 p-val.
hh 28.2 0.17
14
srLD
mc@GeVD
c2 p-val.
hh 28.2 0.17
WW 38.3 0.017
tt 43.5 0.0041
bb 24.2 0.34
ZZ 35.6 0.033
1 10 100
0
2
4
6
8
10
12
14
Eg @GeVD
Eg
2
dNêdEg@10-7
GeVêHcm2
ssrLD
Figure 3: Top: We show the 2 contours, corresponding to 1,2 and 3 , o
hypotheses ! XX for X = {h, W±, Z, t, b}. Vertical dashed lines indicat
for each of these final states. The best fit point in each case is indicated. Bot
the spectra of photons obtained for the corresponding best fit values in the u
central values and the error bars are extracted from [13]. Note that the errors
and the plotted spectra indeed fit the data reasonably well, as indicated by
best fit.
which fits in the envelope between the 4 presented spectra, or one could fit
separately to get a feel for the systematic uncertainty. Here, we take the latt
Out of the 4 spectra Fermi (a,b,c,d) present, one (a) has a shape very di↵
of heavy DM annihilating to electroweak final states. Furthermore, fitting to (
Higgs
bottoms
DM can be heavier
Uncertainties give wiggle
room in final states.
tops
Estimated systematics from
60 diff. emission models
(but smaller than Fermi preliminary)

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Millisecond Pulsars
NASA/CXC/M.Weiss
Accretion
Partner
Star
LMXB to MSP
MSP
Hooper et al. 1010.2752, 1110.0006; Abazajian et al. 1011.4275, 1207.6047 1402.4090
Wharton et al. 1111.4216, Yuan et al. 1404.2318, Mirabal 1309.3248 n.b.: Hooper et al. 1305.0830
MSP Morphology
Degenerate with the
dark matter profile

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The “Hooperon” Goodenough & Hooper (0910.2998, 1010.2752),
Hooper & Linden (1110.0006), Abazajian et al.
(1011.4275, 1207.6047, 1402.4090), Boyarsky et al.
(1012.5839); Gordon & Macias (1306.5725); Daylan et
al. (1402.6703) … .
Hooperon”
= 40 GeV ..
χ
.
¯χ
.
b
.
¯b
Eb = 40 GeV
fits γ spectrum
10 GeV τ also fits
ll normalization set by present annihilation rate
⟨σb¯bv⟩ = ..5 ..(1.5) × 10−26
cm3
s−1
...12 (1402.4090) ..γ =1.26 (1402.6703) ρ ∼ r−γ
(1 + rα
)
γ−β
α
ballpark as thermal relic σ (if s-wave)
ugh & Hooper (0910.2998, 1010.2752), Hooper & Linden (1110.0006), Abazajian et
4275, 1207.6047, 1402.4090), Boyarskiy et al. (1012:5839); Gordon & Macias (1306.5725);
al. (1402.6703). + more recent model building papers
The “Hooperon”
mχ = 40 GeV ..
χ
.
¯χ
.
b
.
¯b
Eb = 40 G
fits γ spect
10 GeV τ als
Overall normalization set by present annihilation rate
⟨σb¯bv⟩ = ..5 ..(1.5) × 10−26
cm3
s−
..γ =1.12 (1402.4090) ..γ =1.26 (1402.6703) ρ ∼ r−γ
(1 + r
Same ballpark as thermal relic σ (if s-wave)
Goodenough & Hooper (0910.2998, 1010.2752), Hooper & Linden (1110.0006), Abaz
al. (1011.4275, 1207.6047, 1402.4090), Boyarskiy et al. (1012:5839); Gordon & Macias
Daylan et al. (1402.6703). + more recent model building papers
.
Flip Tanedo flip.tanedo@uci.edu Heavy Hidden Hooperon 1404.6528
...
.
The “Hooperon”
mχ = 40 GeV ..
χ
.
¯χ
.
b
.
¯b
Eb = 40 GeV
fits γ spectrum
10 GeV τ also fits
Overall normalization set by present annihilation rate
⟨σb¯bv⟩ = ..5 ..(1.5) × 10−26
cm3
s−1
..γ =1.12 (1402.4090) ..γ =1.26 (1402.6703) ρ ∼ r−γ
(1 + rα
)
γ−β
α
Same ballpark as thermal relic σ (if s-wave)
Goodenough & Hooper (0910.2998, 1010.2752), Hooper & Linden (1110.0006), Abazajian et
al. (1011.4275, 1207.6047, 1402.4090), Boyarskiy et al. (1012:5839); Gordon & Macias (1306.5725);
Daylan et al. (1402.6703). + more recent model building papers
.
.
The “Hooperon”
mχ = 40 GeV ..
χ
.
¯χ
.
b
.
¯b
Eb = 40 GeV
fits γ spectrum
10 GeV τ also fits
Overall normalization set by present annihilation rate
⟨σb¯bv⟩ = ..5 ..(1.5) × 10−26
cm3
s−1
..γ =1.12 (1402.4090) ..γ =1.26 (1402.6703) ρ ∼ r−γ
(1 + rα
)
γ−β
α
Same ballpark as thermal relic σ (if s-wave)
Goodenough & Hooper (0910.2998, 1010.2752), Hooper & Linden (1110.0006), Abazajian et
.
ron”
V ..
χ
.
¯χ
.
b
.
¯b
Eb = 40 GeV
fits γ spectrum
10 GeV τ also fits
zation set by present annihilation rate
= ..5 ..(1.5) × 10−26
cm3
s−1
0) ..γ =1.26 (1402.6703) ρ ∼ r−γ
(1 + rα
)
γ−β
α
thermal relic σ (if s-wave)
(0910.2998, 1010.2752), Hooper & Linden (1110.0006), Abazajian et
7, 1402.4090), Boyarskiy et al. (1012:5839); Gordon & Macias (1306.5725);
). + more recent model building papers

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Contact Interactions
Parameterization: UCI 1008.1783; Fit: UCSC 1403.5027
.
Contact Interactions
..Dark Matter . Heavy. sm.
Dirac fermion χ
.
b quark
..
χ
.
¯χ
.
b
.
¯b
. =.
χ
.
¯χ
.
b
.
¯b
DM–SM interaction parameterized by a single coupling Λ−2
.
O =
1
Λ2
(¯χΓχχ) ¯bΓbb
Parameterization in Goodman et al. 1008.1783; see Alves et al. 1403.5027 for Hooperon fit
Flip Tanedo flip.tanedo@uci.edu Heavy Hidden Hooperon 1404.6528 15/47
...
15/47

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18
Decoupled Mediators Disfavored
Requirement: s-wave annihilation
10 1005020 3015 7010-33
10-31
10-29
10-27
10-25
image adapted from Alex Wijangco
LUX SI (D5) bound
thermal relic
XENON100 SD (D8) bound
CMS D5 bound
CMS D8 bound
ruled out
DI
RECT DETECTIO
N
COLLIDER
D2
D4
D5
D6
D7
D8
D9
D10
D12
D14
¯ 5
· ¯qq
¯ 5
· ¯q 5
q
¯ µ
· ¯q µq
¯ µ
5 · ¯q µq
¯ µ
· ¯q µ 5q
¯ µ
5 · ¯q µ 5q
¯ µ⌫
· ¯q µ⌫q
¯ µ⌫
· ¯q µ⌫ 5q
¯ 5 · Gµ⌫Gµ⌫
¯ 5 · Gµ⌫
˜Gµ⌫
CMS 1206.5663, LUX 1310.8214

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19
Decoupled Mediators Disfavored
Requirement: s-wave annihilation
COLLIDER
DI
RECT DETECTIO
N
COLLIDER
D2
D4
D5
D6
D7
D8
D9
D10
D12
D14
¯ 5
· ¯qq
¯ 5
· ¯q 5
q
¯ µ
· ¯q µq
¯ µ
5 · ¯q µq
¯ µ
· ¯q µ 5q
¯ µ
5 · ¯q µ 5q
¯ µ⌫
· ¯q µ⌫q
¯ µ⌫
· ¯q µ⌫ 5q
¯ 5 · Gµ⌫Gµ⌫
¯ 5 · Gµ⌫
˜Gµ⌫
ANNIHIL
ATION
COLLIDER
via D12 & D14
& SM chirality

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20
Suggests non-decoupled mediator
mmed < heavy
act O Exceptions:
orana DM: ¯χγµ
χ = 0
ning of chiral couplings (e.g. Zℓ+
ℓ−
)
n-decoupled mediator: mmed < heavy
..
χ
.
¯χ
.
b
.
¯b
.
Λ−2
. ⇒.
χ
.
χ
.
b
.
¯b
.
λDM
.
λSM

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21
Simplified ModelsSimplified Models
Renormalizable, capture physics of mediator (1105.2838)
..Dark Matter . Mediator. sm.
Dirac fermion χ
.
b quark
.
λSM
.
λDM
.
sm neutral
..
χ
.
χ
.
λDM
.
λSM
Simplest example: Coy Dark Matter
Dolan et al. 1401.6458
Systematic studies:
Chicago 1404.0022
Perimeter 1404.2018
Flip Tanedo flip.tanedo@uci.edu Heavy Hidden Hooperon 1404.6528 18/47
18/47
Simplified Models
Renormalizable, capture physics of mediator (1105.2838)
..Dark Matter . Mediator. sm.
Dirac fermion χ
.
b quark
.
λSM
.
λDM
.
sm neutral
..
χ
.
χ
.
λDM
.
λSM
Simplest example: Coy Dark Matter
Dolan et al. 1401.6458
Systematic studies:
Chicago 1404.0022
Perimeter 1404.2018
Flip Tanedo flip.tanedo@uci.edu Heavy Hidden Hooperon 1404.6528 18/47
18/47
Renormalizable, capture physics of mediator (1105.2838)
Systematic studies:
Chicago:
Perimeter:
1404.0022
1404.2018
Explicit examples
Coy Dark Matter 1401.6458
Boehm, Dolan, et al.
Z’ portal 1501.03490
Alves, Berlin, Profumo, Queiroz

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22
Simplest Simplified Models (off shell)
14
Model
DM Mediator Interactions
Elastic Near Future Reach?
Number Scattering Direct LHC
1 Dirac Fermion Spin-0 ¯ 5
, ¯ff SI ⇠ (q/2m )2
(scalar) No Maybe
1 Majorana Fermion Spin-0 ¯ 5
, ¯ff SI ⇠ (q/2m )2
(scalar) No Maybe
2 Dirac Fermion Spin-0 ¯ 5
, ¯f 5
f SD ⇠ (q2
/4mnm )2
Never Maybe
2 Majorana Fermion Spin-0 ¯ 5
, ¯f 5
f SD ⇠ (q2
/4mnm )2
Never Maybe
3 Dirac Fermion Spin-1 ¯ µ
, ¯b µb SI ⇠ loop (vector) Yes Maybe
4 Dirac Fermion Spin-1 ¯ µ
, ¯f µ
5
f SD ⇠ (q/2mn)2
or
Never Maybe
SD ⇠ (q/2m )2
5 Dirac Fermion Spin-1 ¯ µ 5
, ¯f µ
5
f SD ⇠ 1 Yes Maybe
5 Majorana Fermion Spin-1 ¯ µ 5
, ¯f µ
5
f SD ⇠ 1 Yes Maybe
6 Complex Scalar Spin-0 †
, ¯f 5
f SD ⇠ (q/2mn)2
No Maybe
6 Real Scalar Spin-0 2
, ¯f 5
f SD ⇠ (q/2mn)2
No Maybe
6 Complex Vector Spin-0 B†
µBµ
, ¯f 5
f SD ⇠ (q/2mn)2
No Maybe
6 Real Vector Spin-0 BµBµ
, ¯f 5
f SD ⇠ (q/2mn)2
No Maybe
7 Dirac Fermion Spin-0 (t-ch.) ¯(1 ± 5
)b SI ⇠ loop (vector) Yes Yes
7 Dirac Fermion Spin-1 (t-ch.) ¯ µ
(1 ± 5
)b SI ⇠ loop (vector) Yes Yes
8 Complex Vector Spin-1/2 (t-ch.) X†
µ
µ
(1 ± 5
)b SI ⇠ loop (vector) Yes Yes
8 Real Vector Spin-1/2 (t-ch.) Xµ
µ
(1 ± 5
)b SI ⇠ loop (vector) Yes Yes
TABLE V. A summary of the simplified models identified in our study as capable of generating the observed gamma-
ray excess without violating the constraints from colliders or direct detection experiments. In the last two columns,
we indicate whether the model in question will be within the reach of near future direct detection experiments (LUX,
XENON1T) or of the LHC. Models with an entry of “Never” predict an elastic scattering cross section with nuclei that
Berlin et al. 1404.0022 and Izaguirre et al. 1404.2018 for a detailed survey of off-shell
simplified models. See Boehm et al. 1401.6458 for a prototype.
Berlin et al. 1404.0022
Looks like we’re all done?
Comprehensive study of
s- and t-channel diagrams.

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23
On-Shell mediators
• Can be dominant mode
• Separates λDM from λSM
• Admits λDM ≫ λSM
Simplified Hooperons + on-shell mediators
But: the mmed < heavy regime also includes mmed < mχ
i.e. mediator is accessible as an ..on-shell annihilation mode
..
χ
.
χ
.
b
. b.
b
.
b
.
on shell
• Can be dominant mode
• Separates λDM from λSM
• Admits limit λSM ≪ λDM
• Hides indirect detection signal from
direct det. & collider bounds
Application to Hooperon: FT et al. ..1404.6528 (this talk)
See also Dolan et al. 1404.4977 and Martin et al. 1405.0272
Previously: axion portal (Nomura & Thaler, 0810.5397),
cascade annihilation (+ Mardon, Stolarski 0901.2926)
Flip Tanedo flip.tanedo@uci.edu Heavy Hidden Hooperon 1404.6528
2
The mmed < heavy regime also includes mmed < m 𝝌 where
the mediator is accessible as an on shell annihilation mode
Application to the Hooperon:
FT et al.
Dolan et al
Martin et al.
Elor et al.
1404.6528, 1503.05919
1404.4977
1405.0272
Previously: PAMELA
Axion Portal
Cascades
0810.5397
0901.29261503.01773

24. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
24
On-Shell Simplified ModelsOn-Shell Simplified Models
..Dark Matter . Mediator. sm.
Dirac fermion χ
.
ϕ, V
.
b quark
.
λSM
.
sm neutral
.
λDM
.
sm neutral
..Annihilation, ⟨σv⟩
γ-ray excess, relic abundance
..Constraints
direct detection, colliders
.
Requirements:
mV,ϕ > 2mb λDM ∼ 1 λSM ≪ 1
Flip Tanedo flip.tanedo@uci.edu Heavy Hidden Hooperon 1404.6528 21/47
21/4
.
On-Shell Simplified Models
..Dark Matter . Mediator. sm.
Dirac fermion χ
.
ϕ, V
.
b quark
.
λSM
.
sm neutral
.
λDM
.
sm neutral
..Annihilation, ⟨σv⟩
γ-ray excess, relic abundance
..Constraints
direct detection, colliders
.
Requirements:
mV,ϕ > 2mb λDM ∼ 1 λSM ≪ 1
COLLIDER
DIRECT DETECTIO
N
ANNIHIL
ATION

25. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
25
On-Shell Options .
On-Shell Simplified Options
Require: s-wave annihilation:
. . . .
Med. S (P) V (A) S (P) V (A)
ℓ-Wave p (p) s (s) p (s) p (p)
mχ ≈ 80 GeV ≈ 80 GeV ≈ 120 GeV ≈ 120 GeV
Further Requirements:
2mχ >
⎧
⎪⎨
⎪⎩
2mV for a spin-1 mediator
3mϕ for a spin-0 mediator
.
On-Shell Simplified Options
Require: s-wave annihilation:
. . . .
Med. S (P) V (A) S (P) V (A)
ℓ-Wave p (p) s (s) p (s) p (p)
mχ ≈ 80 GeV ≈ 80 GeV ≈ 120 GeV ≈ 120 GeV
Further Requirements:
2mχ >
⎧
⎪⎨
⎪⎩
2mV for a spin-1 mediator
3mϕ for a spin-0 mediator
22
Require s-wave annihilation
New

26. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
26
Back of the Envelope
m ⇡ n (40 GeV)⇥
h vi ⇡ n ⇥ h vibb
i.e. mediator is accessibl
..
χ
.
χ
.
b
. b.
b
.
b
.
on shell
Application to Hoopero
See also Dolan et al. 1404.49
Previously: axion portal (Nomura &
cascade annihilation (+ Mardon, Stol
Using bb final state as a reference fit
k-of-the-Envelope
dΦ(b, ℓ)
dEγ
=
⟨σv⟩ann
16π
dNγ
dEγ los
dx
ρ
mχ
2
dΦ(b, ℓ)
dEγ
= ..n
⟨σv⟩b¯b
8πm2
χ
..
dNγ
dEγ
..
los
dx ρ2
(rgal (b, ℓ, x))
..Particle Physics
mDM ≈ n×(40 GeV) n=2(3) for spin-1(0)
λDM ≈ 0.35 (1.25) for spin-1(0)
final states requires smaller ⟨σv⟩ann for signal flux
ets injection energy, larger for more final states
flip.tanedo@uci.edu Heavy Hidden Hooperon 1404.6528 24/47
24/47

27. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
27
mc= 80 GeV
mV=15 GeV mV=30 GeV
mV=55 GeV mV=60 GeV
0 20 40 60 80
b Energy @GeVD
mc= 120 GeV
mj=15 GeV
mj=45 GeV
mj=55 GeV
mj=60 GeV
20 40 60 80 100
b Energy @GeVD
mc= 120 GeV
mj=15 GeV
mj=45 GeV
mj=55 GeV
mj=60 GeV
20 40 60 80 100
f Energy @GeVD
Boosted Mediators
change spectrum
of SM primaries,
change spectrum
of secondary γ’s
ominance over off-shell
⎛
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎝
..
on shell
⎞
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎠
∼ λdm
2
≫ . ∼ λdmλsm
⎛
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎝
..
on shell
⎞
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎠
∼
λdm
3
√
4π
≫ . ∼ λdmλsm
edo flip.tanedo@uci.edu Heavy Hidden Hooperon 1404.6528 23/47
23/47
.
ominance over off-shell
⎛
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎝
..
on shell
⎞
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎠
∼ λdm
2
≫ . ∼ λdmλsm
⎛
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎝
..
on shell
⎞
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎠
∼
λdm
3
√
4π
≫ . ∼ λdmλsm
23/47

28. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
28
Spectral Shape
Simona Murgia
Fermi Collaboration
Fermi Symposium ‘14
��� � � �� ��
�� × ��-�
�� × ��-�
�� × ��-�
�� × ��-�
�� × ��-�
������ ������ [���]
����[���/���
/�]
¯ ! V V ! 4b
Factor of 2 on envelope size
= 81 GeV mVm = 39 GeV
FT, Smolinsky
& Rajaraman
arXiv:1503.05919
Plots using FT, “PPPC Machine” tools based on PPPC4DMID by M. Cirelli 1012.4515

29. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
29
Spectral Shape
FT, Smolinsky & Rajaraman arXiv:1503.05919
��� � � �� ��
�� × ��-�
�� × ��-�
�� × ��-�
�� × ��-�
�� × ��-�
������ ������ [���]
����[���/���
/�]
��� � � �� ��
�� × ��-�
�� × ��-�
�� × ��-�
�� × ��-�
�� × ��-�
������ ������ [���]����[���/���
/�]
= 150 GeV mVm = 15 GeV = 150 GeV mVm = 141 GeV
• Boost factor can bend shape!
• Fermi analysis allows heavier DM
See also Calore et al. 1502.02805, Agrawal et al. 1411.2592
Shape is not just a function of SM primary
¯ ! V V ! q¯q ¯ ! V V ! q¯q

30. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
Dominance over off-shell
⎛
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎝
..
on shell
⎞
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎠
∼ λdm
2
≫ .
⎛
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎝
..
on shell
⎞
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎠
∼
λdm
3
√
4π
≫ .
Flip Tanedo flip.tanedo@uci.edu Heavy Hidden Hooperon 1404.6528
...
30
Fit: on-shell vector mediator
Similar for annihilation into light quarks
n.b. vector mediators typically couple flavor universally
(shape fit) (normalization fit).
Dominance over off-shell
⎛
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎝
..
on shell
⎞
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎠
∼ λdm
2
≫ . ∼ λdmλsm
⎛
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎝
..
on shell
⎞
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎠
∼
λdm
3
√
4π
≫ . ∼ λdmλsm
Flip Tanedo flip.tanedo@uci.edu Heavy Hidden Hooperon 1404.6528 23/47
...
23/47
FT, Smolinsky & Rajaraman arXiv:1503.05919

31. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
31
On Shell Vector
⎛
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎝
..
on shell
⎞
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎠
∼
⎛
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎝
..
on shell
⎞
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎠
∼
λ
√
Flip Tanedo flip.tanedo@uci.edu
...
h vitarget = 3 ⇥ 10 26
cm3
/sFT, Smolinsky & Rajaraman arXiv:1503.05919

32. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
32
Fit: on-shell pseudoscalar mediator
Similar for annihilation into light quarks
n.b. scalar mediators typically couple ~ mass
⎛
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎝
..
on shell
⎞
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎠
∼ λdm
2
≫ .
⎛
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎝
..
on shell
⎞
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎠
∼
λdm
3
√
4π
≫ .
Flip Tanedo flip.tanedo@uci.edu Heavy Hidden Hooperon 1404.65
...
Thermal relic doesn’t
seem compatible!
cross section
(shape fit) (normalization fit)
⎛
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎝
..
on shell
⎞
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎠
∼ λdm
2
≫ . ∼ λdmλsm
⎛
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎝
..
on shell
⎞
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎠
∼
λdm
3
√
4π
≫ . ∼ λdmλsm
Flip Tanedo flip.tanedo@uci.edu Heavy Hidden Hooperon 1404.6528 23/47
...
23/47
FT, Smolinsky & Rajaraman arXiv:1503.05919

33. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
33
On Shell Pseudoscalar
on shell
⎛
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎝
..
on shell
⎞
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎠
∼
Flip Tanedo flip.tanedo@uci.edu
...
h vitarget = 3 ⇥ 10 26
cm3
/sFT, Smolinsky & Rajaraman arXiv:1503.05919

34. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
34
Relic Abundanceρ(r) = ρ0
⎛
⎝
r
r0
⎞
⎠
γ
⎛
⎜
⎝1 +
rα
rα
0
⎞
⎟
⎠
γ−β
α
...
¯χ
.
b
.
¯b
⟨σb¯bv⟩ = ..(1.5) ..5 × 10−26
cm3
s−1
.
..γ =1.26 (1402.6703) ..γ =1.12 (1402.4090)
Ballpark of thermal relic σ
.
⟨σv⟩ann. between 3 – 10 ×10−26
cm3
s−1
Vector mediator works for Dirac χ
.
Flip Tanedo flip.tanedo@uci.edu Heavy Hidden Hooperon 1404.6528 36/
...
36/
Works for vector mediator; back of the envelope:
Traditional “Hooperon” (𝝌𝝌 to bb)
.
elic
ballpark for thermal relic (s-wave)
3
/s
Ωχh2
obs.
= 0.12
er ⟨σv⟩:
..
Nγ
Eγ
..
los
dx ρ2
(rgal (b, ℓ, x))
⇒ ⟨σv⟩ann ≈ n⟨σb¯bv⟩

35. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
35
Relic Abundance
Vector mediator can accommodate thermal relic.
.
Spin-0 Mediator as Thermal Relic
Scalar mediator is more difficult,
1. ⟨σv⟩ann = 3 × ⟨σv⟩b¯b
2. p-wave irreducible contributions
..
χ
.
χ
.
on shell
∼
λdm
√
4π
xf
3
..
χ
.
χ
.
on shell
Is there any way to same thermal freeze out?
?
Spin-0 Mediator as Thermal Relic
Scalar mediator is more difficult,
1. ⟨σv⟩ann = 3 × ⟨σv⟩b¯b
2. p-wave irreducible contributions
..
χ
.
χ
.
on shell
∼
λdm
√
4π
xf
3
..
χ
.
χ
.
on shell
Is there any way to same thermal freeze out?
.
pin-0 Mediator as Thermal Relic
Scalar mediator is more difficult,
1. ⟨σv⟩ann = 3 × ⟨σv⟩b¯b
2. p-wave irreducible contributions
..
χ
.
χ
.
on shell
∼
λdm
√
4π
xf
3
..
χ
.
χ
.
on shell
Is there any way to same thermal freeze out?

36. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
36
ANNIHIL
ATION
COLLIDER
DI
RECT DETECTIO
N
Outline0
B
B
B
B
B
B
B
B
@
on shell
1
C
C
C
C
C
C
C
C
A
⇠
3
dm
p
4⇡
0
B
B
B
B
B
@
ave also inserted an explicit factor of
p
4⇡ for the additional phase sp
section of a three- versus two-body final state.
oth (2.5) and (2.6) impose the limit sm ⌧ 1 to suppress the s-channel
fixed (for given masses) to give the correct galactic center photon yi
s addressed in Sec. 4. The limit of a very small coupling to the Sta
vated by the dearth of observational evidence for dark matter intera
t detection experiments. This limit also occurs naturally in models
ng or compositeness. In our scenario, parametrically suppressing this
me of the mediator. This has little phenomenological consequence
Experiments
Simplified Models
Nature
Michelangelo Buonarroti,
“Creation of Adam” (1510)
UV Models

37. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
37
Direct Detection
Pseudoscalar mediator
Spin-dependent interaction
del Nobile et al. 1406.5542, 1307.5955, 1502.07682
dible regions, 99% CL limits
y excess + relic abundance
⇤a⌘ma/
p
gDMg
99%CLDAMAcredibleregions,99%CL
8fgf
[GeV]
roduct
ma/
p
gDMg
edible regions, 99% CL limits
gf = mf /v
By-product
Lint = i
gDM
p
2
a ¯ 5 ig
X
f
gf
p
2
a ¯f 5f
KIMS experiment
Gal. Center & Thermal Relic
del Nobile et al. 1406.5542
Based on non-rel. EFT
Fitzpatrick et al. 1203.3542, 1211.2818, 1308.6288
DI
RECT DETECTIO
N

38. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
38
Collider: mono-b
.
Collider: mono-b
See talk by Tongyan Lin, (1303.6638).
See Daylan et al. 1402.4090 (EFT), Izaguirre et al. 1404.1373 (simplified model). Mono-object
analyses: UCI (1005.1286, 1008.1783, 1108.1196), Fermilab (1005.3757, 1103.0240), others.
λϕ
SM 0.2 λV
SM 0.6
Conservative estimate: mq/M3
∗ → λDMλSMs−1.
Simplified model > EFT: Graesser, Shoemaker, et al. (1107.2666, 1112.5457); UCI (1111.2359);
Busoni et al. (1307.2253); Dolan, et al. (1308.6799).
Flip Tanedo flip.tanedo@uci.edu Heavy Hidden Hooperon 1404.6528 31/47
...
31/47
Lin et al (1303.6638), Daylan et al. 1402.4090 (EFT), Izaguirre et al. 1404.1373 (simplified model).
Mono-object analyses: UCI (1005.1286, 1008.1783, 1108.1196), Fermilab (1005.3757, 1103.0240)
See talk by Tongyan Lin, (1303.6638).
See Daylan et al. 1402.4090 (EFT), Izaguirre et al. 1404.1373 (simplified model). Mono-objec
analyses: UCI (1005.1286, 1008.1783, 1108.1196), Fermilab (1005.3757, 1103.0240), others.
λϕ
SM 0.2 λV
SM 0.6
Conservative estimate: mq/M3
∗ → λDMλSMs−1.
Simplified model > EFT: Graesser, Shoemaker, et al. (1107.2666, 1112.5457); UCI (1111.235
Busoni et al. (1307.2253); Dolan, et al. (1308.6799).
Flip Tanedo flip.tanedo@uci.edu Heavy Hidden Hooperon 1404.6528
...
More recently, simplified model analysis: Harris et al. 1411.0535; Buckley et al. 1410.6497
Linetal.(1303.6638)
COLLIDER

39. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
39
Collider: multi-jet analysis
Buchmueller et al. 1505.07826 (Imperial); based on 1310.4491
(Oxford) and 1203.1662 (FNAL, Razor analysis)
Pseudoscalar mediator
multi-jet + MET
monojet + MET
production by
gluon fusion
ruled out
smallSMcouplingissafe tion terms are
Lint = igDMA¯ 5
+ igSM
X
q
mq
v
A ¯q 5
q ,
where is a Dirac fermion, the sum is over all quark
is the quark mass and v = 246 GeV is the Higgs vac
expectation value. Motivated by the Minimum Fla
Violation hypothesis [60], we assume the couplings o
pseudoscalar to quarks are proportional to mq. This
pling structure implies that the production of A is
inated by gluon fusion. This simple model can ex
the Fermi-LAT excess while remaining consistent
other constraints and is a useful proxy for the stru
found in 2HDM models and in extended 2HDM
have mixing with a singlet-like pseudoscalar (`a la
NMSSM) [61]. We consider gDM ⇠ gSM ⇠ O(1) as a
ticularly interesting benchmark case to compare di↵
tion terms are
Lint = igDMA¯ 5
+ igSM
X
where is a Dirac fermion, the sum
is the quark mass and v = 246 GeV
expectation value. Motivated by t
Violation hypothesis [60], we assum
pseudoscalar to quarks are proporti
pling structure implies that the pro
inated by gluon fusion. This simp
the Fermi-LAT excess while rema
other constraints and is a useful p
found in 2HDM models and in e
have mixing with a singlet-like p
NMSSM) [61]. We consider gDM ⇠
ticularly interesting benchmark cas
searches since couplings of this size

40. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
40
Alternative: search for the mediator
How Dark Matter talks to the Standard Model
..
χ
.
χ
.
sm
.
sm
..
χ
.
sm
.
χ
.
sm
..
sm
.
sm
.
χ
.
χ
ANNIHIL
ATION
DI
RECT DETECTION COLLIDER
Ωχh2
1 Work in
rather than this… … use this
See, for example: Shepherd et al. (1111.2359), Busoni et al. (1402.1275, 1405.3101),
Buchmueller et al (1308.6799, 1407.8257), Harris et al. (1411.0535), Abdullah et al. (1409.2893), …
sm
sm
g
gSM
without this

41. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
41
Constraints on mediator—SM coupling
Carone & Murayama, hep-ph/9411256; Dobrescu & Frugiuele, 1404.3947
hep-ph/9411256
Template:
gauged U(1)B
with O(10) GeV
gauge boson
SM . 1
not very
constrained!

42. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
42
Inclusive diphotons
Work in Progress with I. Galon
[GeV]φ
m
50 55 60 65 70 75 80 85 90
)[pb]γγ→φ→(ppσ95%CLupperlimit
1
1.5
2
2.5
3
3.5
4
4.5
5
γγ=8 TeV,s
0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1
SelectionEfficiency
courtesy of D. Whiteson
COLLIDER
CPYuanetal.RESBOS

43. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
43
ANNIHIL
ATION
COLLIDER
DI
RECT DETECTIO
N
Outline0
B
B
B
B
B
B
B
B
@
on shell
1
C
C
C
C
C
C
C
C
A
⇠
3
dm
p
4⇡
0
B
B
B
B
B
@
ave also inserted an explicit factor of
p
4⇡ for the additional phase sp
section of a three- versus two-body final state.
oth (2.5) and (2.6) impose the limit sm ⌧ 1 to suppress the s-channel
fixed (for given masses) to give the correct galactic center photon yi
s addressed in Sec. 4. The limit of a very small coupling to the Sta
vated by the dearth of observational evidence for dark matter intera
t detection experiments. This limit also occurs naturally in models
ng or compositeness. In our scenario, parametrically suppressing this
me of the mediator. This has little phenomenological consequence
Experiments
Simplified Models
Nature
Michelangelo Buonarroti,
“Creation of Adam” (1510)
UV Models
UV Models Part I

44. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
44
Model BuildingModel Building
Spin-1 Mediator
Prototype is gauged U(1)B, expect universal coupling to quarks.
Exception? ρ-like states in composite Higgs? (Contino et al. 1109.1570)
Spin-0 Mediator
Lϕ-sm =
λuyu
ij
Λ
ϕH · ¯QuR +
λdyd
ij
Λ
ϕ ˜H · ¯QdR +
λℓyℓ
ij
Λ
ϕ ˜H · ¯LℓR
Recent UV completion through ‘Higgs-portal’-portal: Ipek et al. 1404.3716
..Dark Matter .Mediator. Higgs. sm
Exception? χ¯χ → ϕ1ϕ2 is s-wave on-shell (Nomura & Thaler 0810.5397)
See also Agrawal et al. 1404.1373 for flavored DM.
Recently: many studies mapping this to (N)MSSM, 2HDM
See also singlet scalar model, Profumo et al. 1412.1105

45. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
45
Pseudoscalar without the scalar
Work in progress with A. Wijangco and J. Serra
G
HglobalHgauge
H
EW
EM
G
Hgauge
Hoblique
H0
⇠ =
✓
v
f
◆2
Figure 10: Pattern of symmetry breaking. (left, tree level) Strong dynamics breaks G ! Hglobal
pontaneously, while Hgauge ⇢ G is explicitly broken through gauging. The unbroken group H =
Hgauge Hglobal contains the sm electroweak group, SU(2)L ⇥ U(1)Y. (right, loop level) Vacuum
misalignment from sm interactions shifts the unbroken group H ! H0
and breaks the electroweak
group to U(1)EM. The degree of misalignment is parametrized by ⇠, the squared ratio of the ewsb
vev to the G ! H vev. Adapted from [152].
We assume that the sm electroweak group is a subgroup of H = Hgauge [ Hglobal so that it is
gauged and preserved by the strong dynamics. This is shown on the left of Fig. 10. This results
n dim Hgauge transverse gauge bosons and (dim G dim Hglobal) Goldstone bosons. The breaking
G ! Hglobal also breaks some of the gauge group so that there are a total of (dim Hgauge H)
massive gauge bosons and (dim G dim H) ‘uneaten’ massless Goldstones.
Now we address the white elephant of the Higgs interactions—can we bequeath to our Goldstone
bosons the necessary non-derivative interactions to make one of them a realistic Higgs candidate?
This is indeed possible through vacuum misalignment, which we illustrate on the right of Fig. 10.
EM
G
Hgauge
Hoblique
H0
⇠ =
✓
v
f
◆2
(left, tree level) Strong dynamics breaks G ! Hglobal
ly broken through gauging. The unbroken group H =
k group, SU(2)L ⇥ U(1)Y. (right, loop level) Vacuum
Higgs as a pNGB (composite Higgs)
with non-minimal coset
analogy: π0 vs π±
FT, adapted from Nature Physics 7, 23 (2011)

46. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
46
Composite Mediators
Work in progress with A. Wijangco and J. Serra
Higgs as a pNGB (composite Higgs)
with non-minimal coset
Λ Λ Λ
Recent UV completion through ‘Higgs-portal’-portal: Ipek et al. 1404.3716
..Dark Matter .Mediator. Higgs. sm
Exception? χ¯χ → ϕ1ϕ2 is s-wave on-shell (Nomura & Thaler 0810.5397)
See also Agrawal et al. 1404.1373 for flavored DM.
ip Tanedo flip.tanedo@uci.edu Heavy Hidden Hooperon 1404.6528 40/47
40/47
SM singlet
“extra” Goldstone
These interactions are given
by nonlinear sigma model and
are distinct from 2HDM
New Matter
incomplete rep. adds to
global symmetry breaking Connects:
• Dark Matter
• Mediators
• EWSB
No 2HDM required!
different phenomenology
and constraints

47. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
47
Composite Mediators
In Progress; J. Serra, FT, A. Wijangco
���� ��� ����
��-��
���-��
��-��
���� ������� �χ
σ
�
[���
/�]
hvi[cm
3
/s]
preliminary
Fermi Excess
h vi =
3m2
b
2⇡f2
y2
m2
(4m2 m2
⌘)2 + m2
⌘
2
⌘
s
1
m2
b
m2
m⌘ ⇡ y f
m = 50 GeV
f = 500 GeV
partial SO(5)
multiplet

48. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
48
ANNIHIL
ATION
COLLIDER
DI
RECT DETECTIO
N
Outline0
B
B
B
B
B
B
B
B
@
on shell
1
C
C
C
C
C
C
C
C
A
⇠
3
dm
p
4⇡
0
B
B
B
B
B
@
ave also inserted an explicit factor of
p
4⇡ for the additional phase sp
section of a three- versus two-body final state.
oth (2.5) and (2.6) impose the limit sm ⌧ 1 to suppress the s-channel
fixed (for given masses) to give the correct galactic center photon yi
s addressed in Sec. 4. The limit of a very small coupling to the Sta
vated by the dearth of observational evidence for dark matter intera
t detection experiments. This limit also occurs naturally in models
ng or compositeness. In our scenario, parametrically suppressing this
me of the mediator. This has little phenomenological consequence
Experiments
Simplified Models
Nature
Michelangelo Buonarroti,
“Creation of Adam” (1510)
UV Models

49. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
49
Dwarf Bounds from FERMI
1503.02632 (Fermi + DES candidates)
only a sketch
ANNIHIL
ATION
possibly a problem
model building?
Reticulum II?
Hooper & Linden (1503.06209)
Agrawal
et al. (2014)

50. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
50
Anti-protons
See also Park et al. 1404.3741; Bringmann et al. 1406.6027
Einasto MIN
Einasto MAX
AMS-02 sensitivity
10
-22
10
-23
10
-24
10
-25
10
-26
10
-27
10 50 100 500
thermal relic
PAMELA bounds
Einasto MED[cm3
/ s]
adapted from 1301.7079
Antiproton Flux Constraints
PAMELA p+ bounds:
currently not constraining.
Maybe AMS-02...
... but large propagation
uncertainty, still lots of
wiggle room.
ANNIHIL
ATION
Cirelli & Giesen

51. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
51
Anti-protons
See also Park et al. 1404.3741; Bringmann et al. 1406.6027
Einasto MIN
Einasto MAX
AMS-02 sensitivity
10
-22
10
-23
10
-24
10
-25
10
-26
10
-27
10 50 100 500
thermal relic
PAMELA bounds
Einasto MED[cm3
/ s]
adapted from 1301.7079
Antiproton Flux Constraints
AMS-02: b quark mode
more constrained
... but large propagation
uncertainty, still lots of
wiggle room.
ANNIHIL
ATION
Model our way out of this?
Giesen et al.
1504.04276
“eyeballed” uncertainty
stronger at low masses:
accounted for solar
modulation effects

52. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
52
ANNIHIL
ATION
COLLIDER
DI
RECT DETECTIO
N
Outline0
B
B
B
B
B
B
B
B
@
on shell
1
C
C
C
C
C
C
C
C
A
⇠
3
dm
p
4⇡
0
B
B
B
B
B
@
ave also inserted an explicit factor of
p
4⇡ for the additional phase sp
section of a three- versus two-body final state.
oth (2.5) and (2.6) impose the limit sm ⌧ 1 to suppress the s-channel
fixed (for given masses) to give the correct galactic center photon yi
s addressed in Sec. 4. The limit of a very small coupling to the Sta
vated by the dearth of observational evidence for dark matter intera
t detection experiments. This limit also occurs naturally in models
ng or compositeness. In our scenario, parametrically suppressing this
me of the mediator. This has little phenomenological consequence
Experiments
Simplified Models
Nature
Michelangelo Buonarroti,
“Creation of Adam” (1510)
UV Models
UV Models Part II

53. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
53
Avoiding the Dwarf Bounds
Kaplinghat, Linden, Yu, 1501.03507
Dwarf Spheroidals: mostly DM, little stellar matter
… so should to see same GeV excess as Gal. Center if it’s DM annihilation
Usual assumption:
Dark Matter Annihilation 𝛾-ray photons
Instead, revise the relation:
Dark Matter Annihilation 𝛾-ray photons
+ ambient starlight
But: requires annihilation into electrons … spectrum doesn’t fit?

54. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
54
Avoiding Dwarf Bounds
Kaplinghat, Linden, Yu, 1501.03507
Photon spectrum from
FSR doesn’t fit
(Weiszacker-Williams)
2
Ê
Ê
Ê
Ê
Ê
Ê
Ê
Ê
Ê
Ê
Ê
Ê
Ê
Ê
Ê
Ê
Ê
Ê
Ê
Ê
Ê
Ê
Ê
Inverse Compton+FSR
FSR HpromptL
0.3 0.5 1 3 5 10 30 50
0
2
4
6
8
E HGeVL
E2
dNêdEH10-6
GeV2
êcm2
êsêsrêGeVL
FIG. 1. -ray spectrum from Inverse Compton emission and
final state radiation produced by annihilation of a 50 GeV
dark matter particle through a light mediator into e+
e fi-
nal state. The spectrum is compared to the Galactic Center
excess [10].
of the dark matter mass, as it absent for masses closer to
But: this leaves an imprint on positron fraction (AMS-02)
and can be constrained by mono-photon searches at LEP
Inverse Compton can
upscatter starlight into a
diffuse GeV spectrum
2 Upscatter
e
e
star
(GeV)
Bonus: self-interacting dark matter

55. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
55
Flavor Violating Modes
Work in Progress with I. Galon; FT, Smolinsky & Rajaraman arXiv:1503.05919
¯ ! ¯tc
m
Consider: lepton-flavor-violating decay of 𝜑
• 𝜑 into eμ smears out e+ spectrum, avoids bumps?
• Also helps avoid collider, (g-2), etc. bounds
• Achieve: SIDM, Galactic Center, avoid Dwarfs
• Froggat-Nielsen mechanism
• No direct detection
Also: quark flavor decays
• top — charm mode is
accessible
COLLIDER
ANNIHIL
ATION
DI
RECT DETECTIO
N
Agrawal et al. 1405.6709, 1404.1373, 1402.7369

56. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
56
Flavor Violating Modes
Work in Progress with I. Galon and A. Kwa
Preliminary: thermal relic cross sections
¯ ! ⌧ ¯⌧
¯ ! b¯b
¯ ! (' ! ⌧µ)2
⌧
µ
⌧
µ
'
'
3 Mediator Decays
'
e
⌫µ
⌫e
e
µ
CPV
in dark

57. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
100
101
102
E [GeV]
100
101
102
E3
J(E)[GeV2
m2
s1
sr1
]
AMS e bound
AMS e+
bound
PAMELA e+
bound
! 3 ! 3(µe), m =2 GeV
! ee, m =50 GeV
m =20 GeV
m =30 GeV
m =40 GeV
m =50 GeV
m =60 GeV
m =70 GeV
m =80 GeV
m =90 GeV
m =100 GeV
! ⌧µ, Benchmark 1
! ⌧µ, Benchmark 2
57
LFV mediators vs. positrons
Work in Progress with I. Galon and A. Kwa (UCI)
preliminary
1501.03507
Kaplinghat et al.
m = 50 GeV
mV = 50 MeV
V ! e+
e

58. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
58
Avoiding anti-protons
1. Upscattered starlight (c.f. avoiding dwarf bounds)
2. Mediator decays to light mesons, not protons
Liu, Weiner, Xue (1412.1485)
quark couplings, but mmed < ΛQCD
Simplified model + chiral Lagrangian.
4 Loop Diagrams
g
g
5 Pion heuristic
⇡
⇡
'
Analogous to very light Higgs
in Higgs Hunter’s Guide

59. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
59
Summary⎛
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎝
..
on shell
⎞
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎠
∼ λdm
2
≫ . ∼ λdmλ
⎛
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎝
..
on shell
⎞
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎠
∼
λdm
3
√
4π
≫ . ∼ λdmλ
Flip Tanedo flip.tanedo@uci.edu Heavy Hidden Hooperon 1404.6528
...
Dominance over off-shell
⎛
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎝
..
on shell
⎞
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎠
∼ λdm
2
≫ . ∼ λdm
⎛
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎜
⎝
..
on shell
⎞
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎟
⎠
∼
λdm
3
√
4π
≫ . ∼ λdm
Flip Tanedo flip.tanedo@uci.edu Heavy Hidden Hooperon 1404.6528
...
This is collection of useful sample Feynman diagrams and pieces ty
1 Work in Progress
Thisi
1Wo
mediator
g
gSM
ANNIHIL
ATION
COLLIDERDI
RECT DETECTIO
N
Department o
This is collection of
1 Work in Pr
µ
e
��� � � �� ��
�� × ��-�
�� × ��-�
�� × ��-�
�� × ��-�
�� × ��-�
������ ������ [���]
����[���/���
/�]
Sample Feynm
Vol. I: Simple
Department of Physics & Ast
This is collection of useful sample
1 Work in Progress
LFV
χral
spectrum
𝛾𝛾+j
Not
2HDM
4 Loop Diagrams
g
g
5 Pion heuristic
⇡
⇡
'

60. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
60
ANNIHIL
ATION
COLLIDER
DI
RECT DETECTIO
N
0
B
B
B
B
B
B
B
B
@
on shell
1
C
C
C
C
C
C
C
C
A
⇠
3
dm
p
4⇡
0
B
B
B
B
B
@
ave also inserted an explicit factor of
p
4⇡ for the additional phase sp
section of a three- versus two-body final state.
oth (2.5) and (2.6) impose the limit sm ⌧ 1 to suppress the s-channel
fixed (for given masses) to give the correct galactic center photon yi
s addressed in Sec. 4. The limit of a very small coupling to the Sta
vated by the dearth of observational evidence for dark matter intera
t detection experiments. This limit also occurs naturally in models
ng or compositeness. In our scenario, parametrically suppressing this
me of the mediator. This has little phenomenological consequence
UV Models
Experiments
Simplified Models
Nature
Michelangelo Buonarroti,
“Creation of Adam” (1510)
Thanks!

61. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
61
CCW v. FERMI
mc@GeVD
c2 p-val.
hh 28.2 0.17
WW 38.3 0.017
tt 43.5 0.0041
bb 24.2 0.34
ZZ 35.6 0.033
1 10 100
0
2
4
6
8
10
12
14
Eg @GeVD
Eg
2
dNêdEg@10-7
GeVêHcm2
ssrLD
Figure 3: Top: We show the 2 contours, corresponding to 1,2 and 3 , ob
hypotheses ! XX for X = {h, W±, Z, t, b}. Vertical dashed lines indicate
for each of these final states. The best fit point in each case is indicated. Bot
the spectra of photons obtained for the corresponding best fit values in the up
central values and the error bars are extracted from [13]. Note that the errors
and the plotted spectra indeed fit the data reasonably well, as indicated by
best fit.
which fits in the envelope between the 4 presented spectra, or one could fit
separately to get a feel for the systematic uncertainty. Here, we take the latte
Out of the 4 spectra Fermi (a,b,c,d) present, one (a) has a shape very di↵e
of heavy DM annihilating to electroweak final states. Furthermore, fitting to (a
Agrawal et al. 1411.2592
w/ uncertainties from
Calore et al. 1409.0042.
Simona Murgia
Fermi Collaboration
Fermi Symposium ‘14

62. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
62
Self-Interacting Dark Matter
Tulin et al. 1302.3898
This framework contains all the pieces for SIDM
See talk by Ian Shoemaker.
Ê
Ê
Ê Ê
Ê
Ê Ê
Ê
Ê
Ê
Ê
4q, mc=2
2b
GCE
4g, mc=2
0.5 1
10-8
10-7
Eg HGeVL
E2
dNgêdEgHGeVcm-2
s-1
L
mV = 1 GeV, preliminary only
Non-trivial fit: small scale structure sets mV light and m
dNγ/dEγ is more subtle near mV ∼ ΛQCD. ✭✭✭✭✭✭✭✭✭
Work in progress with Hai-Bo Yu.
Free feature: e final state allows
very light mediator, natural for
self-interactions.
Long range self-interactions can
address small scale structure
anomalies (e.g. core vs. cusp).
Open question: SIDM target
space for pseudoscalars, which
generate a singular potential.
Bellazzini, Cliche, FT 1307.1129
This is collection of useful sample Feynman diagrams and pieces typeset in Tik
1 Work in Progress

63. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
63
Decoupled Mediators Disfavored
Requirement: s-wave annihilation
D2
D4
D5
D6
D7
D8
D9
D10
D12
D14
¯ 5
· ¯qq
¯ 5
· ¯q 5
q
¯ µ
· ¯q µq
¯ µ
5 · ¯q µq
¯ µ
· ¯q µ 5q
¯ µ
5 · ¯q µ 5q
¯ µ⌫
· ¯q µ⌫q
¯ µ⌫
· ¯q µ⌫ 5q
¯ 5 · Gµ⌫Gµ⌫
¯ 5 · Gµ⌫
˜Gµ⌫
CMS 1206.5663, LUX 1310.8214

64. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
64
Decoupled Mediators Disfavored
Requirement: s-wave annihilation
D2
D4
D5
D6
D7
D8
D9
D10
D12
D14
¯ 5
· ¯qq
¯ 5
· ¯q 5
q
¯ µ
· ¯q µq
¯ µ
5 · ¯q µq
¯ µ
· ¯q µ 5q
¯ µ
5 · ¯q µ 5q
¯ µ⌫
· ¯q µ⌫q
¯ µ⌫
· ¯q µ⌫ 5q
¯ 5 · Gµ⌫Gµ⌫
¯ 5 · Gµ⌫
˜Gµ⌫
Ignore spin-2 mediators
… even heavy ones

65. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
65
Decoupled Mediators Disfavored
Requirement: s-wave annihilation
10 1005020 3015 7010-33
10-31
10-29
10-27
10-25
image adapted from Alex Wijangco
LUX SI (D5) bound
thermal relic
XENON100 SD (D8) bound
CMS D5 bound
CMS D8 bound
ruled out
DI
RECT DETECTIO
N
COLLIDER
D2
D4
D5
D6
D7
D8
D9
D10
D12
D14
¯ 5
· ¯qq
¯ 5
· ¯q 5
q
¯ µ
· ¯q µq
¯ µ
5 · ¯q µq
¯ µ
· ¯q µ 5q
¯ µ
5 · ¯q µ 5q
¯ µ⌫
· ¯q µ⌫q
¯ µ⌫
· ¯q µ⌫ 5q
¯ 5 · Gµ⌫Gµ⌫
¯ 5 · Gµ⌫
˜Gµ⌫
CMS 1206.5663, LUX 1310.8214

66. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
66
Decoupled Mediators Disfavored
Requirement: s-wave annihilation
D2
D4
D5
D6
D7
D8
D9
D10
D12
D14
¯ 5
· ¯qq
¯ 5
· ¯q 5
q
¯ µ
· ¯q µq
¯ µ
5 · ¯q µq
¯ µ
· ¯q µ 5q
¯ µ
5 · ¯q µ 5q
¯ µ⌫
· ¯q µ⌫q
¯ µ⌫
· ¯q µ⌫ 5q
¯ 5 · Gµ⌫Gµ⌫
¯ 5 · Gµ⌫
˜Gµ⌫
Chiral SM Couplings
e.g. we expect D5 & D7 to
have same order couplings
¯q µ 5q ⇢ ¯q µ
PL,Rq

67. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
67
Decoupled Mediators Disfavored
Requirement: s-wave annihilation
D2
D4
D5
D6
D7
D8
D9
D10
D12
D14
¯ 5
· ¯qq
¯ 5
· ¯q 5
q
¯ µ
· ¯q µq
¯ µ
5 · ¯q µq
¯ µ
· ¯q µ 5q
¯ µ
5 · ¯q µ 5q
¯ µ⌫
· ¯q µ⌫q
¯ µ⌫
· ¯q µ⌫ 5q
¯ 5 · Gµ⌫Gµ⌫
¯ 5 · Gµ⌫
˜Gµ⌫
doesn’t seem to fit
gluon spectrum
¯ ! gg
Alves, Profumo, Quieroz, Shepherd, “The Effective Hooperon” (1403.5027)
ANNIHIL
ATION
COLLIDER

68. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
68
Decoupled Mediators Disfavored
Requirement: s-wave annihilation
D2
D4
D5
D6
D7
D8
D9
D10
D12
D14
¯ 5
· ¯qq
¯ 5
· ¯q 5
q
¯ µ
· ¯q µq
¯ µ
5 · ¯q µq
¯ µ
· ¯q µ 5q
¯ µ
5 · ¯q µ 5q
¯ µ⌫
· ¯q µ⌫q
¯ µ⌫
· ¯q µ⌫ 5q
¯ 5 · Gµ⌫Gµ⌫
¯ 5 · Gµ⌫
˜Gµ⌫
Alves, Profumo, Quieroz, Shepherd, “The Effective Hooperon” (1403.5027)
looks okay?

69. flip . ta nedo 60uci . ed u@ ON SHELL MEDIATORS
69
Decoupled Mediators Disfavored
Requirement: s-wave annihilation
`1 q2
3 Loop Diagrams
g
g
D2
D4
D5
D6
D7
D8
D9
D10
D12
D14
¯ 5
· ¯qq
¯ 5
· ¯q 5
q
¯ µ
· ¯q µq
¯ µ
5 · ¯q µq
¯ µ
· ¯q µ 5q
¯ µ
5 · ¯q µ 5q
¯ µ⌫
· ¯q µ⌫q
¯ µ⌫
· ¯q µ⌫ 5q
¯ 5 · Gµ⌫Gµ⌫
¯ 5 · Gµ⌫
˜Gµ⌫
Alves, Profumo, Quieroz, Shepherd, “The Effective Hooperon” (1403.5027)