Camilo Garcia Cely, ULBCamilo Garcia Cely, ULB lines from Dark Matter Neutrinos are similar to...
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Neutrino lines from Dark Matter Camilo Garcia Cely, ULB The 13th International Workshop on the Dark Side of the Universe Daejeon, Korea July 11th, 2017 In collaboration with Chaimae El Aisati, Thomas Hambye, Julian Heeck and Laurent Vanderheyden. Based on arXiv:1706.06600 and JCAP 1703 (2017) no.03, 054
Transcript of Camilo Garcia Cely, ULBCamilo Garcia Cely, ULB lines from Dark Matter Neutrinos are similar to...
Neutrino lines from Dark Matter
Camilo Garcia Cely, ULB
The 13th International Workshop on the Dark Side of the UniverseDaejeon, Korea
July 11th, 2017
In collaboration with Chaimae El Aisati, Thomas Hambye, Julian Heeck andLaurent Vanderheyden.
Based on arXiv:1706.06600 and JCAP 1703 (2017) no.03, 054
Outline
Motivation: why neutrino lines?
Part I: neutrino lines from annihilating dark matter
Part II: neutrino lines from the decay of Majoron dark matter
Camilo Garcia Cely, ULB ν lines from Dark Matter
Indirect detection of DM with photon lines
HESS collaboration 2013
Camilo Garcia Cely, ULB ν lines from Dark Matter
One looks for DMDM→ γγ.
Photons point to the place where theycome from.
Monochromatic photons (lines) standout of the featureless astrophysicalbackground.
Indirect detection of DM with photon lines
HESS collaboration 2013
Camilo Garcia Cely, ULB ν lines from Dark Matter
One looks for DMDM→ γγ.
Photons point to the place where theycome from.
Monochromatic photons (lines) standout of the featureless astrophysicalbackground.
Dark matter indirect searches with neutrino lines
IceCube observations will improve these limits in the near future.
El Aisati, CGC, Hambye, Vanderheyden, 2017
Camilo Garcia Cely, ULB ν lines from Dark Matter
Neutrinos are similar to photons. They point to the direction where theywere produced.
With current resolutions, neutrino lines can be disentangled from theatmospheric and astrophysical background.
MILKY WAYNFW
Unitarity
Lim
it
IceCube 2014
IceCube 2016
Antares IceCubeHLine-orientedL
HESS HΝΤL
100 101 10210-24
10-23
10-22
10-21
mDM HTeVL
Σv
Hcm3
�sL
Dark matter indirect searches with neutrino lines
IceCube observations will improve these limits in the near future.
El Aisati, CGC, Hambye, Vanderheyden, 2017
Camilo Garcia Cely, ULB ν lines from Dark Matter
Neutrinos are similar to photons. They point to the direction where theywere produced.
With current resolutions, neutrino lines can be disentangled from theatmospheric and astrophysical background.
MILKY WAYNFW
Unitarity
Lim
it
IceCube 2014
IceCube 2016
Antares IceCubeHLine-orientedL
HESS HΝΤL
100 101 10210-24
10-23
10-22
10-21
mDM HTeVL
Σv
Hcm3
�sL
Dark matter indirect searches with neutrino lines
IceCube observations will improve these limits in the near future.El Aisati, CGC, Hambye, Vanderheyden, 2017
Camilo Garcia Cely, ULB ν lines from Dark Matter
Neutrinos are similar to photons. They point to the direction where theywere produced.
With current resolutions, neutrino lines can be disentangled from theatmospheric and astrophysical background.
MILKY WAYNFW
Unitarity
Lim
it
IceCube 2014
IceCube 2016
Antares IceCubeHLine-orientedL
HESS HΝΤL
100 101 10210-24
10-23
10-22
10-21
mDM HTeVL
Σv
Hcm3
�sL
Dark matter indirect searches with neutrino lines
What sort of models can be probed in the near future?
Question partially addressed. Lindner, Merle, Niro, 2010.
Consider simple models where the annihilation into neutrinosfixes the freeze-out process: σv ∼ 3× 10−26 cm3/s in theEarly Universe.
Calculate the Sommerfeld effect and see what are the neutrinoindirect detection prospects.
Hisano et al, 2004
In practice, this means that today σv � 3× 10−26 cm3/s.
ICamilo Garcia Cely, ULB ν lines from Dark Matter
Annihilation into into neutrino lines
Final state νν
Lepton Number Hypercharge Angular Momentum J
0 0 ≥ 1
Annihilations are p-wave suppressed for scalar or MajoronaDM: σv � 3× 10−26 cm3/s.
The simplest possibility is Dirac DM.
Final state νν
Lepton Number Hypercharge Angular Momentum J
2 2 ≥ 0
At the TeV scale, it requires a DM particle with hypercharge
Too large neutrino masses might be induced by the sameprocess leading to DM annihilations.
Camilo Garcia Cely, ULB ν lines from Dark Matter
Annihilation into into neutrino lines
Final state νν
Lepton Number Hypercharge Angular Momentum J
0 0 ≥ 1
Annihilations are p-wave suppressed for scalar or MajoronaDM: σv � 3× 10−26 cm3/s.
The simplest possibility is Dirac DM.
Final state νν
Lepton Number Hypercharge Angular Momentum J
2 2 ≥ 0
At the TeV scale, it requires a DM particle with hypercharge
Too large neutrino masses might be induced by the sameprocess leading to DM annihilations.
Camilo Garcia Cely, ULB ν lines from Dark Matter
Annihilation into into neutrino lines
Final state νν
Lepton Number Hypercharge Angular Momentum J
0 0 ≥ 1
Annihilations are p-wave suppressed for scalar or MajoronaDM: σv � 3× 10−26 cm3/s.
The simplest possibility is Dirac DM.
Final state νν
Lepton Number Hypercharge Angular Momentum J
2 2 ≥ 0
At the TeV scale, it requires a DM particle with hypercharge
Too large neutrino masses might be induced by the sameprocess leading to DM annihilations.
Camilo Garcia Cely, ULB ν lines from Dark Matter
Classification of simple models
Camilo Garcia Cely, ULB ν lines from Dark Matter
AnnihilationDM Mediator
mν OK Suppressed`+`− Model
Channel at 1-loop? by vEW/mDM?
DMDM→ νν Dirac
T0 s-chann. vector S
Yes No =
F1T0 t-chann. scalar D F2S s-chann. vector S F3S t-chann. scalar D F4
DMDM→ νν
Real Scalar
D s-chann. scalar T2 ± No
/
Sr1
S
t-chann. Majorana
D
No
Yes Sr2
D S No Sr3
D T0 No Sr4
D T2 Yes Sr5
T0 D Yes Sr6
T2 D Yes Sr7
Majorana
D s-chann. scalar T2 ± No Fm1
S
t-chann. scalar
D
No
Yes Fm2
D S No Fm3
D T0 No Fm4
D T2 Yes Fm5
T0 D Yes Fm6
T2 D Yes Fm7
Complex ScalarS
t-chann. MajoranaD
Yes YesS1
T0 D S2
DiracS
t-chann. scalarD
Yes YesF4
T0 D F2El Aisati, CGC, Hambye, Vanderheyden, 2017
Two benchmark models
Model F1: Dirac DM coupled to a heavier Z ′
We want Sommerfeld effect → Take DM in a triplet with Y = 0.DM∈ T0
DM ∈ T0
ν
ν
Z ′
Model S r1 : Scalar DM coupled to a scalar triplet with Y = 2.
We want Sommerfeld effect → Take DM as an Inert Higgs.
DM∈ D
DM∈ D
ν
ν
T2
Type-II seesaw mechanism → Neutrino masses at tree level.
El Aisati, CGC, Hambye, Vanderheyden, 2017
Camilo Garcia Cely, ULB ν lines from Dark Matter
Two benchmark models
Model F1: Dirac DM coupled to a heavier Z ′
We want Sommerfeld effect → Take DM in a triplet with Y = 0.DM∈ T0
DM ∈ T0
ν
ν
Z ′
Model S r1 : Scalar DM coupled to a scalar triplet with Y = 2.
We want Sommerfeld effect → Take DM as an Inert Higgs.
DM∈ D
DM∈ D
ν
ν
T2
Type-II seesaw mechanism → Neutrino masses at tree level.
El Aisati, CGC, Hambye, Vanderheyden, 2017
Camilo Garcia Cely, ULB ν lines from Dark Matter
Two benchmark models
Model F1: Dirac DM coupled to a heavier Z ′
We want Sommerfeld effect → Take DM in a triplet with Y = 0.DM∈ T0
DM ∈ T0
ν
ν
Z ′
Model S r1 : Scalar DM coupled to a scalar triplet with Y = 2.
We want Sommerfeld effect → Take DM as an Inert Higgs.
DM∈ D
DM∈ D
ν
ν
T2
Type-II seesaw mechanism → Neutrino masses at tree level.
El Aisati, CGC, Hambye, Vanderheyden, 2017
Camilo Garcia Cely, ULB ν lines from Dark Matter
Two benchmark models
Model F1: Dirac DM coupled to a heavier Z ′
We want Sommerfeld effect → Take DM in a triplet with Y = 0.DM∈ T0
DM ∈ T0
ν
ν
Z ′
Model S r1 : Scalar DM coupled to a scalar triplet with Y = 2.
We want Sommerfeld effect → Take DM as an Inert Higgs.
DM∈ D
DM∈ D
ν
ν
T2
Type-II seesaw mechanism → Neutrino masses at tree level.
El Aisati, CGC, Hambye, Vanderheyden, 2017
Camilo Garcia Cely, ULB ν lines from Dark Matter
Model F1
Camilo Garcia Cely, ULB ν lines from Dark Matter
DM belongs to ψ, a hyperchargeless triplet T0 DM∈ T0
DM ∈ T0
ν
ν
Z ′
LZ ′ ⊃ gDZ′µ
(ψγµψ + QLαγ
µLα).
At freeze-out σv ∼ 2.3× 10−26 cm3/s.
Unitarity Limit
Per
turb
ati
vit
y
IceCube
Antares
e+ e
- � Μ+ Μ
-
Τ+ Τ
-
mZ'=1.5mDM
GZ'=0.01mDM
Per flavor
MILKYWAY
Total
100 101 10210-26
10-25
10-24
10-23
10-22
10-21
10-200.01 0.05 0.11 0.25 0.56 1.22
mDM HTeVL
Σv
Hcm3
�sL
QΑD
In the Milky way (v ∼ 2× 10−3c )
Unitarity Limit
Per
turb
ati
vit
y
Τ+Τ-
Μ+Μ-
mZ'=1.5 mDM
GZ'=0.01 mDM
Per flavor
Total
dSphs
100 101 10210-26
10-25
10-24
10-23
10-22
10-21
10-200.01 0.05 0.11 0.25 0.56 1.22
mDM HTeVL
Σv
Hcm3
�sL
QΑD
In dwarf galaxies ( v ∼ ×10−5c)
Model F1
Camilo Garcia Cely, ULB ν lines from Dark Matter
DM belongs to ψ, a hyperchargeless triplet T0 DM∈ T0
DM ∈ T0
ν
ν
Z ′
LZ ′ ⊃ gDZ′µ
(ψγµψ + QLαγ
µLα).
At freeze-out σv ∼ 2.3× 10−26 cm3/s.
Unitarity Limit
Per
turb
ati
vit
y
IceCube
Antares
e+ e
- � Μ+ Μ
-
Τ+ Τ
-
mZ'=1.5mDM
GZ'=0.01mDM
Per flavor
MILKYWAY
Total
100 101 10210-26
10-25
10-24
10-23
10-22
10-21
10-200.01 0.05 0.11 0.25 0.56 1.22
mDM HTeVL
Σv
Hcm3
�sL
QΑD
In the Milky way (v ∼ 2× 10−3c )
Unitarity Limit
Per
turb
ati
vit
y
Τ+Τ-
Μ+Μ-
mZ'=1.5 mDM
GZ'=0.01 mDM
Per flavor
Total
dSphs
100 101 10210-26
10-25
10-24
10-23
10-22
10-21
10-200.01 0.05 0.11 0.25 0.56 1.22
mDM HTeVL
Σv
Hcm3
�sL
QΑD
In dwarf galaxies ( v ∼ ×10−5c)
Model F1
Camilo Garcia Cely, ULB ν lines from Dark Matter
DM belongs to ψ, a hyperchargeless triplet T0 DM∈ T0
DM ∈ T0
ν
ν
Z ′
LZ ′ ⊃ gDZ′µ
(ψγµψ + QLαγ
µLα).
At freeze-out σv ∼ 2.3× 10−26 cm3/s.
Unitarity Limit
Per
turb
ati
vit
y
IceCube
Antares
e+ e
- � Μ+ Μ
-
Τ+ Τ
-
mZ'=1.5mDM
GZ'=0.01mDM
Per flavor
MILKYWAY
Total
100 101 10210-26
10-25
10-24
10-23
10-22
10-21
10-200.01 0.05 0.11 0.25 0.56 1.22
mDM HTeVL
Σv
Hcm3
�sL
QΑD
In the Milky way (v ∼ 2× 10−3c )
Unitarity Limit
Per
turb
ati
vit
y
Τ+Τ-
Μ+Μ-
mZ'=1.5 mDM
GZ'=0.01 mDM
Per flavor
Total
dSphs
100 101 10210-26
10-25
10-24
10-23
10-22
10-21
10-200.01 0.05 0.11 0.25 0.56 1.22
mDM HTeVL
Σv
Hcm3
�sL
QΑD
In dwarf galaxies ( v ∼ ×10−5c)
Model S r1
Camilo Garcia Cely, ULB ν lines from Dark Matter
DM belongs to φD =
(H+
(H0 + iA0)/√
2
)DM∈ D
DM∈ D
ν
ν
T2
L = µφDφTφD − Y Lαβ LαφTL
cβ + h.c .
At freeze-out σv ∼ 2.3× 10−26 cm3/s.
IceCube
Antares
Unitarity Limit
Un
itarity
Lim
itin
the
Early
Un
iverse
ΝΝ
mH+-mH0=0.35 GeV
mA0-mH0=1. GeV
MILKYWAY
100 101 10210-26
10-25
10-24
10-23
10-22
10-21
10-20
mH0 HTeVL
Σv
Hcm3
�sL
In the Milky way (v ∼ 2× 10−3c )
HESS WW
WW+ZZ+hh
ΓZ�2+ΓΓ
HESS ΓΓ
mH+-mH0=0.35 GeV
mA0-mH0=1. GeV
MILKYWAY
101 10210-29
10-28
10-27
10-26
10-25
10-24
10-23
mH0 HTeVL
Σv
Hcm3
�sL
No charged leptons.
Model S r1
Camilo Garcia Cely, ULB ν lines from Dark Matter
DM belongs to φD =
(H+
(H0 + iA0)/√
2
)DM∈ D
DM∈ D
ν
ν
T2
L = µφDφTφD − Y Lαβ LαφTL
cβ + h.c .
At freeze-out σv ∼ 2.3× 10−26 cm3/s.
IceCube
Antares
Unitarity Limit
Un
itarity
Lim
itin
the
Early
Un
iverse
ΝΝ
mH+-mH0=0.35 GeV
mA0-mH0=1. GeV
MILKYWAY
100 101 10210-26
10-25
10-24
10-23
10-22
10-21
10-20
mH0 HTeVL
Σv
Hcm3
�sL
In the Milky way (v ∼ 2× 10−3c )
HESS WW
WW+ZZ+hh
ΓZ�2+ΓΓ
HESS ΓΓ
mH+-mH0=0.35 GeV
mA0-mH0=1. GeV
MILKYWAY
101 10210-29
10-28
10-27
10-26
10-25
10-24
10-23
mH0 HTeVL
Σv
Hcm3
�sL
No charged leptons.
Model S r1
Camilo Garcia Cely, ULB ν lines from Dark Matter
DM belongs to φD =
(H+
(H0 + iA0)/√
2
)DM∈ D
DM∈ D
ν
ν
T2
L = µφDφTφD − Y Lαβ LαφTL
cβ + h.c .
At freeze-out σv ∼ 2.3× 10−26 cm3/s.
IceCube
Antares
Unitarity Limit
Un
itarity
Lim
itin
the
Early
Un
iverse
ΝΝ
mH+-mH0=0.35 GeV
mA0-mH0=1. GeV
MILKYWAY
100 101 10210-26
10-25
10-24
10-23
10-22
10-21
10-20
mH0 HTeVL
Σv
Hcm3
�sL
In the Milky way (v ∼ 2× 10−3c )
HESS WW
WW+ZZ+hh
ΓZ�2+ΓΓ
HESS ΓΓ
mH+-mH0=0.35 GeV
mA0-mH0=1. GeV
MILKYWAY
101 10210-29
10-28
10-27
10-26
10-25
10-24
10-23
mH0 HTeVL
Σv
Hcm3
�sL
No charged leptons.
The flavor triangle
Camilo Garcia Cely, ULB ν lines from Dark Matter
In contrast to photons, neutrinos carry flavor
0. 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1.
0.
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1. 0.
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1.
Pure Ν Μ
Pure Νe
Pure ΝΤ Αe
Å
Α ΤÅ ΑΜ Å
1 Σ
3 Σ
NH
IH
Neutrinos from F1 , 3
H flavor universalL
Neutrinos from
astrophysics, F2 , 4 or S1
H flavor eigenstatesL
Neutrinos
from S1r
H mass eigenstatesL
øø
1 Σ
3 Σ
NH
IH
How about DM decays into neutrinos?
If neutrinos are Majorona particles, Lepton number L or (B-L)is broken. If it is spontaneously broken there must exist a(pseudo-)Goldstone boson.
For sufficiently a large symmetry-breaking scale, the Majoronhas a lifetime larger than the age of the Universe and istherefore a DM candidate: axion-like particle.
Below a few TeV, Majorons decay and mainly producemonochromatic neutrinos that are mass eigenstates.Above a few TeV, three-body and four-body final statesdominate the decay. Dudas, Mambrini and Olive (2015).
Camilo Garcia Cely, ULB ν lines from Dark Matter
How about DM decays into neutrinos?
If neutrinos are Majorona particles, Lepton number L or (B-L)is broken. If it is spontaneously broken there must exist a(pseudo-)Goldstone boson.
For sufficiently a large symmetry-breaking scale, the Majoronhas a lifetime larger than the age of the Universe and istherefore a DM candidate: axion-like particle.
Below a few TeV, Majorons decay and mainly producemonochromatic neutrinos that are mass eigenstates.Above a few TeV, three-body and four-body final statesdominate the decay. Dudas, Mambrini and Olive (2015).
Camilo Garcia Cely, ULB ν lines from Dark Matter
How about DM decays into neutrinos?
If neutrinos are Majorona particles, Lepton number L or (B-L)is broken. If it is spontaneously broken there must exist a(pseudo-)Goldstone boson.
For sufficiently a large symmetry-breaking scale, the Majoronhas a lifetime larger than the age of the Universe and istherefore a DM candidate: axion-like particle.
Below a few TeV, Majorons decay and mainly producemonochromatic neutrinos that are mass eigenstates.Above a few TeV, three-body and four-body final statesdominate the decay. Dudas, Mambrini and Olive (2015).
Camilo Garcia Cely, ULB ν lines from Dark Matter
How about DM decays into neutrinos?
If neutrinos are Majorona particles, Lepton number L or (B-L)is broken. If it is spontaneously broken there must exist a(pseudo-)Goldstone boson.
For sufficiently a large symmetry-breaking scale, the Majoronhas a lifetime larger than the age of the Universe and istherefore a DM candidate: axion-like particle.
Below a few TeV, Majorons decay and mainly producemonochromatic neutrinos that are mass eigenstates.
Above a few TeV, three-body and four-body final statesdominate the decay. Dudas, Mambrini and Olive (2015).
Camilo Garcia Cely, ULB ν lines from Dark Matter
How about DM decays into neutrinos?
If neutrinos are Majorona particles, Lepton number L or (B-L)is broken. If it is spontaneously broken there must exist a(pseudo-)Goldstone boson.
For sufficiently a large symmetry-breaking scale, the Majoronhas a lifetime larger than the age of the Universe and istherefore a DM candidate: axion-like particle.
Below a few TeV, Majorons decay and mainly producemonochromatic neutrinos that are mass eigenstates.Above a few TeV, three-body and four-body final statesdominate the decay. Dudas, Mambrini and Olive (2015).
Camilo Garcia Cely, ULB ν lines from Dark Matter
Majoron DM
Camilo Garcia Cely, ULB ν lines from Dark Matter
Neutrino experiments can beused as DM detectors.
0. 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1.
0.
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1. 0.
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1.
Pure Ν Μ
Pure Νe
Pure ΝΤ Αe
Å
Α ΤÅ ΑΜ Å
øø
øø
øø
1 Σ
3 Σ
QD
NH
IH
astrophysical
neutrinos
QD
NH
Cosmology,
from J ® invisible
atm.ΝΜ+ΝΜ
ΝΜ+ΝΜanisotropy, SK
Νe
Bor
exin
o
Νe
Kam
LA
ND
Νe
SK
Νe
10-3 10-2 10-1 100 101 102108
109
1010
1011
1012
1013
1014
1015
mJ HGeVL
Low
erlim
iton
fHG
eVL
Neutrinos from Majoron decayare mass eigenstates, whichleads to very particular flavorratios at Earth.
CGC, Heeck (2017)
Majoron DM
Camilo Garcia Cely, ULB ν lines from Dark Matter
Neutrino experiments can beused as DM detectors.
0. 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1.
0.
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1. 0.
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1.
Pure Ν Μ
Pure Νe
Pure ΝΤ Αe
Å
Α ΤÅ ΑΜ Å
øø
øø
øø
1 Σ
3 Σ
QD
NH
IH
astrophysical
neutrinos
QD
NH
Cosmology,
from J ® invisible
atm.ΝΜ+ΝΜ
ΝΜ+ΝΜanisotropy, SK
Νe
Bor
exin
o
Νe
Kam
LA
ND
Νe
SK
Νe
10-3 10-2 10-1 100 101 102108
109
1010
1011
1012
1013
1014
1015
mJ HGeVL
Low
erlim
iton
fHG
eVL
Neutrinos from Majoron decayare mass eigenstates, whichleads to very particular flavorratios at Earth.
CGC, Heeck (2017)
Conclusions
Multi-TeV DM models predict a significant annihilation crosssections due to the Sommerfeld effect. Much above thecanonical thermal value.
I discussed models whose main signature is the annihilationinto neutrino lines. They can be probed in the near future.
Majoron DM is a consistent model that provides neutrino linesas its most important signature.
Thanks for your attention!
Camilo Garcia Cely, ULB ν lines from Dark Matter
Conclusions
Multi-TeV DM models predict a significant annihilation crosssections due to the Sommerfeld effect. Much above thecanonical thermal value.
I discussed models whose main signature is the annihilationinto neutrino lines. They can be probed in the near future.
Majoron DM is a consistent model that provides neutrino linesas its most important signature.
Thanks for your attention!
Camilo Garcia Cely, ULB ν lines from Dark Matter
Charged final states
J
J
ni
nj
ni
nj
ℓ
ℓ̄
W
Z
ℓ, q
ℓ̄, q̄
a)
b)
È-Kee+KΜΜ+KΤΤÈfrom J®e+e-
ÈKee-KΜΜ+KΤΤÈ, ÈKeΜÈfrom J®Μ+Μ-
ÈKee+KΜΜ-KΤΤÈ, ÈKeΤÈ, ÈKΜΤÈfrom J®Τ+Τ-
ÈKee+KΜΜ+KΤΤÈfrom J®bb
ÈKee+KΜΜ+KΤΤÈfrom J®ΓΓ
CMBΓ-ray telescopesAMS-02 p� p
AMS-02 e+
10-3 10-2 10-1 100 101 10210-23
10-22
10-21
10-20
10-19
10-18
10-17
10-16
10-15
10-14
10-13
10-12
mJ HGeVL
Up
pe
rlim
its
on
K{{'
Camilo Garcia Cely, ULB ν lines from Dark Matter
There are final states taking place at one-loop and two-loop level.They depend on different parameters. CGC, Heeck (2017)
General calculation of the rates for DM DM → γγ
Camilo Garcia Cely, ULB ν lines from Dark Matter
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