Theory: Particle Cosmology - Filippo Sala 87th PRC meeting, 21 May 2019 - DESY Indico
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Theory: Particle Cosmology
87th PRC meeting, 21 May 2019
Filippo Sala
People - Staff
★ Wilfried Buchmüller (honorary member)
★ Valerie Domcke (5yrs)
★ Thomas Konstandin
★ Rafael Porto* (Zeuthen, but located in Hamburg)
★ Andreas Ringwald
★ Filippo Sala (5yrs)
★ Geraldine Servant
★ Alexander Westphal*
*External fundings: 2 ERC consolidator grants
PRC meeting 5/2019 | Theoretical physics: cosmology Filippo Sala !1
People - Staff
★ Wilfried Buchmüller (honorary member)
★ Valerie Domcke (5yrs) Offered 6 year CERN-EPFL staff position
(starting date negotiated to May 2020)
★ Thomas Konstandin
★ Rafael Porto* (Zeuthen, but located in Hamburg)
★ Andreas Ringwald
★ Filippo Sala (5yrs) Ranked 1st in CNRS section02 competition
(starting date etc to be negotiated)
★ Geraldine Servant
★ Alexander Westphal*
*External fundings: 2 ERC consolidator grants
PRC meeting 5/2019 | Theoretical physics: cosmology Filippo Sala !1
People - Postdocs/Students/Other
+ more later
★ Federico Carta* ★ Felix Giese
★ Luca Di Luzio*(arrives Fall 2019) ★ Yann Gouttenoire
★ Yohei Ema* ★ Jakob Moritz*
★ Nayara Fonseca ★ Henrique Rubira
★ Ryusuke Jinno* ★ Peera Simachakorn
★ Enrico Morgante ★ Stefan Sanders
★ Kyohei Mukaida*
★ Ryosuke Sato
★ Prof. Jorge Gamboa (Humboldt visitor Apr-July 2019)
★ Yvette Welling*
*External fundings (partial or all) - japanese JSPS fellowships, ERC, Marie Curie
PRC meeting 5/2019 | Theoretical physics: cosmology Filippo Sala !2
External Fundings and Networks
★ Excellence Cluster (participation to “Quantum Universe” proposal)
★ ERC consolidator grant “Stringflation” (Alexander)
★ ERC consolidator grant “LHCtoLISA” (Rafael, Zeuthen but located in Hamburg)
★ Cost European Network “Fundamental Connections”
★ Invisibles-Plus RISE and Elusives European ITN Network
(Horizon2020 projects, University of Goettingen-DESY node)
★ PIER Seed project funding (Filippo&Geraldine)
“Dark Matter at 10 TeV and beyond, a new goal for cosmic-ray experiments”
★ Nordic Network of Dark Matter (Thomas, funds Danish Research Council)
★ Member of ANTARES collaboration (Filippo, observer status)
PRC meeting 5/2019 | Theoretical physics: cosmology Filippo Sala !3
Event Organisation (since 2018) PARTICLE PHYSICS
CHALLENGESª
Local DESY Theory Workshop
25 - 28 September 2018
Hamburg, Germany
★ 6 Apr 2018 - Gravitational Waves: windows of opportunities Plenary Talks
U. Blumenschein (London)
N. Craig (Santa Barbara)
M. Czakon (Aachen)
J. Kopp (Mainz)
F. Maltoni (Louvain)
T. Mannel (Siegen)
M. Pospelov (Perimeter)
J. Rademacker (Bristol)
M. Schmaltz (Boston)
L. Tancredi (CERN)
A. Urbano (Trieste)
C. Vallée (Marseille & DESY)
A. Denner (Würzburg) F. Moortgat (CERN) K. Schmidt-Hoberg (DESY) L. Verde (Barcelona)
A. Eichhorn (Heidelberg) I. Moult (Berkeley) M. Spannowsky (Durham) L.-T. Wang (Chicago)
DESY Heinrich-Hertz Lecture on Physics 27 September 2018
★ 18-22 Jun 2018 - 14th Patras Axion-WIMP workshop
George Sterman (Stony Brook University)
Parallel Sessions
Contributions by young researchers are especially encouraged.
Deadline for abstract submission in early July 2018
ªStrings & Mathematical Physics: O. Schlotterer (Potsdam & Perimeter Inst.), E. Pomoni (DESY)
e−γ
ªCosmology & Astroparticle Physics: F. Kahlhoefer (Aachen), V. Domcke (DESY)
ªParticle Phenomenology: S. Gieseke (Karlsruhe), M. Bauer (Heidelberg)
★ 21-23 Aug 2018 - Probing strong-field QED in interactions ORGANIZING COMMITTEE:
K. Borras, C. Grojean, B. Heinemann,
G. Heinrich, G. Hiller, J. Jäckel, M. Krämer (Chair),
A. Kulesza, P. Marquard, G. Moortgat-Pick,
S. Schumann, P. Schwaller,
T. Schwetz-Mangold, F. Tackmann
http://th-workshop2018.desy.de
★ 25-28 Sep 2018 - DESY theory workshop
Accelerators | Photon Science | Particle Physics
Deutsches Elektronen-Synchrotron
A Research Centre of the Helmholtz Association
★ 19-20 Mar 2019 - Quantum Universe Kickoff meeting
External
★ 14-18 May 2018, CERN
Primordial vs Astrophysical origin of Black Holes
★ 9-21 July 2018, Corsica, Cargese Summer School
★ 7-13 April 2019, Benasque, Light Scalars Workshop
★ 10-21 June 2019, ICTP Trieste, Particle Physics summer school
★ 7-12 July 2019, Valencia, GR22
PRC meeting 5/2019 | Theoretical physics: cosmology Filippo Sala !4
Lectures and Teaching (since 2018)
★ Summer semester 2018, Uni. Hamburg, Theoretical Cosmology course [Servant+Westphal]
★ Summer semester 2018, DESY, “Workshop Seminar” on Flavour Physics, 11 lectures
★ June 2018, Erice, “Erice international school of science journalism”, 1 lecture [Servant]
★ July 2018, Mainz, “MITP Summer School 2018”, 4 lectures [Domcke]
★ July 2018, Trieste, “Jennifer summer school on particle physics and detectors”, 2 lectures [Sala]
★ Winter semester 2018, DESY, “Workshop Seminar” on Hot Topics in QFT&String theory, 12 lectures
★ Summer semester 2019, DESY, “Workshop Seminar” on Semiclassical objects in QFT, 11 lectures
★ Summer semester 2019, Uni. Hamburg, Theoretical Cosmology course [Domcke+Servant]
★ August 2019, Ljubljana, Summer School, 2 lectures + 2 tutorings [Sala+Gouttenoire]
PRC meeting 5/2019 | Theoretical physics: cosmology Filippo Sala !5
Research: The Big Picture
We work to understand: Our lab:
★ Dark Matter
★ Baryon Asymmetry
★ Neutrino Oscillations
★ Quantum Gravity
★ Inflation
★ Dark Energy
★ EW symmetry breaking
★ Strong CP problem
★ Origin of SM flavour
★ ….
PRC meeting 5/2019 | Theoretical physics: cosmology Filippo Sala !6
SMASH
Self-contained and consistent description of particle physics and cosmology
SMASH
• Added to Standard Model (SM) singlet complex
scalar field featuring spontaneously broken Peccei- BRF
ADMX
IAXO
ADMX3 + X3
Quinn symmetry, a vector-like quark, and three MADMAX
ORPHEUS
right-handed singlet (sterile) neutrinos
ADMX2
• Model solves several problems of particle physics CULTASK
and cosmology in one stroke: -
- - - -
-
• Inflation (non-minimal chaotic PQ/H field inflation)
• Baryogenesis (leptogenesis)
• Dark matter (axion)
• Strong CP problem (axion)
• Neutrino masses and mixing (seesaw)
[Ballesteros,Redondo,Ringwald,Tamarit 1608.05414; 1610.01639]
PRC meeting 5/2019 | Theoretical physics: cosmology Filippo Sala !7
GUT SMASH
Self-contained and consistent description of particle physics and cosmology
Non-SUSY GUT SMASH
• Non-SUSY and
models addressing both neutrino masses
and gauge coupling unification predict
axion mass in window accessible in axion
DM direct detection CASPEr-Electric
• Intriguing possibility that Higgs field
required for GUT breaking may be
responsible for inflation
[Ernst 18; CASPEr prospects from Kimball et al. 17]
[Ernst,Ringwald,Tamarit 1801.04906; Di Luzio,Ringwald,Tamarit 1807.09769]
PRC meeting 5/2019 | Theoretical physics: cosmology Filippo Sala !8Flavour-Electroweak symmetry
breaking cosmological interplay
● Effect of varying Yukawas on EW phase transition
Baldes, Konstandin, Servant, 1604.04526
● Implementation in Froggatt-Nielsen
Baldes, Konstandin, Servant, 1608.03254
● Natural realisation of Yukawa variation in Randall-Sundrum
Von Harling, Servant, 1612.02447
● Calculation of baryon asymmetry in models of variable Yukawas
Bruggisser, Konstandin, Servant, 1706.08534
● Outcome in composite Higgs models Bruggisser, VonHarling, Matsedonskyi,
Servant, 1803.08546 & 1804.07314
● High scale EW phase transition Baldes, Servant, 1807.08770
PRC meeting 5/2019 | Theoretical physics: cosmology Filippo Sala !9Cosmological relaxation
of the electroweak scale
● UV completion in Randall-Sundrum type of models
Fonseca, Von Harling, De Lima, Machado, 1712.07635
● Higgs relaxation after inflation Fonseca, Morgante, Servant, 1805.04543
● Relaxation dark matter Fonseca, Morgante, 1809.04534
n
V( )
l Evolution after inflation
t=0
t=t c
B. Low Temperature
Inflation
c = ⇤/g 0 : µh = 0
Most of its energy is transferred
Figure 1. Sketch of the relaxion field evolution.
PRC meeting 5/2019 | Theoretical physics: cosmology
Filippo Sala !10GW spectra from fluid models
Predictions of gravitational waves
from cosmological phase transitions
often rely on hydrodynamic lattice
simulations.
These simulations are limited by
grid resolutions and time scales.
Semi-analytic models can assess
these regimes. They are based on
energy considerations and fluid
modelling from the simulations.
[TK ’17]
PRC meeting 5/2019 | Theoretical physics: cosmology Filippo Sala !11als
0.25 Planck TT+lowP+lensing+ext
Planck TT+lowP the
test string theory
+BK14
Planck TT+lowP+BKP
+lensing+ext
N=
N=
60
with inflation & CMB
0.20
50
2
2
• V
r =r T /S
0.15
Co
0.002
nv
Co ex
nc
ave • V
strings!
0.10
2/3
0.05 • V /
0.00
0.95 0.96 0.97 0.98 0.99 1.00
ns ns
Fig. 21. Left: Constraints on the tensor-to-scalar ratio r0.002 in the ⇤CDM model, using Planck TT+lowP and Planck
TT+lowP+lensing+BAO+JLA+H0 (red and blue, respectively) assuming negligible running
FIG. 7. Constraints in the and
cosmological CMB data
r vs.the
nsinflationary
plane whenconsistency
using Planck rela-
tion. The result is model-dependent; for example, the grey contours show
plus how the results
additional change
data, and whenif there
also were additional
adding relativistic
BICEP2/Keck
degrees of freedom with Ne↵ = 0.39 (disfavoured, but not excluded, by Planck).
data through Dotted
the end of thelines
2014show loci
season of approximately
including new 95 GHz con-
p
stant e-folding number N, assuming simple V / ( /mPl ) single-field inflation.
maps—the Solid lines
constraint onshow the approximate
r tightens from r0.05ns –r
< relation
0.12 tofor
quadratic and linear potentials to first order in slow roll; red lines rshow the approximate allowed range assuming 50 < N < 60 and
0.05 < 0.07. This figure is adapted from Fig. 21 of Ref. [2]—
a power-law potential for the duration of inflation. The solid blacksee line (corresponding to a linear potential) separates concave and
the string theory landscape:
there for further details.
convex potentials. Right: Equivalent constraints in the ⇤CDM model when adding B-mode polarization results corresponding to the
default configuration of the BICEP2/Keck Array+Planck (BKP) likelihood. These exclude the quadratic potential at a higher level
of significance compared to the Planck-alone constraints. many isolated vacua, connected by tunneling
some mountain slopes drive inflation
⇤
limited by cosmic variance of the dominant scalar anisotropies, from tensor modes. The constraints shown by the blue contours [13
jmkovac@cfa.harvard.edu
†
and it is also model dependent. In polarization, in addition to B- in Fig. 21, which add Planck lensing, BAO, and other astrophys-
pryke@physics.umn.edu
modes, the EE and T E spectra also contain a signal from tensor icalA.
[1] data, are therefore
A. Penzias and R. tighter in the nAstrophys.
W. Wilson, s direction and shifted to
J. 142, 419 [14
modes coming from reionization and last scattering. However, slightly higher values, but marginally weaker in the r-direction.
(1965).
in this release the addition of Planck polarization constraints at [2] Planck Collaboration
The 95 % limits 2015 XIII, ArXiv e-prints (2015),
on r0.002 are [15
` 30 do not significantly change the results from temperature arXiv:1502.01589. [16
string theory’s 6 compact dimensions:
and low-` polarization (see Table 5). r0.002
[3] 0.10, Planckand
M.als
0.25 Planck TT+lowP+lensing+ext
Planck TT+lowP the
test string theory
+BK14
Planck TT+lowP+BKP
+lensing+ext
N=
N=
60
with inflation & CMB
0.20
50
2
2
• V
r =r T /S
0.15
Co
0.002
nv
Co ex
nc
ave • V
strings!
0.10
2/3
0.05 • V /
0.00
0.95 0.96 0.97 0.98 0.99 1.00
ns ns
Fig. 21. Left: Constraints on the tensor-to-scalar ratio r0.002 in the ⇤CDM model, using Planck TT+lowP and Planck
TT+lowP+lensing+BAO+JLA+H0 (red and blue, respectively) assuming negligible running
FIG. 7. Constraints in the and
cosmological CMB data
r vs.the
nsinflationary
plane whenconsistency
using Planck rela-
tion. The result is model-dependent; for example, the grey contours show
plus how the results
additional change
data, and whenif there
also were additional
adding relativistic
BICEP2/Keck
degrees of freedom with Ne↵ = 0.39 (disfavoured, but not excluded, by Planck).
data through Dotted
the end of thelines
2014show loci
season of approximately
including new 95 GHz con-
p
stant e-folding number N, assuming simple V / ( /mPl ) single-field inflation.
maps—the Solid lines
constraint onshow the approximate
r tightens from r0.05ns –r
< relation
0.12 tofor
quadratic and linear potentials to first order in slow roll; red lines rshow the approximate allowed range assuming 50 < N < 60 and
0.05 < 0.07. This figure is adapted from Fig. 21 of Ref. [2]—
a power-law potential for the duration of inflation. The solid blacksee line (corresponding
there to a linear potential) separates concave and
for further details.
moduli & axions:
convex potentials. Right: Equivalent constraints in the ⇤CDM model when adding B-mode polarization results corresponding to the
default configuration of the BICEP2/Keck Array+Planck (BKP) likelihood. These exclude the quadratic potential at a higher level
of significance compared to the Planck-alone constraints.
limited by cosmic variance of the dominant scalar anisotropies,
⇤
light scalars …
from tensor modes. The constraints shown by the blue contours
jmkovac@cfa.harvard.edu [13
†
and it is also model dependent. In polarization, in addition to B- in Fig. 21, which add Planck lensing, BAO, and other astrophys-
pryke@physics.umn.edu
modes, the EE and T E spectra also contain a signal from tensor icalA.
[1] data, are therefore
A. Penzias and R. tighter in the nAstrophys.
W. Wilson, s direction and shifted to
J. 142, 419 [14
modes coming from reionization and last scattering. However, slightly higher values, but marginally weaker in the r-direction.
(1965).
in this release the addition of Planck polarization constraints at [2] Planck Collaboration
The 95 % limits 2015 XIII, ArXiv e-prints (2015),
on r0.002 are [15
` 30 do not significantly change the results from temperature arXiv:1502.01589. [16
string theory’s 6 compact dimensions:
and low-` polarization (see Table 5). r0.002
[3] 0.10, Planckand
M.machine learning for axion monodromy inflation
Steps:
1. Identify relevant scales (class of models)
2. Learn the mapping from parameters µ p …
uii to observables …
3. Study how predictions change according
fiff to prior choice ns
Use numerical methods developed 2
✓ ◆2 !p/2
3
in previous work to generate a L=
1
(@ )2 V0 4 1 + 15 + Vp,np
large sample assuming 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
2 µ
µ ⇠ U(0.1, 1) p ⇠ U(0.1, 2)
• Take a random draw of µ and p
• Solve background equations of motion
• Solve equations of motion for the
perturbations and compute ns
• Repeat many times
• Use machine learning to get ns (µ, p)
Dias, Frazer, Mulryne, Seery: Implementations in C++, Python and Mathematica public at https://transportmethod.com
PRC meeting 5/2019 | Theoretical physics: cosmology Filippo Sala !13machine learning for axion monodromy inflation
[Dias, Frazer & AW ’18]
Steps:
1. Identify relevant scales (class of models)
2. Learn the mapping from parameters µ p …
uii to observables …
3. Study how predictions change according
fiff to prior choice ns
Use numerical methods developed 2
✓ ◆2 !p/2
3
in previous work to generate a L=
1
(@ )2 V0 4 1 + 15 + Vp,np
large sample assuming 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
2 µ
µ ⇠ U(0.1, 1) p ⇠ U(0.1, 2)
AAACA3icdVDLSsNAFJ3UV62PRl26GSyCi1KSNLR1V9SFywr2AW0ok+m0HTqZhJlJsYQu/Qq3unInbv0QF/6Lk7aCih64cDjnXu69x48Ylcqy3o3M2vrG5lZ2O7ezu7efNw8OWzKMBSZNHLJQdHwkCaOcNBVVjHQiQVDgM9L2J5ep354SIWnIb9UsIl6ARpwOKUZKS30z37siTCHY6ie8yKN53yxYpfNaxXEr0CpZVtV27JQ4VbfsQlsrKQpghUbf/OgNQhwHhCvMkJRd24qUlyChKGZknuvFkkQIT9CIdDXlKCCyOJjSSC6ol9wtnpjDU+0O4DAUuriCC/X7dIICKWeBrzsDpMbyt5eKf3ndWA1rXkJ5FCvC8XLRMGZQhTBNBA6oIFixmSYIC6rvhniMBMJK56bz+Hoa/k9aTskul5wbt1C/WCWTBcfgBJwBG1RBHVyDBmgCDGLwAB7Bk3FvPBsvxuuyNWOsZo7ADxhvn+rEmCg=
Vn,np : full model — 12 parameters !
• Take a random draw of µ and p
• Solve background equations of motion
• Solve equations of motion for the
perturbations and compute ns
• Repeat many times
• Use machine learning to get ns (µ, p) lower bound r & 0.015
µ
AAACAHicdVDLSsNAFJ34rPVVdelmsAguJCRpbOuu6MZlBfuANpbJdNIOnUzCzKRYQjd+hVtduRO3/okL/8VJW0FFD1w4nHMv997jx4xKZVnvxtLyyuraem4jv7m1vbNb2NtvyigRmDRwxCLR9pEkjHLSUFQx0o4FQaHPSMsfXWZ+a0yEpBG/UZOYeCEacBpQjJSWbkV3oLQZQsu07LNeoWiZ59Wy45YzwarYjp0Rp+KWXGhrJUMRLFDvFT66/QgnIeEKMyRlx7Zi5aVIKIoZmea7iSQxwiM0IB1NOQqJPO2PaSxn1EvvZh9M4bF2+zCIhC6u4Ez9Pp2iUMpJ6OvOEKmh/O1l4l9eJ1FB1UspjxNFOJ4vChIGVQSzOGCfCoIVm2iCsKD6boiHSCCsdGg6j6+n4f+k6Zh2yXSu3WLtYpFMDhyCI3ACbFABNXAF6qABMBDgATyCJ+PeeDZejNd565KxmDkAP2C8fQKdN5ba
independent of AAAB9XicdVDLSsNAFJ3UV62vqks3g0VwISFJQ1t3RTcuK9oHtKFMJpN26EwSZibVUvoJbnXlTtz6PS78FydtBRU9cOFwzr3ce4+fMCqVZb0buZXVtfWN/GZha3tnd6+4f9CScSowaeKYxaLjI0kYjUhTUcVIJxEEcZ+Rtj+6zPz2mAhJ4+hWTRLicTSIaEgxUlq66fG0XyxZ5nmt4rgVaJmWVbUdOyNO1S270NZKhhJYotEvfvSCGKecRAozJGXXthLlTZFQFDMyK/RSSRKER2hAuppGiBN5FoxpIufUm97Pz57BE+0GMIyFrkjBufp9eoq4lBPu606O1FD+9jLxL6+bqrDmTWmUpIpEeLEoTBlUMcwygAEVBCs20QRhQfXdEA+RQFjppHQeX0/D/0nLMe2y6Vy7pfrFMpk8OALH4BTYoArq4Ao0QBNgMAAP4BE8GXfGs/FivC5ac8Zy5hD8gPH2Cd0dkzI=
Dias, Frazer, Mulryne, Seery: Implementations in C++, Python and Mathematica public at https://transportmethod.com
PRC meeting 5/2019 | Theoretical physics: cosmology Filippo Sala !13Particle production during inflation
Slow-roll inflation very flat scalar potential
Reheating after inflation coupling to the SM
Inflaton as Pseudo Goldstone Boson with shift-symmetric couplings
Fµ⌫ F̃µ⌫ (@µ ) ¯ µ 5
explosive helical gauge boson production chiral fermion production
additional friction modifies dynamics of baryogenesis through spontaneous CPT
inflation, see also relaxion models violation
Strongly enhanced non-gaussian polarized backreaction through induced current
GW spectrum at scales. of LIGO and LISA modifies gauge boson production
PRC meeting 5/2019 | Theoretical physics: cosmology Filippo Sala !14Particle production during inflation
Domcke, Mukaida ‘18
10-3 vacuum
2
One example: + gauge fields
s
scalar power spectrum
Scalar power spectrum
10-5
+ fermions
at small scales
10-7 CMB
Domcke, Mares, Muia, Pieroni ‘18
10-9
10-3
non-Abelian 0 10 20 30 40 50
Abelian N [e-folds]
10-5 vacuum Same scalar
potential and
coupling strength Different inflaton couplings
10-7 to gauge fields can be probed by
observations!
10-9
(PBHs, UCMHs, mu-distortions)
CMB
10-11
Similar effects (expected)
10 20 30 40 50 in GW spectrum
PRC meeting 5/2019 | Theoretical physics: cosmology Filippo Sala !15Light Dark Matter at Neutrino Experiments
MDM
AAAB9HicbVA9TwJBEJ3DL8Qv1NLmIphYkTsstCRqYUOCiXwkcCF7ywIb9vbO3TkiufA7bCw0xtYfY+e/cYErFHzJJC/vzWRmnh8JrtFxvq3M2vrG5lZ2O7ezu7d/kD88augwVpTVaShC1fKJZoJLVkeOgrUixUjgC9b0RzczvzlmSvNQPuAkYl5ABpL3OSVoJK9Y7XaQPWFyW50Wu/mCU3LmsFeJm5ICpKh181+dXkjjgEmkgmjddp0IvYQo5FSwaa4TaxYROiID1jZUkoBpL5kfPbXPjNKz+6EyJdGeq78nEhJoPQl80xkQHOplbyb+57Vj7F95CZdRjEzSxaJ+LGwM7VkCdo8rRlFMDCFUcXOrTYdEEYomp5wJwV1+eZU0yiX3ouTelwuV6zSOLJzAKZyDC5dQgTuoQR0oPMIzvMKbNbZerHfrY9GasdKZY/gD6/MHBx+Rmw==
Experiment Erecoil . keV
AAACB3icbVC7SgNBFJ2NrxhfUUtBBhPBKuzGQsugCJYRzAOSJcxObpIhsw9m7ophiZWNv2JjoYitv2Dn3zhJttDEAwOHc+7lzjleJIVG2/62MkvLK6tr2fXcxubW9k5+d6+uw1hxqPFQhqrpMQ1SBFBDgRKakQLmexIa3vBy4jfuQGkRBrc4isD1WT8QPcEZGqmTPyxeddoI95go4KGQY9qWoLUWfvFhCPVOvmCX7CnoInFSUiApqp38V7sb8tiHALlkWrccO0I3YQoFlzDOtWMNEeND1oeWoQHzQbvJNMeYHhulS3uhMi9AOlV/byTM13rke2bSZzjQ895E/M9rxdg7dxMRRDFCwGeHerGkGNJJKbQrTHqUI0MYV8L8lfIBU4yjqS5nSnDmIy+SernknJbsm3KhcpHWkSUH5IicEIeckQq5JlVSI5w8kmfySt6sJ+vFerc+ZqMZK93ZJ39gff4AJY6Zeg==
Standard Detectors not sensitive (Xenon1T,…)
Theory New connections in recent years (w/flav. anomalies, hierarchy problem, …)
PRC meeting 5/2019 | Theoretical physics: cosmology Filippo Sala !16Light Dark Matter at Neutrino Experiments
MDM
AAAB9HicbVA9TwJBEJ3DL8Qv1NLmIphYkTsstCRqYUOCiXwkcCF7ywIb9vbO3TkiufA7bCw0xtYfY+e/cYErFHzJJC/vzWRmnh8JrtFxvq3M2vrG5lZ2O7ezu7d/kD88augwVpTVaShC1fKJZoJLVkeOgrUixUjgC9b0RzczvzlmSvNQPuAkYl5ABpL3OSVoJK9Y7XaQPWFyW50Wu/mCU3LmsFeJm5ICpKh181+dXkjjgEmkgmjddp0IvYQo5FSwaa4TaxYROiID1jZUkoBpL5kfPbXPjNKz+6EyJdGeq78nEhJoPQl80xkQHOplbyb+57Vj7F95CZdRjEzSxaJ+LGwM7VkCdo8rRlFMDCFUcXOrTYdEEYomp5wJwV1+eZU0yiX3ouTelwuV6zSOLJzAKZyDC5dQgTuoQR0oPMIzvMKbNbZerHfrY9GasdKZY/gD6/MHBx+Rmw==
Experiment Erecoil . keV
AAACB3icbVC7SgNBFJ2NrxhfUUtBBhPBKuzGQsugCJYRzAOSJcxObpIhsw9m7ophiZWNv2JjoYitv2Dn3zhJttDEAwOHc+7lzjleJIVG2/62MkvLK6tr2fXcxubW9k5+d6+uw1hxqPFQhqrpMQ1SBFBDgRKakQLmexIa3vBy4jfuQGkRBrc4isD1WT8QPcEZGqmTPyxeddoI95go4KGQY9qWoLUWfvFhCPVOvmCX7CnoInFSUiApqp38V7sb8tiHALlkWrccO0I3YQoFlzDOtWMNEeND1oeWoQHzQbvJNMeYHhulS3uhMi9AOlV/byTM13rke2bSZzjQ895E/M9rxdg7dxMRRDFCwGeHerGkGNJJKbQrTHqUI0MYV8L8lfIBU4yjqS5nSnDmIy+SernknJbsm3KhcpHWkSUH5IicEIeckQq5JlVSI5w8kmfySt6sJ+vFerc+ZqMZK93ZJ39gff4AJY6Zeg==
Standard Detectors not sensitive (Xenon1T,…)
Theory New connections in recent years (w/flav. anomalies, hierarchy problem, …)
Ema Sala Sato PRL 122 (2019) no.18:
High-speed DM component unavoidably generated by Cosmic-ray scatterings!
Electrons
Dark Matter
PRC meeting 5/2019 | Theoretical physics: cosmology Filippo Sala !16Light Dark Matter at Neutrino Experiments
MDM
AAAB9HicbVA9TwJBEJ3DL8Qv1NLmIphYkTsstCRqYUOCiXwkcCF7ywIb9vbO3TkiufA7bCw0xtYfY+e/cYErFHzJJC/vzWRmnh8JrtFxvq3M2vrG5lZ2O7ezu7d/kD88augwVpTVaShC1fKJZoJLVkeOgrUixUjgC9b0RzczvzlmSvNQPuAkYl5ABpL3OSVoJK9Y7XaQPWFyW50Wu/mCU3LmsFeJm5ICpKh181+dXkjjgEmkgmjddp0IvYQo5FSwaa4TaxYROiID1jZUkoBpL5kfPbXPjNKz+6EyJdGeq78nEhJoPQl80xkQHOplbyb+57Vj7F95CZdRjEzSxaJ+LGwM7VkCdo8rRlFMDCFUcXOrTYdEEYomp5wJwV1+eZU0yiX3ouTelwuV6zSOLJzAKZyDC5dQgTuoQR0oPMIzvMKbNbZerHfrY9GasdKZY/gD6/MHBx+Rmw==
Experiment Erecoil . keV
AAACB3icbVC7SgNBFJ2NrxhfUUtBBhPBKuzGQsugCJYRzAOSJcxObpIhsw9m7ophiZWNv2JjoYitv2Dn3zhJttDEAwOHc+7lzjleJIVG2/62MkvLK6tr2fXcxubW9k5+d6+uw1hxqPFQhqrpMQ1SBFBDgRKakQLmexIa3vBy4jfuQGkRBrc4isD1WT8QPcEZGqmTPyxeddoI95go4KGQY9qWoLUWfvFhCPVOvmCX7CnoInFSUiApqp38V7sb8tiHALlkWrccO0I3YQoFlzDOtWMNEeND1oeWoQHzQbvJNMeYHhulS3uhMi9AOlV/byTM13rke2bSZzjQ895E/M9rxdg7dxMRRDFCwGeHerGkGNJJKbQrTHqUI0MYV8L8lfIBU4yjqS5nSnDmIy+SernknJbsm3KhcpHWkSUH5IicEIeckQq5JlVSI5w8kmfySt6sJ+vFerc+ZqMZK93ZJ39gff4AJY6Zeg==
Standard Detectors not sensitive (Xenon1T,…)
Theory New connections in recent years (w/flav. anomalies, hierarchy problem, …)
Ema Sala Sato PRL 122 (2019) no.18:
High-speed DM component unavoidably generated by Cosmic-ray scatterings!
Electrons
Dark Matter
PRC meeting 5/2019 | Theoretical physics: cosmology Filippo Sala !16Light Dark Matter at Neutrino Experiments
MDM
AAAB9HicbVA9TwJBEJ3DL8Qv1NLmIphYkTsstCRqYUOCiXwkcCF7ywIb9vbO3TkiufA7bCw0xtYfY+e/cYErFHzJJC/vzWRmnh8JrtFxvq3M2vrG5lZ2O7ezu7d/kD88augwVpTVaShC1fKJZoJLVkeOgrUixUjgC9b0RzczvzlmSvNQPuAkYl5ABpL3OSVoJK9Y7XaQPWFyW50Wu/mCU3LmsFeJm5ICpKh181+dXkjjgEmkgmjddp0IvYQo5FSwaa4TaxYROiID1jZUkoBpL5kfPbXPjNKz+6EyJdGeq78nEhJoPQl80xkQHOplbyb+57Vj7F95CZdRjEzSxaJ+LGwM7VkCdo8rRlFMDCFUcXOrTYdEEYomp5wJwV1+eZU0yiX3ouTelwuV6zSOLJzAKZyDC5dQgTuoQR0oPMIzvMKbNbZerHfrY9GasdKZY/gD6/MHBx+Rmw==
Experiment Erecoil . keV
AAACB3icbVC7SgNBFJ2NrxhfUUtBBhPBKuzGQsugCJYRzAOSJcxObpIhsw9m7ophiZWNv2JjoYitv2Dn3zhJttDEAwOHc+7lzjleJIVG2/62MkvLK6tr2fXcxubW9k5+d6+uw1hxqPFQhqrpMQ1SBFBDgRKakQLmexIa3vBy4jfuQGkRBrc4isD1WT8QPcEZGqmTPyxeddoI95go4KGQY9qWoLUWfvFhCPVOvmCX7CnoInFSUiApqp38V7sb8tiHALlkWrccO0I3YQoFlzDOtWMNEeND1oeWoQHzQbvJNMeYHhulS3uhMi9AOlV/byTM13rke2bSZzjQ895E/M9rxdg7dxMRRDFCwGeHerGkGNJJKbQrTHqUI0MYV8L8lfIBU4yjqS5nSnDmIy+SernknJbsm3KhcpHWkSUH5IicEIeckQq5JlVSI5w8kmfySt6sJ+vFerc+ZqMZK93ZJ39gff4AJY6Zeg==
Standard Detectors not sensitive (Xenon1T,…)
Theory New connections in recent years (w/flav. anomalies, hierarchy problem, …)
Ema Sala Sato PRL 122 (2019) no.18:
High-speed DM component unavoidably generated by Cosmic-ray scatterings!
Electrons
Dark Matter
PRC meeting 5/2019 | Theoretical physics: cosmology Filippo Sala !16Ema Sala Sato PRL 122 (2019) no.18
Light Dark Matter at Neutrino Experiments
Energies > 10 MeV go to biggest existing detectors!
PRC meeting 5/2019 | Theoretical physics: cosmology Filippo Sala !17Ema Sala Sato PRL 122 (2019) no.18
Light Dark Matter at Neutrino Experiments
Energies > 10 MeV go to biggest existing detectors!
Our
Ne w Li
mits
PRC meeting 5/2019 | Theoretical physics: cosmology Filippo Sala !17Cosmo approaches to the Big Picture
We work to understand:
★ Dark Matter
★ Baryon Asymmetry
★ Neutrino Oscillations
★ Quantum Gravity
★ Inflation
★ Dark Energy
★ EW symmetry breaking
★ Strong CP problem
★ Origin of SM flavour
★ ….
PRC meeting 5/2019 | Theoretical physics: cosmology Filippo Sala !18You can also read
