Dark Matter, Sterile Neutrinos and Icecube Events Riccardo Biondi Dark Matter, Sterile Neutrinos and Icecube

Dark Matter, Sterile Neutrinos and IceCube Events Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube

Contents Events IceCube Data Hot topics in Modern Cosmology - Spontaneous Workshop IX Standard Neutrinos

Sterile Neutrinos R. Biondi, Z. Berezhiani, G. Di Panﬁlo, A. Gazizov Model

Asymmetric Mirror Matter Dipartimento di Scienze Fisiche e Chimiche, Universita` degli studi dell’Aquila Conclusions INFN, Laboratori Nazionali del Gran Sasso (LNGS)

27 April 2015

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Contents

Dark Matter, Sterile Neutrinos and IceCube Events Riccardo Biondi 1 IceCube Data

Contents IceCube Data 2 Standard Neutrinos Standard Neutrinos Sterile 3 Sterile Neutrinos Neutrinos

Model Asymmetric 4 Model Mirror Matter

Conclusions 5 Asymmetric Mirror Matter

6 Conclusions

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events IceCube

Dark Matter, Sterile Neutrinos and Large Volume Cherenkov IceCube Events Detector(1 km3) Riccardo Biondi South Pole Contents 1450 – 2450 m under IceCube Data Antarctic Ice Standard Neutrinos 5160 PMT’s (DOM) Sterile Neutrinos Energy Range: TeV- PeV Model

Asymmetric Mirror Matter

Conclusions

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events The Detector

Dark Matter, Sterile All neutrinos Charged Current interactions (CC) deposits its energy into a Neutrinos and IceCube Events charged lepton and an hadronic shower Riccardo Biondi ⇒ Energy resolution: 15% beyond i 10 TeV. Contents IceCube Data Two topologies: Standard Neutrinos Tracks: Showers: Sterile Neutrinos

Model νµ CC interaction νe o ντ CC interaction Asymmetric Mirror Matter Angular resolution ≤ 1◦ Angular resolution ∼ 15◦ Conclusions Background: Neutrinos and Muons from cosmic rays (Atmospheric)

Event selection: Interaction vertex in the ﬁducial volume, muon veto (external layers) and deposited charge in PMT > 600 (E & 30 TeV)

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Events

Dark Matter, Sterile After three years of data taking: 35 events from 30 TeV to 2 PeV, over an Neutrinos and +5.9 IceCube Events expected background of 8.4 ± 4.2 for cosmic muons and 6.6−1.6 from Riccardo Biondi atmospheric neutrinos ⇒ exess di 5.7 σ

Contents 16 IceCube events IceCube Data Tracks 14 Sum of traks Showers Gap 400 T eV − 1 P eV Sum of events Standard 12 Bkg. atm. muon flux s

Neutrinos y Bkg. atm. neutrinos (π/K) a

D 10 Atm. ν0s (90% CL Charm Limit) Isolated events at E ∼ 1P eV 8

Sterile 8 9

Neutrinos r 8 e p Cut-Off at E > 2P eV s t

n 6

Model e v E Asymmetric 4 Abundance of showers (28) Mirror Matter 2 over tracks (7) Conclusions 0 105 106 E, GeV ⇒ Tracks are compatible with the expected background ⇒ From 100 TeV to 2 PeV only one track and 11 Showers

⇒ Cosmic neutrinos component dominating at E > 60 TeV which for some reason prefers νe and/or ντ over νµ.

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Standard Neutrinos

Dark Matter, Sterile Neutrinos and IceCube Events ⇒ Can we understand something on the origin of this neutrinos studying Riccardo Biondi their ﬂavor content?

Contents ⇒ Suppose that this neutrinos come from some distant Astrophysical IceCube Data source (Cosmic Ray, Dark Matter decay ...) Standard Neutrinos 0 Sterile ⇒ Can we explain the fraction of tracks F (E,E ) detected at IceCube in Neutrinos some model or production mechanism thats take into account only the Model three standard neutrinos? Asymmetric Mirror Matter Conclusions ⇒ Starting from different ﬂavor composition at the source we will compute F (E,E0) expected at IceCube considering different power-law spectra and the effective area of the detector

⇒ We will also take into account the experimental uncertainties on the parameters of the standard neutrinos mixing matrix

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Expected νµ Fraction

Dark Matter, Sterile Expected tracks fraction in certain energy range can be expressed: Neutrinos and IceCube Events Z E0 Riccardo Biondi dE φµ(E) Aµ(E) 0 Nt E Contents F (E,E ) = = 0 Nt + Ns Z E IceCube Data X dE φα(E) Aα(E) Standard E Neutrinos α

Sterile −γ Neutrinos Assuming a power-law spectra: φα(E) ∝ E

Model 1.0 Asymmetric

Mirror Matter 0.8 0 rµ fµ Conclusions F (E,E ) = fe + rµ fµ + rτ fτ 0.6

rΜ 0.4 R E0 −γ rΤ dE E Aµ,τ (E) E 0.2 with: rµ,τ = R E0 −γ E dE E Ae(E) 0.0 50 100 200 500 1000 E TeV

@ D γ = 2.4 + δγ − 0.4 < δγ < 0.4

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Uncertainties on Mixing Parameters

Dark Matter, Source Flavor Composition: =⇒ f˜α Sterile 2 2 Neutrinos and P Averaged Oscillation Probability: =⇒ Pαβ = i |Vαi| |Viβ | IceCube Events ˜ Riccardo Biondi Composition ad Earth: =⇒ fα = Pαβ fβ

1.0 Contents 6 Independent Elements Pee PeΜ IceCube Data 0.8 P PΜΤ 3 Bounds: Pαβ = 1 α PΜΜ Standard 0.6 Neutrinos 0.4 Sterile =⇒ 3 Independent Elements Neutrinos 0.2 We choose: Pee, Peµ e Pµτ Model 0.0 0.0 0.5 1.0 1.5 2.0 Asymmetric ∆ Π Mirror Matter ˜ Conclusions If rµ = rτ = 1 =⇒ F = fµ ' Peµ − (Peµ − Pµτ ) 1 − fe

Peµ is the key parameter! To take into account experimental uncertanties on neutrino mixing angles we choose to marginalize every Pαβ matrix elements with the combination of 1 σ interval extremes that maximize or minimize Peµ. ± ± ∓ ∓ Pαβ = Pαβ (θ23, θ13, θ12)

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events ˜ Source Composition fα I

Dark Matter, Sterile Many possibilities: Neutrinos and IceCube Events Most common scenario: (π and µ decay) (1/3 : 2/3 : 0) Riccardo Biondi Depending on EMeson we can also have: (0 : 1 : 0) or (1 : 0 : 0) Contents Neutron Decay:(1 : 0 : 0) IceCube Data

Standard Symmetric case (1/3 : 1/3 : 1/3) Neutrinos

Sterile Only ντ production (0 : 0 : 1) (DM decay) Neutrinos

Model Oscillation Effects: f˜ → P f˜ Asymmetric α αβ α Mirror Matter

Conclusions (1/3 : 1/3 : 1/3) → (1/3 : 1/3 : 1/3) (1/3 : 2/3 : 0) → (0.34 : 0.33 : 0.33) (1 : 0 : 0) → (0.55 : 0.24 : 0.21) (0 : 1 : 0) → (0.24 : 0.38 : 0.38) (0 : 0 : 1) → (0.21 : 0.38 : 0.41)

After oscillation the Atmospheric case reduces to the Symmetric one

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events ˜ Source Composition fα II

Dark Matter, Sterile We can also think at more exotic production mechanism such as Neutrinos and IceCube Events neutrinos from Dark Matter direct decay Riccardo Biondi ⇒ Which can product neutrino Mass Eigenstate: ν1, ν2 and ν3 Contents IceCube Data ⇒ Mass Eigenstate are are not Affected by oscillation Standard Neutrinos

Sterile Flavor composition at earth is given by projecting mass eigenstate in the Neutrinos 2 ﬂavor eigenstate base: fα = |Vαi| Model

Asymmetric Mirror Matter 1.0

Conclusions 0.8 2 Ve1

0.6 È 2 VΜ3

0.4 È

V 2 0.2 e2 2 VΜ1 È 0.0 È 0.0 0.5 1.0 1.5 2.0 ∆ Π

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Results I

Dark Matter, Now we can compute F (E,E0): Sterile Neutrinos and IceCube Events We are interested in the area above 60 TeV and expecially in the two sub-region where 60T eV < E < 100T eV (Low 100T eV < E < 2P eV Riccardo Biondi Background) and (No Background)

Contents E [Tev] 60 < E < 2000 60 < E < 100 100 < E < 2000 IceCube Data ˜ ˜ ˜ fe : fµ : fτ FIC = 0.2 FIC = 0.375 FIC = 0.083 Standard Neutrinos 1/3 : 1/3 : 1/3 .229 + .045 δγ .153 + .0012 δγ .249 + .031 δγ Sterile −.005 −.005 −.005 Neutrinos 1/3 : 2/3 : 0 .235 + .045 δγ .150 + .0012 δγ .245 + .031 δγ +.015 +.013 +.016 Model +.029 +.019 +.032 (1 : 0 : 0) .156 + .035 δγ .096 + .0012 δγ .174 + .029 δγ Asymmetric −.032 −.020 −.035 Mirror Matter −.025 −.021 −.025 (0 : 1 : 0) .264 + .046 δγ .185 + .0012 δγ .284 + .032 δγ Conclusions +.046 +.039 +.047

−.009 −.004 −.011 (0 : 0 : 1) .279 + .045 δγ .200 + .0012 δγ .298 + .031 δγ −.005 −.007 −.004

+.058 +.035 +.065 ν .106 + .029 δγ .062 + .001 δγ .120 + .021 δγ 1 −.052 −.031 −.058

−.054 −.039 −.057 ν .278 + .056 δγ .191 + .001 δγ .300 + .036 δγ 2 +.044 +.034 +.046

−.021 −.019 −.022 ν .341 + .037 δγ .275 + .001 δγ .355 + .026 δγ 3 +.031 +.028 −.031

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Results II

Dark Matter, Sterile Neutrinos and IceCube Events Cumulative: (E0 = 2P eV ) Riccardo Biondi

Contents Spectral Index Oscillation Parameters IceCube Data 0.4 0.4

ΝΜ Standard ΝΜ 0.3 0.3 Neutrinos Νe

Sterile Atm L Atm L E E H H 0.2 0.2 F

Neutrinos F Νe Model 0.1 0.1 Ν1 Asymmetric Ν1 Mirror Matter 0.0 0.0 Conclusions 50 100 200 500 1000 2000 50 100 200 500 1000 2000 E TeV E TeV ⇒ None of this scenarios can explain the ﬂavor content observed at @ D @ D IceCube in both the Interesting Energy region.

⇒ Signal of New Physics ?!?

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Sterile Neutrinos

Dark Matter, Sterile Neutrinos and IceCube Events What if this cosmic neutrinos were created in some Hidden Gauge Riccardo Biondi Sector as Sterile Neutrinos? Contents IceCube Data Dark Sector Standard Model Standard Neutrinos We can think to some kind of Heavy Dark Matter MDM ∼ PeV that Sterile Neutrinos decade into neutrinos of that sector which are Sterile for us.

Model DM → DMstable + νs + ... Asymmetric Mirror Matter −10 1 Conclusions Then they oscillate with small probabilities (P ∼ 10 ) in our neutrinos

νs → νe, νµ, ντ

Which are then detected by IceCube.

1 2 4 −6 2 BBN → δms sin θs < 10 eV Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Mixing Matrix

Dark Matter, Extra sterile neutrino with small mixing angles si Sterile Neutrinos and   IceCube Events 1 0 0 s1 Riccardo Biondi  0 1 0 s2  2 RS (si) =   + O(si ) Contents  0 0 1 s3  IceCube Data −s1 −s2 −s3 1

Standard Neutrinos So, the mixing matrix is given by: Sterile   Neutrinos Ve1 Ve2 Ve3 Ve4 Model  Vµ1 Vµ2 Vµ3 Vµ4  2 U =   + O(si ) Asymmetric Vτ1 Vτ2 Vτ3 Vτ4 Mirror Matter   Vs1 Vs2 Vs3 1 Conclusions

|Vsi| 1 ⇒ Pαβ Between the three ordinary neutrinos remain the same On the other hand:

3 2 X 2 2 Psα = |Vα4| + |Vsi| |Vαi| i=1

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Different Scenarios:

Dark Matter, Sterile One can think about different mixing pattern between active and sterile Neutrinos and IceCube Events neutrinos. Riccardo Biondi

Contents As an example we can choose: s2 = s3 = 0 e s1 = s

IceCube Data 2.0

Standard Neutrinos 1.5

2 2 Sterile Pse = s [1 + Pee] Pse ∆ s 1.0 P ∆ s2 Neutrinos sΜH L P ∆ s2 2 sΤH L Model Psµ = s Peµ 0.5 H L Asymmetric 2 Mirror Matter Psτ = s Peτ 0.0 0.0 0.5 1.0 1.5 2.0 Conclusions ∆ Π

So we have:

2 0 s rµ (1 + Peµ) F (E,E ) = 2 s (1 + Pee + rµ Peµ + rτ Peτ )

F (E,E0) is independent from s! (if s 1)

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Results I

Dark Matter, Sterile Neutrinos and IceCube Events ⇒ Initial composition: f˜ = (0 : 0 : 0 : 1) Riccardo Biondi

−γ Contents ⇒ Power-Law Spectra: φs(E) ∝ E IceCube Data Standard ⇒ Three different scenarios: when the sterile neutrino is mixed with only Neutrinos one of the standard neutrinos: Msα : νs να Sterile Neutrinos

Model E [Tev] 60 < E < 2000 60 < E < 100 100 < E < 2000

Asymmetric FIC = 0.2 FIC = 0.375 FIC = 0.083 Mirror Matter +.012 +.007 +.014 M .071 + .021 δγ .040 + .001 δγ. 080 + .016 δγ Conclusions se −.014 −.008 −.016

−.019 −.023 −.017 M .572 + .058 δγ. 457 + .002 δγ. 596 + .039 δγ sµ +.032 +.038 +.031

−.005 −.003 −.005 M .137 + .022 δγ .101 + .001 δγ .145 + .016 δγ sτ −.002 −.002 −.001

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Results II

Dark Matter, 0 Sterile Cumulative: (E = 2P eV ) Neutrinos and IceCube Events Riccardo Biondi Spectral Index Oscillation Parameters

0.8 0.8 Contents

IceCube Data 0.6 0.6

Ν <-> Ν ΝΜ <-> Νs Standard Μ s L L E E H H 0.4 0.4 Neutrinos F F

Sterile Neutrinos 0.2 0.2 Νe <-> Νs Νe <-> Νs Model 0.0 0.0 Asymmetric 50 100 200 500 1000 2000 50 100 200 500 1000 2000 Mirror Matter E TeV E TeV

Conclusions @ D @ D ⇒ In the No Background region: IceCube ∼ Mse : νs νe

⇒ In the Low Background region: IceCube ∼ Msµ : νs νµ

Can this be a Clue?

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Idea

Dark Matter, Sterile Neutrinos and IceCube Events The ideal scenario to explain this ﬂavor content is a mechanism that Riccardo Biondi creates νs mixed with νe over 100 TeV and νs mixed with νµ below.

Contents

IceCube Data We can think at two different species of Dark Matter with different

Standard masses and different decay modes whose as decay product have two Neutrinos different kind of sterile neutrinos. Sterile Neutrinos DMe → ... + νs νe Model

Asymmetric Mirror Matter DMµ → ... + νs νµ Conclusions But... What ﬁxes DM decay time? and What deﬁnes oscillation probabilities?

All of this can be naturally obtained in the framework of Asymmetric Mirror Dark Matter

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Mirror Universe

Dark Matter, Sterile Neutrinos and IceCube Events Riccardo Biondi

Contents

IceCube Data

Standard Neutrinos

Sterile Neutrinos Particle physics will is described by such a Lagrangian: Model

Asymmetric Mirror Matter 0 Conclusions Ltot = LSM + LSM + Lmix

Invariant under two identical gauge groups: G × G0 Identical ﬁeld contents Mirror Parity P (G ↔ G0) (no new parameters)

Gravity is not the only common interaction! → Lmix

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events History Of Mirror World

Dark Matter, Sterile Neutrinos and Ideas of Mirror Matter: IceCube Events Riccardo Biondi 1956 Left-Right symmetry can be restored in nature (Lee and Yang) Contents

IceCube Data 1966 Mirror fermions cannot have common Interactions EM, Weak Standard and Strong but only common Gravity (Kobzarev, Okun, Neutrinos Pomeranchuk ) Sterile Neutrinos 1991 Two Standard Models: SM and SM 0 (Foot et al.) Model

Asymmetric 1995 Lepton number violation in ordinary and mirror matter Mirror Matter (Berezhiani, Mohapatra) Conclusions 1995 Asymmetric Mirror Universe (Berezhiani, Dolgov, Mohapatra) 2001 MM as a viable candidate for DM if T 0/T 1 (Berezhiani, Comelli, Vilante) 2006 Baryon number violation in ordinary and mirror matter (Berezhiani)

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Mirror Particle Physics

Dark Matter, Sterile Neutrinos and For Ordinary particles we have the Standard Model: IceCube Events G = SU(3) × SU(2) × U(1) Riccardo Biondi Gauge Symmetry: W ± Contents Particles: quarks, leptons, photon, gluons, , Z, Higgs. IceCube Data Interactions: long-range EM forces, Strong interaction conﬁnement Standard (ΛQCD), Weak scale MW Neutrinos

Sterile Neutrinos

Model In the Mirror Sector we have the same: 0 0 0 0 Asymmetric Mirror Gauge Symmetry: G = SU(3) × SU(2) × U(1) Mirror Matter 0 0 0 0 0± 0 Conclusions Mirror Particles: quarks , leptons , photon , gluons , W , Z , Higgs0. Mirror Interactions: long-range EM forces, Strong interaction 0 0 conﬁnement (ΛQCD), Weak scale MW

Lmix −→ O-M Interactions

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Mirror Cosmology

Dark Matter, Sterile Same Physics Different Stories: Neutrinos and IceCube Events Riccardo Biondi ⇒ Mirror Matter: ∆Nν ' 6.14 (BBN limit: ∆Nν . 0.5 )

Contents But if after Inﬂation → T 0 < T Mirror Matter can full-ﬁt BBN bounds and IceCube Data also we obtain for free: Standard Neutrinos 0 ⇒ ηB & ηB → Mirror Matter is a natural candidate for Dark Matter Sterile Neutrinos

Model ⇒ Mirror BBN: ∼ 75% of He and ∼ 25% of H

Asymmetric Mirror Matter How Mirror Universe would look like? Conclusions Mirror stars are older than ordinary ones; some populate the galaxy halo as MACHOs; many has exploded as Super Novae. Like for OM most of MM is in the form of gas clouds rather than stars and planets. MM clouds consists of interacting gas at different temperatures and density.

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Mirror Phenomenology

Dark Matter, Sterile Are there any Window to the Mirror World? Neutrinos and IceCube Events Riccardo Biondi Lmix Contents

IceCube Data is responsible for many O-M Interactions

Standard Neutrinos Sterile We can build up higher dimension operator that generate interactions Neutrinos such as: Model Asymmetric Photon Kinetic Mixing: −F µν F 0 Mirror Matter µν 0 1 0 0 0 Conclusions n − n Oscillation: M (uud)(u u d ) 0 1 0 0 ν − ν Oscillations: M (φl)(l φ ) π0 − π00 and K0 − K00 Mixing (with common Gauge or Higgs 1 µ 0 0 Boson) M (¯qγ q) (¯q γµq ) ⇒ n − n0 and ν − ν0 Oscillation Violate B-L Symmetry in both sector ⇒ Baryon and Lepton Asymmetry in the Early Universe

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Distorted Mirror

Dark Matter, What if Mirror Parity is broken for some reason? Sterile Neutrinos and IceCube Events ⇒ In can be done in many ways, the most intriguing one is to have a Riccardo Biondi mechanism that make different the Higgs VEV of the two sectors Contents 0 IceCube Data v 6= 1 Standard v Neutrinos 0 Sterile ⇒ This introduces only one Extra Parameter: ζ = v Neutrinos v

Model

Asymmetric ⇒ Elementary mirror fermions and gauge bosons will have different Mirror Matter masses from the Ordinary ones. Conclusions ⇒ It will also affect the Running of Coupling constants

⇒ Depending on the value of ζ we can have many different scenarios

We will show that an highly Asymmetric Mirror Matter scenario can give an explenation of what is observed at IceCube

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Breaking of Mirror Parity

Dark Matter, We choose a SUSY + GUT scenario: Sterile Neutrinos and IceCube Events 16 ⇒ Below GUTs scale (MG ∼ 10 GeV ) both sectors are given by Riccardo Biondi identical SUSY GUTs groups such as SU(5) × SU(5)0 or 0 Contents SU(6) × SU(6) and Mirror Parity in conserved. IceCube Data 16 Standard ⇒ MG ∼ 10 GeV : SSB of GUTs group in both sectors: Neutrinos SU(5) → SU(3) × SU(2) × U(1) Sterile Neutrinos SU(5)0 → SU(3)0 × SU(2)0 × U(1)0 Model

Asymmetric 0 11 Mirror Matter ⇒ MS ∼ 10 GeV : Soft Breaking of SUSY in the Mirror Sector due to a Conclusions non zero F or D Term of some Auxiliary Field

02 MS ⇒ This induces SUSY Breaking in our sector at MS ∼ ∼ 1T eV MP l (Transmitted by Gravity or Planck Scale Mediator)

0 0 MS MS −→ v v Mirror Parity is Broken

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Running of Coupling Constant

Dark Matter, Sterile All elementary fermions and gauge bosons in the Mirror Sector are Neutrinos and rescaled by the factor: ζ = v0/v = 109 IceCube Events Riccardo Biondi ⇒ We can compute the running of the three gauge coupling constant: Contents

IceCube Data 140 Α-1 Standard 120 -1 Neutrinos Α3 Μ Α¢-1 100 -1 Sterile Α2 Μ H L Neutrinos 80 Α -1 Μ 1 H L ¢ ¢ -1 Model 60 MZ MZ Α Μ 3 H L Α -1 ¢ -1 Asymmetric 40 5 Α Μ 2 H L Mirror Matter 20 Α¢ -1 Μ 1 H L Conclusions 0 9 13 17 0.001 10 105 10 10 10 H L Μ

0 ⇒ ΛQCD ∼ 100T eV : There are no Light Quarks in the Mirror World

⇒ No conﬁnement effects in Hadrons P ⇒ M-Hadrons are Bound States of Heavy Quark : MHadr = Mq0

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Asymmetric Mirror World

Dark Matter, Sterile How this Asymmetric Mirror World would look like? Neutrinos and IceCube Events Riccardo Biondi Our sector:

Contents SUSY scale: MS ∼ 1T eV IceCube Data EW SSB: v ' 100GeV Standard Neutrinos conﬁnement: Λ ' 200MeV Sterile Neutrinos Mirror sector: Model 11 Asymmetric SUSY scale: MS ∼ 10 GeV Mirror Matter EW SSB: v 1011GeV Conclusions . conﬁnement: Λ ' 100T eV

Mirror Universe is popolated by Neutrinos, Photons, lightest Leptons and the lightest Mirror Baryon

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Quark and Lepton Masses

Dark Matter, Sterile At GUT scale we have two Identical sector, with identical fermions and Neutrinos and IceCube Events Yukawa couplings:

Riccardo Biondi e c d c u c LY = (Yij liej h1 + Yij qid h1 + Yij qiuj h2) Contents 0 e 0 0c 0 d 0 0c 0 u 0 0c 0 IceCube Data LY = (Yij liej h1 + Yij qid h1 + Yij qiuj h2)

Standard Neutrinos But, down to lower energies we have to take into account RG running:

Sterile 3 Neutrinos me = YeReηev1 md = YdRdηdv1 mu = YuRuηuv2Bt Model 0 0 0 3 me0 = YeRe0 ηe0 v md0 = YdRd0 ηd0 v mu0 = YuRu0 ηu0 v B 0 Asymmetric 1 1 2 t Mirror Matter RG in SUSY SM: Reηe ∼ 1.5 , Rdηd ∼ Ruηu ∼ 1.5 and Bt ∼ 0.7 Conclusions 0 RG in SUSY SM : Re0 ηe0 ∼ 1.1 , Rd0 ηd0 ∼ Ru0 ηu0 ∼ 1.3 and Bt0 ∼ 1. Our sector: Mirror sector:

me ' 0.5MeV me0 ' 0.4P eV

md ' 4.8MeV md0 ' 1.1P eV

mu ' 2.3MeV mu0 ' 1.9P eV

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Mirror Neutrinos

Dark Matter, Sterile We Assume that neutrino masses emerge by Plack Scale Operators and Neutrinos and IceCube Events a Ul−l0 (1) Symmetry Riccardo Biondi Y χ ¯ ¯ Y χ ¯0 0 ¯0 0 Z ¯ ¯0 0 Contents Lmν = 2 (5H)(5H) + (5 H )(5 H ) + 2 (5H)(5 H ) MP l MP l MP l IceCube Data 15 0 Standard Ul−l (1) Symmetry is broken by the χ ﬁeld ( Vχ ∼ 10 GeV ) Neutrinos 2 Sterile Vχ v −10 Neutrinos 1-st Op: practically irrelevant δm ' 2 ∼ 10 eV MP l Model 02 0 YVχv Asymmetric 2-nd Op: ν Majorana Masses: Mν0 = ∼ MeV Mirror Matter MP l 0 Conclusions 0 Zvv 3-rd Op: Mixing Dirac Masses between ν and ν mD = ∼ KeV MP l 3-rd Op: Active-Sterile Mixing Θ = mD ∼ 10−4 Mν0 This “see-saw” mechanism induces Majorana Mass term to Ordinary 2 mD −2 neutrinos: mν = ∼ 10 eV Mν0 ⇒ Oscillation probabilities: P ∝ Θ2 ∼ 10−8 − 10−10

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Hadron Masses and Decays

Dark Matter, Sterile Neutrinos and IceCube Events 0− 0 0 0 Riccardo Biondi Lightest and Stable Mirror Baryon: ∆ ∼ (d d d ) with M∆ ' 3.3P eV

Contents 0− 0− 0 In SUSY SU(5) in decays ∆ → ρ +ν ¯x (Mρ0 ' 3.1P eV ) IceCube Data 4 5 5 −1 Standard with: τ∆0 ∼ MG(αGm∆0 ) ∼ 10 − 100Gyr (∼ τU ) Neutrinos

Sterile 4 5 5 −1 31 Neutrinos instead of: τP ∼ MG(αGmP ) ∼ 10 Gyr

Model M2 0 1 ρ0 Asymmetric ⇒ ν E = M 0 1 − ' 200T eV x: Mono-energetic M-Neutrinos: x 2 ∆ M2 Mirror Matter ∆0 Conclusions ⇒ Also resonance of ρ0−(d0u¯0) can be produced giving rise to several lines in the spectra

0 ⇒ νx Superposition of Mirror Neutrino Flavor Eigenstates.

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Neutrino Energy Spectrum

Dark Matter, 0 0− 0− 0 0 0 Sterile All ρ decay into pions ρ → π (d u¯ ) + γ with M ± ' 3P eV Neutrinos and π IceCube Events 0− 0 0 0− 00 0 0 Riccardo Biondi ⇒ π → e +ν ¯e or π → π + e +ν ¯e Γ2 ' Γ3

Contents 0 ⇒ νe is the Mirror Electron Neutrino IceCube Data Standard ⇒ Now we can reconstruct the spectra that would be observed in Neutrinos IceCube taking into account Galactic (z = 0) and Cosmic (z > 0) Sterile Neutrinos contributions: Model 102 1 IC events maximum background from NC scattering τ = 10H − Galaxy ∆ 0 ∆− ρi− + ¯νx 5 average background average background +mirror → dN(E)/dlog10E Asymmetric -3 f =1 Universe mirror neutrinos only 10 ∆ π− + γ Mirror Matter

1 1

− 10 r 0 e π− π +e−+¯ν s Conclusions t e y s →

-4 a 1 10 d − c 8 e 8 s 9 2 − r

e 0 m

p 10 c

, -5 ) ) 10 E ν ( E ( N J

ν π− e−+¯νe

E → 10-1 10-6

104 105 106 105 106 Eν , GeV E, GeV And Compare it with what IceCube Observe

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Flavor Content

Dark Matter, Sterile Neutrinos and IceCube Events Riccardo Biondi Assuming that:

Contents 0 ⇒ νe Is mixed only with our Electron Neutrino IceCube Data Standard ⇒ ν0 Neutrinos x Superposition prefers to Oscillate in our Muon Neutrino

Sterile Neutrinos ⇒ We can compute the Tracks Fraction using the spectra from Model Asymmetric Mirror Dark Matter decay: Asymmetric Mirror Matter

Conclusions E [Tev] 60 < E < 100 100 < E < 2000

FIC = 0.375 FIC = 0.083

−.022 +.021 Asym-MM .456 +.036 .122 −.024

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events Conclusions

Dark Matter, Sterile Neutrinos and IceCube Events It is hard to explain IceCube neutrino events in the framework of known Riccardo Biondi Neutrino Physics and Astrophysics Contents A better agreement it’s possible if we take into account Sterile IceCube Data Neutrinos Standard Neutrinos This Neutrino could be produced from Dark Matter decay in an Sterile Neutrinos Hidden Gauge Sector Model Then they Oscillate into our active neutrino with small probabilities Asymmetric −10 Mirror Matter P ∼ 10 Conclusions Using the paradigm of Asymmetric Mirror Dark Matter we can have a model that naturally explain all the features of neutrino observed at IceCube The validity of our model will be tested with increasing statistics by IceCube Collaboration

Riccardo Biondi Dark Matter, Sterile Neutrinos and IceCube Events