Pathways to Discovering Supernova Neutrinos Thomas D. P . Edwards , - - PowerPoint PPT Presentation

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Pathways to Discovering Supernova Neutrinos Thomas D. P . Edwards , - - PowerPoint PPT Presentation

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Pathways to Discovering Supernova Neutrinos Thomas D. P . Edwards , Sebastian Baum, Bradley J. Kavanagh, Patrick Stengel, Andrzej K. Drukier, Katherine Freese, Maciej Grski, Christoph Weniger 1906.05800 1 Quantamagazine 2 Thomas D. P

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Pathways to Discovering Supernova Neutrinos

Thomas D. P . Edwards, Sebastian Baum, Bradley J. Kavanagh, Patrick Stengel, Andrzej K. Drukier, Katherine Freese, Maciej Górski, Christoph Weniger

1 1906.05800

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

2

Quantamagazine

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

What are the Difgerent Ways of Observing SN Neutrinos

3

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

What are the Difgerent Ways of Observing SN Neutrinos

Direct observation of a SN event in our Galaxy

3

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

What are the Difgerent Ways of Observing SN Neutrinos

Direct observation of a SN event in our Galaxy

3

Observing the Diffuse background from SN throughout the Universe

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

What are the Difgerent Ways of Observing SN Neutrinos

Direct observation of a SN event in our Galaxy

3

Observing the collective emission of SN from within the galaxy Observing the Diffuse background from SN throughout the Universe

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

Typical Recoil Energies for SN Neutrinos

  • Recoil energy of a collision is O(1) KeV - very

small energy deposit to detect

  • Although neutrinos have a small mass, there

increased velocities lead to O(1-10) KeV recoils

4

ER ≤ 2 m2

χMT

(mχMT )2 v2

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10−1 100 101 102 Eν [MeV] 10−1 100 101 102 dφ/dEν [cm−2 s−1 MeV−1] DSNB galactic

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

Small Damage Track Features can be Observed in Minerals

  • Paleo-detectors are minerals from far below the Earths

surface (5-10 km). Importantly they are 1 billion years old

  • Permanent damage track features in the structure of the

mineral.

5

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

Basics of Building a Detector: Mass vs Exposure

6

Recoil Rate ∝ Target Mass × Observation Time

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

Basics of Building a Detector: Mass vs Exposure

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Recoil Rate ∝ Target Mass × Observation Time

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Smallish Exposure Huge Targets

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

Basics of Building a Detector: Mass vs Exposure

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Recoil Rate ∝ Target Mass × Observation Time

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

Basics of Building a Detector: Mass vs Exposure

7

Huge Exposure Small Targets

Recoil Rate ∝ Target Mass × Observation Time

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

Reading the Tracks: X-ray Tomography

8

Holler et al. 14

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

Cosmic Rays Induce Large Backgrounds

9

Depth [km] 2 5 7.5 10 Neutron Flux [1/cm2/Gpc] 103 101 10-4 10-8

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

Natural Radioactivity: Single alphas

  • Natural radioactivity, most importantly Uranium-238 causes multiple backgrounds

10

238U α

− → 234Th

β−

− → 234mPa

β−

− → 234U

α

− → 230Th

α

− → 226Ra

α

− → 222Rn

α

− → . . . − → 206Pb

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

Natural Radioactivity: Single alphas

  • Natural radioactivity, most importantly Uranium-238 causes multiple backgrounds

10

238U α

− → 234Th

β−

− → 234mPa

β−

− → 234U

α

− → 230Th

α

− → 226Ra

α

− → 222Rn

α

− → . . . − → 206Pb

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  • Half life of the second alpha in the decay chain

is 105 yr

  • Alpha does not leave a track, but the daughter

nucleus does

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

Natural Radioactivity: Spontaneous Fission

  • Sometimes uranium spontaneously splits into two lighter nuclei, whilst emitting fast neutrons
  • These neutrons cause many well separated tracks - huge background

11

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

Natural Radioactivity: Spontaneous Fission

  • Sometimes uranium spontaneously splits into two lighter nuclei, whilst emitting fast neutrons
  • These neutrons cause many well separated tracks - huge background

11

101 102 103 x [nm] 10−4 10−2 100 102 104 106 dR/dx [nm−1 kg−1 Myr−1] Epsomite; C238 = 0.01 ppb Galactic SN ν-bkg n-bkg

234Th-bkg

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

Natural Radioactivity: Spontaneous Fission

  • Sometimes uranium spontaneously splits into two lighter nuclei, whilst emitting fast neutrons
  • These neutrons cause many well separated tracks - huge background

11

101 102 103 x [nm] 10−4 10−2 100 102 104 106 dR/dx [nm−1 kg−1 Myr−1] Epsomite; C238 = 0.01 ppb Galactic SN ν-bkg n-bkg

234Th-bkg

Uranium-238 Concentration ∼ 0.01 ppb

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

101 102 103 x [nm] 10−4 10−2 100 102 104 106 dR/dx [nm−1 kg−1 Myr−1] Epsomite; C238 = 0.01 ppb Galactic SN ν-bkg n-bkg

234Th-bkg

Background Neutrinos: Solar and Atmospheric

12

p + p → d + e+ + νe

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

101 102 103 x [nm] 10−4 10−2 100 102 104 106 dR/dx [nm−1 kg−1 Myr−1] Epsomite; C238 = 0.01 ppb Galactic SN ν-bkg n-bkg

234Th-bkg

Background Neutrinos: Solar and Atmospheric

12

p + p → d + e+ + νe

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

Galactic Signal much Larger than the Difguse Background

Signal from galactic supernova is much larger than DSNB

13

10−1 100 101 102 Eν [MeV] 10−1 100 101 102 dφ/dEν [cm−2 s−1 MeV−1] DSNB galactic

Galactic SN spectrum peaks at different energy due to redshift

z ∼ 0

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z ∼ 1

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

Paleo-detectors can Observe Galactic Supernovae

  • 3-sigma detection if we achieve

low enough concentrations of Uranium-238

  • Here we assume a constant rate of

SNe throughout the history of the galaxy

14

10−3 10−2 10−1 100 101

Uranium-238 Concentration [ppb]

10−2 10−1 100 101

Minimum Detectable Rate [yr−1]

M = 100 g, tage = 1 Gyr

Epsomite - C&C Epsomite Halite Nchwaningite Olivine

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

10−3 10−2 10−1 100

Uranium-238 Concentration [ppb]

1 2 3 4 5

Discrimination Significance [σ]

Mor et al. SFR (1901.07564) Cosmological SFR (1403.0007)

Star Formation Rates

15

0.0 0.2 0.4 0.6 0.8 1.0

Look-back Time [Gyr]

1.00 1.25 1.50 1.75 2.00 2.25 2.50 2.75

SFR, (t?)/ (0)

Mor et al. SFR (1901.07564) Cosmological SFR (1403.0007)

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

10−3 10−2 10−1 100

Uranium-238 Concentration [ppb]

1 2 3 4 5

Discrimination Significance [σ]

Mor et al. SFR (1901.07564) Cosmological SFR (1403.0007)

Star Formation Rates

15

0.0 0.2 0.4 0.6 0.8 1.0

Look-back Time [Gyr]

1.00 1.25 1.50 1.75 2.00 2.25 2.50 2.75

SFR, (t?)/ (0)

Mor et al. SFR (1901.07564) Cosmological SFR (1403.0007)

Estimate of the Milky Way SFR from Gaia

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

10−3 10−2 10−1 100

Uranium-238 Concentration [ppb]

1 2 3 4 5

Discrimination Significance [σ]

Mor et al. SFR (1901.07564) Cosmological SFR (1403.0007)

Star Formation Rates

15

0.0 0.2 0.4 0.6 0.8 1.0

Look-back Time [Gyr]

1.00 1.25 1.50 1.75 2.00 2.25 2.50 2.75

SFR, (t?)/ (0)

Mor et al. SFR (1901.07564) Cosmological SFR (1403.0007)

Estimate of the Milky Way SFR from Gaia Baseline case can rule

  • ut constant rate at 2

sigma depending on model

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

Conclusions

16

1 2 3

Paleo-Detectors represent a new way to probe keV scale interactions Paleo-Detectors can detect neutrinos from supernovae within our galaxy With enough clean samples, we can learn about the galactic star formation history

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Thomas D. P . Edwards | TAUP 2019 | 1906.05800

We use swordfjsh to Analyse the Spectra Easily

17

Counting Experiment S(θ): Signal B : Background K :

  • Bkg. Covariance

E : Exposure Fisher Information Matrix Iij(θ) = D

ln L(D|θ) ∂θiθj

E

D(θ)

Information Geometry gij(θ) = Iij(θ) Tensor field visualization Confidence Contours Euclideanized Signal (S(θ), B) ! x(θ) Model Discrimination TS ' kx(θ1) x(θ2)k2 Information Flux F(Ω|θ)ij = δI(θ)ij

δE(Ω)

Strategy optimization Equivalent Counts (S, B) ! (seq, beq) Exclusion Limits seq ' Z p seq + beq Discovery Reach 2 ln

P (seq+beq|beq) P (seq+beq|seq+beq) = Z2

S ( θ ) = S F i x e d s i g n a l s h a p e E q u a l

  • g

e

  • d

e s i c

  • d

i s t a n c e c

  • n

t

  • u

r

1704.05458, 1712.05401 https://github.com/cweniger/swordfish

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Thomas D. P . Edwards | GRAPPA | 1906.05800

We can Constrain Burst Like Events

18

0.0 0.2 0.4 0.6 0.8 1.0

Burst look-back time t? [Gyr]

107 108 109

Minimum Detectable N10 kpc

?

1 ppb 0.1 ppb 0.01 ppb 0.001 ppb Epsomite, M = 100 g 10 samples, ∆tage = 0.1 Gyr

Number of normal SN at a distance

  • f 10 kpc

F ∝ L d2

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Thomas D. P . Edwards | GRAPPA | 1906.05800

Constraining Burst Like Events

19 0.0 0.2 0.4 0.6 0.8 1.0

Burst look-back time t? [Gyr]

107 108 109

Minimum Detectable N10 kpc

?

1 ppb 0.1 ppb 0.01 ppb 0.001 ppb Epsomite, M = 100 g 10 samples, ∆tage = 0.1 Gyr

Bursts that happened recently can be detected more easily Bursts a long time ago must be brighter

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Thomas D. P . Edwards | GRAPPA | 1906.05800

Star Burst Scenario

20

100 101 102 103 104 105 106 107 108 109

Number of burst CC SN, N?

10−3 10−2 10−1 100 101 102 103

Distance to burst region, D? [kpc]

LMC NGC 3603 GC

Star Formation Rate: [0.1, 1000] M yr1 ∆tstarburst = 10 Myr

107 108 109

Number of CC SN at 10 kpc, N10 kpc

?

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Thomas D. P . Edwards | GRAPPA | 1906.05800

Close by Supernova

21

100 101 102 103 104 105 106 107 108 109

Number of burst CC SN, N?

10−3 10−2 10−1 100 101 102 103

Distance to burst region, D? [kpc]

LMC NGC 3603 GC

Star Formation Rate: [0.1, 1000] M yr1 ∆tstarburst = 10 Myr

107 108 109

Number of CC SN at 10 kpc, N10 kpc

?