CROSS-CORRELA TIONSWITH INTENSITY MAPPING OF NEUTRALHYDROGEN with: - - PowerPoint PPT Presentation

DARK MA TTERAND COSMOLOGYTHROUGH CROSS-CORRELA TIONSWITH INTENSITY MAPPING OF NEUTRALHYDROGEN

Toyama, 10-09-2019 TAUP2019

with: S. Camera, N. Fornengo, M. Regis Arxiv: 1909.nnnn

Elena Pinetti University of Turin& INFN

elena.pinetti@edu.unito.it

Elena Pinetti UNITO/INFN

2

CONTENTS

❑ Why the cross-correlation technique is a powerful approach to indirect detection of DM particles? ❑ Intensity mapping of neutral hydrogen ❑ Angular power spectrum ❑ Detectability of astrophysical sources with current and future detectors ❑ Bounds in Dark Matter parameter space

Elena Pinetti UNITO/INFN

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DARK MATTER IN THE UNIVERSE

➢ Milky Way ➢ External galaxies ➢ Clusters of galaxies ➢ Cosmic web

Elena Pinetti UNITO/INFN

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DARK MATTER SEARCHES

• Production at collider (e.g. LHC)
• Direct detection

Detection in underground laboratories (e.g. LNGS)

• Indirect detection

Detection of messenger produced by annihilation o decay of DM particles:

• γ
• ν
• Cosmic rays (𝑓± , ҧ

𝑞 , ഥ 𝐸 , antinuclei)

Elena Pinetti UNITO/INFN

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GAMMA-RAY FLUX FROM DARK MATTER

Φ𝛿

𝐸𝑁 𝐹𝛿, 𝜔 = 1

4𝜌 𝜏𝑏𝑜𝑜𝑤 2𝑛𝐸𝑁

2

𝑕𝛿 𝐹𝛿 𝐽 𝜔 Particle properties Energy spectrum per annihilation event

𝐽 𝜔 = න

𝑚.𝑝.𝑡

𝜍2 𝑠 𝜇, 𝜔 𝑒𝜇

Line of sight Angle in the sky DM density

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ANISOTROPIES

The Unresolved Gamma-Ray Background is given by the sum of independent astrophysical sources/DM)

• At first approximation: isotropic
• At deeper level: there are anisotropies

Elena Pinetti UNITO/INFN

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ANISOTROPIES

The Unresolved Gamma-Ray Background is given by the sum of independent astrophysical sources/DM)

• At first approximation: isotropic
• At deeper level: there are anisotropies

Cross-correlation of an EM signal with a gravitational tracer

Elena Pinetti UNITO/INFN

8

Elena Pinetti UNITO/INFN

9

CONTENTS

✓ Why the cross-correlation technique is a powerful approach to indirect detection of DM particles? ❑ Intensity mapping of neutral hydrogen ❑ Angular power spectrum ❑ Detectability of astrophysical sources with current and future detector ❑ Bounds in Dark Matter parameter space

Elena Pinetti UNITO/INFN

10

OBSERVABLES

Gravitational tracers Galaxy catalogues Clusters catalogues Weak lensing cosmic shear HI EM signals 𝛿-rays X-rays IR emission Radio waves NEW! Cross-correlation 𝛿-rays x HI

Camera+, ApJLett 771 (2013) L5 Fornengo+, Frontiers in Physics, 2 (2014) 6 Camera+, JCAP 06 (2015) 029 Fornengo+, Ap. J. Lett. 802 (2015) 1 L1 Cuoco+, PRD 77 (2008 )123518 Ando+, PRD 90 (2014) 023514 Ando, JCAP 1410 (2014) 061 Shirasaki+, PRD 90 (2014) 063502 Xia+, APJS 217 (2015) 15 Shirasaki+, PRD 92 (2015) 123540 Regis+, ApJS 221 (2015) 29 Shirasaki+, PRD 94 (2016) 063522 Troester+, MNRAS 467 (2017) 2706 Branchini+, ApJS 228 (2017) 1 Ammazzalorso+, PRD98 (2018) 103007 Colavincenzo+, arXiv:1907.05264 Ammazzalorso+, arXiv:1907.13484

Elena Pinetti UNITO/INFN

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GAMMA-RAYS

• Dark Matter
• BL Lacertae
• Flat-Spectrum Radio Quasar
• Misaligned Active Galactic

Nuclei

• Star-Forming Galaxies

Elena Pinetti UNITO/INFN

INTENSITYMAPPING

Discovering the unknown

12

Elena Pinetti UNITO/INFN

IM is a mapping of the intensity fluctuations

• f a tracer of the haloes mass

It allows to map the large-scale structure of the Universe with a measure of the intensity

• f the redshifted 21 cm line of HI.

Advantages: 𝑤𝑝 𝑤𝑓 = 1 + 𝑨 −1 Not necessary to resolve galaxies individually

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INTENSITY MAPPING

Discovering the unknown

Elena Pinetti UNITO/INFN

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CONTENTS

✓ Why the cross-correlation technique is a powerful approach to indirect detection of DM particles? ✓ Intensity mapping of neutral hydrogen ❑ Angular power spectrum ❑ Detectability of astrophysical sources with current and future detector ❑ Bounds in Dark Matter parameter space

Elena Pinetti UNITO/INFN

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POWER SPECTRA

𝑄𝑗𝑘

1ℎ =

න

𝑁𝑛𝑗𝑜 𝑁𝑛𝑏𝑦

𝑒𝑁 𝑒𝑜 𝑒𝑁 𝑔

𝑗 ∗𝑔 𝑘

𝑄𝑗𝑘

2ℎ =

න

𝑁𝑛𝑗𝑜 𝑁𝑛𝑏𝑦

𝑒𝑁1 𝑒𝑜 𝑒𝑁1 𝑐𝑗𝑔

𝑗 ∗

න

𝑁𝑛𝑗𝑜 𝑁𝑛𝑏𝑦

𝑒𝑁2 𝑒𝑜 𝑒𝑁2 𝑐

𝑘𝑔 𝑘 𝑄𝑚𝑗𝑜

𝑄𝑗𝑘 = 𝑄𝑗𝑘

1ℎ + 𝑄𝑗𝑘 2ℎ

𝐷𝑚

(𝑗𝑘) =

1 𝐽𝑗 𝐽

𝑘

න 𝑒𝜓 𝜓2 𝑋

𝑗 𝜓 𝑋 𝑘 𝜓 𝑄𝑗𝑘 𝑙 = 𝑚

𝜓 , 𝜓 Window Functions Non-Linear Power Spectrum Angular Power Spectrum

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CROSS-CORRELATION HI X 𝛿-RAYS

NEW!

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WINDOW FUNCTIONS

E = 5 GeV

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MODEL VALIDATION: AUTOCORRELATION

NEW!

Measure: Martin et al. (2012) Measure: Ackermann et al. (2018)

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EXPERIMENTS

Fermi-LAT

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EXPERIMENTAL CONFIGURATIONS

Bin 𝐅𝐧𝐣𝐨 [𝐇𝐟𝐖] 𝐅𝐧𝐛𝐲 [𝐇𝐟𝐖] 𝐎𝛅 [𝐝𝐧−𝟓𝐭−𝟑𝐭𝐬−𝟐] 𝐠𝐭𝐥𝐳 𝛕𝟏 [𝐞𝐟𝐡] 1 0.5 1.0 1.056 ∙ 10−17 0.134 0.9 2 1.0 1.7 3.548 ∙ 10−18 0.184 0.5 3 1.7 2.8 1.375 ∙ 10−18 0.398 0.3 4 2.8 4.8 8.324 ∙ 10−19 0.482 0.2 5 4.8 8.3 3.904 ∙ 10−19 0.594 0.2 6 8.3 14.5 1.768 ∙ 10−19 0.574 0.1 7 14.5 22.9 6.899 ∙ 10−20 0.574 0.09 8 22.9 39.8 3.895 ∙ 10−20 0.574 0.07 9 39.8 69.2 1.576 ∙ 10−20 0.574 0.07 10 69.2 120.2 6.205 ∙ 10−21 0.574 0.06 11 120.2 331.1 3.287 ∙ 10−21 0.597 0.06 12 331.1 1000 5.094 ∙ 10−22 0.597 0.06

MeerKAT SKA1 S [𝐞𝐟𝐡𝟑] 4000 15000

𝐠𝐭𝐥𝐳

0.097 0.36 t 4000 hr 1 yr 𝐎𝐞 64 133 + 64 𝐄𝐞𝐣𝐭𝐢 [𝐧] 13.5 14.5 𝐄𝐣𝐨𝐮𝐟𝐬𝐠 [𝐥𝐧] 1 10 [𝐴𝐧𝐣𝐨, 𝐴𝐧𝐛𝐲] Band A: [0.0, 0.58] Band B: [0.4, 1.45] Band 1: [0.35, 3.0] Band 2: [0.0, 0.5]

Configuration

Single-dish Interferometer Single-dish Interferometer

Ackermann et al. (2018)

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FORECAST FOR 21 CM LINE X 𝛿-RAYS

Band 2: 0 < z < 0.5 SKA1, 1.0-1.7 GeV MeerKAT, 1.0-1.7 GeV Band A: 0 < z < 0.58

∆𝐷𝑚

𝐼𝐽×𝛿 =

1 2𝑚 + 1 𝑔

𝑡𝑙𝑧

𝐷𝑚

𝐼𝐽×𝛿 2 +

𝐷𝑚

𝛿𝛿 + 𝑂𝛿

𝐶𝑚,𝛿

2

𝐷𝑚

𝐼𝐽×𝐼𝐽 + 𝑂𝐼𝐽

𝐶𝑚,𝐼𝐽

2

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SKA1 MeerKAT

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CONTENTS

✓ Why the cross-correlation technique is a powerful approach to indirect detection of DM particles? ✓ Intensity mapping of neutral hydrogen ✓ Angular power spectrum ❑ Detectability of astrophysical sources with current and future detector ❑ Bounds in Dark Matter parameter space

Elena Pinetti UNITO/INFN

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SNR FOR ASTROPHYSICAL SOURCES

𝑇𝑂𝑆 = 𝑜 𝜏 𝑇𝑂𝑆2 = ෍

𝑗=𝑚,𝐹

𝐷𝑗

𝐼𝐽 × 𝑇

∆𝐷𝑗

𝐼𝐽 ×𝑇 2

SKA 1 Single-dish Combined Band 1 5.5σ 8.1σ Band 2 6.2σ 6.6σ Band 1: 0.35 < z < 3 Band 2: 0 < z < 0.5 MeerKAT Single-dish Combined Band A 3.5σ 3.8σ Band B 3.9σ 5.4σ Band A: 0 < z < 0.58 Band B: 0.4 < z < 1.45

Elena Pinetti UNITO/INFN

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FORECAST FOR DARK MATTER BOUNDS

Δ𝜓2 𝜏𝑤 = 4 95% CL ∆𝜓2 = 𝜓𝐸𝑁+𝑇

2

− 𝜓𝑇

2

SKA1 MeerKAT Band A: 0 < z < 0.58 Band B: 0.4 < z < 1.45 Band 1: 0.35 < z < 3 Band 2: 0 < z < 0.5

combined combined combined combined

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SKA2 + FERMISSIMO

SKA2 S [𝐞𝐟𝐡𝟑] 30000 𝐠𝐭𝐥𝐳 0.72 t 1 yr 𝐎𝐞 70000 𝐄𝐞𝐣𝐭𝐢 [𝐧] 3.1 𝐄𝐣𝐨𝐮𝐟𝐬𝐠 [𝐥𝐧] 300 [𝐴𝐧𝐣𝐨, 𝐴𝐧𝐛𝐲] [0.0, 0.5]

Fermissimo Exposure 2 ∙ expFermi Angular resolution Conservative: 0.5 ∙ σb

Fermi

Optimistic: 0.2 ∙ σb

Fermi

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TAKE HOME MESSAGE

𝒏𝝍 = 𝟐𝟏𝟏 𝐇𝐟𝐖

The cross-correlation HI × γ-rays is a very promising channel

1

MeerKAT: SKA1:

2

SNR > 5σ SNR > 8σ Competitive bounds for DM with SKA1 and SKA2+Fermissimo:

3

SKA1+Fermi SKA2+Fermissimo 2σ bound 2σ bound 5σ detection 0.50 × σv th 0.01 × σv th 0.10 × σv th

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TAKE HOME MESSAGE

𝒏𝝍 = 𝟐𝟏𝟏 𝐇𝐟𝐖

The cross-correlation HI × γ-rays is a very promising channel

1

MeerKAT: SKA1:

2

SNR > 5σ SNR > 8σ Competitive bounds for DM with SKA1 and SKA2+Fermissimo:

3

SKA1+Fermi SKA2+Fermissimo 2σ bound 2σ bound 5σ detection 0.50 × σv th 0.01 × σv th 0.10 × σv th

Elena Pinetti UNITO/INFN

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BACKUP SLIDES

‘Cause you never know!

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OTHER RESULTSAND ERROR ESTIMATION

• Forecast for 21 cm line x γ-rays
• Forecast SKA1
• Forecast SKA2 + Fermissimo
• Angular Power Spectrum
• Error estimation
• Noise vs signal for Fermi and Fermissimo

Elena Pinetti UNITO/INFN

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FORECAST FOR 21 CM LINE X 𝛿-RAYS

NEW!

Band 2: 0 < z < 0.5 Combined 𝑛𝐸𝑁 = 100 GeV SKA1, 1.0-1.7 GeV SKA1, 1.7-2.8 GeV MeerKAT, 1.0-1.7 GeV MeerKAT, 1.7-2.8 GeV Band A: 0 < z < 0.58 Combined

Elena Pinetti UNITO/INFN

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FORECAST SKA1

NEW!

Band 2: 0 < z < 0.5 𝑛𝐸𝑁 = 100 GeV Band 2, single-dish Band 2, combined SKA1, 1.0-1.7 GeV Band 1, single-dish Band 1, combined Band 1: 0.35 < z < 3.0

Elena Pinetti UNITO/INFN

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FORECAST SKA2 + FERMISSIMO

NEW!

Band 2: 0 < z < 0.5 𝑛𝐸𝑁 = 100 GeV 1.0-1.7 GeV Interferometer 8.3-14.5 GeV

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ERROR ESTIMATION

∆𝐷𝑚 =

2 2𝑚+1 𝑔𝑡𝑙𝑧 𝐷𝑚 + 𝐷𝑂 𝐶𝑚

2

Auto-correlation ∆𝐷𝑚

𝑗𝑘 =

1 2𝑚 + 1 𝑔

𝑡𝑙𝑧

𝐷𝑚

𝑗𝑘 2

+ 𝐷𝑚

𝑗𝑗 + 𝑂𝑗

𝐶𝑚,𝑗

2

𝐷𝑚

𝑘𝑘 + 𝑂 𝑘

𝐶𝑚,𝑘

2

Cross-correlation 𝑈

𝑡𝑧𝑡 =

30 + 60 300 𝑁𝐼𝑨 𝜉

2.35

𝐿 𝐶𝑚

𝐼𝐽 = 𝑓𝑦𝑞 − 𝑚2

2 1.22 8 ln 2 𝜇𝑝 𝐸 𝐶𝑚

𝐸𝑁 = 𝑓𝑦𝑞 − 𝑚2𝜏𝑐 2

2 𝑂𝑗𝑜𝑢𝑓𝑠𝑔

𝐼𝐽

= 𝑈

𝑡𝑧𝑡 2

∙ 2𝜌 3 𝑔2 𝑚 ∙ 𝑚𝑛𝑏𝑦

2

∙ 𝑢 ∙ ∆𝜉

Maximal resolution Filling factor

𝑂𝑗𝑜𝑢𝑓𝑠𝑔

𝐼𝐽

= 𝑈

𝑡𝑧𝑡 2

∙ 𝑇𝐼𝐽 𝑂𝑒 ∙ 𝑢 ∙ ∆𝜉 𝜏𝑐 = 𝜏0 1 + 0.25𝜏0𝑚 −1 𝜏0

𝐺𝑓𝑠𝑛𝑗 = 𝜏∗ 0.5 GeV ∙

𝐹 0.5 GeV

−0.95

+ 0.05 deg 𝜏0

𝐺𝑓𝑠𝑛𝑗𝑡𝑡𝑗𝑛𝑝 = 𝑂 ∙ 𝜏∗ 0.5 GeV ∙

𝐹 0.5 GeV

−0.95

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NOISE VS SIGNAL FOR FERMI AND FERMISSIMO

1.0-1.7 GeV 69.2-120.2 GeV

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MODELLING THE ASTROPHYSICAL SOURCES

• GLF
• Numbers
• Bias
• Window functions at different

energies

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GAMMA LUMINOSITY FUNCTIONS

𝜚𝐶𝑀 𝑀𝑏𝑑 = 𝜚0 ∙ 1 + 𝑨 1 + 𝑨𝑑

−4.50

+ 1 + 𝑨 1 + 𝑨𝑑

12.88 −1

𝜚𝐺𝑇𝑆𝑅 = 𝜚0 ∙ 1 + 𝑨 1 + 𝑨𝑑

−7.35

+ 1 + 𝑨 1 + 𝑨𝑑

6.51 −1

𝜚𝑛𝐵𝐻𝑂 = 𝜚0 ∙ 1 + 𝑨 𝛽−2 𝜚𝑇𝐺𝐻 = 𝜚𝐽𝑆 𝑀𝐽𝑆 ∙ 𝑒𝑀𝐽𝑆 𝑒𝑀𝛿 𝜚𝐽𝑆 = 𝜚𝑡𝑞𝑗𝑠𝑏𝑚 + 𝜚𝑡𝑢𝑏𝑠𝑐𝑣𝑠𝑡𝑢 + 𝜚𝑇𝐺−𝐵𝐻𝑂 𝜚𝑗,𝐽𝑆 = 𝜚0 ∙ 𝑀𝐽𝑆 𝑀0,𝑗

1−𝛾𝑗

𝑓𝑦𝑞 − 1 2𝜏𝑗

2 ∙

𝑚𝑝𝑕10 1 + 𝑀𝐽𝑆 𝑀0,𝑗

2

𝑀𝐽𝑆 = 𝑀𝛿

1 𝛽𝐽𝑆 ∙ 10 10−𝛾𝐽𝑆 𝛽𝐽𝑆 𝑀⨀

𝜚𝐶𝑀 𝑀𝑏𝑑: Ajello et al. (2014) 𝜚𝐺𝑇𝑆𝑅: Ajello et al. (2012) 𝜚𝑛𝐵𝐻𝑂: Di Mauro et al. (2018) 𝜚𝑇𝐺𝐻: Gruppioni et al. (2012)

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BIAS

𝑐𝑇 = න

𝑀𝑛𝑗𝑜 𝑀𝑛𝑏𝑦

𝑒𝑀 𝑀 𝜚 < 𝑕𝑡 > 𝑐1 𝑐1 = 1 + 𝜁1 + 𝐹1 𝜁1 = 𝑟𝜉 − 1 𝜀𝑡𝑑(𝑨) 𝐹1 = 2𝑞 𝜀𝑡𝑑(𝑨)(1 + (𝑟𝜉)𝑞) 𝑟 = 0.707 p= 0.3 𝜉 = 𝜀𝑡𝑑

2

𝜏2 𝜏2~ න 𝑒𝑙 𝑄𝑚𝑗𝑜

𝑐1: Cooray & Sheth (2002)

𝑐𝐼𝐽 = 1 ҧ 𝜍𝐼𝐽 න

𝑁𝑛𝑗𝑜 𝑁𝑛𝑏𝑦

𝑒𝑁 𝑒𝑜 𝑒𝑁 𝑁𝐼𝐽(𝑁) 𝑐1

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NUMBERS, NUMBERS, STILL NUMBERS…

• BL Lac

𝑀𝑛𝑗𝑜 = 7 ∙ 1043 𝑓𝑠𝑕 𝑡−1 𝑀𝑏𝑡𝑢𝑠𝑝 = 1052 𝑓𝑠𝑕 𝑡−1 𝛽 = 2.11

• FSRQ

𝑀𝑛𝑗𝑜 = 1044 𝑓𝑠𝑕 𝑡−1 𝑀𝑏𝑡𝑢𝑠𝑝 = 1052 𝑓𝑠𝑕 𝑡−1 𝛽 = 2.44

• mAGN

𝑀𝑛𝑗𝑜 = 1040 𝑓𝑠𝑕 𝑡−1 𝑀𝑏𝑡𝑢𝑠𝑝 = 1050 𝑓𝑠𝑕 𝑡−1 𝛽 = 2.37

• SFG

𝑀𝑛𝑗𝑜 = 1037 𝑓𝑠𝑕 𝑡−1 𝑀𝑏𝑡𝑢𝑠𝑝 = 1040 𝑓𝑠𝑕 𝑡−1 𝛽 = 2.7

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WINDOW FUNCTIONS

𝑋

𝐼𝐽 𝑨 = 𝑋 0𝑈𝑝𝑐𝑡(𝑨)

WHI: Battye et al. 2012 𝑋

𝛿 𝐹, 𝑨 =

1 4𝜌 𝜏𝑤 2 ∆2 Ω𝐸𝑁 𝜍𝑑 𝑛𝐸𝑁

2

1 + 𝑨 3 𝑒𝑂 𝑒𝐹 𝐹 1 + 𝑨 𝑓−𝜐 dN/dE: Cembranos et al. 2010 τ: Finke et al. 2009

𝑋

𝑡 𝛿(𝐹, 𝑨) =

𝑒𝑀 1 + 𝑨

2

∙ න

𝑀𝑛𝑗𝑜 𝑀𝑛𝑏𝑦

𝑒𝑀 𝑒𝐺 𝑒𝐹 ∙ 𝜚

E = 5 GeV

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WINDOW FUNCTIONS

15 GeV 5 GeV

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BACKGROUND

• Astrophysical background
• Intensity Mapping background

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ASTROPHYSICAL BACKGROUND

The astrophysical background is due to the EM emitters.

• White dwarfs
• Neutron stars
• Sun
• BHs
• Hot gas

X-rays γ-rays

• Galactic emission
• Resolved astrophysical sources
• UGRB (blazar, star-forming galaxies,

millisecond pulsar) IR

• Dust

Radio

• Synchrotron emission
• Free-free emission
• Bright radio galaxies
• AGN
• Star-forming galaxies

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INTENSITY MAPPING BACKGROUND

Galactic Extra-galactic

• Synchrotron emission
• Free-free emission
• Bright radio galaxies
• AGN
• Star-forming galaxies

Atmospherical noise Radio interference

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45

POWER SPECTRUM

• Linear PS
• HI - HI
• δ - HI
• δ2 − δ2
• δ2 - HI
• Comparison among PS
• Astro-Astro
• HI - gamma

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46

LINEAR POWER SPECTRUM

𝑄𝑚𝑗𝑜 = 2𝜌2 𝑑 𝐼0

𝑜+3

𝜀𝐼

2 𝑙𝑜 𝑈2(𝑙)

𝐸(𝑨) 𝐸(𝑨 = 0)

2

Primordial power spectrum Growth factor

Δ𝜍 ҧ 𝜍 ≪ 1

CAMB: Code for Anisotropies in the Microwave Background

Transfer function

Elena Pinetti

Elena Pinetti UNITO/INFN

47

HI POWER SPECTRUM

𝑄𝐼𝐽−𝐼𝐽

1ℎ

(𝑙) = න

𝑁𝑛𝑗𝑜 𝑁𝑛𝑏𝑦

𝑒𝑁 𝑒𝑜 𝑒𝑁 ෤ 𝑤𝐼𝐽 𝑙, 𝑁 2 𝑄𝐼𝐽−𝐼𝐽

2ℎ

𝑙 = න

𝑁𝑛𝑗𝑜 𝑁𝑛𝑏𝑦

𝑒𝑁 𝑒𝑜 𝑒𝑁 𝑐 𝑁 ෤ 𝑤𝐼𝐽 𝑙, 𝑁

2

𝑄𝑚𝑗𝑜 𝑙

𝜍𝐼𝐽: Padmanabhan et al. MNRAS, Volume 469, Issue 2, p.2323-2334 (2017)

Elena Pinetti UNITO/INFN

48

CROSS-CORRELAZIONE DM-HI

NEW!

𝑄

𝜀−𝐼𝐽 1ℎ

𝑙 = න

𝑁𝑛𝑗𝑜 𝑁𝑛𝑏𝑦

𝑒𝑁 𝑒𝑜 𝑒𝑁 𝑁𝐼𝐽(𝑁)෤ 𝑤𝐸𝑁 𝑙, 𝑁 ෤ 𝑤𝐼𝐽 𝑙, 𝑁 𝑄

𝜀−𝐼𝐽 2ℎ

𝑙 = න

𝑁𝑛𝑗𝑜 𝑁𝑛𝑏𝑦

𝑒𝑁 𝑒𝑜 𝑒𝑁 𝑐 𝑁 ෤ 𝑤𝐸𝑁 𝑙, 𝑁 න

𝑁𝑛𝑗𝑜 𝑁𝑛𝑏𝑦

𝑒𝑁 𝑒𝑜 𝑒𝑁 𝑁𝐼𝐽(𝑁) 𝑐 𝑁 ෤ 𝑤𝐼𝐽 𝑙, 𝑁 𝑄𝑚𝑗𝑜 𝑙

Elena Pinetti UNITO/INFN

49

DARK MATTER ANNIHILATION

𝑄

𝜀2𝜀2 1ℎ (𝑙) =

න

𝑁𝑛𝑗𝑜 𝑁𝑛𝑏𝑦

𝑒𝑁 𝑒𝑜 𝑒𝑁 ෤ 𝑤𝐸𝑁 ∆2

2

𝑄

𝜀2𝜀2 2ℎ (𝑙) =

න

𝑁𝑛𝑗𝑜 𝑁𝑛𝑏𝑦

𝑒𝑁 𝑒𝑜 𝑒𝑁 𝑐 𝑁 ෤ 𝑤𝐸𝑁 ∆2

2

𝑄𝑚𝑗𝑜(𝑙) ∆2 𝑨 = 𝜍2 ҧ 𝜍2 = න

𝑁𝑛𝑗𝑜 𝑁𝑛𝑏𝑦 𝑒𝑜

𝑒𝑁 න 𝑒3𝑦 𝜍2 ҧ 𝜍2 1 + 𝐶𝑡𝑣𝑐(𝑁, 𝑨) Clumping factor Without boost With boost

Elena Pinetti UNITO/INFN

50

CROSS-CORRELATION𝜀2- HI

𝑄

𝜀2−𝐼𝐽 1ℎ

𝑙 = න

𝑁𝑛𝑗𝑜 𝑁𝑛𝑏𝑦

𝑒𝑁 𝑒𝑜 𝑒𝑁 ෤ 𝑤𝐸𝑁(𝑙, 𝑁) ∆2 ෤ 𝑤𝐼𝐽 𝑙, 𝑁 𝑄

𝜀2−𝐼𝐽 2ℎ

𝑙 = න

𝑁𝑛𝑗𝑜 𝑁𝑛𝑏𝑦

𝑒𝑁 𝑒𝑜 𝑒𝑁 𝑐 𝑁 ෤ 𝑤𝐸𝑁(𝑙, 𝑁) ∆2 න

𝑁𝑛𝑗𝑜 𝑁𝑛𝑏𝑦

𝑒𝑁 𝑒𝑜 𝑒𝑁 𝑐 𝑁 ෤ 𝑤𝐼𝐽 𝑙, 𝑁 𝑄𝑚𝑗𝑜 𝑙

NEW!

∆2 𝑨 = 𝜍2 ҧ 𝜍2 = න

𝑁𝑛𝑗𝑜 𝑁𝑛𝑏𝑦 𝑒𝑜

𝑒𝑁 න 𝑒3𝑦 𝜍2 ҧ 𝜍2 1 + 𝐶𝑡𝑣𝑐(𝑁, 𝑨)

𝐶𝑡𝑣𝑐: Moliné et al. Volume 466, Issue 4, p. 4974–4990 (2017)

Boost Factor

Elena Pinetti UNITO/INFN

51

COMPARISON AMONG POWER SPECTRA

𝜀2 − 𝜀2: auto − correlation 𝛿𝑏𝑜𝑜 HI − HI: auto − correlation HI δ2 − HI: cross-correlation 𝛿𝑏𝑜𝑜 x HI δ − HI: cross-correlation Galaxies x HI cross-correlation Shear x HI δ2 − δ: cross-correlation 𝛿𝑏𝑜𝑜 x Shear cross-correlation 𝛿𝑏𝑜𝑜 x Galaxies

Elena Pinetti UNITO/INFN

52

AUTO-CORRELATION PS FOR ASTROPHYSICAL SOURCES

𝑄

𝑡𝑡 1ℎ = න 𝑀𝑛𝑗𝑜 𝑀𝑛𝑏𝑦

𝑒𝑀 𝑀 ∙ 𝜚 ∙ 𝑀 < 𝑕𝑡 >

2

𝑄

𝑡𝑡 2ℎ = න 𝑀𝑛𝑗𝑜 𝑀𝑛𝑏𝑦

𝑒𝑀 𝑀 ∙ 𝜚 ∙ 𝑐𝑡 ∙ 𝑀 < 𝑕𝑡 >

2

∙ 𝑄𝑚𝑗𝑜 𝑐𝑡 = න

𝑀𝑛𝑗𝑜 𝑀𝑛𝑏𝑦

𝑒𝑀 𝑀 ∙ 𝜚 < 𝑕𝑡 > ∙ 𝑐1 < 𝑕𝑡> = න

𝑀𝑛𝑗𝑜 𝑀𝑛𝑏𝑦

𝑒𝑀 𝑀 ∙ 𝜚

where:

Elena Pinetti UNITO/INFN

53

CROSS-CORRELATION HI x 𝛿-RAYS

𝑄𝐼𝐽−𝑇

1ℎ

= න

𝑀𝑛𝑗𝑜 𝑀𝑛𝑏𝑦

𝑒𝑀 𝑀 < 𝑕𝑇 > ∙ 𝜚 ∙ 𝑣𝐼𝐽 𝑁 𝑀 ∙ 𝑁𝐼𝐽 𝑁 𝑀 ҧ 𝜍𝐼𝐽 𝑄𝐼𝐽−𝑇

2ℎ

= ׬

𝑁𝑛𝑗𝑜 𝑁𝑛𝑏𝑦 𝑒𝑁 𝑒𝑜 𝑒𝑁 𝑣𝐼𝐽 ∙ 𝑐1 ∙

׬

𝑀𝑛𝑗𝑜 𝑀𝑛𝑏𝑦 𝑒𝑀 𝜚 ∙ 𝑁𝐼𝐽 𝑁 𝑀 ഥ 𝜍𝐼𝐽

𝑄𝑚𝑗𝑜 NEW!

Elena Pinetti UNITO/INFN

54

OTHER STUFF

• DM particle properties
• Radiotelescopes
• Intensity of the gamma-ray flux
• Bounds for DM from UGRB intensity
• Comparison among DM bounds
• What’s next?
• Multiwavelength research
• Definition APS

Elena Pinetti UNITO/INFN

55

PROPERTIES OF A DARK MATTER PARTICLE

The relevant properties of a DM particle that we can derive from indirect detection of an astrophysical signal are: ➢ Annihilation cross-section or decay rate ➢ Mass ➢ BR in the different final states Signal amplitude 𝑛𝐸𝑁 , 𝜏𝑤 , Γ Spectral features: 𝑛𝐸𝑁 , BR

Elena Pinetti UNITO/INFN

56

RADIOTELESCOPES AND SKA PRECURSORS

Green Bank Telescope (USA) CHIME (Canada) MeerKAT (South Africa) ASKAP (Australia)

Elena Pinetti UNITO/INFN

57

INTENSITY OF THE GAMMA-RAY FLUX

𝐽𝛿 = න

𝑨𝑛𝑗𝑜 𝑨𝑛𝑏𝑦

𝑒𝑨 𝑑 𝐼(𝑨) 𝑋

𝛿

𝑋

𝛿 =

𝑒𝑀 1 + 𝑨

2

∙ න

𝑀𝑛𝑗𝑜 𝑀𝑛𝑏𝑦

𝑒𝑀 𝑒𝐺 𝑒𝐹 ∙ 𝜚 𝑒𝐺 𝑒𝐹 = 𝑀 2 − 𝛽 4𝜌 𝑒𝑀

2

100 1 + 𝑨

2−𝛽

− 0.1 1 + 𝑨

2−𝛽

∙ 𝐹 GeV

−𝛽

𝑓−𝜐 𝐹 1+𝑨

Elena Pinetti UNITO/INFN

58

BOUNDS ON DM FROM THE UGRB INTENSITY

Diffused extragalactic emission Dwarfs Spheroidals galaxies

Fornasa, Sanchez-Conde, Phys.

• Rep. 598 (2015) 1

Elena Pinetti UNITO/INFN

59

COMPARISON AMONG DARK MATTER BOUNDS

MeerKAT SKA1

combined combined combined combined

Elena Pinetti UNITO/INFN

60

Particle DM

➢X-HI ➢IR-HI ➢Radio-HI

Cosmology

➢Gravitational lensing-HI ➢Galaxy-HI ➢Cluster-HI

Elena Pinetti UNITO/INFN

61

MULTIWAVELENGTH RESEARCH OF DARK MATTER

𝐹𝛿 ≤ 𝑛𝐸𝑁

Elena Pinetti UNITO/INFN

62

ANGULAR POWER SPECTRUM

𝜀𝐽𝑕 ≡ 𝐽𝑕 ෤ 𝑜 − 𝐽𝑕 = 𝐽𝑕 σ𝑚,𝑛 𝑏𝑚𝑛 𝑍

𝑚𝑛(ො

𝑜)

𝐽𝑕 ො 𝑜 = න 𝑒𝜓 𝑕(𝜓, ො 𝑜) ෩ 𝑋(𝜓)

Angular Power Spectrum 𝐷𝑚

𝑗𝑘 ≡

1 2𝑚 + 1 ෍

𝑛=−𝑚 𝑚

𝑏𝑚𝑛

(𝑗)𝑏𝑚𝑛 ∗(𝑘)

𝐷𝑚

(𝑗𝑘) =

1 𝐽𝑗 𝐽

𝑘

න 𝑒𝜓 𝜓2 𝑋

𝑗 𝜓 𝑋 𝑘 𝜓 𝑄𝑗𝑘 𝑙 = 𝑚

𝜓 , 𝜓

𝑏𝑚𝑛 = 1 𝐽𝑕 න 𝑒 ො 𝑜 𝜀𝐽𝑕 ො 𝑜 𝑍

𝑚𝑛 ∗

ො 𝑜 = 1 𝐽𝑕 න 𝑒 ො 𝑜 𝑒𝜓 𝑔

𝑕 𝜓, Ԧ

𝑠 𝑋 𝜓 𝑍

𝑚𝑛 ∗

ො 𝑜 𝑔

𝑕 = 𝑕

𝑕 − 1

𝑔

𝑗(𝑙)𝑔 𝑘 ∗(𝑙′) = (2𝜌)3 𝜀3 𝑙 − 𝑙′ 𝑄𝑗𝑘(𝑙)