Non-Accelerator Experiments Astro-particle Physics Cosmology Dark - - PowerPoint PPT Presentation

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Non-Accelerator Experiments Astro-particle Physics Cosmology Dark - - PowerPoint PPT Presentation

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Non-Accelerator Experiments Astro-particle Physics Cosmology Dark Matter The 40th Anniversary Symposium of the US-Japan Science and Technology Cooperation Program in High Energy Physics April 16, 2019 @ University of Hawaii Akito Kusaka

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Non-Accelerator Experiments

Astro-particle Physics Cosmology Dark Matter

The 40th Anniversary Symposium of the US-Japan Science and Technology Cooperation Program in High Energy Physics April 16, 2019 @ University of Hawaii Akito Kusaka (Berkeley Lab. & University of Tokyo)

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Disclaimer & Acknowledgement

  • Blame me for mistakes and bias/unfairness.
  • And perhaps the organizer for selecting me. (but thanks!)
  • Acknowledgement: inputs/lectures from colleagues.
  • Peter Sorensen (LBNL) for Dark Matter
  • Kohta Murase (Penn State) for Astroparticle
  • Hironao Miyatake (Nagoya), David Schlegel, Natalie Roe (LBNL) for Optical

Surveys

  • Osamu Tajima (Kyoto); US-Japan Japan PI
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SLIDE 3

Higgs Yukawa n ത 𝐶/𝐶 Dark Matter Dark Energy Inflation 5th force? TeV Light New Particle?

My summary of “Snowmass Questions” 2014 (But I cannot trace citation path at this point)

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SLIDE 4
  • Early Universe: extreme and clean

environment

  • Inflation
  • Relics: Baryogenesis, Dark Matter,

Neutrinos, Unknown Unknown

  • Gravity: with other forces

suppressed

  • Dark Matter and Dark Energy
  • Neutrinos
  • Vacuum:
  • Axions
  • Dark Energy
  • Particle acceleration

What/Why do we learn from the Universe?

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Cosmic Microwave Background

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CMB: primordial gravitational waves

“Cosmic background is absolutely exciting – I’ve never expected it to be as exciting as it is now. I mean, finding the B modes is just unbelievably important.” (Rainer Weiss, Segre lecture at UC Berkeley, 2016)

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SLIDE 7

CMB: primordial gravitational waves

  • We only observe t=380k yr.
  • Really want to know: t≪1 sec.
  • Things happened in between:
  • Bad: things get washed out.
  • Good: physics well understood.

Preserved “signal”?

  • Gravitational Waves
  • Inflation, gravity quantization
  • Sound waves
  • “Seed” of structure
  • Non-Gaussianity

I want to know this I can only see this Lots of things happened…

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CMB: “backlight” shedding on cosmic evolution

Order ~1 improvement by next-generation instruments  Leap in cosmology and HEP. A huge HEP laboratory Axion? Sterile n? 𝜀 ∑𝑛𝜉 ~30meV Implication on hierarchy Understanding Vacuum

Redshi hift+1 +1

Primord

  • rdial

al (quantum ntum) fluctua ctuatio tion

credits: ESO

380k yr

Thermal relics

100M yr

Reioni niza zati tion

1B yr

Sum of Neutrino mass

4B yr 8B yr 13.8B yr

Galaxy Evolution

Dark Energy

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CMB Polarization: where do we stand now?

r S mn Neff

Compilation by L. Page

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SPT-3G BICEP3 Keck Array  BICEP Array Site at South Pole (near IceCube etc.) AdvACT POLARBEAR / Simons Array CLASS Site in Northern Chile (near ALMA) GroundBIRD SPIDER LiteBIRD

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Timeline

2020 2025 2030

BICEP Array AdvACT, SPT-3G

Simons Array Simons Observatory

GroundBIRD

CMB-S4 LiteBIRD

𝜏(𝑠)

~ 0.006 0.003 ~ 0.002 ~ 0.001

POLARBEAR

Current Experiments w/ Significant US-Japan Collaboration

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SLIDE 12

US-Japan: acknowledgement and shameless advertisement

TES

Broadband antenna

MKIDs

Next Generation of

Superconducting

Devices for Photon and Particle Sensing: Universal Detector and

Readout Systems for

Large-Format Arrays PIs: O. Tajima & A. Kusaka Applications:

CMB Dark Matter 0n2b Quantum Sensing

Collaborators:

Kyoto, IPMU, Tohoku, KEK LBNL, SLAC, UCB, NIST

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US-Japan: acknowledgement and shameless advertisement

CMB CMB

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Cosmology: Optical Surveys

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Cosmology: optical surveys

measuring gravity in a broad sense Gravity acting on spacetime Gravity acting on matter

Type Ia Supernovae Baryon Acoustic Oscillation Cluster Number Count Weak Gravitational Lensing Redshift Space Distortion

Image credit: BOSS/SDSS Image credit: ESA

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Cosmology: spectroscopic surveys

DESI

4m telescope Automated, robotic, 5000 fibers Ten spectrographs

3D map of 35M galaxies Expansion history: z=0~3.5 Dark Energy Equation of State Neutrinos mass and species, …

PFS and Euclid are also starting soon.

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Cosmology: imaging surveys

Image credit: M. Oguri

Subaru/HSC

8.2m telescope 1B pixels 1.5 deg. FoV Current: HSC, DES, Pan-STARRS, KiDS Upcoming: LSST, Euclid, WFIRST US-Japan: Yet another shameless advertisement

Dark Energy Matter fluctuation Growth of Structure Neutrinos Modified gravity

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Direct Dark Matter Search

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Evidence for “cold” dark matter

Clowe et al. (2006) Begeman, Broels & Sanders (1991) Planck Collaboration (2014 & 2015)

Cold = non relativistic (for a while) Weak (or no) interaction other than gravity. Energy density: 1/4 of the current universe.

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Dark Matter model space

Inspired by Neil Weiner’s slide (2017)

WIMPs (SUSY) Cold Axions

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Dark Matter: Noble liquid detectors

LUX/LZ (Xe 250kg  7t) XENON (Xe 2t  6t) PandaX (Xe 580kg  4t) DarkSide (Ar 46kg  20t) XMASS (Xe 835kg) DEAP-3600 (Ar 3.2t)

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Dark Matter: Noble liquid detectors

Reaching neutrino floor “soon.”

Plot from A. Manalaysay’s talk (2019)

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Dark Matter: cryogenic detectors

Super CDMS EDELWEISS CRESST And others PICO, NEWS-G, DAMIC, SENSEI, …

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Dark Matter: cryogenic detectors

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Dark Matter: Axion searches

Plot from PDG (2017)

HAYSTAC

Plot from Zhong et al. (2018) ADMX gen-2 (e.g., talk by Carosi 2019)

ADMX

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Dark Matter model space

WIMPs (SUSY) Cold Axions

  • Ex. non-DM Axions
  • Ex. Sub-GeV DMs

Lots of effort blooming

  • Ex. QIS  DM

LDMX @ SLAC

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SLIDE 27

Astroparticle

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SLIDE 28

Astroparticle

Neutrinos

IceCube, Super-K, ANITA, KM3Net, …

Gravitational Waves

LIGO, Virgo, KAGURA

Gamma Rays

Fermi, HAWC HESS, MAGIC, VERITAS, CTA, …

Cosmic Rays

PAMELA, AMS-02 Auger, Telescope Array, …

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SLIDE 29

Astroparticle

LIGO, Virgo, Fermi, INTEGRAL, … (2017) Fermi 2016 Auger 2018

Extremely rich astrophysics expected

GWs, High energy n, … Multi-purpose, multi-particle detector system

Particle physics implication?

Ex.: 𝑑 − 𝑑𝐻𝑋 /𝑑 < 𝑃(10−15) Exploration of unknowns: DM, Axion, Unknown unknowns History: early days of particle physics, n oscillation, …

Energy Flux

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Summary

Tremendous progress in these area in the past decade, and expected in the next decade

  • New CMB surveys coming online: Simons Observatory, CMB-S4, …
  • New optical surveys coming online: DESI, PFS, LSST, Euclid, …
  • Dark Matter: gen-2 (and gen-3) getting to neutrino floor, Axion

searches cutting into plausible parameter region.

  • Astroparticle: turning into “multi-purpose detector complex.”
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SLIDE 31

Possibility of no new physics in next 10 years?

  • Cosmology: no primordial gravitational waves.
  • Cosmology: no BSM thermal relics.
  • Cosmology: no deviation from w=-1.
  • Cosmology: no detection of primordial non-Gaussianity.
  • DM: no detection of WIMP.
  • DM: no detection of Axion.
  • Astroparticle: no detection of unknown unknown.
  • No to all other possibilities of Unkown Unkowns.
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Possibility of no new physics in next 10 years?

  • Cosmology: no primordial gravitational waves.
  • Cosmology: no BSM thermal relics.
  • Cosmology: no deviation from w=-1.
  • Cosmology: no detection of primordial non-Gaussianity.
  • DM: no detection of WIMP.
  • DM: no detection of Axion.
  • Astroparticle: no detection of unknown unknown.
  • No to all other possibilities of Unkown Unkowns.

And we are measuring very fundamental quantities.