Imaging Multi-Astroparticles
with NTA
Clear Identification of Astroparticle Emitters& Astro Beam Particle Physics•Air-shower imaging telescope for SubPeV-EeVν＆γwithsummit array

Multi-messenger Astronomy Workshop•

IACT-lilke resolution (< 0.2°) covering large FOV (>πsr) andwatching huge air-mass.

•Simultaneous Obs. SubPeV-EeVν,γ, and CR hadrons bothwith air Cheren. and fluores.

•2017.03.02 ICHA Chiba Univ.
Makoto Sasaki（NTA Int. Promotion WG）

Near future, it will be the most sensitive and preciseνdetector.
The first subPeV-EeV wide E-range γ-ray imaging telescope.
M. Sasaki, Imaging Multi-Astroparticles with NTA

March 2, 2017

1Very High Energy Particle Astronomy Workshop

Short History

Toward PeV-EeV Neutrinos!

2013: NTA LoI: by Sasaki & Hou
2014: VHEPA2014 @ Kashiwa
IAC：A.Watson,F.Halzen,T.Kifune

2015: VHEPA2015 @ Taipei
IAC：A.Watson,F.Halzen,T.Kifune

2015: NTA Forum @ ICRC2015 Hague
Kampert, Sokolsky, Watson, Kifune
Hou/Sasaki + several young persons

2016: VHEPA2016 @ Honolulu, Jan.7-9
Set up NTA (PWG)
Halzen（UWM）, Browder（UHM）, Hou(NTU)、Mussa(INF)、Ogawa(Toho)、Sasaki(UT-ICRR)...

M. Sasaki, Imaging Multi-Astroparticles with NTA

March 2, 20172

Modified from F. Halzen, VHEPA2016

Detect All VHE Particles

GW

Origin of p accelerator:
p acceleration -> observed CR fluxor

νfrom pp follows CR-p spectrum
Eν～ 1/20 Ep
GeV-PeVγcascade baund for ν
M. Sasaki, Imaging Multi-Astroparticles with NTA

Detect All of them even if transient (time domain <1s)
 Imaging AS in wide FOV at same time => NTA
March 2, 20173

Observable
Energy & Distance
NTA ν => source flux
NTA γ => propagated flux (cascaded)•Source location & mechanism•Probing media & particle physics

1) Source physics mechanism: pγ or pp？
2) CR high-end cut-off: GZK or composition?

3) “Highest Energy γ-ray physics”:
Search for highest E γ-ray in the Universe
interaction with BG photons
4) Dark matter:5) Search for non-standard physics:
Lorentz invariance violation
Extra Dimension6) Transient objects:
M. Sasaki, Imaging Multi-Astroparticles with NTA

March 2, 20174

Image ν & γ Air-showers
Earth-skimming tau neutrino (ES-ντ)Ｅν＞10 PeV

10-100 times higher sensitivity
than IceCube
but Ldecay = 49m (Eτ/PeV)
Deep penetrating e & tau neutrino (DP-νe,τ)
0.3 PeV< Ｅν <10 PeV
Compensate ES-ντ
Realize cross obs. with IceCube-> Complementary mutual confirm.
Interestign (anti-) electron neutrinos
AS from γ’s and CR-hadrons
Counter part obj. & AS develop.
-> p / γ separation
M. Sasaki, Imaging Multi-Astroparticles with NTA

March 2, 20175Mauna Loa
one of the best sites for imaging astroparticles

The largest subaerial volcano in both mass and volume, Mauna Loa hashistorically been considered the largest volcano on Earth. It is an active shield
volcano with relatively gentle slopes, with a volume estimated at approximately
18,000 cubic miles (75,000 km3). [en.wikipedia.org/wiki/Mauna_Loai]Stereo Obs. ES Tau Showers

M. Sasaki, Imaging Multi-Astroparticles with NTA

March 2, 20177

Topographic map implemented in NTA simulation

Summit Array Baseline Design
４ Stations （■） at 3000-3500m asl. on Mauna Loa

Ashra-1

9 detector units / 1 stationZenith angle=30° (65°-95°),

Azimuth angle = 240°with 9 detector units→ Stereo obs. at almost all azimuth angles
Nothernmost station = Ashra-1 Mauna Loa Site

NTA DUNTA Detector Unit = Multi-Tel.
with 4 LCs
Ashra-1 x 1.5 scaled-up＋same trigger & readout
Light Collector (LC)
Optics with f1.5m pupil
FOV 30〫= focal sphere f50cm

Detector Unit (DU)
4 LCs watch same FOV
Coadded 4 images⇒ Effective pupil = f3m
M. Sasaki, Imaging Multi-Astroparticles
with toNTAreject CR-μ⇒ Easy

Enhance sensitivity ~PeV
More air-mass can be used
Better multi-static ratio
Better environ. Condition
old layout design“surrounded-by-mtn’s”
March 2, 20178FOV and ExposureGCδ= ‐71°https://icecube.wisc.edu/science/highlights

νGalactic
M. Sasaki, Imaging Multi-Astroparticles with NTA

Detector

Latitude Zenith

Dec. min, max

KASCADE
EAS-TOPGAMMA
UMC
CASA-MIA
Tibet
NTAγ
HAWC
GRAPES-3
IceTop49.0°N
42.5°N
40.5°N
40.2°N
40.2°N
30.1°N
19.5°N
19.0°N
11.4°N
90.0°S

14°, 84°
7°, 78°10°, 71°
0°, 80°-20°, 90°-20°, 80°-71°, 90°-26°, 64°-14°, 36°-90°, -60°

< 35°
< 35°
< 30°
< 40°
< 60°
< 50°
< 95°
< 45°
< 25°
< 30°
March 2, 201792005年
2007年夏建設開始
建設完了

Observation – 1：2008年6月28日－2009年6月5日
Observation – 2：2009年10月7日－2011年1月4日
Observation – 3：2012年1月11日－2013年3月25

M. Sasaki, Imaging Multi-Astroparticles with NTA

集光器

March 2, 2017

トリガーハット

10M. Sasaki, Imaging Multi-Astroparticles with NTA

March 2, 201711

Ashra-1 Detector Unit System
as NTA baseline design

Transfer light images but not electric current.
• simultaneous Cher. & fluo. Trigger• affordable reduction of pixel cost
M. Sasaki, Imaging Multi-Astroparticles with NTA

March 2, 201712

Backup Option of Focal Sphere Camera
with 128×128 pix MAPMT Array

MAPMT+ light guides

NTA White Paper describes the cost performance evaluationsof options. The TDR will fix the unique design of NTA.
M. Sasaki, Imaging Multi-Astroparticles with NTA

March 2, 201713

2-3 arcmin. Resol. Over 42deg FOV with Ashra-1 LC
12Mag./1sexposure

42deg.

M. Sasaki, Imaging Multi-Astroparticles with NTA

March 2, 201714Real Shower Images• All AS images -> Hillas image parameters, i.e. Width, Length, …
• Same threshold and cluster cuts are applied as nt search.

M. Sasaki, Imaging Multi-Astroparticles with NTA

March 2, 201715

Proof of Concept by Ashra-1

M. Sasaki, Imaging Multi-Astroparticles with NTA

March 2, 201716

Simulated Images of ES-ντ Air-showers

Ashra-1
FOV

Y. Asaoka and M. Sasaki, Astropart. Phys. 41, 7 (2013).

NTA
light gather. eff. = 10 x Ashra-1⇒ Triggerable enough ＠１PeV

M. Sasaki, Imaging Multi-Astroparticles with NTAMarch 2, 201717

NTA Simulated Event# old station layout

Even a low photon-stat. event has good point-back resolution.

Y. Asaoka and M. Sasaki, Astropart. Phys. 41, 7 (2013).

τ Propagationin Rock

1PeV １００ TeV

Can point back to Pevatron
within 0.1 arcmin with ES-ντt

M. Sasaki, Imaging Multi-Astroparticles with NTA

1PeV １００ TeVMarch 2, 201719

Reconstructed Angular Resolution
M. Sasaki & G. Hou, NTA LOI

Y. Asaoka & M. Sasaki, Astropart. Phys. 41 (2013) 7–16

Fluorescence

Cerenkov mono.

Shower axis

Detector-showerPlane# old station layout Point-back resolution < 0.2 deg.
i.e. Cherenkov monostatic caseShower axis

NTA Station

ES+DP-ν Sensitivities

Tau decay length proglem for ES-ντ isrecovered at Eν = 300 TeV - 10 PeVNote）
DP-νμ not yet implemented in the simulation.

Definition of Aeff :Nevt = Φν ・ Aeff ・ ΩFOV ・ Tobs
１ ＰｅＶ
M. Sasaki, Imaging Multi-Astroparticles with NTA

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21

pp

Glashow共鳴
νe e − → W → X @ E = 6.3PeV
 崩壊 ハドロン70%、レプトン30%
WB流束仮定 ＩｃｅＣｕｂｅで３，４例/年 期待
ＮＴＡ DP- νe 空気シャワーで検定
DPではほぼ νe のみ、他フレーバＢＧなし

ＥＳ比べエネルギー決定も容易

pγ

M. Sasaki, Imaging Multi-Astroparticles with NTA

March 2, 201722

Diffuse ν Sensitivities
Best sensitivity above 1PeV but
suffered by the duty factor (15%)
NTA FOV is nearly horizontal
 Possible obs. under the Moon(Moon Run)
After successful R&D
duty factor 15% => 30%

M. Sasaki, Imaging Multi-Astroparticles with NTA

March 2, 201723

Karl-Heinz Kampert, VHEPA2014

M. Sasaki, Imaging Multi-Astroparticles with NTA

March 2, 201724

Resolve “GZK Effect/Exhausted Source” ProblemneutrinosNTA νNTA ν

Ahler & Halzen (2012)
Composision dependence

Test the hypothesis by searching for the GZK-ν flux
⇒ NTA can rule it out completely
M. Sasaki, Imaging Multi-Astroparticles with NTA

March 2, 2017

25

5km
γ 1PeV15km

New γ-ray Imaging Method with
PeV γ-ray Air Fluorescence Light
Air depth 690g/cm2 @ 3300m asl. ~Air-shower Xmax = 600g/cm2 at Eγ = 1 PeV=>

690g/cm2 @3300m asl.

NTA can image Xmax
of PeV γ-ray air-shower in the FOV.

Xmax ～600g/cm2=>
NTA γ effective area is equivalent toan grand array detector at ~3000m asl.

~1000 photons

with the area of Rp < 2km @ 1 PeVＣＯＲＳＩＫＡ full

Mauna Loa
M. Sasaki, Imaging Multi-Astroparticles with NTA

1kmMarch 2, 201726

Integrated γ-ray Flux Sensitivities
Photon sensitivities (５σ、>１０events)

IceCube PeVνPeV accelerator?
NTA γ-ray Cherenkov(1yr)

HESS Sgr A* γ-rayspectrum

NTA γ-ray fluorescence(1yr)

TeVPeVCompact Star Clusters in GP
SNR γ-ray ＆ν Emissions
１σ，２σ error circles from the center position ofthe ＩｃｅＣｕｂｅ ＰｅＶν
Evoluting young SNR:Westerlund 1 and HESS J1806-204

Colliding steller flow (CSF) model

Bykov et al., AIP Conference Proceedings 1792, 020003 (2017)

NTA νNTAPSFNTA γHESS J1806-204
M. Sasaki, Imaging Multi-Astroparticles with NTA

March 2, 201728

Pevatron Candidate Sgr A*
Combined Observation of PeV ν & γ-ray

HESS Image GC (Nature 531, 476)
M. Sasaki, Imaging Multi-Astroparticles with NTA

March 2, 201729

Possible Confirmation with
NTA for HESS GC γ-rays

HESS GC
Diffuse γ×10

If NTA γ confirm no cut-off below 100 PeV
 NTA must observe ν flux from GC

1 PeV

100 PeVNTA γ confirm no cut-off below 100 PeVand no ν flux=> Non-standard accel. scenario or

NTA γNTA can observe ν’s if
γ-ray cut-off energy higher

M. Sasaki, Imaging Multi-Astroparticles with NTA

March 2, 201730

PRD 90 (2014):023010

Galactic Plane
TeV-PeV Diffuse γ-rays
Hypernova
Galactic Plane：~1200 SNRs
~20個 Hypernova

Kink

加速された核子が滞在
星間物質とpp散乱⇒
拡散γ線やνを放出が期待される

TeV-PeV γ-ray Observation：
GC ( α= 266.4°, δ= -28.9°)
GP ( |b|<2°)
are not included in FOV efficiently
Powerful ＮＴＡ γ-ray imaging
observation with wide FOV
M. Sasaki, Imaging Multi-Astroparticles with NTA

March 2, 201731

GRB Neutrino Search Comparison（Note) Evaluated with old detector layout

Complement IceCube:• Methodology• Energy• Self-trigger for Tau Neutrino
0. Auger, PRD 79 (2009) 102001
1. IceCube, Nature 484 (2012) 351• IC40+IC59 stacked 117+181GRBs• Very strong bias for time window (28s)around Satellite Triggers to suppresshuge BG

2. Murase et al. ApJ 651 (2006) L5• Nearby Low luminosity (LL) GRB (ex.
GRB 060218/SN 2006aj ) dominate total
neutrino fluxes at Earth• X or g Satellites cannot detect
3. Hummer et al. PRL 108 (2012) 231101• Recalculated neutrino flux =>Ashra Energy Region more important

NTA Survey Depth: z ~ 0.15 (600Mpc) for GRBn flux (by Hummer et al.)
LIGO等とのクロス観測 重要 ← NTAν GRB探査領域はLIGOと大きく重なる
March 2, 201732

M. Sasaki, Imaging Multi-Astroparticles with NTA

ＮＡＳＡ： https://www.nasa.gov/feature/goddard/nasagoddard-scientist-gives-outlaw-particles-less-room-to-hide

Lorentz Invariance Violation
PeV-EeV ν を使えば基本物理を探れる•

超光速ニュートリノ⇒ 他の粒子放出⇒ スペクトルに鋭い切断⇒ ＩｃｅＣｕｂｅ PeV ν から制限？
⇒ 高エネルギー側の高統計が必要•

突発天体からν速度への制限：

ＮＴＡが相補的に高統計で検定例）PKS B1424–418 とHESE-35 PeVν 一致？
⇒ (v−c)/c < O(10−11)⇒ 対応天体との一致の信頼度が重要⇒ ＮＴＡ νM. Sasaki, Imaging Multi-Astroparticles with NTA

March 2, 201733

Extra Dimension Search
重力が3+1次元で弱いのは他次元に伝達したため減少Ｐｌａｎｃｋ質量以上でマイクロＢＨの生成⇒ νＮ散乱断面積の増加
もしくは、散乱長の変化による、

1 PeV

A.Connolly et al., PRD 83, 113009 (2011)

地球との散乱角度分布の変化
LHC(7TeV)でも探査、μＢＨ質量制限

NTA ＥＳ-ντＮＴＡ ES-ν では：
地球かすり角(θ)分布異常
ＮＴＡ ES-ν / DP-ν の事例数の比に反映される
検定に高統計と高い角度分解能が必要⇒ ＮＴＡ νM. Sasaki, Imaging Multi-Astroparticles with NTA

March 2, 201734

NTA 観測に向けて
2016

NTA

2017

予算請求

2018

2019

2020

2021

2022

建設/部分的観測

2023

山上アレイ
@3000m asl

完全観測

国際共同観測拠点

実地試験観測/ 多粒子観測/ 自動化・データ流・解析技法の確立
Ashra1
国際実証開発拠点

Akeno

アセンブリ/統合化/レーザー観測/長期安定性・試験

国内開発拠点国内外のラボ要素開発・試験
M. Sasaki, Imaging Multi-Astroparticles with NTA

March 2, 201735

Open a new chapter of physics with NTA
ν & γ telescope with < 0.2°resolution, > π sr FOV,and high sensitivity in subPeV-EeV.
•ν & γ cross detection with IceCube around 1 PeV•Check ν & γ wide range spectra in subPeV-EeV•

ν & γ survey of GP including GC=> Clear ID of position and mechanism of Pevatrons•Summary

Search for ν & γ short burst with LIGO and others=> Significant & complementary contributions to Time Domain Astronomy=> NTA can also issue ν & γ burst alerts rapidly•Probing astroparticles propagating in BG photons=> Solving out GZK-problem with testing diffuse-ν flux=> ν & γ combination to reveal BG photon density more precisely•Probing non-standard physics at energy frontier=> Highest energy ν particle physics
Extra dimension, Lorentz invariance violation, ...
=> Highest energy γ-ray observation
New “Super-Cutoff Problem” a la Super-GZK

Toward Comprehensive Understandings for VHE Particle Universe
M. Sasaki, Imaging Multi-Astroparticles with NTA

March 2, 201736