prospects in eutrino astronomy - ncatlab.org · 5. cosmic rays neutrinos gamma rays. neutrinos from...
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PROSPECTS IN UHE NEUTRINO ASTRONOMY
Stephanie Wissel Penn State
XXIX International Conference on Neutrinos June 30
1
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➤Why Ultra-high-energy (UHE, > PeV) Neutrinos?
➤Experimental landscape, particular focus on radio instruments
➤New results from ANITA-4
2
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➤Why Ultra-high-energy (UHE, > PeV) Neutrinos?
➤Experimental landscape, particular focus on radio instruments
➤New results from ANITA-4
3
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MESSENGER PARTICLES
4
Cosmic Rays
Neutrinos
Gamma Rays
www.particlezoo.net
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MESSENGER PARTICLES
5
Cosmic Rays
Neutrinos
Gamma Rays
Neutrinos from charged pion, neutron decay from pp & p𝛾 interactions
www.particlezoo.net
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MESSENGER PARTICLES
6
Cosmic Rays
Neutrinos
Gamma Rays
Neutrinos from charged pion, neutron decay from pp & p𝛾 interactions
Photons from neutral pion, from pp & p𝛾 interactions
www.particlezoo.net
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MULTI-MESSENGER ASTROPHYSICS
7
Cosmic Rays
Neutrinos
Gamma Rays
Gravitational Waves
www.particlezoo.netNASA/GSFC
ESA–C.Carreau
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COSMOGENIC NEUTRINOS POINT TO THE HIGHEST ENERGY ACCELERATORS
8
Planck
CR
p𝛾, etc.
Cosmic rays
𝜈
Cosmic Ray
CMB photon
p + γ → Δ+ → π+ + nπ+ → μ+ + νμ
μ+ → e+ + ν̄μ + νe
➤ Even Flavor ratios* expected due to flavor oscillations over Gpc length scales
*Deviations from standard flavor ratios expected from Beyond-Standard-Model scenarios
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DIFFUSE UHE NEUTRINOS - COSMOGENIC NEUTRINOS
9
Spectrum Encodese.g. proton fraction
in distant sources
Best fits based on cosmic ray data predict this range of fluxes
Plus!steady beam for fundamental physics at untapped energy scale
1901.03338 1901.01899
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UHE NEUTRINOS - ASTROPHYSICAL NEUTRINOS
10
Neutrinos from sources might be
stronger than cosmogenics!
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DIFFUSE UHE NEUTRINOS - EXPERIMENTAL CONSTRAINTS
11
IceCube < 1 EeV
IceCube / Auger < 30 EeVANITA > 30 EeV
~ extension of astrophysical flux
~ peak of predicted cosmogenic flux
end of the neutrino spectrum
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DIFFUSE UHE NEUTRINOS - NEXT GENERATION RADIO DETECTORS
12
In-Ice Detectors All Flavor
Air Shower Detectors Primarily 𝜈𝜏
Space-Borne Detectors All Flavor
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➤Why Ultra-high-energy (UHE, >PeV) Neutrinos?
➤Experimental landscape, particular focus on radio instruments - ice, air, space
➤New results from ANITA-4
13
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14
Radio Detector
vertex
Askaryan Radiation
ν
depth
2000 m
200 m
Surface
not to scale
In-ice Radio Detection Technique
forward view
E-field polarization
side view
E-field polarization
Askaryan emission: radiation from net negative charge excess in showers
1906.01670
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15
Radio Detector
depth
2000 m
200 m
Surface
not to scale
Doesn’t need to be this deep because radio propagates
long distances
In-ice Radio Detector
Depth
vertex
Askaryan Radiation
ν
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16
Radio Detector
depth
2000 m
200 m
Surface
not to scale
In-ice Radio Detector
Depth
vertex
Askaryan Radiation
ν
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17
Radio Detector
depth
2000 m
200 m
Surface
not to scale
In-ice Radio Detector
Design Principles
Space them by ~ attenuation length so effective volume increases linearly
kmLatten ∼ 1
vertex
Askaryan Radiation
ν
Multiple antennas at each station reconstruct radio signal via
interferometry
Use polarization to reconstruct neutrino direction to ~ degree scale
1911.02093
1912.00987
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Radio Detector
depth
2000 m
200 m
Surface
not to scale
200 m depth accesses large ice volume Low anthropogenic noise
Phased arrays for low trigger thresholds Modest drilling requirements ~ 1 day/hole
Use larger high gain antennas Precision reconstruction
No drilling, Fast deployment Simple cosmic ray veto
Tau neutrinos from nearby mountains
In-ice Radio Detector Designs Surface Design ARIANNA
Deep Design ARA
ARIANNA : Ross Ice Shelf
ARA : South Pole
Max depth: 200 m
See poster #485
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RADAR ECHO TELESCOPE
➤ T576 lab experiments confirm radar bounce off particle showers in dense dielectric HPDE
191410 1510 1610 1710 1810 1910
Energy [eV]
10−10
9−10
8−10
7−10
]-1 s
r-1
s-2
dN
/dE
[GeV
cm
2 E
Kotera '10 Auger '19IceCube HESE ARA 2022 projectionIceCube best fit GRAND (200,000 RX, 3yr) IceCube EHE RNO (61 stations, 5yr) RET (1 station, 5yr) RET (10 stations, 5yr)
PRELIMINARY
RET-CR
RET-N
➤ Proposed prototype to demonstrate with in-ice CR showers at Taylor Dome
➤ Targeting PeV to EeV energy scale
See posters #469, 4761910.12830
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20
ARIANNA
➤ 7 stations, 4.5 years
➤ Analysis efficiency roughly constant at all energies
ARA
➤ 2 stations, 4 years
➤ Ongoing work to analyze full data set (~30 station years) & take advantage of low threshold events on ARA5
See poster #485
1912.00987
1909.00840
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RNO-G : Greenland
➤ Scalable to few 100 km2 Autonomous, low power, low cost, efficient & low threshold
➤ Hybrid Design builds on ARA & ARIANNA:
➤ Surface: CRs, vetos, reconstruction
➤ Deep Phased Trigger: Effective Volume
35 stations
1.25 km
Production Station Electronics
See posters #455, 510
25 W station power
LTE / LoraWan comms
24 channels of LAB4D Digitizer
Low threshold phased trigger ~ SNR of 2
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22
Prototypes
Mid-scale
Planned for 2020 to 2028+
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23
IceCube-Gen2-Radio 10x better sensitivity at EeV scale Building on prototypes & midscale
instruments
Full scale construction
See poster #409
Mid-scale
Planned to start 2025
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AIR SHOWER TECHNIQUES
24
ν𝜏 τGeomagnetic radio
emission
CR
Upgoing tau neutrinos interact with rock
fewkms
Tau decay → inclined shower
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AIR SHOWER TECHNIQUES
25
ν𝜏 τ
CR
The BEACON Concept100-1000 stations with ~10 antennas each
Efficient detector due to large area at top of mountain
Targeting 𝜈𝜏 > 100 PeV
Similar to Taroge (Antarctica), Trinity (imaging Cherenkov)
See poster #427
BEACON Prototype Array:4 cross-dipole antennas, 30-80 MHz, phased array trigger + digitizer 500 MSPS, 50 WGoal: RF-only cosmic ray triggerOperating since 2018 at White Mountain Research Station CA
See also a PeV tau telescope concept TAMBO (Colca Valley)
2004.12718
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AIR SHOWER TECHNIQUES
26
The GRAND Concept200'000 radio antennas over 200'000 km2
~20 hotspots of 10'000 antennas over favorable sites in China and worldwide
ν𝜏 τ
CR
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27
• 300 antennas over 200 km²• autonomous radio detection
of very inclined air-showers• cosmic rays 1016.5-18 eV• 1.3 M€ (fully funded, China)
2021 2025 203X
• 104 antennas over 104 km2
• 1st GRAND subarray• discovery of EeV neutrinos for
optimistic fluxes• 13 M€ (mostly China)
• 200k antennas over 200k km2
• 20 hotspots of 10k antennas on different continents
• 1st EeV neutrino detectionand/or neutrino astronomy!
• 150 M€
GRANDProto300 GRAND200kGRAND10k2021 2025 203X
105 106 107 108 109 1010 1011
Neutrino energy En [GeV]
10°11
10°10
10°9
10°8
10°7
All-
flavo
r(n
+n̄ )
E2 nF
n(E
n)
[GeV
cm°
2s°
1sr
°1 ]
ARA-37 (3 yr)IceCube (2018)
_ _
_
IceCube (2015)
Cosmogenic n
PessimisticStandard
GRAND200k
(3yr)
GRAND10k (3
yr)
GRAND200k integrated (3 yr)
GRAND200k integrated (10 yr)
POEMM
A(3
yr)
ne : nµ : nt = 1:1:1
ARIANNA (3 yr)
Stat
us D
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l Ele
ctro
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Elec
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boar
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The
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supp
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Prob
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betw
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FPGA
and
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Solu
tions
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akin
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new
boar
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solu
tion)
Rem
ove
the
FPGA
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ithco
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trou
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rem
ount
Fast
solu
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to m
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desig
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sy!!!
!
GRAND’s staged approach
HorizonAntenna, successfully tested in the field (August, December 2018)
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NEUTRINOS FROM SPACE : ANITA
28
1
2
T-510 Collab., PRL, 2017High altitude → large instantaneous
detector volume
credit: J. Alvarez-Muniz ICRC 2017
See poster #552
Best constraints on the end of the neutrino spectrum
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NEUTRINOS FROM SPACE : PUEO
29
See poster #486
Lower threshold by phasing 2x antennas at
trigger level
Planning for flight in 2023
Constrain the end of the neutrino spectrum by 4-10x
High effective area for transients
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NEUTRINOS FROM SPACE : POEMMA➤ Upgoing tau neutrinos detected via
Optical Cherenkov from stereo satellites
➤ Tuned for neutrino transients like binary neutron stars, short gamma ray bursts,…
30
ntautau
POEMMA IceCube GRAND-200k
arXiv:1906.07209
Expected Number of Neutrinos from
Binary Neutron Star Mergers
See poster #519
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➤Why Ultra-high-energy (UHE, >PeV) Neutrinos?
➤Experimental landscape, particular focus on radio instruments
➤New results from ANITA-4
31
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ANITA-IV COSMIC RAY RESULTS
32
Peng Cao, DelawareRemy Prechelt, Hawaii Poster #552
Peter Gorham, Hawaii
Andrew Ludwig,
UCLA, ChicagoCosmin Deaconu, Chicago Poster #486
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ANITA COSMIC RAY AND COSMIC RAY-LIKE EVENTS
➤ Geomagnetic radio signal from cosmic rays expected to arrive both directly pointed at the payload and reflected off the ice, predominantly Hpol
➤ Polarity (phase) indicates whether event is direct or reflected
33
37 km
ANITA
Direct Reflected
1005.0035
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ANITA COSMIC RAY AND COSMIC RAY-LIKE EVENTS
➤ ANITA Anomalous Events: 2 steep, direct CR-like ~0.5 EeV events with polarity inconsistent with their geometry (>3σ, A1 𝜃H ~ -30°, Effective area Aeff ~ at 0.5 EeV)𝒪(0.01 m2)
34
37 km
ANITA
Direct Reflected
➤ Tau neutrinos expected at shallower angles near the horizon (Aeff ~ at 0.5 EeV), but difficult to reconcile steep events with the Standard Model & experimental limits
𝒪(100 − 1000 m2)
ANITA 3 Anomalous Event, -35°
See poster #476, 1811.07261
Anomalous
1803.05088, 1603.05218
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20 25 30 35 40 45 50 55 60 65
time, ns
-0.6
-0.4
-0.2
0
0.2
0.4
0.6
0.8
1
norm
aliz
ed a
mplit
ude
event 9734523, H
= +0.31 0.18 deg.
20 25 30 35 40 45 50 55 60 65
time, ns
-0.8
-0.6
-0.4
-0.2
0
0.2
0.4
0.6
0.8
1
norm
aliz
ed a
mplit
ude
event 51293223, H
= +0.38 0.22 deg.
20 25 30 35 40 45 50 55 60 65
time, ns
-1
-0.5
0
0.5
1
norm
aliz
ed a
mplit
ude
ANITA-IV Reflected CR, normalized average overlay
ANITA-4 CR WAVEFORMS
➤ Events classified by 1st Dominant Pole* ➤Reflected: Down or Down first ➤Direct: Up or Up first
35
21 Reflected Events, Below Horizon
*Polarity reconstruction via 4 deconvolution methods using Stokes amplitude to find the peak lobe(s)
2 Direct Events, Near & Above Horizon
20 25 30 35 40 45 50 55 60 65
time, ns
-0.6
-0.4
-0.2
0
0.2
0.4
0.6
0.8
1
norm
aliz
ed a
mplit
ude
event 9734523, H
= +0.31 0.18 deg.
20 25 30 35 40 45 50 55 60 65
time, ns
-0.8
-0.6
-0.4
-0.2
0
0.2
0.4
0.6
0.8
1
norm
aliz
ed a
mplit
ude
event 51293223, H
= +0.38 0.22 deg.
𝜃H =+0.38±0.24°𝜃H =+0.31±0.20°
Down
Up
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20 25 30 35 40 45 50 55 60 65
time, ns
-0.6
-0.4
-0.2
0
0.2
0.4
0.6
0.8
1
norm
aliz
ed a
mplit
ude
event 9734523, H
= +0.31 0.18 deg.
20 25 30 35 40 45 50 55 60 65
time, ns
-0.8
-0.6
-0.4
-0.2
0
0.2
0.4
0.6
0.8
1
norm
aliz
ed a
mplit
ude
event 51293223, H
= +0.38 0.22 deg.
20 25 30 35 40 45 50 55 60 65
time, ns
-1
-0.5
0
0.5
1
norm
aliz
ed a
mplit
ude
ANITA-IV Reflected CR, normalized average overlay
ANITA-4 CR WAVEFORMS
➤ Events classified by 1st Dominant Pole* ➤Reflected: Down or Down first ➤Direct: Up or Up first
36
21 Reflected Events, Below Horizon
*Polarity reconstruction via 4 deconvolution methods using Stokes amplitude to find the peak lobe(s)
2 Direct Events, Near & Above Horizon
20 25 30 35 40 45 50 55 60 65
time, ns
-0.6
-0.4
-0.2
0
0.2
0.4
0.6
0.8
1
norm
aliz
ed a
mplit
ude
event 9734523, H
= +0.31 0.18 deg.
20 25 30 35 40 45 50 55 60 65
time, ns
-0.8
-0.6
-0.4
-0.2
0
0.2
0.4
0.6
0.8
1
norm
aliz
ed a
mplit
ude
event 51293223, H
= +0.38 0.22 deg.
𝜃H =+0.38±0.24°𝜃H =+0.31±0.20°
4 additional events near the horizon, but below it
Expect the same polarity as the reflected events: Down
Down
Up
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20 25 30 35 40 45 50 55 60 65
time, ns
-0.6
-0.4
-0.2
0
0.2
0.4
0.6
0.8
1
norm
aliz
ed a
mplit
ude
event 9734523, H
= +0.31 0.18 deg.
20 25 30 35 40 45 50 55 60 65
time, ns
-0.8
-0.6
-0.4
-0.2
0
0.2
0.4
0.6
0.8
1
norm
aliz
ed a
mplit
ude
event 51293223, H
= +0.38 0.22 deg.
20 25 30 35 40 45 50 55 60 65
time, ns
-1
-0.5
0
0.5
1
norm
aliz
ed a
mplit
ude
ANITA-IV Reflected CR, normalized average overlay
ANITA-4 CR WAVEFORMS
➤ Events classified by 1st Dominant Pole* ➤Reflected: Down or Down first ➤Direct: Up or Up first
37
21 Reflected Events, Below Horizon
*Polarity reconstruction via 4 deconvolution methods using Stokes amplitude to find the peak lobe(s)
20 30 40 50 60
time, ns
-1
-0.5
0
0.5
1
norm
aliz
ed a
mplit
ude
event 4098827, H
= -0.25 0.21 deg.
20 30 40 50 60
time, ns
-1
-0.5
0
0.5
1
norm
aliz
ed a
mplit
ude
event 19848917, H
= -0.65 0.20 deg.
20 30 40 50 60
time, ns
-1
-0.5
0
0.5
1
norm
aliz
ed a
mplit
ude
event 50549772, H
= -0.81 0.20 deg.
20 30 40 50 60
time, ns
-0.5
0
0.5
1
norm
aliz
ed a
mplit
ude
event 72164985, H
= -0.19 0.10 deg.
2 Direct Events, Near & Above Horizon
4098827, 𝜃H = -0.25±0.21° 19848917, 𝜃H=-0.65±0.20°
50549772, 𝜃H = -0.81±0.20° 72164985, 𝜃H = -0.19±0.10°
4 Direct Events, Near & Above Horizon
Preliminary
20 25 30 35 40 45 50 55 60 65
time, ns
-0.6
-0.4
-0.2
0
0.2
0.4
0.6
0.8
1
norm
aliz
ed a
mplit
ude
event 9734523, H
= +0.31 0.18 deg.
20 25 30 35 40 45 50 55 60 65
time, ns
-0.8
-0.6
-0.4
-0.2
0
0.2
0.4
0.6
0.8
1
norm
aliz
ed a
mplit
ude
event 51293223, H
= +0.38 0.22 deg.
𝜃H =+0.38±0.24°𝜃H =+0.31±0.20°
3 notch event, see backup
Down
Up
But observe Up
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ANITA-4 AIR SHOWER RESULTS
➤ 29 on background of 0.37+0.27-0.17 events result from blinded search for Hpol, impulsive, isolated events. Remained blind to polarity*
38
*Polarity reblinded to account for errors in system impulse response used to reconstruct polarity.
Polarity reconstruction in A4 is more complicated than than in earlier flights due to the time-dependent system response imposed by programmable notch filters in the signal chain.
SteepNear
Horizon
Angle wrt horizon > 1° < 1°
Total Events 23 6
Total 29
Results from targeted CR search
Preliminary
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Preliminary
ANITA-4 AIR SHOWER RESULTS
➤ 29 on background of 0.37+0.27-0.17 events result from blinded search for Hpol, impulsive, isolated events. Remained blind to polarity*
➤ 4 / 27 near horizon events with inconsistent polarity with significance ~3σ
➤ Systematics in significance estimate include : ➤ anthropogenic background per polarity (0.19+0.14-0.09 events) ➤ polarity mis-reconstruction (10-2 for 1 event; 10-4 others) ➤ pointing error ( = 0.1°, bias ±0.1°) ➤ radio propagation effects (refraction, ice surface,
ray defocusing) ➤ No new steep events with inconsistent polarity like in
ANITA-1 & ANITA-3
δθ
39
SteepNear
Horizon
Angle wrt horizon > 1° < 1°
Total Events 23 6
Consistent with Geometry
Reflected (Down) 21 0
Direct (Up) 0 2
Inconsistent with Geometry
Direct (Up) 0 4
Indeterminate Polarity
2 0
Total 29
Preliminary
Results from targeted CR search
See posters #552 (ANITA-4) and #486 (PUEO)
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SUMMARY AND OUTLOOK
➤ Exciting Things on the Horizon:
➤ While still consistent with backgrounds, ANITA-4 may be observing a new class of events near the horizon
➤ No new steep anomalous events in ANITA-4 dataset
➤ Followup with PUEO and other experiments will be important
40
Preliminary
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SUMMARY AND OUTLOOK
➤ Exciting Things on the Horizon:
➤ While still consistent with backgrounds, ANITA-4 may be observing a new class of events near the horizon
➤ No new steep anomalous events in ANITA-4 dataset
➤ Followup with PUEO and other experiments will be important
➤ Radio experiments are maturing
➤ Experiments preparing for mid-scale sensitivities at least an order of magnitude lower than current state-of-the art
➤ Several promising proposed experimental designs
➤ Next gen detectors hold promise to discover UHE neutrinos within 10 years & begin neutrino astronomy in new energy regime
41
Preliminary
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BACKUP SLIDES
42
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43
In-ice Detectors Sky Coverage
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ANITA BLINDED NEUTRINO SEARCH
➤ Clustering identifies isolated singlet events candidates
➤ Neutrinos: vertical polarization
➤ Cosmic rays: horizontal polarization
44
3000� 2000� 1000� 0 1000 2000 3000Easting (km)
3000�
2000�
1000�
0
1000
2000
3000
Nor
thin
g (k
m)
EAS Candidates
VPol Candidate
Flight path
ANITA-3 Search ANITA PRD 98 022001 2018
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ANITA-4 NEUTRINO SEARCH RESULTS
45
• Two analyses each find 1 candidate event on backgrounds of 0.34 and 0.64
• Set strongest upper limit on isotropic flux above 1019.5 eV
ANITA arXiv:1902.04005
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POLARITY RECONSTRUCTION
➤ Polarity reconstructed by deconvolving the response of the ANITA instrument, which disperses and attenuates the signal
➤ Average of four deconvolution methods → Polarity measure
➤ Polarity predominately determinedly the sign of the leading pole, but in practice depends on waveform shape
➤ In Monte Carlo with different noise realizations, polarity CL at the 1e-4 level, except 19848917 (2e-2)
21 Reflected Cosmic Rays
Down first
46
Preliminary
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POINTING RESOLUTION, RECONSTRUCTION & SYSTEMATICS AT THE HORIZON
➤ Calibration pulsers in remote location (WAIS Divide) reconstruct known location within = 0.1°
➤ Difference between the apparent horizon and the apparent reconstructed position requires refraction correction (+0.1°) and reconstruction of the apparent horizon (+0.1°)
➤ Systematic bias near the horizon observed with WAIS pulsers, HiCal pulser (on separate payload) ,and RFI from the South Pole suggest possible bias ±0.1°. Studies ongoing.
➤ Horizon buffer in significance tests included due to occultation of reflected rays near the horizon, validated with GPS measurements
δθ
47
Preliminary
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SIGNIFICANCE TESTS
48
Background assumed Horizon buffer Pointing bias
P-value Normal statistics σ
Anthropogenic non-inverted + above-horizon pointing errors + polarity flips, producing 4 or more non-inverted below-horizon events out of 27
0.0 0.0 3.9e-4 3.36
0.1 0.0 1.1e-4 3.69
0.0 -0.1 3.7e-3 2.68
0.1 -0.1 3.9e-4 3.36
0.0 +0.1 1.2e-4 3.67
0.1 +0.1 7.5e-5 3.8
Preliminary
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THREE NOTCH EVENTS
➤ Two three-notch events observed with opposite polarity
➤ 4098827: anomalous near horizon
➤ 36785931: normal, steep cosmic ray
➤ Deconvolution complicated by programmable notch filters, each combination of filters requires different system impulse response
49
Preliminary
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ANITA-3 AND ANITA-4 CR EVENT STATISTICS
➤ A4 had a 20% lower threshold and 50% higher livetime compared with A3, but notch filters at low frequency reduced sensitivity to the steep spectrum of cosmic rays
➤ A4 trigger and notches biased for flatter spectrum and weaker CR events, closer to the Cherenkov angle
➤ Results in comparable numbers of cosmic ray events, but more near horizon events
50
Total CR Events Near Horizon Events
ANITA-3 28 3
ANITA-4 29 6
Preliminary
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POEMMA Summary Slides
POEMMA: Transient Cosmic Neutrino Sensitivity: see arXiv:1906.07209
6/28/20 51
IceCube, ANTARES, Auger Limits for NS-NS merger GW170817
Short Bursts: - 500 s to slew to source after alert - 1000 s burst duration - Source celestial location optimal - Two independent Cher measurements
- 300 km Satellite Separation - 20 PE threshold: - Background rate < 10-3/year
Long Bursts: - 1 day to set SatSep to 50 km - Burst duration ≳ 105 s (models in plot) - Average Sun and moon effects - Simultaneous Cher measurements
- 50 km Satellite Separation - 10 PE threshold (time coincidence): - Background rate < 10-3/year
νtau tau
Optical Cherenkov ‘spot’ at 525 km altitude from τ-lepton upward EAS
100 km
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POEMMA Summary Slides6/28/20 52
POEMMA: ToO sky sensitivity vs Ground Experiments: see arXiv:1906.07209