Angela V. Olinto

(1)

Angela V. Olinto

The University of Chicago

(2)

Voyager 1 and 2 leave the Heliosphere

Ed Stone & Voyager

The Great Voyage

1977 to now and onwards...

(3)

William H. Gerstenmaier Associate Administrator HEOMD, NASA

Precision

Exploration

(4)

The HE* Physics Journey

2013,

H

⁰

*Particle & Astroparticle

(5)

The (Astro)Particle Physics Journey

2013,

H

⁰

(6)

Journey toward Planck

(7)

Journey through the Desert toward Planck

10¹³ eV 14 o.o.m. 10²⁷ eV

(8)

eV

^-1

2 x 10

^-5

cm

10 -9cm 10 -12cm 10 -15cm 10 -18cm 10 -21cm 10 -24cm 10 -27cm 10 -30cm 10 -33cm

(9)

10⁹ eV 10¹²eV 10¹⁵ eV 10¹⁸ eV 10²¹eV 10²⁴eV 10²⁷eV

GeV TeV PeV EeV ZeV YeV XeV

eV cm

(10)

10⁹ eV 10¹²eV 10¹⁵ eV 10¹⁸ eV 10²¹eV 10²⁴eV 10²⁷eV

10⁹ cm 10¹²cm 10¹⁵ cm 10¹⁸ cm 10²¹ cm 10²⁴ cm 10²⁷ cm

R

_Earth

d

Earth-Moon

6 x 108 cm 50pc ~ 1015 cm

Solar System

4 x 1011 cm Near Stars 1 pc = 3 1018 cm

1 AU = 1.5 x 1013 cm 1 kpc = 3 1021 cm 1Mpc = 3 1024 cm 1Gpc = 3 1021 cm

Milky Way thickness

Near Galaxies

Our Neighborhood of the Universe

(11)

10⁹ eV 10¹²eV 10¹⁵ eV 10¹⁸ eV 10²¹eV 10²⁴eV 10²⁷eV

10⁹ cm 10¹²cm 10¹⁵ cm 10¹⁸ cm 10²¹ cm 10²⁴ cm 10²⁷ cm

R

_Earth

d

Earth-Moon

6 x 108 cm 50pc ~ 1015 cm

Solar System

(12)

10⁹ eV 10¹²eV 10¹⁵ eV 10¹⁸ eV 10²¹eV 10²⁴eV 10²⁷eV

10⁹ cm 10¹²cm 10¹⁵ cm 10¹⁸ cm 10²¹ cm 10²⁴ cm 10²⁷ cm

R

_Earth

d

Earth-Moon

6 x 108 cm 50pc ~ 1015 cm

Solar System

Precision

Exploration

(13)

10⁹ eV 10¹²eV 10¹⁵ eV 10¹⁸ eV 10²¹eV 10²⁴eV 10²⁷eV

10⁹ cm 10¹²cm 10¹⁵ cm 10¹⁸ cm 10²¹ cm 10²⁴ cm 10²⁷ cm

R

_Earth

d

Earth-Moon

50pc ~ 1015 cm

Solar System

6 x 108 cm

Precision

Exploration

LHC

Precision

(14)

10⁹ eV 10¹²eV 10¹⁵ eV 10¹⁸ eV 10²¹eV 10²⁴eV 10²⁷eV

10⁹ cm 10¹²cm 10¹⁵ cm 10¹⁸ cm 10²¹ cm 10²⁴ cm 10²⁷ cm

R

_Earth

d

Earth-Moon

50pc ~ 1015 cm

Solar System

6 x 108 cm

Precision

Exploration

LHC

Exploration Precision

IceCube ν Aug er/T A

(15)

10⁹ eV 10¹²eV 10¹⁵ eV 10¹⁸ eV 10²¹eV 10²⁴eV 10²⁷eV

10⁹ cm 10¹²cm 10¹⁵ cm 10¹⁸ cm 10²¹ cm 10²⁴ cm 10²⁷ cm

R

_Earth

d

Earth-Moon

50pc ~ 1015 cm

Solar System

6 x 108 cm

Precision

Exploration

LHC

IceCube ν Aug er/T A ARA/ EV A JEM -EUSO

(16)

10⁹ eV 10¹²eV 10¹⁵ eV 10¹⁸ eV 10²¹eV 10²⁴eV 10²⁷eV

10⁹ cm 10¹²cm 10¹⁵ cm 10¹⁸ cm 10²¹ cm 10²⁴ cm 10²⁷ cm

R

_Earth

d

Earth-Moon

50pc ~ 1015 cm

Solar System

6 x 108 cm

Precision

Exploration

LHC

IceCube ν Aug er/T A ARA /EV A JEM -EUSO

(17)

The Most Energetic

Cosmic Particles

(18)

1937: Pierre Auger ~ 10

¹⁵

eV

Extensive Air Showers

(19)

1962 John Linsley

~ 10

²⁰

eV event

Ultra High Energy Cosmic Rays

(20)

AAS meeting 1/5/14 Angela Olinto 20

(21)

GammaRays

Cosmic Rays

Neutrinos

~ double the energy range for Astrophysics

High Energy Particles

(22)

Proton, Helium, heavier nuclei

~1%

Gamma-ray ~ 0.1%

IceCube Neutrinos

(23)

PhysPAG 8/14/12 23 Angela Olinto 23

Solar

Influence Galactic Cosmic Rays Extragalactic Cosmic Rays

(24)

Solar Influenc

e

Galactic Cosmic Rays Extragalactic Cosmic Rays

Ground Experiments

Space

Experiments

(25)

Solar Influenc

e

Voyager I & II

ACE/CRIS PAMELA

AMS

Satellites ISS

Space Missions Now

Super- TIGER

Balloon

(26)

Solar Influenc

e

AMS

Satellites ISS

ISS-CREAM

JEM-EUSO

CALET

HN X

SmEx

Space Missions Future

EVA Balloon

(27)

Solar Influenc

e

Galactic Cosmic Rays Extragalactic Cosmic Rays NOW

Ground Experiments

(28)

ankle knee

(29)

ankle knee

(30)

ankle knee

500 TeV

10

²⁰

eV

(31)

31

A. Watson

(32)

ankle knee

Sources?

(33)

33

Super-novae

Cosmic Rays from Super-novae Baade & Zwicky (1934)

(34)

Blasi & Amato 2012 34

Supernova Remnants

to 10¹⁷eV

Vladimir Ptuskin

(35)

π ⁰ decay!

Ackermann et al (Fermi Collab) ’13 arXiv:1302.3307

IC 443 & W44 Fermi & AGILE

π⁰ decay

(36)

ankle knee

Galactic Sources

PhysPAG 8/14/12 36

~1%

Galactic Supernova Remnants

(37)

ankle knee

Extragalactic Sources

PhysPAG 8/14/12 37

~1%

Galactic Supernova Remnants

(38)

ankle knee

?

(39)

Galactic – Extragalactic Transition

39

Heavy

Light

(40)

ankle knee

New light Component

(41)

ankle knee

ankle

Ultrahigh Energy Cosmic Rays

E > 10¹⁸ eV

= 1 EeV

(42)

ankle knee

1 km

^-2

yr

^-¹

0.1 km

^-2

century

^-¹

1 m

^-2

yr

^-1

(43)

Current Observatories of

Ultrahigh Energy Cosmic Rays

Pierre Auger Observatory

Mendoza, Argentina (19 country collaboration)

3,000 km

²

array

4 fluorescence telescopes

Telescope Array

Utah, USA (5 country

collaboration)

700 km

²

array

3 fluorescence

telescopes

(44)

Pierre Auger Observatory

~ 500 Scientists, 19 Countries

3,000 km² water cherenkov detectors array

4 fluorescence Telescopes, Malargue, Argentina

(45)

Telescope Array

3 FD stations overlooking an array of 507 scintillator surface detectors (SD)

Area: 700 km²

Belgium Japan Korea

Russia USA

45

(46)

46

~175000 events

from 32,000 km² sr y

A. Watson

(47)

CERN UHECR 2012 Working Group

Unified Spectrum

Dawson et al ‘13 47

Energies re-scaled ~10%

(48)

48

(49)

49

(50)

50

(51)

ankle knee

GZK

(52)

“Cosmologically Meaningful Termination”

GZK Cutoff

Greisen, Zatsepin, Kuzmin 1966

p+

_cmb

 

⁺

 p + 

⁰

 n + 

⁺

Proton Horizon

~5 x 10

¹⁹

eV

(53)

Greisen-Zatsepin-Kuzmin effect

53

Kotera & AO 11

(54)

Greisen-Zatsepin-Kuzmin effect

Gpc

~100 Mpc

~10 Mpc

54

(55)

(56)

Greisen-Zatsepin-Kuzmin effect

Gpc

~100 Mpc

~10 Mpc

56

Isotropic Isotropic Anisotropic Anisotropic

(57)

Propagation of UHE protons

Berezinsky, Gazizov, Grigoriev ‘05

Modification factor

Spectrum Recovery

(58)

CERN UHECR 2012 Working Group

Unified Spectrum

Dawson et al ‘13 58

Energies re-scaled ~10%

(59)

Kotera, AO ‘11 To fit the spectrum, need:

SOURCE MODEL

+

PROPAGATION

(60)

Modern Propagation Codes

Public:

CRPropa

1.0 Armengaud et al ‘06 2.0 Kampert et al. ’12 3.0 Alvez Batista et al ’13 SimProp

Aloisio et al ’12

Private:

Allard et al ’04 Taylor ’07

Ahlers ‘10 others...

(61)

Interaction Cross Sections, z evolution Background Fields: CMB, UV/Opt/IR Primary, Secondary nuclei, nucleons, e+e-, gamma-rays, neutrinos,...

InterGal Magnetic Fields

Modern Propagation

Codes

(62)

Source Model:

•injection spectrum: E^-s

•injected composition

•redshift distribution

Propagation Codes

(63)

Source Model:

Propagation Codes

Source redshift evolution

(64)

Source Model:

Propagation Codes

Spectrum

Anisotropies

Composition

Multi-messengers

(65)

Kotera, AO 2011

injection spectrum: E^-s, E_max injection composition

Transition Gal/Extragal model

Source evolution: FRII, SFR, uniform

(66)

Kotera, AO 2011

(67)

UHECRs Current Status

Leading Observatories: Auger & Telescope Array agree on the shape of the spectrum Energy scale: ~10% difference

Composition?

67

(68)

68

(69)

Composition observable:

shower maximum

average and fluctuations

(70)

70

See Dembinski

(71)

71

See Dembinski

Fe

p O He

(72)

Auger

TA

Telescope Array

Auger sees change slope:

Change in Composition or interactions

TA: not confirmed yet

72

X_max in the atmosphere

X_max in the detector

(73)

GZK ?

(TA ICRC11)

Kotera, AO ‘11 ⁷³

(74)

GZK or E _max ?

(TA ICRC11)

Kotera, AO ‘11 Fang, Kotera, AO ‘13

74

(75)

GZK vs E _max

(TA ICRC11)

Kotera, AO ‘11

Fang, Kotera, AO ‘13

75

(76)

LHC white dwarf

Kotera & AO‘11

LHC

white dwarf

Hillas Plot: E _max required

(77)

LHC white dwarf

Kotera & AO‘11

LHC

white dwarf

Hillas Plot: E _max required

(78)

Birth of ultrafast spinning

Pulsars

(79)

Young Neutron Stars & Magnetars

Closed Line Open Lines

Blasi, Epstein & AVO ’00, Arons ‘03 M ~1 M_solar R~10km compact stars

born Fast spinning (P<< 300 ms)

– slows down due to magnetic breaking (and gravitational radiation early on) born B ~ 10^12-13G

Ω

(80)

Birth of ultrafast Pulsars

Newborn Pulsar with:

At the light cylinder:

Magnetic wind can accelerate particles up to

Spectrum too hard:

Blasi, Epstein, AVO ‘00

Maximum Energy?✔

Spectrum is hard ~ E^-1

(81)

Escape from Supernova Remnant :

maximum 10^4.2/s

Fang, Kotera, AVO ‘12

softens the spectrum bet protons and iron + pulsar distribution & propagation

(82)

Fast Spinning Newborn Pulsars fit Spectrum !

(83)

Fast Spinning Newborn Pulsars fit Spectrum & Auger Composition !

(84)

Galactic Newborn Pulsars?

(85)

Galactic Cosmic Rays

Amato & Blasi ‘12

fill the gap

(86)

Multi-messenger Predictions

Fang, Kotera, Murase, AVO ‘13 86

(87)

UHECRs Current Status

Leading Observatories: Auger & Telescope Array agree on the shape of the spectrum Energy scale: ~10% difference

Composition: controversial Multi-messenger clues

87

(88)

Cosmogenic (GZK, BZ*) Neutrinos & Photons

p+

_cmb

 

⁺

 p + 

⁰

 γγ  n + 

⁺

n  p + e

^-

+ 

_e



⁺

 

⁺

+ 

_



⁺

 e

⁺

+ 

_e

+

_

Berezinsky & Zatsepin ‘69

(89)

Neutrino Detectors

Flux Lower Limit

Current Limits

(90)

Highest Energy Neutrino

Observatories

IceCube ANITA

ANTARES

(91)

Next Generation UHE

from Vieregg CSS13

(92)

Neutrino Detectors

Next Generation (ARA)

Flux Lower Limit

Current Limits

(93)

Solar Influenc

e

AMS

Satellites ISS

ISS-CREAM

JEM-EUSO

CALET

HN X

SmEx

Space Missions Future

EVA Balloon

(94)

94 APS meeting 1/14/15

P. Gorham CosmicSIG

EVA

(95)

95

P. Gorham CosmicSIG

(96)

P. Picozza

(97)

P. Picozza

(98)

98

(99)

(100)

23 days Super Pressure Balloon = SPB

http://www.csbf.nasa.gov/map/balloon9/flight662nt.htm

(101)

UHECRs Current Status

Leading Observatories: Auger & Telescope Array agree on the shape of the spectrum Energy scale: ~10% difference

Composition: controversial

Multi-messenger clues: not yet

Anisotropies?

101

(102)

No Galactic Plane Anisotropy

E>20 EeV Cosmic Rays are EXTRAGALACTIC

Auger Anisotropy limits: rule out Galactic protons to CNO as dominant CR component E > 1 EeV and Fe above 20 EeV

102 102

Giacinti et al ‘11

(103)

ankle knee

ankle

Ultrahigh Energy Cosmic Rays

E > 10¹⁸ eV

= 1 EeV

ankle

Extragalactic

(104)

Cosmic Magnetic Fields

Halo B?

Extra-galactic B?

B < nG



weak deflection R_L = kpc Z^-1 (E / EeV) (B / G)^-1

R_L = Mpc Z^-1 (E / EeV) (B / nG)^-1

kpc 10 kpc

strong deflection

Milky way B ~ G

E > 10¹⁹eV

E < 10¹⁸eV

“Known unknown”

1 EeV = 10¹⁸ eV

Galactic B deflection

<< 10^o Z (40 EeV/E) anisotropic in sky

(105)

Greisen-Zatsepin-Kuzmin effect

Gpc

~100 Mpc

~10 Mpc

105

(106)

Greisen-Zatsepin-Kuzmin effect

Gpc

~100 Mpc

~10 Mpc

106

Isotropic Isotropic Anisotropic Anisotropic

(107)

(108)

108

(109)

109

Correlation has fallen from ~ 68% to ~ 28% (2007 –> 2014) compared with 21% for isotropy: about 1.4% probablity Cen A may be a source: in 13º circle around: 12 seen/1.7

A clear message from the Pierre Auger Observatory:-

We made it too small (2 per month at energy of interest)

A. Watson

(110)

Anisotropy Hints > 60 EeV

E > 5.7x 10¹⁹ eV 20^o smoothing

Auger Observatory

≈ 3 σ pretrial

(111)

Telescope Array

Anisotropy Hints > 60 EeV

E > 5.7x 10¹⁹ eV 20^o smoothing ≈ 5 σ pretrial

Telescope Array

Soon to be announced!

(112)

Anisotropy Hints > 60 EeV

E > 5.7x 10¹⁹ eV 20^o smoothing ≈ 5 σ pretrial

Telescope Array

≈ 3 σ pretrial

overlap

(113)

Anisotropy Hints > 60 EeV

(114)

IceCube 37 Events

Phys. Rev. Lett. 113, 101101 (2014) 114

3 yr data; 30 TeV to 2 PeV

(115)

115

(116)

116

(117)

117

(118)

118

Neutrino & UHECR Coincidence

Fang, Fujii, Linden, AO ‘14

~2σ

(119)

Anisotropy Hints > 60 EeV

E > 5.7x 10¹⁹ eV 20^o smoothing ≈ 5 σ pretrial

Statistically limited

Telescope Array

≈ 3 σ pretrial

overlap

(120)

Anisotropy Hints > 60 EeV

Statistically limited

A clear message from the Pierre Auger Observatory:-

We made it too small (2 per month at energy of interest)

A. Watson

(121)

121

(122)

Nadir

Fluorescence from SPACE

Tilt

122

Tilt

Nadir John Linsley

(1925-2002)

(123)

123

JEM-EUSO

Japan, USA, Korea, Mexico, Russia, Algeria

Europe: Bulgaria, France, Germany, Italy, Poland, Slovakia, Spain, Switzerland, Sweden

16 Countries, 300 researchers Leading institution: RIKEN

PI: Piergiorgio Picozza

(124)

JEM-EUSO Mission

Extreme Universe Space Observatory (EUSO)

in the Japanese Experiment Module (JEM)

of the International Space Station (ISS)

(125)

125

JEM-EUSO goals

- pioneer the study of EECR from Space - increase exposure to EECR by 1 order of magnitude

- discover the nearby sources of UHECRs

(126)

126

Rear Fresnel Lens

Iris

Front Fresnel lens DAQ Electronics

Support Structure

Focal Surface Detector

Optics

Payload

Precision Fresnel lens

Housekeeping

On-board Calibration

Atmospheric Monitoring BUS System : JAXA

Ground Based Calibration

Simulation : Worldwide

Ground Support Equipment Telescope Structure

(127)

127

(128)

128

(129)

129

(130)

130

(131)

131

(132)

132

(133)

133

Full Sky Coverage

with nearly uniform exposure

http://www.nlsa.com/

Inclination: 51.6°

Height: ~400km

The ISS ORBIT

(134)

JEM-EUSO Sky Coverage

134

(135)

JEM-EUSO

135

annual exposure = 10 x Auger 6 10⁴ km² sr yr

(136)

ZeV neutrinos?

136

(137)

10⁹ eV 10¹²eV 10¹⁵ eV 10¹⁸ eV 10²¹eV 10²⁴eV 10²⁷eV

10⁹ cm 10¹²cm 10¹⁵ cm 10¹⁸ cm 10²¹ cm 10²⁴ cm 10²⁷ cm

R

_Earth

d

Earth-Moon

50pc ~ 1015 cm

Solar System

6 x 108 cm

Precision

Exploration

LHC

IceCube ν Aug er/T A ARA /EV A JEM -EUSO

(138)

Super Heavy Dark Matter

138

Aloisio, Matarrese, AO ‘15

JEM-EUSO ARA

β inflaton potential

(139)

SHDM

Mass scale given by r

Lifetime given by EECRs

(140)

Super Heavy Dark Matter

140

(141)

141

NASA

Astrophysics Roadmap

2014

(142)

How many UHECRs > 60 EeV?

Auger + TA ~30 events/yr

JEM-EUSO

~200 events > 60 EeV/yr

Earth - surface ~ 5 10

⁸

km

²

~3.4 10

⁶

events/yr

142

(143)

Monitored Area

» few ´ 10

¹²

tons

JEM-EUSO: Extreme Universe Space Observatory onboard Japanese Experiment Module

~ 4 ~

JEUSO-110025-01-E-TR-ZZZ

since the mean distance to EAS and atmospheric absorption both increase. First few years of the then later to

Figure 1-2. Artistic illustration of the JEM-EUSO telescope attached to the Japanese Experiment Module of the International Space Station, under nadir (left) and tilt (right) mode of observation.

The JEM-EUSO telescope can reconstruct the incoming direction of the EECRs with accuracy better than few degrees. Its observational aperture of the ground area is a circle with 250 km radius, and its atmospheric volume above it, with a 60° FoV, is ~1 Tera-ton or more. The target volume for upward neutrino events exceeds 10 Tera-tons. The instantaneous aperture of JEM- EUSO is larger than the Pierre Auger Southern Observatory by a factor ranging from 65 to 280, depending on its observation mode (nadir or tilted, Fig.1-3).

JEM-EUSO, planned to be attached to JEM/EF of ISS, will be launched in the JFY 2016 by H2B rocket and conveyed to ISS by HTV (H-II transfer Vehicle).

Figure 1-3. Area observed by the JEM-EUSO telescope in one shot under mode.

(144)

How many UHECRs > 60 EeV?

Auger + TA ~30 events/yr

JEM-EUSO

~200 events > 60 EeV/yr

Earth - surface ~ 5 10

⁸

km

²

~3.4 10

⁶

events/yr

144

(145)

(146)

146

Extreme Energy Frontier Mysteries to be Resolved from Space!

Thanks!

(147)

Extreme Energy Frontier Mysteries to be

Resolved from Space!

Thanks!

(148)

(149)

149

(150)

150

(151)

151

(152)

152

Shower Simulation

64 pixel MAPMT

10²⁰eV 60 deg

Detected photoelectrons are recorded every Gate Time Unit (GTU) of 2.5s continuously.

Simulated air shower image on the focal surface detector.

2x10²⁰eV 65 deg

(153)

153

(154)

154 154

(155)

GLS

12 stations:

12 with Xe Flashlamps 6 with Steered Lasers 1 airborne System

Angela V. Olinto

Angela V. Olinto

The University of Chicago

The Great Voyage

The HE* Physics Journey

H

The (Astro)Particle Physics Journey

H

Journey toward Planck

Journey through the Desert toward Planck

eV

2 x 10

cm

eV cm

R

d

R

d

R

d

R

d

LHC

R

d

LHC

IceCube ν Aug er/T A

R

d

LHC

IceCube ν Aug er/T A ARA/ EV A JEM -EUSO

R

d

LHC

IceCube ν Aug er/T A ARA /EV A JEM -EUSO

The Most Energetic

Cosmic Particles

1937: Pierre Auger ~ 10

eV

Extensive Air Showers

1962 John Linsley

~ 10

eV event

Ultra High Energy Cosmic Rays

~ double the energy range for Astrophysics

High Energy Particles

Ground Experiments

Space

Experiments

Space Missions Now

JEM-EUSO

Space Missions Future

Ground Experiments

10

eV

Sources?

Super-novae

Supernova Remnants

π 0 decay!

IC 443 & W44 Fermi & AGILE

?

Galactic – Extragalactic Transition

1 km

yr

0.1 km

century

1 m

yr

Current Observatories of

Ultrahigh Energy Cosmic Rays

Pierre Auger Observatory

3,000 km

array

4 fluorescence telescopes

Telescope Array

700 km

array

3 fluorescence

telescopes

Pierre Auger Observatory

π ⁰ decay!

GZK or E _max ?

GZK vs E _max

Hillas Plot: E _max required

Hillas Plot: E _max required