SuperCANGAROO SuperCANGAROO Symposium on Future Projects in - - PowerPoint PPT Presentation

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SuperCANGAROO SuperCANGAROO Symposium on Future Projects in - - PowerPoint PPT Presentation

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SuperCANGAROO SuperCANGAROO Symposium on Future Projects in Symposium on Future Projects in Cosmic Ray Physics, Cosmic Ray Physics, June 26- - 28, 2003 @ICRR 28, 2003 @ICRR June 26 Masaki Mori Masaki Mori ICRR, University of Tokyo ICRR,

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SuperCANGAROO SuperCANGAROO

Symposium on Future Projects in Symposium on Future Projects in Cosmic Ray Physics, Cosmic Ray Physics, June 26 June 26-

  • 28, 2003 @ICRR

28, 2003 @ICRR

Masaki Mori Masaki Mori

ICRR, University of Tokyo ICRR, University of Tokyo On behalf of the CANGAROO team On behalf of the CANGAROO team

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CANGAROO team CANGAROO team (as of April 2003)

(as of April 2003)

  • Institute of Physical and

Institute of Physical and Chemical Research Chemical Research

  • Shinshu

Shinshu University University

  • Institute for Space and

Institute for Space and Aeronautical Science Aeronautical Science

  • Tokai University

Tokai University

  • Tokyo Institute of

Tokyo Institute of Technology Technology

  • Yamagata University

Yamagata University

  • Yamanashi

Yamanashi Gakuin Gakuin University University

  • University of Adelaide

University of Adelaide

  • Australian National

Australian National University University

  • Ibaraki University

Ibaraki University

  • Ibaraki

Ibaraki Prefectural Prefectural University University

  • Kanagawa University

Kanagawa University

  • Konan University

Konan University

  • Kyoto University

Kyoto University

  • Nagoya University

Nagoya University

  • National Astronomical

National Astronomical Observatory of Japan Observatory of Japan

  • Osaka city University

Osaka city University

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CANGAROO history CANGAROO history

CANGAROO-II 7m (1999) CANGAROO-III T1 10m (2000) CANGAROO-III (2003) CANGAROO-III T1,T2,T3 (2002)

upgraded

CANGAROO-I 3.8m (1992)

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CANGAROO results CANGAROO results

  • "Search for

"Search for TeV TeV gamma gamma-

  • rays from SN1987A in 2001

rays from SN1987A in 2001“ “ Enomoto Enomoto, R. et al., Astrophysical Journal (Letters), 591, L25 , R. et al., Astrophysical Journal (Letters), 591, L25-

  • L28 (2003)

L28 (2003)

  • "Evidence for

"Evidence for TeV TeV gamma gamma-

  • ray emission from the nearby starburst galaxy NGC 253

ray emission from the nearby starburst galaxy NGC 253“ “ Itoh Itoh, C. et al., Astronomy and Astrophysics, 402, 443 , C. et al., Astronomy and Astrophysics, 402, 443-

  • 455 (2003)

455 (2003)

  • "Detection of diffuse

"Detection of diffuse TeV TeV gamma gamma-

  • ray emission from the nearby starburst galaxy NGC253

ray emission from the nearby starburst galaxy NGC253“ “ Itoh Itoh, C. et al., Astronomy and Astrophysics 396, L1 , C. et al., Astronomy and Astrophysics 396, L1-

  • L4 (2002)

L4 (2002)

  • "Development of an atmospheric

"Development of an atmospheric Cherenkov Cherenkov imaging camera for the CANGAROO imaging camera for the CANGAROO-

  • III experiment

III experiment “ “ Kabuki, S. et al., Kabuki, S. et al., Nucl Nucl. . Instr Instr. . Meth

  • Meth. A500, 318

. A500, 318-

  • 336 (2003)

336 (2003)

  • "Observation of gamma

"Observation of gamma-

  • rays greater than 10

rays greater than 10 TeV TeV from from Markarian Markarian 421 421 Okumura, K. et al., Okumura, K. et al., Astrophys

  • Astrophys. J.

. J. Lett Lett . 579, L9 . 579, L9-

  • L12 (2002)

L12 (2002)

  • "The Acceleration of Cosmic

"The Acceleration of Cosmic-

  • ray Protons in the Supernova Remnant RX J1713.7

ray Protons in the Supernova Remnant RX J1713.7-

  • 3946

3946“ “ Enomoto Enomoto, R. et al., Nature, 416, 823 , R. et al., Nature, 416, 823-

  • 826 (2002)

826 (2002)

  • "Design Study of CANGAROO

"Design Study of CANGAROO-

  • III, stereoscopic imaging

III, stereoscopic imaging atmosphereic atmosphereic Cherenkov Cherenkov Telescopes for Sub Telescopes for Sub-

  • TeV

TeV Gamma Gamma-

  • ray Detection

ray Detection“ “ Enomoto Enomoto, R. et al., , R. et al., Astropart Astropart . Phys. 16, 235 . Phys. 16, 235-

  • 244 (2002)

244 (2002)

  • "The Optical Reflector System for the CANGAROO

"The Optical Reflector System for the CANGAROO-

  • II Imaging Atmospheric

II Imaging Atmospheric Cherenkov Cherenkov Telescope Telescope“ “ Kawachi Kawachi, A. et al., , A. et al., Astropart Astropart . Phys. 14, 261 . Phys. 14, 261-

  • 269 (2001)

269 (2001)

  • "Observations of the Supernova Remnant W28 at

"Observations of the Supernova Remnant W28 at TeV TeV Energies Energies“ “ Rowell, G.P. et al., Astron. Rowell, G.P. et al., Astron. Astrophys

  • Astrophys. 359, 337

. 359, 337-

  • 346 (2000)

346 (2000)

  • "Very High

"Very High-

  • Energy Gamma

Energy Gamma-

  • Ray Observations of PSR B1509

Ray Observations of PSR B1509-

  • 58 with the CANGAROO 3.8m Telescope

58 with the CANGAROO 3.8m Telescope“ “ Sako Sako, T. et al., , T. et al., Astrophys

  • Astrophys. J. 537, 422

. J. 537, 422-

  • 428 (2000)

428 (2000)

  • "Evidence for

"Evidence for TeV TeV Gamma Gamma-

  • ray Emission from the Shell Type SNR RXJ1713.7

ray Emission from the Shell Type SNR RXJ1713.7-

  • 3946

3946“ “ Muraishi Muraishi, H. et al., Astron. , H. et al., Astron. Astrophys Astrophys., 354, L57 ., 354, L57-

  • L61 (2000)

L61 (2000)

  • "

"TeV TeV Gamma Gamma-

  • ray Observations of Three X

ray Observations of Three X-

  • ray Selected BL

ray Selected BL Lacs Lacs“ “ Roberts, M.D. et al., Astron. Roberts, M.D. et al., Astron. Astrophys Astrophys., 343, 691 ., 343, 691-

  • 696 (1999)

696 (1999)

  • "

"TeV TeV Gamma Gamma-

  • ray Observations of Southern BL

ray Observations of Southern BL-

  • Lacs

Lacs with the CANGAROO 3.8m Telescope with the CANGAROO 3.8m Telescope“ “ Roberts, M.D. et al., Astron. Roberts, M.D. et al., Astron. Astrophys Astrophys., 337, 25 ., 337, 25-

  • 30 (1998)

30 (1998)

  • "Discovery of

"Discovery of TeV TeV Gamma Rays from SN 1006: Further Evidence for the Supernova Rem Gamma Rays from SN 1006: Further Evidence for the Supernova Rem nant Origin of Cosmic Rays nant Origin of Cosmic Rays“ “ Tanimori Tanimori, T. et al., , T. et al., Astrophys

  • Astrophys. J.

. J. Lett Lett ., 497, L25 ., 497, L25-

  • L28 and Plate L2 (1998)

L28 and Plate L2 (1998)

  • "Detection of Gamma Rays of up

"Detection of Gamma Rays of up tp tp 50 50 TeV TeV from the Crab Nebula from the Crab Nebula“ “ Tanimori Tanimori, T. et al., , T. et al., Astrophys

  • Astrophys. J.

. J. Lett Lett ., 492, L33 ., 492, L33-

  • 36 (1998)

36 (1998)

  • "Very High Energy Gamma Rays from the Vela Pulsar Direction

"Very High Energy Gamma Rays from the Vela Pulsar Direction“ “ Yoshikoshi Yoshikoshi, T. et al., , T. et al., Astrophys

  • Astrophys. J.

. J. Lett Lett ., 487, L65 ., 487, L65-

  • 68 (1997)

68 (1997)

  • "Very High Energy Gamma Rays from PSR1706

"Very High Energy Gamma Rays from PSR1706-

  • 44

44“ “ Kifune Kifune, T. et al., , T. et al., Astrophys

  • Astrophys. J.

. J. Lett Lett., 438, L91 ., 438, L91-

  • 94 (1995)

94 (1995)

  • "Observation of 7

"Observation of 7 TeV TeV Gamma Rays from the Crab using the Large Zenith Angle Air Gamma Rays from the Crab using the Large Zenith Angle Air Cherenkov Cherenkov Imaging Technique" Imaging Technique" Tanimori Tanimori, T. et al., , T. et al., Astrophys

  • Astrophys. J.

. J. Lett Lett ., 429, L61 ., 429, L61-

  • 64 (1994)

64 (1994)

  • "First Test Data from the CANGAROO Project for Stereo

"First Test Data from the CANGAROO Project for Stereo Cherenkov Cherenkov Imaging" Imaging" Edwards, P.G. et al., Astronomical Soc. of Australia Proc., v10: Edwards, P.G. et al., Astronomical Soc. of Australia Proc., v10: 4, p.287 (1993) 4, p.287 (1993)

  • "3.8m Imaging

"3.8m Imaging Cherenkov Cherenkov Telescope for the Telescope for the TeV TeV Gamma Gamma-

  • ray Astronomy Collaboration between Japan and Australia"

ray Astronomy Collaboration between Japan and Australia" Hara, T. et al., Hara, T. et al., Nucl Nucl. . Instr

  • Instr. and

. and Meth Meth., A332, pp.300 ., A332, pp.300-

  • 309 (1993)

309 (1993)

21 papers in refereed journals

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5 5

TeV TeV gamma gamma-

  • ray sky 2002

ray sky 2002

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6 6

Gamma Gamma-

  • ray astrophysics

ray astrophysics in the 10 in the 10 GeV GeV region region

  • Origin of cosmic rays

Origin of cosmic rays

  • Gamma

Gamma-

  • rays pin

rays pin-

  • point accelerators

point accelerators

  • Galactic and extragalactic sources

Galactic and extragalactic sources

  • High

High-

  • energy astrophysics

energy astrophysics

  • More distant

More distant AGNs AGNs; time variability study ; time variability study

  • Highest energy end of pulsar emission / pulsar

Highest energy end of pulsar emission / pulsar nebula nebula

  • Gamma

Gamma-

  • ray bursts (in FOV and afterglow)

ray bursts (in FOV and afterglow)

  • Astroparticle

Astroparticle physics physics

  • Dark matter annihilation

Dark matter annihilation

  • And there should be

And there should be surprises surprises… …

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SNR origin of cosmic rays SNR origin of cosmic rays

  • Theoretical preference:

Theoretical preference:

  • (Good)

(Good) Pros Pros: :

  • Energetics

Energetics ( ( dE/ dt) dE/ dt) SN

SN ~ 10 (

~ 10 ( dE/ dt) dE/ dt) CR

CR

  • Diffusive shock acceleration

Diffusive shock acceleration → → p p-

  • 2

2 spectrum

spectrum

  • (Weak?)

(Weak?) Cons Cons: :

  • Maximum energy <

Maximum energy < PeV PeV ~ ~ E Eknee

knee

  • Experimental situation:

Experimental situation:

  • We already have some evidence

We already have some evidence… …

  • How many

How many “ “gamma gamma-

  • ray

ray SNRs SNRs” ”? ?

  • Systematic survey of galactic plane

Systematic survey of galactic plane

  • Hadronic

Hadronic or

  • r leptonic

leptonic? ?

  • Wide

Wide-

  • band energy spectrum

band energy spectrum

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Systematic survey of Systematic survey of SNRs SNRs

RX J1 7 1 3 .7 -3 9 4 6 （ CANGAROO） RCW 8 6 （

CANGAROO under analysis）

SN1 0 0 6 （ CANGAROO） Crab nebula （ ”Standard candle”）

Chandra ・

  • ptical

ASCA ASCA ROSAT Chandra ROSAT Chandra

RX J0 8 5 2 -4 6 （

CANGAROO under analysis）

Cas A （ HEGRA） Vela （ CANGAROO）

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Wide Wide-

  • band study of SNR spectrum

band study of SNR spectrum

10GeV SED of RX J1713.7 SED of RX J1713.7-

  • 3946

3946 Spectral shape ↓ Leptonic: [ IC, Brems]

  • r/ and

Hadronic: [ π0] Enomoto et al. 2002 Nature 416, 823

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SNR emission models SNR emission models

n= 10 cm -3 n= 1 cm -3 n= 0.1 cm -3

Dot: IC Dash: π0 Dot-dash: brems (Data: EGRET IC443)

e/ p = 0.01 0.1 1 Baring et al. 1999 ApJ 513, 311

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Other than Other than SNRs SNRs

  • Galactic sources

Galactic sources

  • Galactic jet sources

Galactic jet sources

  • X

X-

  • ray binaries (

ray binaries ( Cen Cen X X-

  • 3

3 * 1

* 1,

,… …) )

  • Microquasars

Microquasars (SS433, (SS433,… …), ),… …

  • Wolf

Wolf-

  • Rayet

Rayet stars stars

  • High velocity winds, CR abundance

High velocity winds, CR abundance

  • Extragalactic sources

Extragalactic sources

  • Starburst galaxies

Starburst galaxies

  • NGC 253

NGC 253 * 2

* 2, M82,

, M82, … …

  • Radio galaxies

Radio galaxies

  • M87

M87 * 3

* 3,

, Cen Cen A, A,… …

  • Clusters of galaxies

Clusters of galaxies

  • Coma,

Coma,… …

  • Gamma

Gamma-

  • ray clusters

* 1 Durham, ApJ 1998 * 2 CANGAROO, AA 2002&2003 * 3 HEGRA, AA 2003

ray clusters

Totani and Kitayama 2000 ApJ 545, 572

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Coma cluster Coma cluster

π0 10GeV B= 1µG Wp= 3x1062/ 3x1061 ergs Atoyan and Voelk 2000 ApJ 535, 45

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Cosmological gamma Cosmological gamma-

  • ray horizon

ray horizon

CMB at z= 100 Cutoff due to γ + γCMB → e+ + e- zmax 10GeV

(Scale not correct)

Fazio & Stecker 1970 Nature 226, 135

10 GeV gamma-rays can explore the Universe up to z= 100!

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10 10 GeV GeV Cherenkov Cherenkov telescopes telescopes

  • Collect photons 20 times more!

Collect photons 20 times more!

  • Hadron

Hadron showers increase but fainter showers increase but fainter

  • Electrons

Electrons, indistinguishable from , indistinguishable from gamma gamma-

  • rays, remain background

rays, remain background

  • Limit sensitivities for diffuse sources

Limit sensitivities for diffuse sources

  • Cf. Rigidity cutoff: 6
  • Cf. Rigidity cutoff: 6-
  • 9GV@Woomera

9GV@Woomera

  • Higher altitude option to be closer to

Higher altitude option to be closer to showers showers

  • Image broadens a little and

Image broadens a little and Cherenkov Cherenkov disk brighter near center disk brighter near center

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Cherenkov Cherenkov photon yield photon yield

p

γ

10 GeV

Total photons: 1/ 20 Total photons: 1/ 400

100 GeV Photons / m 2 / GeV Fegan 1997 JPG 23, 1013

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The The “ “Big Four Big Four” ”

2004 2004 2005

(VERITAS-4)

2003

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Next generation projects Next generation projects

  • 5 @5

5 @5

  • Max Planck Inst. for

Max Planck Inst. for Nuclear Physics Nuclear Physics

  • 50m

50m 2

2 mirror area

mirror area

  • 5 telescopes (4 in

5 telescopes (4 in 100m grid and 1 at 100m grid and 1 at center) at 5000m center) at 5000m a.s.l a.s.l. .

  • 3.2

3.2° ° camera, 721 camera, 721 pixels pixels

  • 5

5 GeV GeV threshold

  • ECO

ECO-

  • 1 0 0 0

1 0 0 0

  • Max Planck Inst. for

Max Planck Inst. for Physics Physics

  • 35m

35m φ φ, , 1000m 1000m 2

2

mirror area mirror area

  • < 5

< 5° ° camera, > 2000 camera, > 2000 pixels pixels

  • 5

5 GeV GeV threshold threshold

Merck et al. ICRC2003

threshold

Aharonian et al. 2001 APh 15, 335

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18 18

SuperCANGAROO SuperCANGAROO

  • “

“Strawman Strawman” ” design parameters design parameters

  • < 10

< 10 GeV GeV energy energy threthold threthold → → 10 times more area x 2 times QE 10 times more area x 2 times QE

  • 30m

30m φ φ, f= 30m (F/ 1.0), parabola , f= 30m (F/ 1.0), parabola

  • Field

Field-

  • of
  • f-
  • view ~ 10

view ~ 10° ° ← ← survey survey mode mode

  • Short barrel preferred to keep long focal

Short barrel preferred to keep long focal length length → → new optical design necessary new optical design necessary

  • 0.1

0.1° ° -

  • class pixel camera with advanced

class pixel camera with advanced photon sensors photon sensors

  • Stereo observation is essential

Stereo observation is essential

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19 19

3 mirror wide 3 mirror wide-

  • field optical design:

field optical design:

an example an example

LSST:

  • Paul-Baker optics
  • 6.9m effective

aperture

  • F/1.25
  • 7sq.deg = 3°φ

http: / / www.lssto.org/ lsst_home.html

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LSST scaled to 30m LSST scaled to 30mφ φ

For Cherenkov

  • bservation:
  • No need for lenses
  • Reflector can be

segmented and mirrors can be plastic or metal- shaved to save weight Camera can be located near the center-of- gravity:

  • Smaller moment,

faster movement

  • No long signal cables
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Large mount example: Lovell 76m Large mount example: Lovell 76m

Jodrell Bank, UK No counter weight !

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2m 2mφ φ camera camera

  • < 0.1

< 0.1° ° pixel to reduce pixel to reduce nightsky nightsky bkgd bkgd. .

  • 3m

3m 2

2 ↔

↔ 1500 x 2 1500 x 2” ”φ φ ~ 6000 x 1 ~ 6000 x 1” ” φ φ

  • Photosensors

Photosensors: :

  • High

High-

  • QE PMT (

QE PMT ( GaAsP GaAsP etc.) etc.)

  • Advanced sensors

Advanced sensors

  • Electronics

Electronics

  • Located next to the camera

Located next to the camera

  • GHz

GHz-

  • class FADC

class FADC

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Sensitivity Sensitivity

(rough estimate)

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Comparison with GLAST Comparison with GLAST

2x10 2x10 -

  • 9

9cm

cm -

  • 2

2s

s-

  • 1

1

( ( 50hr 50hr) ) 3x10 3x10 -

  • 9

9cm

cm -

  • 2

2s

s-

  • 1

1

(> 100MeV, (> 100MeV, 1yr 1yr) ) Sensitivi Sensitivi ty ty > 5yr > 5yr > 2yr > 2yr Life Life ~ 2x10 ~ 2x10 -

  • 2

2sr

sr > 2.5sr > 2.5sr FOV FOV ~ 3 ~ 3’ ’ (stereo) (stereo) 0.5 0.5-

  • 5

5’ ’ Source Source location location ~ 10 ~ 10 5

5m

m 2

2

> 0.8m > 0.8m 2

2

Area Area 30M$?? x N 30M$?? x N 300M$ 300M$ Cost Cost 10GeV 10GeV-

  • 10TeV

10TeV 20MeV 20MeV-

  • 300GeV

300GeV Energy Energy

SuperCANGAROO SuperCANGAROO GLAST GLAST

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Summary Summary

  • 10

10 GeV GeV gamma gamma-

  • ray astrophysics:

ray astrophysics:

  • Systematic study of cosmic ray origin & much

Systematic study of cosmic ray origin & much more fun! more fun!

  • Cherenkov

Cherenkov observation

  • bservation vs

vs satellites: satellites:

  • Sensitive in shorter time

Sensitive in shorter time → → deeper survey & deeper survey & shorter time variability study shorter time variability study

  • R&D items:

R&D items:

  • Larger reflector with shorter barrel, wide FOV,

Larger reflector with shorter barrel, wide FOV, modest optical quality at moderate cost: a modest optical quality at moderate cost: a little challenge little challenge

  • Fast, high

Fast, high-

  • QE optical sensors are desirable

QE optical sensors are desirable

  • Site:

Site: Australia Australia (higher is better, but cost

(higher is better, but cost performance?) performance?)