Status of CANGAROO-III Masaki Mori * for the CANGAROO team * ICRR, - - PowerPoint PPT Presentation

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Status of CANGAROO-III Masaki Mori * for the CANGAROO team * ICRR, - - PowerPoint PPT Presentation

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OG2.7 paper 166 Status of CANGAROO-III Masaki Mori * for the CANGAROO team * ICRR, The University of Tokyo 30 th ICRC, Merida, Mexico, July 02-11, 2007 1 CANGAROO team University of Adelaide Kitasato University Australian National

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Masaki Mori*

for the CANGAROO team *ICRR, The University of Tokyo

1

Status of CANGAROO-III

30th ICRC, Merida, Mexico, July 02-11, 2007

OG2.7 paper 166

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CANGAROO team

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 University of Adelaide  Australian National University  Ibaraki University  Ibaraki Prefectural University  Konan University  Kyoto University  STE Lab, Nagoya University  National Astronomical

Observatory of Japan

 Kitasato University  Australia Telescope National

Facility

 Tokai University  ICRR, University of Tokyo  Yamagata University  Yamanashi Gakuin University  Hiroshima University

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CANGAROO-III: since 2004 March

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T2 T4 T3 T1

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Basic specifications of telescopes

 Location:

 3106’S, 13647’E  160m a.s.l.

 Telescope:

 114 80cm FRP mirrors

(57m2, Al surface)

 8m focal length  Alt-azimuth mount

 Camera:

 T1: 552ch (2.7 FOV)  T2,T3,T4: 427ch (4 FOV)

 Electronics:

 TDC+ADC

4

T2

Enomoto et al., Proc. ICRC 2003

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History of CANGAROO-III

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: Construction : Observation start : Expansion to 10m : Observation : Tuning

T1 T2 T3 T4

2000 1999 2001 2002 2003 2004

3 3 1112 7 3 1 6

Stereo observation

2005

Global trigger system

12 8

Maintenance

2006 2007

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Gamma/hadron separation

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 Square cut  Limit image moments (width, length) in gamma-ray domains  Ex. “Supercut” (Whipple group)  Likelihood ratio  Probability density functions for image moment distributions  Gamma-rays: Monte Carlo, hadrons: background (off-source) data  Cut by certain Likelihood ratio L  Prob()/[Prob()+Prob(bkgd)]  Fisher discriminant Now standard in CANGAROO-III  F  linear combination of image moments, with coefficients are

uniquely determined by matrix inversion to maximize gamma/background separation

 Free from selection bias

R.Enomoto et al., ApJ 638, 397 (2006)

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Vela pulsar/nebula

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  • Pulsar pointing (2004 Jan/Feb)
  • Stereo (T2 & T3 wobble), 1,311 min.
  • Fisher discriminant

Pulsar position 2 from Vela X center Vela X nebula

H.E.S.S., AA 448, L43 (2006)

R.Enomoto et al., ApJ 638, 397 (2006)

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Vela X nebula: spectrum

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H.E.S.S.: Aharonian et al., AA 448, L43 (2006)  E-1.45exp(-E/13.8TeV) R.Enomoto et al., ApJ 638, 397 (2006)

2<0.6 deg2 Excess 561114

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SNR RX J0852.0-4622

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Excess event map

  • Distance ~1 kpc

(NANTEN: Moriguchi et al. ApJ 2005)

  • Stereo (T2 & T3 &T4 wobble)
  • 1,129 min. ON, 1,081 min OFF (2005 Jan/Feb)
  • Independent analysis (ICRR, Kyoto)

2 from SNR center Fisher discriminant

  • R. Enomoto et al, ApJ 652, 1268 (2006)
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SNR RX J0852.0-4622: spectrum

10 Comparison with C-II

  • R. Enomoto et al, ApJ 652, 1268 (2006)
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Starburst galaxy NGC253

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 3-fold, 2004 Oct, 1179min (ON), 753min (OFF)

HESS (extended) HESS (point) C-III (extended) C-III (point)

Erratum: C. Itoh et al, A&A 462, 67 (2007)

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Flare of Blazar PKS 2155-304

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  • Y. Sakamoto et al., K. Nishijima et al., in this conference

 Nearby high-frequency BL Lac (z=0.117)  TeV flare report by H.E.S.S. in July-Aug 2006 (ATel#867)  1,053 min (wobble), 3-fold [8 hour difference in Time-zone!]  Analyzed by independent teams (ICRR, Tokai, Kyoto)

Jul.28

Aug.17-25 av.

 6.8 excess

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Cen A and  Cen (1)

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CenA

  • Radio galaxy, Fanaroff-Riley type I
  • “Misaligned” BL Lac (~ 60o)
  • Distance 3.5 Mpc (z=0.00183)
  • Observations:

639min (ON), 587min (OFF)  Cen

  • Old, heavy globular cluster
  • Many millisecond pulsars
  • Distance 4.9 kpc
  • Observations:

601min (ON), 429min (OFF)

Significance map

Cen A  Cen

Solid: 4850MHz radio (inner lobes and middle lobe ) Dotted: 408MHz radio (outer lobes)

Kabuki et al., ApJ (in press, Oct. 2007) / arXiv:0706.0367 [astro-ph]

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Cen A and  Cen (2)

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Kabuki et al., ApJ (in press, Oct. 2007) / arXiv:0706.0367 [astro-ph]

SED for the jet region of CenA

CANGAROO-III

HESS Bai&Lee 2001

Dotted: IC with 1054erg, 100 TeV cutoff

Upper limits of the CDM density

 Cen CDM density <100Mpc-3: less than its gravitational mass!

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Summary of TeV source status claimed by CANGAROO compared with H.E.S.S results

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More detections are coming!

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MSH15-52 Pulsar wind nebula HESS J1804-216 UnID HESS J1303-631 UnID And upper limits as well…

See: Nakamori et al., in this conference See: Higashi et al., in this conference See: Kushida et al., in this conference

  • Ex. Clusters of galaxies: See Kiuchi et al.,

in this conference

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Summary

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 CANGAROO-III atmospheric Cherenkov telescope system is observing

sub-TeV gamma-rays since 2004 March in stereoscopic mode.

 Observation of Vela pulsar showed no gamma-ray signal, but there is a hint

  • f signal in the Vela X nebula.

 SNR RX J0852.0-4622 was detected as an extended source, and the

morphology seems to follow the X-ray emission profile.

 Starburst galaxy NGC 253 was observed with CANGAROO-III but the

signal reported by CANGAROO-II was not confirmed.

 A flaring activity of a blazar PKS 2155-304 was detected in July-August

2006 showing rapid time variation.

 Radio galaxy Cen A nor globular cluster  Cen were not detected.  Conflicts with H.E.S.S. results are mostly resolved. Analysis of stereo

  • bservations are now established, and application to other sources are

underway.