Aim of this talk

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Aim of this talk?

• From Hagi and Jims e-mail.
• To determine what this U.S.-led science
  investigation is and how it fits in with Key
  Science Programs (KSPs) already being developed
  in Japan. Need to make sure all mission partners
  are happy with Key Science Programs being
  developed and who has responsibility for which
  parts of the KSPs.

YES! Absolutely.
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How to fit

• Blazars US-led
• A number of gamma-loud blazars with GLAST
• gt Statistics
• Blazar(s)JPN-led
• Nearest TeV blazar Mrk421 Campaign obs
• gt Fine structures

Complementary!
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Summary

• Complementary!
• So, we all mission partners can help each
• other and we are happy with Key Science
• Programs being developed.

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Direct obs. of high energy emitting regions in
TeV Blazars TeV blazars with VSOP2

• M. Kino (ISAS/JAXA), K. Asada (ISAS/JAXA), Y.
  Hagiwara (NAOJ), P. Edwards (CSIRO)
• VSOP-2 Sci. Working Group

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GeV gamma sky

• Most of the AGNs Blazars!

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Blazars basic picture
Sikora, Begelman Rees (1994)
Theorists claims that the size of emission
regions typical as R 1016 cm
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Recent progresses (observations)
Day scale variabilities in X-ray. It also
predict the emission region as R 1016 cm
Mrk421ASCA light curves (Takahashi etal2000)
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The problem

• R1016 cm (X-ray 1-zone model)
• is always smaller than VLBI scale.

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Yes, we will haveVSOP-2 !
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Comparison of the resolution
mas
best!
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2. Our strategy

• We focus on close source Mrk 421(z0.031)
• R1016 cm (X-ray 1-zone model)
• R1016 cm (VSOP-2 43GHz)

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Mrk 421 by VLBA 22 GHz
(Pinar Edwards 2005)
No superluminal. Why?
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VSOP-2 deeper inside
Internal shock
Cold ejecta
Central engine
We want to resolve VLBA knots by VSOP-2 and
obtain fine-structure images of the
internal-shock regions.
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Mrk 421 by VLBAshortest variability ever seen

• Charlot et al. 2006

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VSOP-2 catch faster variability
Which ones responsible for the X-ray variability?
Central engine
Corresponding light curve of each blob by VSOP-2
is what we want.
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VSOP-2 will unveil the nature of high-energy
emission regions of blazars.