超高エネルギーガンマ線天文学の現状と将来
10
0
0
全文
(2) . . . . . 277ῌ8582
(3) 5ῌ1ῌ5. e-mail: [email protected].
(4) . !"#$%&'()* . #+ ,-.(/. 012 3 45 6789:;< = >?@A 10 BC DEFGHIJK(LMN
(5) LMOPQRS TUVWXY SZ (CTA) [P\]^( _`G+ aHIEGb TeV JK
(6) ( LM cd2e(f.g 4+ "hij klmnopqr
(7) s tuNvIwx/y*z{ |}h~)* /. (#4 c NI(+. '(%. 1. . P<,- / # . ()# ,- .# . . !. zST1# ,8.. "# $% &
(8). $/DEFz# 08. '()*. +,- .*/ 012. .12 |%7Z/63'<. 34+12%56789:; . ,- ~&4Z|% } ',Z# *. 7<,- =# >%?. */ o 3 Cherenkov Tele-. ,# @A B, X # GeV CDEF@. scope Array (CTA) 4 %. +,-. A# / GHIJKELMNO B, TeV. 100 GeV (10 eV) X/ 10 TeV (10 eV) Z. CDEF PQ'"# 34R6,ST. ,,DEF B,
(9) ()# . UV <,W%/X 4. IJKELM%+Z+,GHIJKE. YZ- TeV D. 10. 13. EF [# X/DEF \,]%. LMNO B . +Z>() !^,M_. NO B,,DEF
(10) 5. E`abc+d,- Z# ef dg# h. ¢# 1989 Whipple NO B,£¤A¥. 4+()i h4+ %jkl4. X/DEF¦l1) §,'# .¨©ª. Y. +,-. ¡*,- GHIJKELM. [mno p B"q?. 2 +# [P# :`K«()# o . *. ++!r 'sRt[6. ¬E# ,y$®6z¯°`©ª. ,P<u&- Z# vw# xy# "#. %±: 6,h4+²³GHDEFNO. z# $ c4. H.E.S.S.2), MAGIC3), VERITAS4) '# ,. {*. +,|%&}7<. ,- ~&4Z&} () ', # o . DEF
(11) %´µ4. mn B"sR
(12) %()6,~c'(%P. ·¸7# ¶·¸¹ # sºs8 100 %,d,,. <"# )*+. DEFw'?*. » 104 ¼. »7½. +,- [# ¶ +,6)- 333.
(13)
(14) . 61 46 <=2 ?@AB . . !. ?@EF0?G HIJK. "#$%&'()*+,- ./ 01. LM02 ?@AB456789N. 2. OPQR. S7T9UV (19), NOPQWU. 3 2 107 456789 :3. (4), 4XUYZ (10), ?@[\ (1), S7T9 (1:. ;<=2 "> ?@AB AC=D=. Crab Pulsar), ]^U_ (1: Westerlund-2), WolfRayet (1: W20), `ab (24) -cd 12 ?@AC Blazar (38), Flat Spectrum ef ? @ (2: 3 C 279, PKS 1222), e f ? @ (5: M-87,. 31. 32. 334. gh ij: MAGIC klm n2o17 m, pS7Pqrst9uvw3) VERITAS kl m n4o12 m, xtysqz{w4) |j: H. E. S. S. k l m n4 o 12 m, s } ~ xw2) CANGAROO klm n4o9 m, 9pq 9ptxw5)2 n w. 33. H.E.S.S. % RX J17133946 10)2 997456789NOPQ 2 Q X Q$;+2. 456789NOPQ (100 GeV) rP n?@w2 2011 1 "> 107 456789 NOPQR (100 GeV) <=6)2 . 2011 7 .
(15) Cen-A, IC310, NGC1275, 3C66B), . I%V$+%% D W< . (2: NGC253, M82)
(16) . !&'()* XY Z[\] . 3 C 279 (z 0.536), PKS 1222 21. ^ _`H%./012304aUb. (4C21.35, z0.432) 7), 8) . ! c < d./01%_` H&'()*4e f$+gh fijk. 2. . !l m!&'()*$+nop %$.
(17) . @ . 4 ! "#$%&'()*% GeV $+. q
(18) b! rLs"%&'()*;. 100 TeV !,- ./0123045 . _`H%2304aU !t%ru!. 6&'()* Cas-A (0.3 kyr) , RX J. c $ -_`H%d./01. TeV 7. D knee 7 (1015 eV) _`H;XY. 9). 10). 1713 (2 kyr) , IC443 (10 kyr). 11). 230489 : 4,$ $. ;vwx ! +!&'(). 10 kyr ;&< =%&'()* W51C (30. *M %Iy!z{p-d./01_. >?. `H4QRS |};z < : 4~. @230;A B%C3 GeV 7!. Du :%ru@!d d. D : +%EFGH4IJK DL MN. % CTA 4 D !s. %E OPB%QRS S+ - pT=U. %4 D . 12). 13). 11). kyr) , W44 (20 kyr) , IC443 (10 kyr). . !"#$%!&. x !-ru! H.E.S.S. % s"%0(y4#$- 0 $+d./01I I%i 4J:zL : +40 @LMN % E O P 0 ( y ; S . 5. H.E.S.S. !r PSR J18261334 M % D 15) 1 4-7$+%&d./0 1EFGH%4+ ./01F ;#! (200ῌ800 GeV), (0.8ῌ2.5 TeV), Z2.5 TeV ^ x 4. » 104 ¼. s ±² & ' ( ) * % s 100 MeVῌ100 TeV ./0123014) = %&'()* W51C (30 kyr), W44 (20 kyr), IC443 (10 kyr) GeV 7 ³! !´b6&'()* Cas-A (0.3 kyr), RXJ 1713 (2 kyr), IC443 (10 kyr) TeV 7 89 CTA rLs"%&'( )* µ@ a¶%&'()*%·¸ 4
(19) ru!@ - CTA 30 GeVῌ300 GeV 7 d%w4 @ L GeV TeV % U % . / 0 1 1¹\];"º : 4
(20) »7½. ./014¡"@ !# B%7 44 : 4,$ d./01I 4¢!£$¤F3F ¥@ 4+¦ : 4,$ CTA 4|§% 6 $+ 2 !£ :%ru@4L;-!¨ rL©@w4!@ - X Hª (x«"16) v¬% !rL ® % [¯%°w4!@" . 335.
(21) 85. HESS J1826j1334 701 ¡¢915)% £H ¤D &01 &¥¦% §& ¨O©ª !«¬&B
(22) e G OPQR^LGH % D® ![G&R^D¯ D°GH D±2 % ~ rs D O<²²OR iX³D3 ´!¯D°GH D±2 %. 86. ,Xz- OPQ&R^D01. 23H outer gap V °GH 32!$%.
(23) MAGIC
(24) 25 GeV . !. "#$% &'()*+!,-./01. 23&0
(25) "4&56!"#$. 17). GeV &:;!<= >?&@A. MAGIC !, ./01 &d~ OPQ56% 25 GeV µ¶& OPQ &·! 33 ms &¸¹
(26) ºy "4DB [$17)% &"4 60 GeV EFGH . 78 69% 25 B3!. opqrstu"V vwB[ x y . DWH23z % $ slot gap . &{|}~ D, GeV. . 60 GeV
(27) C<DEFGH IJKL. - MAGIC &56WH% _`a!UH. M$% N 01 23& OPQRD0. outer gap OPQDB[GH . 1 &STUVWGH . ]D56,y %. YZ[ \]. HX polar gap. S23[$ slot gap. YZ. [ ^ B3!_`a!UH outer gap. YZ. [ ^VWGH . HX\]DbcB[G. H$% 2 25 GeV de OPQDRB [GH RDVW . HXfg23 01 &STU. . . &d~ OPQ. G. Q !ot ). HX\]hiB[$% OPQ. D} z % U&O. HX:;!lHmn. &~! H M87, Cen-A &,X. STU& 4j8k10 G 12. 336. 3.. y \. »¼½. 2011 7 ½.
(28)
(29) . 18), 19). . !" #$. ij9k9l12%m ]T$F nop 12%q>Q%r]34567*O. 20), 21). NGC253, M82 %&'()*+*(. P s34567*et uv/wm=.89:. ,-.$/012 34567*89: . x=.#$"y1$F [z%WX. ;<=. ;<>? @A BCDEF GE. Y*Z*12%(^_6Vuv=.E3456. 3C279, PKS1222 (4C H21.35) %&' zI0.5 J. 7*ef9_gg9h M'{|. K%/0 ;<=.CD. 7), 8). PQ(R*6 U7. ;<%LMN O. @ASST$F. ]'Gz ]N$F. `. GE %V %)(R*6]v. d#$ ".2.
(30) o `aY*;<=.#$"]T. 421 %[\]%4567*(^_6. 22). V34567*e. }~%f9_gg9e ij9k9] N$ SSC (Synchrotron Self-Compton) 6. V #W%XY*Z* Mrk. aF (^_6Vb"c. . &$f9_gg9h. $F U 8. MAGIC. &$ Mrk501, H.E.S.S.. $ PKS2155 %Y* `a. 23), 24). &. F nop. 12x=.EXgXr%X_*6 %f+6f6{ # a$ ]
(31) . VXgXg*Y9e 50 o#$ TA no. p12%% # F GE ".2%v
(32) `aY* e%(]N$F k9_( R*6%eQ2 dE r] U7. U8. » 104 ¼. [\/«¬ Mrk421 %[\;<F 89 : ¢V Fermi, MAGIC %;<F CTA V Fermi 89: % *)S®" &A &A¯%°/0 ±# " %&'f*Y(89: (^_6 5 ² yEA³$"]N$F. V 34567* s\¡t ¢]V v4567*£¤¥ S"`¦=.# $F ayB a§#%e{|. /012. h=.E # 34567*%eV4 567*. GEV% 2 ¨. © E GEª. Mrk501 (MAGIC)23), PKS2155 (H.E.S.S.)24) %´µ vY*F ¶B2 (R*6%|·
(33) o `. #$F CTA ]V "%&'¸¹Y*]V(R*6G]º$"]N$F »7½. 337.
(34) QI . 1'23 ]ba . (B) Chandra $ X 3&X5Y. Z0 c. a (C) VLBA $&X5Y Z,- 1'23FDW EW. dR0 M87. , X 3e
(35) f]ba 3g hi. +j0 >e
(36) kVl< m+V RLh M87 0 VLBA $< 30n60 op4 qo rs f0.21n0.43 tuvg w {|}. xyXz,. R#<0 ~OPZ. Z 0 Le
(37) _` RL >0 QI . 1'23 FDW. #$ 2 h. <
(38) RL0 6YThVR [RL VLBA X. '$. <0 OPZZ 0 QI S9. M87 QI 1'23FDW 25) 1'23FDW LFDW kV l< 6YTh<m+Vh . 1'23FDW. U. ;V; h ] ''`RNL ,1'23U;VRL; h
(39) .
(40) Mrk. 0 w4'< . 501, PKS2155
(41) . ,l0 8>!5$. . # $ 0.01,. ¡A¢, RL ;. *+,- ./. ,£¤¥ ¦0 . 0.03 %&'()!". !". CTA ,0 1'234. !567.
(42) ,- §!0 QI . GeV 8
(43) 9:; $<0 =. . 67%&'()!". ¨©ª"«¬¤U;: Q. >,?@; A. 1'23; ¡A¢. . I . . $< f¯°^®+/±²9:;. BCD'EF GHIJ
(44) K L M87,. 1'23®
(45) 9:; . $<g0 #°³´>,µ¶:}. Cen-A, NGC1275, IC310 MNOP. ·5 ¡A¢¸
(46) +/±. QI . 3C279 MG!Ll #°. 1'23
(47) RL. S 9 2008 1ῌ2 TU;V M87 1'2 Z[: MAGIC .
(48) H.E.S.S., MAGIC $+/±S 10 º$»$RL Primack {¼. VLBA $<\]^
(49) _` +a. 26) HST $ Galaxy count ²9 . MAGIC, VERITAS, H.E.S.S. $<
(50). c/± $l§½RL L. 338. &X5Y. LR¹` ¡A¢ . 5$<0 VERITAS, H.E.S.S., . 3FDW W&. 25). #%T&. 2011 7 T.
(51) 1%RS$%?GH TU.V $ EF567 89GH.$W .XY$W "ZQ> [# 1%R1 !.\ ]^>2 H.E.S.S. MAGIC 2 _O `""a ,D #A56 7 89:;b7c Cerenkov Telescope Array (CTA) de27), 28).$f^>2? CTA #" g%h567 89:;i&jD k. 10 3)p 7)
(52) / "+uqrOs jY-F m0.2ῌ2 mm G³o ´' Primack µ¥O¶ m¦V
(53) o
(54) 2 . '. lXY m1 mCrabn10ῌ14 erg sῌ1 cmῌ2 .( o I V # p ,qrOs . 20 GeVῌ100 TeV t#^ uqrOs )*v.$WV 1 de"w3I%x 1,000 yY+uqrOs ),z"(-$% .),%{0,| CTA /%} v~0$RR,uqrOs ), & 12 p3& * $14+52 6,712R"D.V / CTA [ % { 0 u c q . KL . MNO 89,TU w:;<$%?u GH [^>w3p .VW B. 11 PKS1222 (z·0.432) qrO s E8) Fermi ¥ ¸ H 100 GeV yY¹Iº»³~"z%. @ `6!=,Cj[ 200 D (-2>|~.%x 8 9 . !. ?u @A_. O ` ^> @=, 20. 0.2 mm 3 mm 2
(55) . ^> 567 89 c¡ jD MN. CTA z2.5 z6 . ¢ £] MN¢ . BI ¤bc¥. . !"# $%
(56) $% & '(. b 1985 C Hillas jD$f$%29) Whipple. )*+,-./01 "2. :; 1c¡ _567 89GH.. . ¦'§D^ 1989 C¨©ª . 4. CTA (Cherenkov Telescope Array) ῍ῌ 34567 89:;<=>-%?. «¬^?1) CTA /MN¢ . jD>|:;. L7# I1 jD. m®®,¯&567 89 c¡ I,°'. E.# I1 jDo . @)AB$%>CD EF567 89G. & MN¢ B'.XY^ R?qr. HIJ>KL MNO.P2Q>,. Os )°'. J 104 ¼. J7½. ± .Y²1 "2 339.
(57) ª 12 CTA « ¬ ª3 ( 23 m) (12 m) (6 m) ?+
(58) ®2~?a3 20 GeV 100 TeV %&'()J-bc%& '()C+DE¯-/°3 ª 14 CTA ,tºE MAGIC, MAGICStereo, H.E.S.S. »¼tºE3. J-KMNbcEde f0 U;g;[ 2YZ\)D 23 CTA KU./%&' ()*+,hi MNbcEe
(59) LMNO C+DE*)@H- jj2kl mnYZ1 3 CTA -K 1,000 ABop8a_C+D ª 13 X Ee C+DEe A%&'()C+ DEe±²³´± VµVs3 2010 +m¶ · U 100 A%&'() C+DEe0./4; 3 e±0± ´±zB 0#3 CTA K 1,000 ABA%&'()C+DE e0./4; ¸¹4;3. Ekl0q4; /4;3 rV 8a_klsUtu. q4;. -vw!3 %&'()x 20ῌ30 GeV yi bcz2{vj| kl0./12 s C+DE*)@ H./01 23 }')_K ~?a 4;. 3
(60) . ?+
(61) V . 20 GeV. YZ. 100 TeV . 1,000 GeV %&'()J*)3 . ! 4 "#$. %&'. 3
(62) K 20 GeV . ()*+,-./01 23 4 Fermi.
(63) K . 56 7)8 9#:;< =)>?@2 6 ". 400 m u0" -v3 U;g;. ABC+DE%&'()@FGH' . %?+H #T$ $ !. 0-I3. $0 4;3 }')_K . 14). 20 GeV 200 GeV J-K
(64) LM. 2?+!. 2.
(65) %+X) &'. NO C+DE*)@H PQ1R S T. A( ¡V¢). UVW'X)YZ0[ 2\)D 23. . £ ¤Q¥¦. 3. 200 GeVῌ10 TeV J-K MN
(66) ] MN.
(67) -K C+DE*)@H*§. 7^)_X)`a 10 TeV AB%&'(). H¨+©+H2mn B . 340. k-½.. 2011 + 7 ½.
(68)
(69)
(70) . b. . !. kl&'Y(mK. Astronomy and As-. "#$% $&'( )*+ , - .. trophysics nX Decadal Survey .)o33) 9. /0% MAGIC 12.34 5 23 m. =!5 ZR*+ pab. 67. 67 12 8. !9 :.
(71) ; . LSST (Large Synoptic Survey Telescope), GMST. <
(72) != >?@A BC . (Giant Segmented Mirror Telescope) 5q=. DEF+GHBIJ>KL. $% rs!=. !Q=% ghijK$%!=. ! CTA . MKNOP Q< RS!=. CTA ? tu 3 ,v. Design Study .B`. T "DU.V WXY<. w 3! 2010 , 10 x Preparatory Phase . Z 9: 50 U M[. -S!= . Preparatory Phase ../? 0. 20 K 180. 1. y2 3z[. WKL CTA ? \]#^.. % ]_`$Uab. K Q=. c !!=. X{K5|4}. ~KI0K%]_`$U 56X KL :.I U.%]U %. EU . ESFRI (European Strategy Forum for.
(73) 1278.B0%]U %.i#%. 30). Research Infrastructure) , ASPERA (Astroparti-. 9:W Ri#%KL .%]U . cle Physics Network) , ASTRONET )Astronomy. %K.;7.</R .|4K.=. .dO."#N
(74) e. > . CTA ?.v@ . 31). 32). and Astrophysics Network-. !=]f"#%9=! ZR'(a. A
(75) m"#. !? BC X T ". BR.N
(76) 60 Dl='( EFYR"# CTA-Japan J G. , CTA .H/0%. I }~. !. != D5 30 J.K. L5. =KL. Q 0¡BT ".'(?X¢= £fK ¤K= ?&M.¥NR&O = =¦EP§/RQKQ 0 ¡BT ".¨4©R 01
(77) ª.i#%« )CTA « - Q<¬. !=. :. ®i ¯09=! CTA S ab?ª. 10ῌ20 ,ve! ?R= TU Victor Hess N
(78) ~V =B'(.W°. K ;7.B'(? NR<NR<KZKNO.± ²³ ´S Y 15 "#$% $&'( )*+ , - MERO TSK .4a 23 m. 67 12 @A BC DEF+G HBIJ> Z 50 U Z 104 ¼. Z7½. !Y :.V=W°. KZR 1 H_ µKL¶¬ CTA ab ;7/0%· R D. ! ²³X X ¸¹. !=YºY= »¬ 341.
(79) ῎῍῏ῌ 1) 2) 3) 4) 5) 6) 7) 8) 9) 10) 11) 12) 13) 14) 15) 16) 17) 18) 19) 20) 21) 22) 23) 24) 25) 26) 27) 28). 342. Weekes T., et al., 1089, ApJ 342, 379 HESS: http://www.mpi-hd.mpg.de/hfm/HESS/ MAGIC: http://magic.mppmu.mpg.de/ VERITAS: http://veritas.sao.arizona.edu/ CANGAROO: http://icrhp9.icrr.u-tokyo.ac.jp/ http://www.mppmu.mpg.de/~rwagner/sources/ and http://tevcat.uchicago.edu/ MAGIC Collaboration, 2008, Science 320, 1752 MAGIC Collaboration, 2011, ApJ Lett. 730, L8 MAGIC Collaboration, 2007, A&A 474, 937 HESS Collaboration, 2007, Nature 432, 75 MAGIC Collaboration, 2007, ApJ Lett. 664, L87 Abdo A., et al., 2009, ApJ Lett. 706, L1 Abdo A., et al., 2010, Science 327, 1103 Funk S., private communication HESS Collaboration, 2005, Science 307, 1938 Suzaku: http: / / www. astro. isas. ac. jp / suzaku / index. html.ja MAGIC Collaboration, 2008, Science, 322, 1221 HESS Collaboration, 2006, Science 314, 1424. HESS Collaboration, 2009, ApJ 695, L40 HESS Collaboration, 2009, Science 326, 1080 VERITAS Collaboration, 2009, Nature 472, 770 Panequeb D., private communication MAGIC Collaborationb, 2007, ApJ 669, 862 HESS Collaboration, 2007, ApJ 664, L71 VERITAS, VLBA, HESS, MAGIC Collaborations, 2009, Science 325, 444 Primack J. R., et al., 2005, in High Energy Gamma Ray Astronomy, Vol. 745, AIP Conference Series, p. 23 Design Concept for CTA: arXiv:1008.3703 http://cta.scphys.kyoto-u.ac.jp/index.html. 29) Hillas M., 1985, Proc. 19th ICRC (La Jolla), 3, 445 30) ESFRI Roadmap: http://ec.europa.eu/research/infrastructures/index῍en.cfm?pgῌesfri-roadmap§ionῌ update-2008 31) ASPERA Roadmap: http://www.aspera-eu.org/images /stories/roadmap/aspera῍roadmap.pdf 32) ASTRONET Roadmap: http://www.astronet-eu.org/ IMG/pdf/Astronet-Book.pdf 33) US Decadal Survey: http://sites.nationalacademies. org/BPA/BPA῍049810. Status of Very High Energy Gamma Ray Astronomy and Future Prospects Masahiro TESHIMA Institute for Cosmic Ray Research, The University of Tokyo, Kashiwa-noha 5ῌ1ῌ5, Kashiwa-shi, Chiba 277ῌ8582, Japan Abstract : Very High Energy (VHE) Gamma Ray Astronomy has made a great progress during the past few years and has been recognized as a new field of astronomy and astrophysics. To make further significant progress in this field, the new ground-based VHE gamma ray observatory CTA is in its design study phase within a framework of an international collaboration with members from Japan, US and EU. CTA will o#er us a 10 times better sensitivity than currently existing telescopes with a wider energy coverage, and will show us many interesting features of the extreme Universe through the observation of VHE gamma rays, which are the highest energy photons in the Universe.. ῎ῐ῍ῑ. 2011 ῏ 7 ῍.
(80)
関連したドキュメント
We intend to find the condition of the plasma in order to account for the observed flux ratio ( F RRC /F line ), which is free from specific modeling with iron abundance, the
and availability of reference materials, each method has merits and demerits. Although gamma-ray spectrometry does not require chemical separation before a measurement, a
Whereas tube voltages and HVLs for these four X-ray units did not significantly change over the 103-week course, the outputs of these four X-ray units increased gradually as
The general method of measuring the half-value layer （HVL) for X-ray computed tomography (CT) using square aluminum-sheet filters is inconvenient in that the X-ray tube has to be
Research Institute for Mathematical Sciences, Kyoto University...
Thus, if we color red the preimage by ζ of the negative real half axis and let black the preimage of the positive real half axis, then all the components of the preimage of the
RIMS has each year welcomed around 4,000 researchers in the mathematical sciences in Japan and more than 200 from abroad, who either come as long-term research visitors or
I have been visiting The Nippon Foundation, Kashiwa Company, Japan Aerospace Exploration Agency (JAXA), Ariake Water Reclamation Center, Tokyo University of Marine Science and
