6.2 W Y Z D x w Ô ¹ º ¼ R d e 4 W b c f 5 r g ¹ º 6.2.1 …...6. 145 6.2 6.2.1 ! " # % ') *...

9
6. 145 6.2 6.2.1 Astro-E2 [36] 2005 7 10 12:30 M5 6 (Suzaku, ) ( ) (1979 ) (1983 ) (1987 ) (1993 ) 2000 ASTRO-E 565 km 15 (HXD) [17] [18] [19] (HXD; Hard X-ray Detector) JAXA Stanford HXD 10–600 keV (HXD-S) (HXD-AE) (HXD-DE) 2004 HXD [47] [48] [63] [105] 2 HXD 7 23 DE 25 AE 7 26 64 PIN (500 V) 36 (900 V) 8 5 HXD 20 14 CCD (XIS) (XRS) 8 8 XRS XRS HXD 8 15 19 A [2] HXD XIS HXD HXD HXD ( ) [90] [91] [92] [96] HXD [34] [97] HXD 6.2 a HXD HXD cutoff rigidity HXD [44] [94] 10 20 50 100 200 500 Energy (keV) 10 10 -3 -4 Counts/sec/cm2/keV 6.2 a: Non X-ray backgrounds, per unit effective area, of the HXD (PIN and GSO)[34] compared with that of the BeppoSAX PDS. HXD [13] [48] JAXA HXD [44] [94]

Transcript of 6.2 W Y Z D x w Ô ¹ º ¼ R d e 4 W b c f 5 r g ¹ º 6.2.1 …...6. 145 6.2 6.2.1 ! " # % ') *...

Page 1: 6.2 W Y Z D x w Ô ¹ º ¼ R d e 4 W b c f 5 r g ¹ º 6.2.1 …...6. 145 6.2 6.2.1 ! " # % ') * +,. 0 1 Astro-E2 [36] 2 4 2005 5 7 6 10 7 8 7: < = 12:30 > 4 @ A B D E M5 F

6. � � � � � 145

6.2� � � � �

6.2.1 � � � � � � � � ! " # % ' )* + , . 0 1

Astro-E2 [36] 2 4 2005 5 7 6 10 78 7 : < = 12:30 > 4 @ A B D E 8M5 F H J L 6 MN P Q R 4 S T U W Y Z [ \ ^ ` a c d ^ g 4 i k lm o

(Suzaku, p q ) r t u v ^ g x ( y � � � ) � i kl m o 2 4 i 2 m a � o(1979 5 ) 4 i � � � o

(19835 ) 4 i � � � o(1987 5 ) 4 i � k \ o

(1993 5 ) > � m7 : � N � 8 , . 0 1 � 4 2000 5 ! 6 > ` a c d #$ & x ASTRO-E

8 ( * + N � � - � i k l m o 2/ c 0 1 2 4 5 565 km8 6 7 8 P : a 4 < 7 > /

= P15 > ? k - �

◦ @ B D E G H (HXD) [17] [18] [19]

i k l m o J L M O 8 < Q � � - T , . U V X(HXD;

Hard X-ray Detector) 2 4 Y Z � JAXA 4 \ U ] 4^ _ ] 4 � ` 4 a b ] 4 c ] 4 d e ] 4 Stanford ] fg r h i & � j k & x : 8 � � - � HXD 2 10–600keV

8 \ R l n o q r t r v w � x R y J z { | }~ � P � � & 4 U V X �(HXD-S) 4 � � F { � � ?� �

(HXD-AE) 4 � � � o � � �(HXD-DE) f g8 � ~ � r n ~ L \ ^ � - � � g ^ 2 4 2004 5 � 6� 8 < � � � � � � > � � � v � 2 � 4 �   6 \ ^2 0 1 c � 4 ` a c d ¡ 8 ¢ £ ¤ > ¥ ¦ g � R x �

◦ HXD § ¨ © ª « [47] [48] [63] [105]

` c d 8 ¬2 ­ = ® 4 HXD

8 ¯ a c d � j ° ¦ gx � 7 6 23 7 > 2 DE� 4 � 25 7 > 2 AE

� > �± P ² ³ & 4 7 6 26 \ ^ 2 64 ´ 8PIN µ ¶ · r �

(500 V) r 36 ¸ 8 ¹ º L ¼ ½ r ¾(900 V)

8 0 ¿� ± 8 ² ³ > À � Á �  à � ¿ P Ä Z > 0 w 4 � x

· ~ < = P Å Æ > Ç m k - A È P É Ê 4 8 6 5 7 >2 Ë Ì Í f Î � Ï Ð P Ñ � � Ò x � � g > 4 � HXD8 Ó � � 4 ` a Ô d < 8 Õ Ö f g � × Ø k - � r fm 4 Ù Ú > Û Ö & � R - � r � Ü Ý ¦ g x � x Á &U V X � P Þ ß à � � > Q f � ! ¸ 8 � r L � ¶ �8 a 4 < ¸ � Ö Û � 4 � & x −20◦

� 2 f m 4−14◦ ¡ ® � Ï Q k - � r r f � x �

¡ ® & � 4 i k l m o > J L ¦ g x CCD � |(XIS) r 4 0 � 1 , . � � �

(XRS)8 ¯ a Ô d : �

� & x � & \ & � � j ° 8 � � 8 5 8 6 8 7 4 XRS8 à � � � - � D � � } � � � � > � � k - r R � � � Ò 4 XRS 2 N � P # R 4 � P � & x 0 12 � � � � � r � > � � x � HXD 2 0 ¿ P k � � ·¹ & 4 Þ � 8 � � P � � > U & x � 4 " # f R r$ & ¦ g x 8 � 4 8 6 15 7 \ ^ 0 ¿ 8 ( ¯ a Ô d P

' f � x � � 19 7 > 2 � Ú Ï Q > ) * & , H ~ � }o - .A

8 � � � ¹ 0 r - L | ¶ L P Ñ � & x [2] �� 8 ® i k l m o 1 ,

HXD r XIS8 ! 3 5 8 U V

X � � � P ' � r > f � , 6 � 1HXD Ï Q 8 8

9 : P ; w � R - �◦ HXD § < = ? @ AB C � � � r � P Q R x HXD D F G H &

( I ¶ ~D J Ö f g

), N � U K , Ö Û D L & R M Ù f g P ,

6 � P N O Q À w x [90] [91] [92] [96] � HXD1 S U

� W � Y Z D \ ] D x w , N Ô � ¹ º - ¶ ^ ¼ N �Q 4 - _ R ¶ ` ~ W b c ' f � � / Ô Q d e & , 5D ® D / Ô � r � � g � , L � f ¹ º - ¶ ^ ¼ b ch i � j � k P l k � m y ^ 1 n o p q D � r r &

� , B C � � � r � P Q R � , N Ô r / Ô D ¶ ` ~W b c � | � r � P ¢ t � & x [34] [97] � 5 D u v ,HXD

1 � Í r k - x x y ^ z { | } ~ � P Ñ � & �R - � r � Ü Ý ¦ g x � y 6.2 a1 , ¢ t � ¦ g x

� | � r � � D HXDy ^ z { | } ~ � � � - �¢ t � ¦ g x z { � : ,

HXDy ^ z { | } � 1 <} Q ¢ ] � � � � g J Ö k - � 5 D � � � 1 , / �

� cutoff rigidityQ � � x � � � � 1 D � � Q � �

� � � , � � � � � � � � Ú � � � �   ¡ D ¢ D £¤ ¥ D Þ ß � ¦ § � ¨ Ç C Q 1 , Þ ß � � � D © ª« " # Q ¬ � ¨HXD

1 · ¹ ­ ^ W ® ¯ � « ¡ ¬ � ¡° , ± ^ ² ³ ´ µ ¶ · 1 ¸ ¹ D � � , i � j � k D µ ¶ W ¬ º � « � Q , » �   ¼ ½   ¾ À Â � Ã §

� , Ä Å Ç D � È É � � À ° ¡ [44] [94]¨

10 20 50 100 200 500Energy (keV)

10

10-3

-4Counts

/sec

/cm

2/k

eV

y 6.2 a: Non X-ray backgrounds, per unit effectivearea, of the HXD (PIN and GSO)[34] compared withthat of the BeppoSAX PDS.

◦ HXD § Ê Ë Í Î Ï Ð Ñ Ò [13] [48]Ó Ô Ô D M Ù � Ö × Ø � ¬ D Ã , Ó 3 Ù ¹ W µ Ú ÛD Ü Ý Þ � × È ß à D � ¸ � g ¦ § � ¨ g � h

JAXA� � Q , � � D � � Û � � À ° ¡ ¨Æ 1 , �   ¡ HXD È ß à Q � � � ´ � D� � ¶ ` ¶ W � � g   , � Ü � � Ò È ß à Q J � ��

� � � g ¦ § � ¨ � Ô ¦ D � ` ¶ W b c , £ ¤ ¥I � ¶ D � � , � É - � � W � � � � É � ß � D J

� , � ` ¶ W j � � ¬ º D Û � à � � � ¨ � �� Ù � W µ Ú Û 1 , � ß � ß Q 1 � Ü � � ¬ � ¨ �� 1 , È ß à � � � � � � - � ² W É � � � � � �

D , � � D � � É � ß � ! " k D $ & � , ® ¯ D () � Q Þ � - . / ª D M 0 2 3 ¦ , � � � 1 5 M0 È ß à ` ß - 7 �   ¼ 8 9 : Q � Ü � � � ¨

� � 1 , È ß à � � ½   ¾ À ; < ± ^ ² ³ ´ µ ¶· D » > ? @ � A B C D Q � Ü � � � � ¦ § �

[44][94]

¨ � � Q E A F G H ¬ ± ^ ² ³ ´ µ ¶ · J � ² WÉ D L M A ½   ¾ < N O Q ; < T U � V ¶ W � � ¬

� È ß à � X � É Y L M A Z È É ± [ ² ³ ´ µ ¶ · Y] ^ _ ß É Y � Ü ¬ º A � ` ¬ a b à § d A 9: Y � ß � ß N f g h ¬ ? @ � i j k ¦ § � ¨

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146 6.2. � � � � �

◦ � � � � � � � � � � [76]� � � � � " $ % & ( � * + , . / � � 0 1 2 32004

* 4 & 6 8 � : < & � = > @ � A � � � � �B(SWG) , � C E F H I J K � � 3 XRS & M N PQ , � C S T U � V W � � � X � � K � � ! Y � 2005*10 Z [ \ " � 2 3 SWG ] X _ � # � & a b c d

, e C 0 1 $ E % 3 ! ' ( & . / $ g h � � �2005*

10 Z 12–15 : 3 JAXA , , SWG S 1 c d � .i j ' 3 2006* l Z 4 " � , SWG m � , . / � o

p ( 700 1 $ E F � � � r 2 2

SWG _ � # � m �, 3 Y & + , t u j ' � S 4 � 5 , 6 7 8 w x $ 9

: � u ( ' � < 9 � y z 2 3 = > & { | , ~ o � �� � � � � 2

2006*

4 Z ? ( 3 � S � A � 1 � ,� h � 3 JAXA 3 6 _ � � NASA 3 < e % � �ESA

� � � U , E F j ' � . / � g h j ' � � r 2 9 D� U � . / � � $ F � , 3 . / 6 + $ � � � , � � �SWG 4 � 5 9 A � . / 4 � 5 9 3 t u % � * � �

� � � m � � x 2 � Q � 3 S � � , A . j ' � �

◦ HXD � �   ¢ ¤ � � � ¥ ¦ § ¨ © � ª « [49] [64][93] [95] [98] [99]

HXD & ¬ � � J ® 2 3 ] ¯ ° ± ® � 6 7 ² ³ ´, ¬ � � J � � M N , µ ¶ 3 50 keV – 5 MeV & ·¸ ¹ º 3 » ¼ ½ ¾ ¿ � w Á 3 Ã Ä Å Æ 6 3 Ç � � K

¾ È É Ê Ë � � � � � 3 WAM (Wide-Band All-SkyMonitor) M N � � : � � � 3 � > � 3 � � 3 · �� Ê Ë m L � º 3 WAM , e � . / � � � � �

2006* � Z 4 � º , 3 � º , 50 � � ! � » ¼ ½ ¾ ¿ # wÁ ( $ � � 2 % & ' ( )

� ¯ ° � * , C 3 % & - ® 2Konus-Wind 3 � / & HETE-2 3 0 _ � � & Swift Ê

Ë & 2 É m � 3 � � M Î ¼ Á º $ � �

6.2.2 4 6 8 9 ; = > ? @ B D F HI � K 2

2005* L Z � � � M � � N � 3 O É P ÉQ

BD+30◦ 3639� . / � � � R S 2 Ð T U É W �

X & Ñ Y Ò Ó , Z � 3 [ \ � ] ° � ^ ^ _ ` a É ,Ô b Õ d " & 0 1 º 3 e � É f W ] ° g , h i � �R m º h k l W Ö � 3 n o B p q ½ W Ö y r S s Ut ¾ � ] u � � � . / & v z 3 w S � x t ¾ y z �

� ^ � � � M �CCD � _ p

( { T | u × & } ~ ) ,e C 3 a � � � � � b K & � � � � t ¾ � ¯ ° � �R m , y � � �

( � � � p # � � ) [33] [58]�

w � � Á � b K � � � � � m � � & � 2 3 � � �y � �90 � � � � � � � R S 2 É & � � � � \ & �

® º  34He →12C & ¡ ¢ £ º ¤ K S � � � W   ¥ ¦

, e C � � � � \ & " ® , § © " $ K S   É f m �* ] ° r S * � � v z m ª « º © � [4] [45] [43] [65][82]

� É ¬ ® º & � � £ y m ] ° & ­ ® � W ¯ , ° ¶� ± ² Ê y z º[3] [29] [31]

  I � & > ³ ´ µ & ] X® ¶ m Ê K �

[33] [108] [117]� 2 É & · " $ b K

[ * º & ¹ º » Ö ¼   ½ ¾ ¿ Ê � À Á º $ � �

6.2.3 Â Ä Æ @ Ç É Ê◦ Ë Ì Í � Î Ï � Ð Ñ Ò Ó Ô Õ Ö ×

Ø Ù Ú K ¼  XMM-Newton

º Û Ü r S �12 Ý Þß à � � ß à � � � �   � ² � T U   t ¾ ] u � p q

½   , � � � p q ½ � Þ ¿ ¥ �   � � Þ T U¶ � � � � � � r K ¿ ¥ � � � 2MASS � # � � Þ� � [ ¾ � # � b K   É � ß à � Þ T U Þ � � ¶ �

� � � � � % Þ v � � � S Þ � º �   ß à   � ²� T U   � p q ½ Þ � ¿ � � ¿ � © M � W � R

�   � � � p q ½ � Þ ² � � ¼   � ² � T U � � �� � Ê � � � � � � � � � ^ R � � � � � �

[60][88] [107]

� � M ¿ !6.2 b Þ � # ¿   ß à ¼ � p q

½ � Þ � %   � & � � ' ¿ ( � � * * + � � � RS ¼   ß à W ² � � � ß à � � � ¿ ] - � ^ ^   �� / 0 b 1 * 2 3 5 7 9 � Þ : ¿ ; < = > ? ¾ � R

� � A B �   Ø Ù Ú Þ ¹ º D ³ ´ µ � F & �[32] GH � I M K � N � � ß à � Þ Û Ü M N O r S � G

Fornaxß à � ? ¼  

CCD P Q p ¿ � � ¶ R Þ v �  � p q T � Þ Fe, Si, S

F U ¿ � V   � � ¼ � % [ ¿� W & * , %   � p q T X ¿ � � T U � � � � �� � M ^ R � W Y Z r S �

[74] [87] G R S ¼ Ø Ù ÚÞ ¹ º ´ µ b K M A B r S � v � ?  

II \ �Ia \ Þ] ^ _ Þ � ` a z W b X � c ¾ d R � � A B e � G

1e-05

1e-04

0.001

1 10 100

Rat

io

2D distance (kpc)

Iron-Mass to Light Ratio

!6.2 b: Iron-mass to light ratio profiles of 12 clusters

of galaxies [32]. The iron mass contained in the hotplasma within a given projected radius is divided bythe stellar mass within the same region.

◦ Ë Ì Í f Î Ï g Ë Ì Ó h j k lm n K ¼ H ß à W ß à � 2 3 5 7 9 � Þ : ¿ ; p K­ q ¼   r s e � ß à W ß à � � p q T � b K u v¦ w F x y � z 1 � v � � ª « � c � � G R Þ {| W } � 1 S ~  

X � ¶ � ? � � � � d � à � Þ �� R (� à

) Þ � � % ¼   � � Þ b � � � M ¿ � � e� ¼ � ? � � G� � � ¼ � �

(z = 0.0183) Þ � � � � � � à � �  z = 0.55 Þ CL 0016+1609

� à � ?   � & � � ¿ �� � � � R Þ � � ¶ � � � � � d G � Þ � �   � �

� � � � à � Þ � à ¶ � ¼   � � ¶ � ? � � � � d�  

CL 0016+1609 Þ M Þ ¿ � V   Y � ¿ � ' ¿ (� � c � � � � � � - � d

[61] G   ¡ ¼ ¢ £ � µ ¤ ¥¦ § � © � � c ª H e ~ � K « ¬ ­ P Q ® Þ ¯ N � °

� F U � ± � ª § ² � b ³ � ´ µ ? � � G

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6. � � � � � 147

◦ � � � � � � � � � � � � ! #$ & � ' � ( � ) * + � , - . / 0 1 3 � ( 4 56 7 8 9 ' � ; < = ? @ A C D E 4 � ) * + G I JK L G M � N 3 1 P Q ( R S 7 8 � W X Y 7 [ ' \

] ^ E _ a Q ] b c � d 4 ' \ � ] ^ E BeppoSAXe f c � d 4 g I h i 6 j ; k l 0 n ^ 8 p [ � Wq P r _ Q t u b r 4 Fornax

' \ � i v ; w x '\ � � y S { 9 ( P | 4 CCD } ~ ) (XIS)

; ? @A C D � � (0.3–10 keV)

r 4 I h 6 j ] ^ ; � � 0� � 7 8 4 _ a Q ] b ; � � � � � r 3 9

[87] W � d� x ; ' \ � ] ^ E 4 _ Q t u b

HXDc � � g I h6 j ; � � 0 � � 7 8 � W P 8 � r

NGC 3376i v

� � ; ' \ � ] ^ 4 HXD-PINc � d � ] c g I h� � ; � � 0 n ^ 8 p [ � 0 4 � � � ) � � ;

� � � 0 � � � � � 8 p [ i [ 9 � 4 � � h r E i[ [75][89] W � � 4 � � { 9 � � � ) � � ; � �A � / [ p � n � � � D � � 5 � Q � P ( r 4 ! d

� � i � " � $ 3 9 [ W

6.2.4 % ' ) + - / 1 2 4 6 8 : ; =◦ > ? A � C D E � � � F G� H J �   ^ E J ¡ K c N 3 M 3 4 � 9

JAXA;

N O ^ ( ¢ P { 4 Q R S T Q V W £ X Z � L f( [ ]^ V LMXB) ] ^ ; _ ¤ ¥ 6 j ; ¦ § a ¨ � 9

[39][27] [55] W S T b 0

Eddington c d c e f u g 4 6 jh c ! i k L 0 l © 7 8 4 ª X 9 k m n o c ! i pq r s t 3 v ^ 8 G M 7 8 V 4 g [ x ­ ® a z { }

~ ~ a V W _ ¤ ¥ E 4 G M 7 8 9 k L c ! V g I h �= 6 j ] s } 8 � [ W � Q � u � c ! V � � ;LMXB; y S s � � ] 8 4 � D � 5 � a � � p [ V W

◦ � � � � � � � � �� £ X Z � L � c Q R S T 0 1 3 V g 4 ¤ ¥ � A� D g � i 4 ¯ ° � A Z c E k L � p � � � r

� � c ! V �   ¥ 0 � 8 V W � H 4 ¡ ¢ 4 £ ¤ ^ E� ¦ � ¥ g ¢ P } 4 INTEGRALe �

[20]J

RXTEe �[10] [56] [57]

a / [ 4 [ u ~ ] ; ¤ ¦ � A � D§ � p � � � r � � ? @ A C D ; ¨ K © ª � a ¦§ } « W � ­ � u � § E 4 ¯ s c ? @ A C D ¯ ° D A

; ± ± ² ³ §Her X-1

a[80] 4 � « ´ � � � D ¯ �} «

A0535+26a · ¸ ² ³ § y S }

[24] [81] 4 q 8¹ 8 36 keV g 45 keVc 4 � � z º a � ¼ ½ ­ V P

g 0 § 3 «[30] [66] W A0535+26 E 4× 1035 erg s−1

g [ x w [ ¨ K � � « 0 4 � � ? @ A C D E 4 � ¾ c¨ K 0 � À s � ] � « g 3 S � 7 8 « Á g 4 10% ÂÃ § � Ä } Å [ « W Â $ ; Æ g ] ^ 4 � p � � �r � � ? @ A C D E 4 ¤ ¦ ¨ K c © ª ­ V X Ç s q

x § � [ X Ç s a i 4 È � ³ � É Ê a Ë Ì Z § a V W◦ Í Î Ï Ð � � � � �Ñ Ò Ó Ô � A � D (

� M Ñ Ò ­ V � Õ X ; Z � L�

)§ E 4 Ö × (

Õ X ) Ø (M K ) Ø ( Ù ; � p * )

cÚ Û ­ V ? @ A C D ( Ü Ý ³ c ∼ 1018 eV) � § 4 K

L Þ G M 7 8 Å [ V Æ g Þ ß � 8 Å [ V W � ­ � u �§ E 4 ] c � A � D ( � �33 msec � � 6.2 c) ¯ !

�PSR 1509 − 58 ( � �

150 msec)Þ y S � 8 4

[ � � § � � Þ � � § 3 « W � 4 £ ¤ 4 � ¦ ;� ¢ � E � ; � D � a / [ Å 4 HXD

; � � f � ��

(� � n 5 �

61μ sec)Þ ± } u � [ Å [ V Æ g a

� � } « W SN1987A§ E 4 � � ­ V � � � Þ � � a

G I ­ V Æ g § � � V I ³ � ¦ Þ � u � i ~ ~ � V[67] W � � D � } s � � � Å [ V W

folded at

33.58090 msec

60

80

100

Cou

nts/

sec

Pulse Phase0 0.5 1.51.0 2.0

� 6.2 c: Spin-folded light curves of the Crab pulsar,detected in the 20–50 keV band with the Suzaku HXD[48]. The signal includes unpulsed nebular emission.

◦ � � E � � � � � �� Õ X � � ] [ � E � $ & ; Ñ Ò Ó Ô � � D g� « Ù § � Õ X � K E Z � L � ; s ; ! i À Ö ¥w [ Þ � M K g � p * ; " E � Z � L � ; X Ç a $À Ö ¥ $ Ñ V X Ç Þ � V W ! � Å

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( � �33 1 )

§ 3 Ò ­ V � Õ X � � ] [ �AE Aqr

a � ­� u � c ! i y S } « g Æ | � Q R S T c 5 x I ³

� � ¦ c G 6 � 33 1 ; � � § 7 8 � 8 « g I ³ � _� ¦ a � 9 � u g s ∼ 50 keV � § ; 6 V Æ g c <

= } � > ? a ¼ ½ ­ V Æ g Þ § A « W◦ B C D F H � � I EJ K K s � - . � L M � ¥ g � N § � Q R S T

­ V O P Q R S T U . V a W X[6] [12] � [ Y ~ ,

U Z \ ] ^ s � � � «[110] [113] [115] W

� ­ � Y � ` a i � Cyg X-1[69] [79] � GRO J1655-40[68] [78] � GRS 1915+105, 4U 1630-47 � ¥ U O

P Q R S T d � Þ e f � g � h H � j � U k l aW X « W [ v g s m T o q r ` � i � CCD t u P gHXD

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x � X V , Þ � J � U � � § � V W◦ ULX � �

ULX (Ultra-Luminous compact X-ray) � � j �� � � � O P Q R S T g � Ô � � U � M O P Q RS T g a � � Z � � O P Q R S T U � � � � �§ � �

[11] [28] [40] [53] [54] W � �   L � j L M¡ - . g 0 � } � NGC 1313� ¢ ` � � � ~ U ULXa £ � � � ­ � Y � XIS � XMM-Newton � Chandra �

¥ U È Z ³ � � T � k l a W X « W � U � ¥ � Æ g

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�ULX � � � � � � � � � � � � � � � � � �

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◦ I � J K MN � O � P R S T U V � 4 � � W X �20 Y Z \] 3 _ � ` a b c e g h j

[73] � k � ` a b c e g hj

[72] � l � _ � ` a b c e g [71] � m n e o e � p� h j q s t � h j u � T U � v w � x y � � z� { | q s & } ~ � � k � ` a b c e g NGC 4945

. � Z � � � ; 3[86] � 100 keV Z \ ] 3 � � �� � � � � � � 1 � � ) � � � � � g � b � � � �

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n 9 Z � : � w [25] [37] [42] [59] � 6 ® ¯ + � 6 °4 < = ? t � � + @ � A ; � 2 b n 9 � 2 C D q

; F + & H 4 I J L v w M N � O P 5 � � v q ;�' ( � � � w Cygnus OB2 9 Q R ² e R T U �

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2003³ ` 4 a b � � 2

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f 4 2 + @ h i 4 O j k 3 d e 5 � � v q ;�

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= ´ � 6 � � � k · L � � � � · � � � � ¦ d e � 2� � � � � � ·

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� � �CsI � � � � ª � � ` � 2 � �

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BGO � � 32×32 ³ � ¨ © ´ µ y ¶   � ¸ ´ Ë

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� � ¼ ½ � ¾ ¿ À Ç �  ¥ � ( à z Â Ä ² �80058)

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5.4 % (FWHM) Ç ° ± ² ³ ´ ª « ? � Õ Ö� � �

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) �6× 109 ³ Ç 100 MeV � � � � Ð D $ � Ã � Ï

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6. � � � � � 149

� 6.2 e: Images of uncollimated 662 keV photons,obtained by a gamma-ray imager consisting of 32 × 32pixels of BGO scintillators each 1.5 mm squared. Thesignal is read by a position-sensitive phototube [35].

◦ � � � � � � � � � � �� � � � � � � � � � � � � ( � � � � � ) � ! #� � % � � & � � ( * ! # $ % & + ( [100] [106] �

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; � < ; < ! > 6 > � � ; ? � ? @ A ! $ 2 % B AB C D E / F C [23] [104] �

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` S � Ma � ? }

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[102] �

� Z [ N � � � � } � � c � � � � Z �

% � ! � � & � ~ � ( * � � } � � ^ Y C �LaCl3� D � LaBr3 ? G � } � �

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[103] �

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� S Y � � ∼ 60 keVT � º 2 � c C » ( f (

´ g ( ? � ¼ ½ F ! ¾ ¿ À Á  \ h Ã Ä d i U � !\ Å ± Æ O � � [16]

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w x z � � Î � c � Q : U j Ï Ð Ñ ( * \ Ò Ó B C� ! � F C � 2011 Ô Õ ! Ö k × Ø \ � w � } � Ù �JAXA

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[1] � � � 10 � � � � � � � � � � � � � � � 2006�3 � 26 �

� � � � � � � � �

[2] � � � � � � " ( # % ' ) � * � � � . 0 1 3 45 6 � 7 8 : ; < 6 � > @ A B D F H I J K M O P QR S F J 3 4 U V W Y � > JAXA U [ ] _ ` a b cd � 2005 �8 � 26 � )

[3] e f g > h i j k > � � > l m n � > e o pq > r s t u > � v w > Keith Arnaud > x y k z &� � � � � � " � * � � � . } ~ � � � � � � � �

V J � � � � � � ~ J � � � � ] � ~ � ~ � � > g� J � � � > � � � � � � % � � � � a b c d � �  ¡ > 2006�

3 � 26 � )

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[4] Murashima, M., Kokubun, M., Makishima, K.,Kotoku, J., Murakami, H., Matsushita, K., et al.:“Suzaku Reveals He-burning Products in the X-ray Emitting Planetary Nebula BD +30◦ 3639”,Astrophys. J. Lett., in press (2006)

[5] Young, A., Rudnick, L., Katz, D., DeLaney, T.,Kassim, N.E., & Makishima, K.: “Canonical Par-ticle Acceleration in FRI Radio Galaxies”, Astro-phys. J. 626, 748-766 (2005)

[6] Kubota, A., Ebisawa, K., Makishima, K., &Nakazawa, K.: “On the Temperature Profile ofRadiatively Efficient Geometrically Thin Disks inBlack Hole Binaries with the ASCA GIS § , Astro-phys. J. 631, 1062-1071 (2005)

[7] Isobe, N., Makishima, K., Tashiro, M., & Hong, S.:“The XMM-Newton Detection of Diffuse InverseCompton X-Rays from Lobes of the FR II RadioGalaxy 3C 98”, Astrophys. J. 632, 781-787 (2005)

[8] Ezoe, Y., Kokubun, M., Makishima, K., Seki-moto, Y., & Matsuzaki, K.: “Investigation of Dif-fuse Hard X-Ray Emission from the Massive Star-forming Region NGC 6334”, Astrophys.J. 638,860-877 (2006)

[9] Ueda, Y., Ishisaki, Y., Takahashi, T., Ohashi, T.,& Makishima, K.: “The ASCA Medium SensitivitySurvey (The GIS Catalog Project): Source CatalogII”, Astrophys. J. Suppl. 161, 185-223 (2005)

[10] Nakajima, M., Mihara, T., Makishima, K., &Niko, H.: “A Further Study of the Luminosity-Dependent Cyclotron Resonance Energies of theBinary X-ray Pulsar 4U 0115+63 with RXTE”,Astrophys. J., in press (2006) [astro-ph/0601491]

[11] Tanaka, T., Sugiho, M., Kubota, A., Makishima,K., & Takahashi, T.: “Spectral Evolution of a Lu-minous Compact X-Ray Source in NGC 253 withChandra and XMM-Newton Observatories”, Publ.Astr. Soc. Jp. 57, 507-511 (2005)

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150 6.2. � � � �

[12] Abe,Y., Fukazawa,Y., Kubota,A., Kasama,D., &Makishima,K.: “Three Spectral States of the DiskX-Ray Emission of the Black-Hole Candidate 4U1630- 47”, Publ. Astr. Soc. Jp. 57, 629-641 (2005)

[13] Terada Y., Watanabe, S., Ohno, M., Suzuki, M.,Itoh, T., Takahashi, I., Sato, G., Murashima, M.,Kawano, N., Uchiyama, Y., Kubo, S., Takahashi,T., Tashiro, M., Kokubun, M., Makishima, K. etal.: “Development of a Monte Carlo Simulatorfor the Astro-E2 Hard X-ray Detector (HXD-II)”,IEEE Trans. Nucl. Sci. 52, 902-909 (2005)

[14] Yanagida, T., Takahashi, H., Itoh, T., Kasama,D., Enoto, T., Sato, M., Hirakuri, S., Kokubun,M., Makishima, et al.: “Evaluation of Propertiesof YAG (Ce) Ceramic Ccintillators”, IEEE Trans.Nucl. Sci. 52, 1836-1841 (2005)

[15] Miyawaki, R., Niko, H., Okada, Y., Kokubun, M.,Makishima, K., Negoro, H., Kotoku, J., Terada,Y. al.: “High Resolution Fourier Synthesis HardX-Ray Imaging Based on CdTe Strip Detectors”,IEEE Trans. Nucl. Sci. 52, 2052-2057 (2005)

[16] Tajima, H., Kamae, T., Madejski, G., Mitani, T.,Nakazawa, K., Tanaka, T., Takahashi, T., Watan-abe, S., Fukazawa, Y., Ikagawa, T., Kataoka, J.,Kokubun, M., Makishima, K., Terada et al.: “De-sign and Performance of the Soft Gamma-Ray De-tector for the NeXT Mission”, IEEE Trans. Nucl.Sci. 52, 2749-2757 (2005)

[17] Ohno, M., Fukazawa, Y., Yamaoka, K., Kokubun,M., Terada, Y., et al.: “Preflight Calibration andPerformance of the Astro-E2/HXD-II Wide-BandAll-Sky Monitor”, IEEE Trans. Nucl. Sci. 52,2758-2764 (2005)

[18] Yamaoka,K., Ohno,M., Terada,Y., Hong,S., Ko-toku,J., Okada,Y., Tsutsui,A., Endo,Y., Abe, K.,Fukazawa, Y., Hirakuri, S., Hiruta, T., Itoh, K.,Itoh, T., Kamae, T., Kawaharada, M., Kawano,N., Kawashima, K., Kishishita, T., Kitaguchi, T.,Kokubun, M., et al.: “Development of the HXD-IIWide-Band All-Sky Monitor onboard Astro-E2”,IEEE Trans. Nucl. Sci. 52, 2765-2772 (2005)

[19] Hong, S., Yamaoka, K., Terada, Y., Ohno, M.,Tsutsui, A., Endo, Y., Kotoku, J., Okada, Y.,Mori, M., Fukazawa, Y., Kamae, T., Kokubun, M.,Makishima, K. et al.: “Performance of GRB Moni-tor with Astro-E2 Hard X-ray Detector (HXD-II)”Nuovo Cim. 28C, 821-824 (2005)

( � � � )

[20] Okada, Y., Niko, H., Kokubun, M., Makishima,K. et al.: “A search for Cyclotron Resonance Fea-tures with INTEGRAL”, Proc. 5th INTEGRALWorkshop:“The INTEGRAL Universe” (eds. V.Schonfelder, G. Lichti & C. Winkler), p.467 (2005)

[21] Itoh, T., Kokubun, M., Takashima, T., Yanagida,T., Hirakuri, S., Miyawaki, R., Takahashi, H.,

Makishima, K., et al.: “R&D of a New 1-Dimensional Gamma-Ray Position Sensor UsingScintillators Coupled to a Si Strip Detector”, IEEENucl. Sci. Symp. Conf. Record 1, 186-190 (2005)

[22] Takahashi, H., Yanagida, T., Kasama, D., Itoh, T.,Kokubun, M., Makishima, K., et al.: “The Tem-perature Dependence of Gamma-Ray Responses ofYAG:Ce Ceramic Scintillators”, ibid, 3, 1337-1340

[23] Yanagida,T., Takahashi,H., Itoh,T., Kokubun,M.,Makishima, K., et al.: “Evaluation of Basic Prop-erties of Ce-Nd Codoping YAG (Ce) Ceramic Scin-tillators”, Proc. Radiation Detectors & Their Uses(eds. S. Sasaki, T. Shibata, T. Sanami, H. Taka-hashi, & M. Nakazawa), 19, 251-260 (2005)

[24] Inoue, H., Kunieda, H., White, N., Kelley, R., Mi-hara, T., Terada, Y., Takahashi, H., Kokubun, M.,Makishima, K., & The Suzaku Team: “SuzakuDetection of Cyclotron Line near 50 keV forA0535+26 � , Astronomer � s Telegram, #613 (2005)

[25] Yanagida, T., Ezoe, Y., Kawaharada, M.,Kokubun, M., & Makishima, K.: “Large X-rayFlares from B-type Stars, HD 261902 and HD47777, in NGC 2264 Observed with Chandra”,Proc, Int’l Conf. on Active OB stars (eds. S. Stefl,S. Owocki, & A. Okazaki), in press (2006)

[26] Yanagida, T., Ezoe, Y., Kawaharada, M.,Kokubun, M., & Makishima, K.: “Chandra Ob-servations of OB stars in the Cygnus OB2 Associ-ation”, ibid.

[27] Takahashi, H., & Makishima, K.: “X-ray Studyof Mass-Accretion Flows onto Weakly-MagnetizedNeutron Stars”, Proc. Conference “The X-ray Uni-verse 2005”, p.304 (2006)

[28] Miyawaki, R., Sugiho, M., Kubota, A., Mak-ishima, K., Namiki, M., Tanaka, T., & Tsunoda,N.: “Spectral Study of Ultra-Luminous CompactX-ray Sources with XMM-Newton and Chandra”,ibid., p.433

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6 C D � � E F H 8 : ; L M N O P Q R S (1) = � � �

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[32] Kawaharada, Madoka “X-ray Study on the Spa-tial Distribution of Heavy Elements in Hot Plas-mas Associated with Clusters of Galaxies”, ' © �

§ ¨ �

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[33] Murashima, Mio � “X-ray Study of Planetary Neb-ulae”, � � � � � ( � � � � � )

[34] � � � � � � � � � � � ! " # % & ( ) * + , � - � � . / � � � � �

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1 2 3 4 5

[36] Makishima, K.: “A New X-ray Window to beOpened with Astro-E2”, 6 7 � � � E ( 6 7 9 :

H � , 2005 June 2)

1 � ; 4 5

[37] Yanagida, T., Ezoe, Y., Kawaharada, M.,Kokubun, M., & Makishima, K.: “Large X-rayflares from B-type stars, HD 261902 and HD 47777,in NGC 2264 observed with Chandra”, Int’l Conf.on Active OB stars (Hokkai-Gakuen Univ., Sap-poro; 2005 Aug. 29-Sept. 2)

[38] Yanagida, T., Ezoe, Y., Kawaharada, M.,Kokubun, M., & Makishima, K.: “Chandra Ob-servations of OB Stars in the Cygnus OB2 associ-ation”, ibid

[39] Takahashi, H., & Makishima, K.: “X-ray Studyof Mass-Accretion Flows onto Weakly-MagnetizedNeutron Stars”, “The X-ray Universe 2005” Con-ference (San Lorenzo del Escorial, Spain; 2005September)

[40] Miyawaki, R., Sugiho, M., Kubota, A., Mak-ishima, K., Namiki, M., Tanaka, T., & Tsunoda,N.: “Spectral Study of Ultra-Luminous CompactX-ray Sources with XMM-Newton and Chandra”,ibid.

[41] Itoh, T., Kokubun, M., Takashima, T., Yanagida,T., Hirakuri, S., Miyawaki, R., Takahashi, H.,Makishima, K., Tanaka, T., Nakazawa, K., Taka-hashi, T., Honda, T.: “R&D of a New 1-Dimensional < -Ray Position Sensor Using Scintil-lators Coupled to a Si Strip Detector”, IEEE Nucl.Sci. Symp. (Puerto Rico; 2005 Oct. 25)

[42] Yanagida, T., Ezoe, Y., Kawaharada, M.,Kokubun, M., & Makishima, K.: “X-ray Flaresfrom Young Intermediate Mass Stars in NGC2264Observed with Chandra”, Protostars and PlanetsV) (Waikoloa Village, Hawaii; 2005 Oct. 24-28)

[43] Makishima, K., Murashima, M., Kokubun, M.,Murakami, H., Hayashida, K., Matsushita, K., Ko-toku, J., Arnaud, K., & Hamaguchi, K.: “TheSuzaku PV observation of the Planetary NebulaBD+30 = 3639”, Suzaku Science Working GroupMeeting (ISAS/JAXA; 2006 Feb. 20)

[44] Kokubun, M., Ishisaki, Y., Ogasaka, Y., Anabuki,N., Porter, F., & Takahashi, T.: “Suzaku Obser-vation of the Lockman Hole”, ibid.

[45] Kokubun, M., Murashima, M., Makishima, K.,Matsushita, K., Kotoku, J., Murakami, H., etal. “Suzaku Detection of a Highly Carbon En-riched Plasma in BD +30◦3639”, IAU SymposiumNo.234: Planetary Nebulae in our Galaxy and Be-yond (Waikoloa, Hawaii; 2006 April 3-7)

( D J E F )

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� � � � 5 7 � 9 : ; Si ¡ ¢ £ > $ & ? ¤ ¥ < ( �§ ) * + , ¨ © * C (2) ª � 19aYA-9

[51] � W � � � [ \ i j � � y � � 0 � � � � D P f g �s t v w � � { [ « � ¬ | g ­ � ® W ¯ S � � ° �� y ³ [ ´ µ m > ¶ · ¹ ? º � » � � � YAG:Ce � 5¼ � ½ : , * C ª � 19aYA-10

[52] Hirakuri, S., Kokubun, M., Itoh, T., Yanagida,T., Miyawaki, R., Makishima, K., Kubo, S., & .Honda, T.: “R&D of a Low Background CosmicHard X-ray Imager with a Position Sensitive PMTand an Active Coded Mask”, KD.00011

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· P � � ( � � H � Q 2006 � 3±

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( § � « � Q ¯ ° � Q ¬ ­ � )

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� � I � � ¼ O (i � » � º » s 2005 ¾ 9 ¿ 3 À )

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{ � s 2005 ¾ 11 ¿ 6 À )

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( Cº s 2006 ¾ 2 ¿ 10 À )

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