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(1)

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(3)    525 Davey Lab, University Park, PA 16802, USA e-mail: [email protected]. 

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(32) SDSS !uF  ` CIV d e &  ¯ G 3 b * P 7) MiniBAL

(33) R HV°!uF ` HS1603± 3820  CIV de&8) NAL

(34) ²)*HV° !uF ` HS1700±6416  NV de&9) ³´I§ `2Jv BR &4 µ ,0W v. .y/ >0523 z{U ,|}>  de&~!

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(43) 2000 DK¸L¹º »M0G. N 100 w. N7¼. 6).  341.

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(52) 23234) (1). xy) +

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(54)  56789#. o#"‹#2!).  (H I) :;<=!+"*. Œ  )* NAL BAL  .IJ. >2? 56789>#. 0KLq(.#

(55) !) fMKL . C IV @ A!#BCD+". NAL NŽ#

(56) :;S ‘.  (2) QSO E!"H#H#. +*0#+") ’:;Oq“|9῍2

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(60) !) (fK. ^9_0SG . `/

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(65) !) ( !c.:;1 QSO. NžjQ

(66) R+") :;" QSO \q. "2de

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(77) R:;. " b¡c

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(79) D. Z@2

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(81) D+"qr 2!)  +&'. 0š:0Z@ ¤(AB

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(87) -./23)  !"$*+'K) 012 34 7)$) LMῌ7

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(91) ]  1 j l m NAL n-Z'

(92) ῌoX :p  qr s< 'C4tGcuvw N O m#kxy--9

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(95)  '£ --01234 $$/' C IV s f” 2 

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(98). '‚ƒ„ †‡ˆ# 1,000 km/s ‰$Š) ~.[%$€' ‹ 100 66

(99) .  XŒ`uv}

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(102)  . uv4tGc“ 100 šdj.   2  .

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(106)  QSO   yˆ!ž'm NAL Ÿ5$" . ῌ7 [\' QSO 4tGc ¥¦%§$¨/.676CFGH3

(107) ῌ8 ‘O•T–4tGc t©1/(aªne) j

(108)  ne «! a ‘OŠC

(109) 9l C IV 6  C III ¬‘ONO a  5.3ª10­12 cm3 s­1 -Z®$

(110) ῌ9 .7) XŒ™-=>'V- (? 4tGcCFGH3š¯w° - #24) =>#uv$± kxi -

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(131) /0 m Jn. 03#. ./)+

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(135) 6:  150 }K. ῌ78Œ ExdQeFl#. L!~῍

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(143) ’a)b'MNdQe@H0c/'3# ῍13 'r 0;n.a(

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(145) ®bKL! f6gŸ36: h© ¯HKL!)ij/H QSO KL!~°±<6)# 15 ῍ <:

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(164) 8¶ +·) 5;5; /0¸23 3;(5 QSO )9¹%ºZ+» 

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(167) . kl ;$ 3fg$%m&. . n 

(168) .  !" 1#$ %&'. 4 ` op$q'() 104. (  mini-BAL ) !*# +,-./. cmr3 s t     V u    v % ) 6 w x. 012 34(5. yz{|s}~ ;$ €  op. HS160363820$ 7. $.  QSO  89. )‚ƒ„. 4

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(173) +NŽH

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(180) .  [fg !$ " <. /f :5S+†¦%D `%. 346. 4 ` ¥ . ¼:. 2007  7 ¼.

(181) [7. [6. [ 5 ‰ (1) Š&. qr‹ a: ŒŽNOPQ& $% . MNOPQRSTUVU ‘1. ’1 . x

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(184)  œtu~+() # 8 . 3; >už#$%

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(187) „ªn8%«. ¬­® ¯°UŽ?@ABaŸ 8 +`€ ©

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(191) ῌ W#ktu.  16  QSO . (). ! ". #$% & HS1603'3820 ()*. . # +MNOPQRSTUVU.  [ 6" 8. (Z#+vw x

(192) . + QSO ,-. 1 /0123. 2yz{ +`. 4567

(193)  89:. QSO ;$<=. . x

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(195) 2a +` 347.

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(199) 01234 ) *. !wN&'  xtJ. +5 6  789: !. .. yO BH z QJ {|!}P B. $;, . AD. QR~STU VW. 36). /0,. %&'40) C34€ 2+789:.  3! "#$% ! QSO ) .  X;Y<.D =RSTU DE QJ. <& "#$% . 0C ῍18 X;Y<.D 67P012Q. +,=>?='('@)$2+' A"#. X\DQJ QSO HI.D 67. $%! B .*+  QSO . P0&; ''~S‚ +,C. ) &C 3!.  stJ TUƒYZ+'37), 38) '. 

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(201) 5. 44) +•  Cc/DE /2. 2+ ]>.+3!῍17^ Z+%_,. 1 d km/s !eM @/ 67. `a' bc X 

(202)  789:. P‚ QJ X;Y<–—f˜g. d!e12+'. $E  h/ [†‡I4/ˆ‰‚. "#/* QJ. 37), 38). 6. 

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(206) @8. 3 NAL 45 12;<=6789:0 Elvis47)  BAL + sEFGHI 

(207) J NAL Jtu12 Ganguly 46) BAL + D,J NAL N =;·0 ‹UŒ !'(ˆ~

(208) ¸¹& |>&0. 

(209)  BAL . F>>& ~

(210) #$%&.  . '(|+>&0 >Uˆ~PQ ‹UŒŽ. !" #$%&'()*+  .  ?BAL PQ†A QSO ‘’Z[. ,-./&0 12. &tu l

(211) Fmlo “. 46). 3 NAL 45 6789:. 

(212) ”•&|+>&0 BAL N=. ;<=>& ?@ 8A0 BC 3 NAL. U QSO lo –

(213) F X  —2. !+. F\˜=. .  BAL + DEFGHI

(214) JKLM. 10 cm. N=O  0 PQ 3 NAL. 12 ‹UŒ™š QSO 3 NAL. R

(215) ST&UC . ›

(216) PQ –

(217) F 1022 cm—2 Fœ. VWX YZ[& \+>. \

(218) ž2>&50)0   6C. &0 ]^_`a37)

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(224) ª «  o Xp. |3 NAL

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(259) (&Y? # A ;<2PSQD7S 7(&. |# 2004, TH&# 97, 563 |# ¼. ‚# 2000, TH&# 93, 712. 7) Reichard T. A., et al., 2003, AJ 125, 1711 8) Misawa T., et al., 2007, ApJ 660, 152 9) Misawa T., et al., 2007, ApJS, in press (astro-ph/ 0702101). S?@1 ‘R7("$1 ’L. 10) Hamann F., Sabra B., 2004, ASPC 311, 203. <“%# A 2P"@*[\

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(263) of galaxies. A variety of absorption features (known collectively as quasar absorption lines) are detected in the rest-frame UV spectra of these objects. While absorption lines that have very broad widths originate in gas that is probably physically related to the quasars, narrow absorption lines (NALs) were thought to arise in galaxies and/or the inter-galactic medium between the quasars and us. Using high-resolution spectra of quasars, we have found that a substantial fraction of NALs arise in gas in the immediate vicinity of the quasars. We also found a dramatically variable, moderately-broad absorption line in the spectrum of the quasar HS 1603 3820. We have monitored the variability of this line in a campaign with Subaru telescope. We compared these observational results to models for outflows from the quasars, specifically, models for accretion disk winds and evaporating obscuring tori. It is quite important to determine the mechanism of outflow because of its cosmological implications. The outflow could expel angular momentum from the accretion disk and enable quasars to accrete and shine. In addition, the outflow may also regulate star formation in the early stages of the assembly of the host galaxy and enrich the interstellar and intergalactic medium with metals.. 351.

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