en,JS,et al,2001,A
人民币发行冠号
人民币发行冠号第五套人民币99版5元券至100元券，自第五套人民币公布发行后至2005年初第五套人民币05版券公布发行，其投放时间为七年左右。
随着05版券的投放，99版券已基本投放完毕。
至今，本会会员已收集到第五套人民币99版5元券至100元券投放冠号实物910种，现将第五套人民币99版5元券至100元券收集到的冠号实物列表如下，如有藏友收集到新的冠号请予以补充，以完善资料库数据。
99版5元券（107种）第一大组AG AH AI AJBA BB BC BD BE BF BG BH BI BJCA CB CC CD CE CF CG CH CI CJDA DB DC DD DE DF DG DH DI DJEA EB EC ED EE EF EG EH EI EJFA FB FC FD FE FF FG FH FI FJGA GB GD GE GF GG GH GI GJHA HB HC HD HE HF HG HH HI HJIA IB IC ID IE IF IG IH II IJJA JB JC JD JE JF JG第一大组投放有90种冠号，其中使用AG、AH、AI、AJ4个冠号作为补票冠号。
第二大组PA PB PC PD PE PF PGUH UJZA ZB ZC ZD ZE ZF ZG ZH第一大组投放有17种冠号，其中使用UH、UJ2个冠号作为补票冠号。
99版10元券（201种）第一大组AB AC AD AE AH AI AJBA BB BC BD BE BF BG BH BI BJCA CB CC CD CE CF CG CH CI CJDA DB DC DD DE DF DG DH DI DJEA EB EC ED EE EF EG EH EI EJFA FB FC FD FE FF FG FH FI FJGA GB GC GD GE GF GG GH GI GJHA HB HC HD HE HF HG HH HI HJIA IB IC IE IF IG IH II IJJA JB JC JD JE JF JG JH JI JJ第一大组投放有96种冠号，其中使用AH、AI、AJ3个冠号作为补票冠号。
欧州铝合金标准
Chemische Zusammensetzung der Gußlegierungen1) "Andere Beimengungen" enthalten nicht die Elemente, die zur Kornfeinung oder Veredlung der Schmelze dienen, wie Na, Sr, Sb und P.Auch andere Legierungen aus der DIN EN 1706, nicht mehr genormte Legierungen und Sonderlegierungen können wir für Sie vergießen. Beispiele hierfür sind:Al Si5Mg im Sandguss (nicht mehr genormt)Al Zn10Si8Mg im Sand- und Druckguss (nicht genormt)Magsimal-59 (Sonderlegierung)Silafont-36 (Sonderlegierung)Anmerkung:Getrennt gegossene Probestäbe haben eine wertvolle Funktion zur Überprüfung der Qualität und Schmelze. Jedoch können die Werte, die an den Gussstücken erzielt werden von den in den Tabellen aufgeführten Mindestwerten abweichen, aufgrund von Veränderungen im Gefüge, die durch unterschiedliche Querschnittsdicke und Fehlerfreiheit entstehen. Bei den Streckgrenzen und der Zugfestigkeit dürfen die an den Gussstücken erzielen Werten über den in den Tabellen festgelegten Werten oder darunter liegen, aber nicht unter 70 % der festgelegten Werte. Bei der Dehnung dürfen die an den Gussstücken erzielten Werte über den in den Tabellen festgelegten Werten oder an bestimmten Punkten bis zu 50 % unter diesen Werten liegenMechanische Eigenschaften von Sandgußlegierungenfür getrennt gegossene ProbestäbeMechanische Eigenschaften von Kokillengußlegierungenfür getrennt gegossene ProbestäbeMechanische Eigenschaften für Druckgusslegierungennur zur InformationMindestwerte die von getrennt gegossenen Probestäben mit einem Querschnitt von 20,0mm² und einer Mindestdicke von 2,0mm erwartet werden dürfen.Die Werte die an Proben von aus Gussstücken entnommenen Probestücken ermittelt werden, können von den in den Tabellen festgelegten Mindestwerten abweichen, da sich aufgrund unterschiedlicher Gefüge und eine unterschiedliche Gussstückqualität (Fehlerfreiheit) ergeben können.Die mechanischen Eigenschaften von Druckgussstücken, die an aus getrennt gegossenen Probestücken hergestellten Proben ermittelt werden, haben eine starke Abhängigkeit von den Druckgießparametern. Die in der Tabelle angegebenen Eigenschaften sind deshalb nur Anhaltswerte.Chemische Zusammensetzung von Magnesiumlegierungen für GussstückeAnmerkung 1: Die in dieser Tabelle angegebenen Werte sind nur Anhaltswerte.Anmerkung 2: Die angegebenen Werte gelten für getrennt gegossene Proben mit einer Querschnittsfläche von 20 mm³und einer Mindestwanddicke von 2 mm.Anmerkung 3: N/mm² entspricht 1 MpaMechanische Eigenschaften von Druckguss-Magnesiumlegierungenfür getrennt gegossene Probestäbe。
四版人民币冠号大全
四版人民冠号大全一、一角8001已见发行514种冠号（其中补号29种）第一大组（90种JY为样票）AP、AQ、AR、AS、AT、——AX、AY、AZ BP、BQ、BR、BS、BT、BU、BW、BX、BY、BZCP、CQ、CR、CS、CT、CU、CW、CX、CY、CZ DP、DQ、DR、DS、DT、DU、DW、DX、——EP、EQ、ER、ES、ET、EU、EW、EX、EY、EZ ———FS、FT、FU、FW、FX、FY、FZ GP、GQ、GR、GS、GT、GU、GW、GX、GY、GZ HP、HQ、HR、HS、HT、HU、— HX、HY、HZIP、IQ、IR、IS、IT、IU、IW、IX、IY、IZ JP、JQ、JR、— JT、JU、JW、JX — JZ其中补号5种JT、JU、JW、JX、JZ第二大组（99种）PA、PB、PC、PD、PE、PF、PG、PH、PI、PJ QA、QB、QC、QD、QE、QF、QG、QH、QI、QJRA、RB、RC、RD、RE、RF、RG、RH、RI、RJ SA、SB、SC、SD、SE、SF、SG、SH、SI、SJTA、TB — TD、TE、TF、TG、TH、TI、TJ UA、UB、UC、UD、UE、UF、UG、UH、UI、UJWA、WB、WC、WD、WE、WF、WG、WH、WI、WJ XA、XB、XC、XD、XE、XF、XG、XH、XI、XJYA、YB、YC、YD、YE、YF、YG、YH、YI、YJ ZA、ZB、ZC、ZD、ZE、ZF、ZG、ZH、ZI、ZJ其中补号3种ZH ZI ZJ第三大组（50种）PK、PL、PM、PN、PO QK、QL、QM、QN、QORK、RL、RM、RN、RO SK、SL、SM、SN、SOTK、TL、TM、TN、TO UK、UL、UM、UN、UOWK、WL、WM、WN、WO XK、XL、XM、XN、XOYK、YL、YM、YN、YO ZK、ZL、ZM、ZN、ZO其中补号3种ZM ZN ZO第四大组（50种）其中补号2种JN JOAK、AL、AM、AN、AO BK、BL、BM、BN、BOCK、CL、CM、CN、CO DK、DL、DM、DN、DOEK、EL、EM、EN、EO FK、FL、FM、FN、FOGK、GL、GM、GN、GO HK、HL、HM、HN、HOIK、IL、IM、IN、IO JK、JL、JM、JN、JO第五大组（50种）其中补号2种NY NZKP、KQ、KR、KS、KT、KU、KW、KX、KY、KZ LP、LQ、LR、LS、LT、LU、LW、LX、LY、LZMP、MQ、MR、MS、MT、MU、MW、MX、MY、MZ NP、NQ、NR、NS、NT、NU、NW、NX、NY、NZOP、OQ、OR、OS、OT、OU、OW、OX、OY、OZ第六大组（95种）其中补号7种JA ** JC JG JH JI JJAA、AB、AC、AD、AE、AF、AG、AH、AI、AJ BA、BB、BC、BD、BE、BF、BG、BH、BI —CA、CB、CC、CD、CE、CF、CG、CH、CI、CJ DA — DC、DD、DE、DF、DG、DH、DI、DJEA、EB、EC、ED —— EG、EH、EI、EJ FA、FB、FC、FD、FE、FF、FG、FH、FI、FJGA、GB、GC、GD、GE、GF、GG、GH、GI、GJ HA、HB、HC、HD、HE、HF、HG、HH、HI、HJIA、IB、IC、ID、IE、IF、IG、IH、II、IJ JA ** JC — JE、JF、JG、JH、JI、JJ第七大组（12种）其中补号1种NJKA、KB、KC、KD、KE、KF、KG、KH、KI、KJ —— MC ———————————————— NJ第八大组（68种）其中补号6种ZT ZU ZW ZX ZY ZZPP、PQ、PR、PS、PT、PU、PW、PX、PY、PZ QP、QQ、QR ———— QX、QY、QZ RP、RQ、RR、RS、RT、RU、RW、RX、RY、RZ SP、—— SS — SU、SW、SX、SY —TP、TQ、TR、TS、TT、TU、TW、TX、TY、TZ ? ?? ?? ?US、UUWP、WQ — WS、WT、WU、WW、WX、WY ——— XR、XZYP — YR、YS ——— YX — YZ ZP、ZQ、ZR — ZT、ZU、ZW、ZX、ZY、ZZ注：8001冠号仍在陆续发行中。
G试验GM试验
G试验检测的特点
可检测除隐球菌和接合菌外的多种真菌感染 在浅部真菌感染中，1,3-β-D-葡聚糖未被释放出来， 故其在体液中的量不增高。因此可区分定植和感染。 对于念珠菌血症, G试验检测是首选检查方法[2] 。 检测快速，可在1小时得出检测结果。
革兰阴性菌 革兰阳性菌 真菌
患者数
年 份
Martin GS et al. N Engl J Med. 2003 Apr 17;348(16):1546-54.
少见真菌尸检检出率也有所上升
一项对三级肿瘤监护中心血液肿瘤患者的尸检结果显示
2.0%
尸 检 检 出 率 足放线菌 镰刀菌 1.4％ 0.9％ 0.4％
侵袭性曲霉病(Invasive Aspergillosis, IA
)
侵袭性曲霉病是一种严重的机会性感染性疾病。是指致病性曲霉 菌侵犯皮下组织、黏膜、肌肉和内脏器官等所引起的真菌感染性疾
病，危害性较大。
曲霉是条件致病菌，当机体免疫力下降时，如：粒细胞缺乏或HIV
感染，可侵犯肺、甚至全身各系统；呼吸系统曲霉病主要有三种，
传统诊断方法
培养
问题
血培养作用有限，某些播散性感染常常为假阳性 全身使用抗真菌治疗或其它原因易导致假阴性 非无菌部位标本阳性结果，难以判定是真菌定植或感染。 需侵入性手段获取标本 全身使用抗真菌治疗或其它原因易导致假阴性 其它某些真菌或细菌感染也有可能出现相似征象 在免疫正常宿主相关研究较少 目前方法尚未标准化，尚在研究阶段
以念珠菌最为常见
呼吸系统
常见病原体为 念珠菌和曲霉菌
侵袭性 真菌感染
其它部位
骨关节、心血管系统等 以念珠菌最为常见
四版冠号大全
四版冠号大全(2010-10-26 19:28:04)转载分类：纸钞文库标签：四版冠号大全杂谈8001已见发行514种冠号（其中补号29种）第一大组（90种JY为样票）其中补号5种JT JU JW JX JZAP AQ AR AS AT —— AX AY AZBP BQ BR BS BT BU BW BX BY BZCP CQ CR CS CT CU CW CX CY CZDP DQ DR DS DT DU DW DX ——EP EQ ER ES ET EU EW EX EY EZ ——— FS FT FU FW FX FY FZGP GQ GR GS GT GU GW GX GY GZHP HQ HR HS HT HU — HX HY HZIP IQ IR IS IT IU IW IX IY IZJP JQ JR — JT JU JW JX — JZ第二大组（99种）其中补号3种ZH ZI ZJPA PB PC PD PE PF PG PH PI PJQA QB QC QD QE QF QG QH QI QJRA RB RC RD RE RF RG RH RI RJSA SB SC SD SE SF SG SH SI SJTA TB — TD TE TF TG TH TI TJUA UB UC UD UE UF UG UH UI UJWA WB WC WD WE WF WG WH WI WJXA XB XC XD XE XF XG XH XI XJYA YB YC YD YE YF YG YH YI YJZA ZB ZC ZD ZE ZF ZG ZH ZI ZJ第三大组（50种）其中补号3种ZM ZN ZOPK PL PM PN POQK QL QM QN QORK RL RM RN ROSK SL SM SN SOTK TL TM TN TOUK UL UM UN UOWK WL WM WN WOXK XL XM XN XOYK YL YM YN YOZK ZL ZM ZN ZO第四大组（50种）其中补号2种JN JOAK AL AM AN AOBK BL BM BN BOCK CL CM CN CODK DL DM DN DOEK EL EM EN EOFK FL FM FN FOGK GL GM GN GOHK HL HM HN HOIK IL IM IN IOJK JL JM JN JO第五大组（50种）其中补号2种NY NZKP KQ KR KS KT KU KW KX KY KZLP LQ LR LS LT LU LW LX L Y LZMP MQ MR MS MT MU MW MX MY MZ NP NQ NR NS NT NU NW NX NY NZ OP OQ OR OS OT OU OW OX OY OZ第六大组（95种）其中补号7种JA ** JC JG JH JI JJAA AB AC AD AE AF AG AH AI AJBA BB BC BD BE BF BG BH BI —CA CB CC CD CE CF CG CH CI CJDA — DC DD DE DF DG DH DI DJEA EB EC ED —— EG EH EI EJFA FB FC FD FE FF FG FH FI FJGA GB GC GD GE GF GG GH GI GJHA HB HC HD HE HF HG HH HI HJIA IB IC ID IE IF IG IH II IJJA ** JC — JE JF JG JH JI JJ第七大组（12种）其中补号1种NJKA KB KC KD KE KF KG KH KI KJ —— MC ———————————————— NJ第八大组（68种）其中补号6种ZT ZU ZW ZX ZY ZZPP PQ PR PS PT PU PW PX PY PZQP QQ QR ———— QX QY QZRP RQ RR RS RT RU RW RX RY RZSP —— SS — SU SW SX SY —TP TQ TR TS TT TU TW TX TY TZUS UUWP WQ — WS WT WU WW WX WY ——— XR XZYP — YR YS ——— YX — YZZP ZQ ZR — ZT ZU ZW ZX ZY ZZ注：8001冠号仍在陆续发行中。
铝合金国外相似牌号
铝合金国外相似牌号1050A（L3）国外相似牌号国际标准：Al99.5（ISO）日本：A1050A（JIS）欧洲标准：EN AW 1050A（EN）法国：A5（NF）德国： Al99.5/3.0255（DIN）英国：1B（BS）美国：1050A（AA）1060（L2）国外相似牌号国际标准：Al99.6 (ISO) 日本：Al060（JIS）欧洲标准：EN AW 1060（EN）美国：1060（AA）1100（L5-1）国外相似牌号国际标准：Al99.0(ISO) 日本：Al100/AIN00（JIS)）欧洲标准：EN AW 1100（EN）法国：A45 加拿大：99 0C（CSA）美国：1100（AA）1200（L5）国外相似牌号国际标准：Al99.0（ISO）日本：Al200（JIS）俄罗斯：A0（ГOCT）欧洲标准：EN AW 1200（EN）法国：A4德国：Al99/3.0205（DIN）英国：1C（BS）意大利：Al99(UNI) 美国：1200（AA）2系列铝合金2017A国外相似牌号国际标准：Al Cu4MgSi（A）（ISO）日本：A2017A（JIS）俄罗斯：1120（ГOCT）欧洲标准：EN AW 20 17A（EN）法国：A-U4G（NF）德国：Al CuMg1/3.1325（DIN）英国：DTD150A（BS）美国：2017A（AA）2A01（LY1）国外相似牌号国际标准：~Al Cu2.5Mg（ISO）日本：~A2117（JIS）俄罗斯：Д18П（ГOCT）美国：~2117（AA）2A02（LY2）国外相似牌号俄罗斯：BД17（ГOCT）2A04（LY4）国外相似牌号俄罗斯：Д19П（ГOCT）2A06（LY6）国外相似牌号俄罗斯：Д19（ГOCT）2A10（LY10）俄罗斯：B65（ГOCT）2A11（LY11）国外相似牌号国际标准：Al Cu4MgSi（ISO）日本：A2017（JIS）俄罗斯：Д1（ГOCT）英国：DTD150A（BS）美国：20 17（AA）2A12（LY12）国外相似牌号国际标准：Al Cu4Mg1（ISO）日本：2024（JIS）俄罗斯：Д16/1160（ГOCT）欧洲标准：EN AW 2024（E N）法国：A-U4G1（NF）德国：Al Cu Si Mn/3.1255（DIN）英国：DTD5090（BS）加拿大：CG42（CSA）美国：2024（AA）2B11（LY8）国外相似牌号国际标准：Al Cu4Mg1（ISO）日本：A2017（JIS）俄罗斯：Д111/1111（ГOCT）欧洲标准：EN AW 2017（EN）法国：A-U4G（NF）德国：Al Cu Mg1/3.1325（DIN）美国：2017（AA）2B12（LY9）国外相似牌号国际标准：Al Cu4Mg1（ISO）日本：~A2024（JIS）俄罗斯：Д16П1161（ГOCT）欧洲标准：EN AW ~20 24（EN）法国：A-U4G1（NF）德国：~Al CuMn2/3.1355（DIN）美国：~2024（AA）2A14（LD10）国际标准：Al Cu Si Mg（ISO）日本：A2014（JIS）俄罗斯：AMr4（ГOCT）欧洲标准：EN AW 2014（EN）法国：A-U4SG（NF）德国：Al Cu Si Mn/3.1255（DIN）英国：H15/~L87（BS）意大利：9002/3（UNI）加拿大：CS41M（CSA）美国：2014（AA）2A16（LY16）国外相似牌号国际标准：Al Cu6Mn（ISO）日本：A2219（JIS）俄罗斯：Д20/1201（ГOCT）欧洲标准：EN AW 2219（E N）法国：A-U6MT（NF）英国：DTD5004（BS）意大利：9002/7（UNI）美国：2219（AA）2B16（LY16-1）国外相似牌号国际标准：Al Cu6Mn（ISO）日本：A2219（JIS）俄罗斯：Д20/1201（ГOCT）欧洲标准：EN AW 2219（E N）法国：A-U6MT（NF）英国：DTD5004（BS）意大利：9002/7（UNI）美国：2219（AA）2A17（LY17）国外相似牌号俄罗斯：Д21（ГOCT）日本：A2219（JIS）美国：2219（AA）2A50（LD5）俄罗斯：AK6（ГOCT）2B50（LD6）国外相似牌号俄罗斯：AK6-1（ГOCT）2A70（LD7）国外相似牌号日本：A2618（JIS）俄罗斯：AK4-1（ГOCT）法国：A-U2GN（NF）英国：RR58（BS）美国：2618（AA）2124国外相似牌号俄罗斯：Д16Ч（ГOCT）欧洲标准：EN AW 2124（EN）美国：2124（AA）2214国外相似牌号俄罗斯：AK8（ГOCT）欧洲标准：EN AW 2214（EN）英国：L87（BS）美国：2214（AA）2618A国外相似牌号欧洲标准：EN AW 2618A（EN）法国：A-U2GN（NF）英国：H16（BS）意大利：9002/6（UNI）美国：26 18A（AA）3系列铝合金3A21(LF21)国外相似牌号国际标准：Al Mn1 Cu（ISO）日本：A3003（JIS）俄罗斯：1400/AMЦ 欧洲标准：EN AW3003（EN）法国：A-M1（NF）德国：AlMnCu/3.0517(DIN) 英国：L61（BS）意大利：9003/1（UNI）加拿大：MC10M（CSA）美国：3003（AA）4系列铝合金4A11（LD11）国外相似牌号日本：A4032（JIS）俄罗斯：AK9（ГOCT）欧洲标准：EN AW 4032（EN）法国：A-S12UGN/A-S12UN（N F）意大利：9004/1（UNI）加拿大：SG121（CSA）美国：4032（AA）4A01（LT1）国外相似牌号国际标准：AlSi5（ISO）日本：A4043（JIS）俄罗斯：AK（ГOCT）法国：A-S5（NF）英国：N21（BS）加拿大：S5（CSA）美国：4043（AA）国际标准：Bal92.5Si（ISO）日本：BA4343（JIS）欧洲标准：EN AW 4343（EN）德国：L-AlSi7.5（DIN）美国：4343（AA）5系列铝合金5A02（LF2）国外相似牌号国际标准：Al Mg2.5（ISO）日本：A5052（JIS）俄罗斯：AMr2（ГOCT）欧洲标准：EN AW 5052（EN）法国：A-G2.5C（NF）德国：Al Mn2.5/3.3523（DIN）英国：L56/~N4（BS）意大利：9005/2（UNI）加拿大：GR20（CSA）美国：5052（AA）5A03（LF3）国外相似牌号国际标准：Al Mg3.5（ISO）日本：A5154（JIS）俄罗斯：AMr3（ГOCT）法国：A-G3C（NF）德国：SG-Al Mg3/3.3536（DIN）英国：近似N5（BS）加拿大：近似GR40（CSA）美国：5154（AA）5A05（LF5）国外相似牌号国际标准：Al Mg5Mn1/近似Al MgMn0.4（ISO）俄罗斯：AMr5（ГOCT）欧洲标准：EN AW 5019（EN）英国：近似N61（BS）美国：5456/5056（AA）5B05（LF10）国外相似牌号国际标准：Al Mg5Cr（ISO）日本：A5056（JIS）俄罗斯：AMr5（ГOCT）德国：Al Mg5/3.3555（DIN）英国：2L58/~N6（BS）加拿大：GM50R（CSA）美国：5056（AA）5A06（LF6）国外相似牌号俄罗斯：AMr6（ГOCT）5056（LF5-1）国外相似牌号国际标准：Al Mg5Cr（ISO）日本：A5056（JIS）俄罗斯：AMr5（ГOCT）德国：~AlMg5/3.3555（DIN）英国：2L58/~N6（BS）加拿大：GM50R（CSA）美国：5056（AA）5083（LF4）国外相似牌号国际标准：Al Mg4.5Mn0.7（ISO）日本：A5083（JIS）俄罗斯：AMr4（ГOCT）欧洲标准：EN AW 5083（E N）法国：A-G4.5MC（NF）德国：Al Mg4.5Mn/3.3347（DIN）A英国：N8（BS）意大利：9005/5（UNI）加拿大：GM41（CSA）美国：5083（AA）6系列铝合金国外相似牌号日本：A6165（JIS）俄罗斯：AB（ГOCT）美国：6165（AA）6061（LD30）国外相似牌号国际标准：Al Mg1 Si Cu（ISO）日本：A6061（JIS）俄罗斯：1340/AД33（ГOCT）欧洲标准：EN AW 60 61（EN）法国：A-GSUC（NF）德国：AlMg1CuSi/3.3214（DIN）英国：H20（BS）意大利：9006/2（UNI）加拿大：GS11N（CSA）美国：6061（AA）6063（LD31）国外相似牌号国际标准：Al Mg0.7Si（ISO）日本：A6063（JIS）俄罗斯：AД31（ГOCT）欧洲标准：EN AW 6063（EN）法国：A-GS（NF）英国：H19（BS）意大利：9006/5（UNI）加拿大：GS10（CSA）美国：6063（AA）6063A国外相似牌号国际标准：Al Mg0.7Si（A）（ISO）欧洲标准：EN AW 6063A（EN）德国：AlMgSi0.5（DIN）英国：DTD 372B（BS）美国：6063A（AA）7系列铝合金7A01（LB1）国外相似牌号日本：A7072（JIS）俄罗斯：AC1（ГOCT）欧洲标准：EN AW 7072（EN）德国：AlZn1（DIN）加拿大：Z 1（CSA）美国：7072（AA）7A04（LC4）国外相似牌号国际标准：Al Zn6MgCu（ISO）俄罗斯：B95（ГOCT）欧洲标准：：EN AW 7010（EN）德国：AlZnMgCu1. 5（DIN）意大利：9007/4（UNI）美国：7010（AA）7A09（LC9）国外相似牌号国际标准：Al Zn5MgCu（ISO）日本：A7075（JIS）俄罗斯：B95（ГOCT）欧洲标准：EN AW 7075（EN）法国：A-Z5GU（NF）德国：AlZnMgCu1.5/3.4365（DIN）英国：L96（BS）意大利：9007/2（UNI）加拿大：ZG62（CSA）美国：7075（AA）7005（NC5）国外相似牌号国际标准：Al Zn4.5Mg1.5Mn（ISO）日本：A7NO1（JIS）欧洲标准：EN AW 7005（EN）美国：7005（A A）7050国外相似牌号国际标准：Al Zn6Cu Mg Zr（ISO）日本：A7050（JIS）欧洲标准：EN AW 7050（EN）美国：7050（AA） 7475国外相似牌号国际标准：Al Zn5.5 Mg Cu （A）（ISO）俄罗斯：B95OЧ（ГOCT）欧洲标准：EN AW 7475（EN）美国：7475（AA）产品属性/技术参数：种类变形铝合金产地进口牌号LT98 铝含量余量（%）杂质含量标准（%）粒度标准（目）。
前列腺癌争议话题讨论
17
改善性功能
Calais et al. reported a phase III study on 636 patients with T3–4M0 and M1 disease, showing an improvement in sexual activity on the intermittent arm.
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68例患者 前瞻性随机化期临床研究
—3年疾病进展率间歇组显著低于持续组 (P < 0.01).
6.7 (4.6)%
37.5 (10.8)%
—在20例明显骨转移患者两组3年疾病进展率上无差异 (P=0.3).
Waltregny D, Boca P, Nicolas H et al. Urol 2002; 168 (Supp1l)2: A701
➢ 内分泌治疗可以改善生存质量 ➢ 内分泌治疗是否可以延长生存期？ ➢ 内分泌治疗有不良反应
➢ 内分泌治疗应早期开始还是延缓进行？ ➢ 动物试验研究发现
➢ 中等程度地降低激素水平可以减慢激素依赖性肿瘤 细胞的生长并延缓其转变为自主细胞（autonomy）
➢ 去势可以加速细胞向激素非依赖性自主细胞的转化
5
间歇性内分泌治疗的目的
➢ 延长内分泌治疗的时间,进而达到延长生 存期的目的
➢ 减少内分泌治疗的副作用 ➢ 减少治疗费用
6
间歇性内分泌治疗的理论基础
➢ 克隆选择学说 ➢ 适应学说 ➢ 突变学说 ➢ 多肽生长因子及其受体的作用
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8延长Βιβλιοθήκη 分泌治疗时间？9延长内分泌治疗时间？
Akakura K, et al. Cancer 1993,21: 217082.
冠号大全
第四套人民币冠号大全2010-07-13 02:19第四套人民币冠号发行一览表(80版壹佰元券)（发行有16种冠号）第一大组投放有16种冠号，其中使用JZ个冠号作为补票冠号。
（JY为票样）第四套人民币冠号发行一览表(90版壹佰元券)（发行有204种冠号）第一大组投放有82种冠号，其中使用JS、JT、JU、JX4个冠号作为补票冠号。
第三大组投放有28种冠号，其中使用ZM、ZN、ZO3个冠号作为补票冠号。
（JW为票样）第四套人民币冠号发行一览表(80版伍拾元券)（发行有24种冠号）8050元券第一大组（24种冠号）第一大组投放有24种冠号，其中使用JZ个冠号作为补票冠号。
（JY为票样）第四套人民币冠号发行一览表(90版伍拾元券)（发行有169种冠号）9050元券第二大组（95种冠号）第二大组投放有95种冠号，其中使用ZH、ZI、ZJ3个冠号作为补票冠号。
（JW为票样）第四套人民币冠号发行一览表(80版拾元券)（发行有401种冠号）8010元券第一大组（93种冠号）8010元券第二大组（94种冠号）8010元券第三大组（49种冠号）8010元券第四大组（49种冠号）8010元券第五大组（50种冠号）8010元券第六大组（49种冠号）8010元券第七大组（17种冠号）第四套人民币冠号发行一览表(80版伍元券)（发行有264种冠号）805元券第一大组（99种冠号）805元券第二大组（100种冠号）805元券第三大组（46种冠号）805元券第四大组（19种冠号）第四大组投放有19种冠号，其中使用JN、JO2个冠号作为补票冠号（JY为票样）。
第四套人民币冠号发行一览表（80版贰元券）（发行有54种冠号）802元券第一大组（54种）第一大组投放有54种冠号，其中使用JZ1个冠号作为补票冠号（JY为票样）。
第四套人民币冠号发行一览表（90版贰元券）（发行有133种冠号）902元券第一大组（44种）第一大组投放有44种冠号，其中使用JU、JW、JX3个冠号作为补票冠号。
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T HE A STRONOMICAL J OURNAL ,122:1718È1735,2001October(2001.The American Astronomical Society.All rights reserved.Printed in U.S.A.MULTICOLOR PHOTOMETRY OF THE GALAXIES IN THE CENTRAL REGION OF ABELL 2634Q IRONG Y UAN ,1,2,3X U Z HOU ,1J IANSHENG C HEN ,1Z HAOJI J IANG ,1J UN M A ,1H ONG W U ,1S UIJIAN X UE ,1AND J IN Z HU 1Received 2001April 9;accepted 2001July 11ABSTRACTAn optical photometric observation with the Beijing-Arizona-Taipei-Connecticut multicolor system is carried out for the central region of the nearby cluster of galaxies Abell 2634.From the 2K ]2K CCD images with 14Ðlters,which cover a range of wavelength from 3600to 100005572sources are A ,detected down to V D 20mag in a Ðeld of 56@]56@centered on this regular cluster of galaxies.As a result,we achieved the spectral energy distributions (SEDs)of all sources detected.There are 178pre-viously known galaxies included in our observations,147of which have known radial velocities in the literature.After excluding the foreground and background galaxies,a sample of 124known members is formed for an investigation of the SED properties.The comparison of observed SEDs of the early-type member galaxies with the template SEDs demonstrates the accuracy and reliability of our photometric measurements.Based on the knowledge of SED properties of member galaxies,we performed the selec-tion of faint galaxies belonging to Abell 2634.It is well shown that the color-color diagrams are power-ful in the star-galaxy separation.As a result,359faint galaxies are selected by their color features.The technique of photometric redshift and color-magnitude correlation for the early-type galaxies are applied for these faint galaxies,and a list of 74faint member galaxies is achieved.On the basis of the newly generated sample of member galaxies,the spatial distribution and color-magnitude relation of the gal-axies in the core region of Abell 2634are discussed.There exists a tendency that the color index disper-sion of the early-type members is larger for the outer region,which might reÑect some clues about the environmental e†ect on the evolution of galaxies in a cluster.Key words:galaxies:clusters:individual (Abell 2634)Ègalaxies:distances and redshifts Ègalaxies:fundamental parameters1.INTRODUCTIONIt is widely appreciated that the observations of galaxy clusters can provide useful constraints on the theories of formation and evolution of large-scale structure,since they are the largest gravitationally bound systems in the uni-verse.A great volume of observational data has been achieved for the galaxies belonging to a cluster,particularly for the nearby clusters of galaxies.The rich cluster of gal-axies,Abell 2634,is one example.Extensive observational e†orts are being made to expand the kinematic database for Abell 2634because it has many intriguing observational features.First,its central galaxy,NGC 7720,classiÐed as a cD galaxy Ðrst by Matthews,Morgan,&Schmidt (1964)and then as a D galaxy by Dressler (1980a),was found to have a companion galaxy,namely NGC 7720A,with a pro-jected distance of 7.2kpc and a velocity di†erence ofh 75~1about 1000km s ~1.Second,a surprisingly large negative peculiar velocity for Abell 2634was derived when the fun-damental plane (FP)relation (Dressler et al.1987)was D n -p sketchily extended to estimate the distance of Abell 2634(Lucey et al.1991),which is challengable for the universality of the FP and Tully-Fisher (TF)relations.With the e†ort for several years of Lucey et al.(1997)and Scodeggio,Gio-vanelli,&Haynes (1997),larger samples of member galaxies with more accurate photometric measurements (includingÈÈÈÈÈÈÈÈÈÈÈÈÈÈÈ1National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100012,China;zhouxu =,chen =.2Department of Physics,Nanjing Normal University,NingHai Road 122,Nanjing 210097,China;qirongwy =.3Visiting Astronomer,National Optical Astronomy Observatories,Tucson,AZ 85726;under contract to China Scholarship Council;yuan =.I -band observations)are constructed.Abell 2634was found to have a negligibly small peculiar velocity with respect to the cosmic microwave background reference frame.The FP distance estimate of Abell 2634is in good agreement with that given by the TF relation.Additionally,the prototypical wide-angle tailed radio source,3C 465,is found to coincide with the central cD galaxy,NGC 7720(Gri†en 1963;Eilek et al.1984;OÏDonoghue,Owen,&Eilek 1990).A study of this cluster by Pinkney et al.(1993)suggested that the large-scale turbu-lent gas motions fueled by a cluster-subcluster merging process might be responsible for the observed bending of radio tails.To investigate issues related to the kinematics of NGC 7720,Scodeggio et al.(1995;hereafter SSGH)carried out the multiÐber spectroscopy and 21cm line observations and particularly analyzed the structure,kinematics,and morphological segregation of galaxies within the central half-degree region (HDR).There are 99member galaxies brighter than in the inner region,which ism vD 16.00¡.5called the HDR sample.The completeness of the inner region of 1deg 2reached As a result,the mor-m pgD 16.0.phological dependence of spatial and kinematic properties was found:the early-type galaxies appear to be a relaxed system,while the spiral galaxies have a much larger velocity dispersion.Studies of the luminosity function of cluster galaxies show that most intrinsically bright galaxies in clusters,are giant elliptical galaxies.Down to M B \[16,m v D 18.5in Abell 2634,the majority of apparently faint member gal-axies are still intrinsically bright.There should be many giant elliptical galaxies within the apparent magnitude range of In order to enrich our under-16.0\m v\18.5.standing of the structure and dynamics of Abell 2634,these faint member galaxies should be taken into account.1718PHOTOMETRY OF GALAXIES IN ABELL 26341719However,the spectroscopic observations are not available yet for a great number of galaxies fainter than 16.0mag in Abell 2634.The multicolor optical photometric observation therefore becomes a common alternative means for study -ing some properties of the member galaxies,such as the color-magnitude relation (Bower,Lucey,&Ellis 1992),the Butcher-Oemler e†ect (Butcher &Oemler 1978),and the morphology-density relation (Dressler 1980b).Due to a large Ðeld of view,the Schmidt Telescope (1m class),equipped with a large-format CCD,is one of most suitable facilities for obtaining photometric data for the nearby clusters of galaxies.The multicolor photometry can provide the spectral energy distributions (SEDs)of all the objects within the Ðeld of paring the integration times required for spectroscopy with a certain depth on a large telescope,the amount of observing times for multi-color photometry are much shorter and therefore more readily scheduled.The Beijing-Arizona-Taipei-Connecticut (BATC)multicolor photometric survey is designed to obtain the SED information of cluster galaxies and other types of objects (Fan et al.1996).This paper will present the multicolor optical photometry of the central region of Abell 2634using the 60/90cm Schmidt Telescope of the Beijing Astronomical Observatory (BAO),with 14BATC Ðlters covering a wide wavelength range from 3800to nearly 10000The comparison of observed SEDs for the pre-A .viously known member galaxies with the template SEDs demonstrates the accuracy and reliability of our photo-metric measurements.Our multicolor photometry contains a large quantity of bright member galaxies with sufficiently small photometric errors,which allows a veriÐcation of color-magnitude correlation,as well as a testing application of the technique of photometric redshift.After performing a reliable star-galaxy separation by the color-color diagrams,we carried out a membership selection based on the SED features of known member galaxies.The technique of photometric redshift and color-magnitude correlation have provided useful constraints on the membership selection.As a result,we cataloged the SEDs of the newly selected faint members,based on which some properties of the enlarged sample of member galaxies can be addressed.We believe that current study will not only supplement the databases of member galaxies in this well-studied cluster,but also extend the investigations on the spatial distribution and color-magnitude relation of the galaxies in the core of Abell 2634to an unprecedented depth.This paper is structured as follows:In °2,we will present our observations and data reduction,as well as the photo-metric catalogs of the objects (including the known member galaxies)in the central Ðeld of Abell 2634.The analysis of the SEDs for the known member galaxies is shown in °3.An SED selection of faint member galaxies is given in °4,and the spatial distribution and color properties of the enlarged sample of member galaxies is presented in °5.Finally,we will give a summary in °6.The cosmological parameters km s ~1Mpc ~1and have beenH 0\50q 0\0.5assumed.2.OBSERVATIONS AND DATA REDUCTION2.1.BAT C ObservationsAbell 2634is a nearby (z D 0.03)regular cluster of gal-axies,classiÐed by Abell (1958)as of richness class 1.Dress-ler (1980a)listed 132galaxies in his catalog,and the fractionof early-type galaxies (E/S0)is about 63%.In the HDRsample of SSGH,the fraction of early-type galaxies reaches D 71%.This cluster appears to be at a distance of D 9000km s ~1,projected on the main ridge of the Pisces-Perseus Supercluster (PPS;see Fig.1in Wegner,Haynes,&Giova-nelli 1993).Its companion,Abell 2666,is closely located at approximately 3¡to the east,with a heliocentric redshift of D 8154km s ~1(Struble &Rood 1999).Our multicolor optical photometry concentrates on a region of 56]56arcmin 2centered on NGC 7720.The 60/90cm f/3Schmidt Telescope of BAO,located at the Xinglong site with an altitude of 900m,was used to obtain the photometric observations.A Ford 2048]2048CCD camera was equipped at the prime focus of the telescope.The Ðeld of view was 0.95deg 2,and the spatial scale was pixel ~1.The details of the Schmidt Telescope,CCD 1A .67camera,and data acquisition system can be found elsewhere (Fan et al.1996;Yan et al.2000).We make use of the BATC Ðlter system,which includes 16intermediate-band Ðlters covering the whole optical wavelength range from D 3000to 10000The transmissions of these Ðlters can been seen A .in Figure 1of Zhou et al.(2001).Only 14Ðlters,from b to p ,were used for the observations of Abell 2634.The Ðlter number,Ðlter name,e†ective wave-length centroid,and FWHM for each Ðlter are listed in Table 1.In total,we have made more than 40hr of expo-sures and obtained 214images on the central region of Abell 2634.After a check of the image quality,173images with nearly 36hr of exposure were selected to be combined.The combined images cover an area deÐned by a right ascension range from 23h 36m 16s to 23h 40m 23s and a decli-nation range from 26¡33@30A to 27¡30@01A (for the J2000equinox).The seeing of the combined images were quite di†erent from band to band,but the typical seeing of the combined image for each Ðlter band was about 5A .Almost all nights were thought to be photometric by the observers.The standard stars were observed between air masses of 1and 2for each program Ðlter band.Normally,four to six Ðlters were selected to make Ñux calibrations during each photometric night.The standard stars were put near the CCD center and only 300]300subimages were taken for the standard stars to save readout time and disk space.The extinction coefficient and magnitude zero point obtained from standard stars were used for making the Ñux calibration on the BATC Ðeld images.The details of the observation for calibration are described in Yan et al.(2000).Table 1also gives the parameters for our obser-vations.2.2.Data ReductionThe bias subtractions and dome Ñat-Ðeld corrections were done on the CCD images.The cosmic-ray and bad-pixel e†ects were corrected by comparing the images.The images were recentered,and position calibration was per-formed by using the Guide Star Catalog.The Ñuxes of the intermediate-band Ðlter images were calibrated by Oke &Gunn standard stars (Oke &Gunn 1983;Fukugita et al.1996).As in other works on this image Ðeld,we are preparing the SED catalog of sources.The magnitudes were measured by the aperture photometry with a detection threshold of 4p of the sky Ñuctuation per pixel.A minimum of 1pixel above the threshold was required for detection.This might introduce a false detection,particularly for the nearby very1720YUAN ET AL.TABLE 1P ARAMETERS OF THE BATC F ILTERS AND THE S TATISTICS OF O UR O BSERVATIONSFilter Central j FWHM ExposureNumber of Seeing a Calibration Stars Limiting (A )(A )(s)Images(arcsec)ImagesDetected Magnitude 1....b 38902912310029 5.363142719.52....c 421030936003 6.120b 219020.03....d 455033245006 5.293305020.54....e 49203741398015 3.943356120.55....f 5270344654016 4.703301020.06....g 579528984007 5.904383720.07....h 6075308534014 4.096391919.58....i 6660491632012 5.026391019.59....j 7050238421016 4.214418219.010...k 7490192888010 3.774557220.011...m 80202551096013 4.463435619.012...n 84801671848016 4.801394819.013...o 919024747406 3.780b 343218.514...p97452758340104.793222017.5a This column lists the seeings of the combined images.b No calibration image was taken.The intrinsic magnitudes for the c and o Ðlters are determined by the method of the SED model (Zhou et al.1999).bright stars.Since most of galaxies in the images are obvi-ously extended,we Ðnally selected a Ðxed aperture of 5pixels to do the photometry,which is large enough to make di†erent seeing e†ects negligible.Although the resulting magnitudes given by photometry with Ðxed aperture are not the same as the total magnitudes of galaxies in the literature,this is a proper way to obtain the reliable color indices (i.e.,relative SEDs)of all the sources.The pho-tometry program developed by Bertin &Arnouts (1996),SExtractor (Version 2.1.6)namely,was used for the pho-tometry.During extraction of the sources,a Ðlter of 3]3““all-ground ÏÏconvolution mask with a FWHM \2pixels was used.Since the adopted aperture size is rather large,contamination of the light by nearby objects may some-times not be negligible.The number of sources detected in the combined images are shown in Table 1.We used four standard stars,namely BD ]17¡4708,BD ]26¡2606,HD 19445,and HD 84937,in Oke &Gunn (1983)for the BATC Ñux calibration.The absolute Ñuxes of these stars were taken from Fukugita et al.(1996).The deÐ-nitions of BATC magnitudes are in the system of Oke AB l &Gunn (1983):Once them BATC \[2.5log F l[48.6.aperture photometry on the images of standard stars is done,the extinction coefficients,K ,and magnitude zero points,C ,can be obtained by Ðtting the extinction curve of magnitude versus air mass:m inst [m BATC\KX ]C ,where X is the air mass of the image.The values of K and C were derived by a median Ðtting of the data points with a straight line.The procedures of Ñux calibration are detailed in Zhou et al.(2001).For c and o Ðlters,we do not have the calibration images.Fortunately,we developed a method to calibrate the SEDs of objects for our large Ðeld multicolor photometric system based on the SED library (Zhou et al.1999),which is the so-called model calibration.This method heavily improved the quality of the observations taken under not-so-perfect photometric conditions.The SED calibration was done for our combined images.Then we derived the calibrated mag-nitudes in the c and o bands from the information of the calibrated SEDs.For other Ðlter bands,the magnitudes derived by ordinary standard calibrations were adopted for further analyses.2.3.Photometric CatalogWe achieved the photometric magnitudes within 14Ðlter bands for 5572sources in the central region (56@]56@)of Abell 2634.This SED catalog will be electronically provid-ed upon request.To cross identify all the known galaxies within our Ðeld,we made use of the NASA/IPAC Extra-galactic Database (NED).As a result,178known galaxies were found to have counterparts in our SED catalog.The identiÐcation is unambiguous for a majority of these gal-axies,according to their positional o†sets and apparent magnitudes.The SEDs of these 178galaxies are cataloged in Table 2,which is structured as follows:Column (1):Number of the galaxies,sorted by the R.A.in the J2000epoch.Columns (2)and (3):R.A.and decl.in the J2000epoch given by our photometric measurements.Column (4):Redshift,in kilometers per second,provided by NED.Column (5):Membership code.Member galaxies are identiÐed as ““m,ÏÏforeground galaxies are marked as ““f,ÏÏbackground galaxies are marked by ““b,ÏÏand a ““?ÏÏmeans possible membership (see text for details).Columns (6)È(19):Photometric magnitudes in b -through p -Ðlter bands.The value of 0.0means no detection in this Ðlter band.It should be noted that the photometric magnitudes given in Table 2might be somewhat di†erent from the total magnitudes of galaxies given in some catalogs,since we used a Ðxed aperture to do the photometry.What we attempted to obtain was the relative SEDs of objects in the central region of Abell 2634.We checked two kinds of errors respectively given by the photometric program SExtractor and by a comparison with the stellar spectral templates of Gunn &Stryker (1983).The statistic errors given by the SExtractor are smaller than the real measurement errors.We compared the errors using di†erent images with the same Ðlter.By separating stars into di†erent subgroups of magnitudes with an interval of 0.5mag,the mean measurement errors at speciÐed magni-tudes were derived.We found that the measurement errorsT A B L E 2S E D C A T A L O G O F 178K N O W N G A L A X I E S I N T H E C E N T R A L R E G I O N O F A B E L L 2634N o .R .A .(J 2000)D e c l .(J 2000)c z M b c d e f g h i j k m n o p (1)(2)(3)(4)(5)(6)(7)(8)(9)(10)(11)(12)(13)(14)(15)(16)(17)(18)(19)1.......233623.74271321.7719666b 19.1118.6918.3617.9517.8317.3017.2117.0416.9016.7416.6016.6116.4016.372.......233626.11272355.799133m 17.7617.0816.6516.1816.1015.6415.3815.2515.1914.9214.9114.6714.5314.533.......233626.87263921.599212m 18.4718.0317.9517.7117.5417.3017.2617.0717.0116.9016.8616.8516.8116.524.......233627.61270217.90...?19.3618.9418.4518.0517.7717.4817.2717.0816.9416.8016.6716.6216.4216.335.......233638.97271824.198415m 18.8218.1917.9017.5117.4117.0216.8316.7316.6816.4216.3216.2616.1316.196.......233639.00265435.898934m 18.7818.0417.7317.2617.1216.7316.6016.4916.2616.1216.0015.9815.8115.797.......233640.85264131.508738m 17.9017.6917.6317.4817.2917.2517.2117.0017.0216.9216.9016.9916.8516.788.......233642.62271721.82...?18.1117.7017.4717.2417.1616.8716.7516.7216.6616.5216.4416.5316.4516.489.......233643.11271351.2217631b 19.1718.6218.2017.6217.4417.0516.8116.7016.5616.3716.1816.1516.0015.8910......233646.45263947.558790m 17.9717.7417.7417.5217.2917.2317.2116.9316.9816.8816.8416.9116.8216.6211......233656.60271824.429869m 18.8218.2818.0017.6617.5217.1616.9616.7616.6716.4916.3616.2516.1416.0112......233700.55264917.2531139b 19.6219.2418.8218.5218.2718.0717.9617.8417.6517.4717.5217.4217.2417.2813......233702.10270342.6710295m 17.2516.9116.8316.6516.5916.4316.3116.0416.0016.0015.9115.9015.7715.7414......233706.10264849.80...?19.0618.6418.5018.2718.0417.8817.8217.6617.1817.4317.3017.3917.2217.0315......233709.57265803.129477m 18.5717.8317.4117.0116.8316.4716.2816.1616.0115.8215.7215.6315.4615.4216......233713.35265420.559295m 19.5318.8618.5618.1717.9617.6317.5117.3917.2117.0416.9816.9016.7816.8817......233717.30270109.987660m 13.0712.6412.7911.9011.3611.2011.3111.1510.9911.0011.1411.5311.6611.6718......233719.58264633.008892m 19.1918.4318.0117.6317.4017.0316.9916.8216.6216.4416.3716.3116.1416.1019......233720.09270852.209185m 19.2318.5718.1117.7417.5517.2517.0316.9116.7316.5816.4916.3616.2516.2120......233720.23265242.418626m 17.7917.0416.5216.1415.9215.5515.4515.2515.0614.8914.7814.7014.5214.4521......233723.59271450.5337924b 17.1116.6116.2816.0715.9515.7315.6015.6015.4615.4015.3715.4015.3515.3822......233725.00270303.9410114m 19.7119.0518.8318.5618.3718.1718.0717.8817.6317.6917.5817.5217.5017.3823......233725.86264245.8525752b 17.8317.9817.5817.2816.8616.5916.6016.2816.1816.0715.8915.8815.6315.6224......233726.12270419.3510075m 17.9717.4117.0416.6616.4716.1315.9215.7415.5715.4415.3115.1915.0614.9925......233727.16270401.769354m 19.2018.7218.3217.9717.8117.5217.3417.2017.0516.9016.8216.7116.5816.5226......233727.38264504.768934m 18.8518.5618.5918.4718.2818.2118.2117.9717.9617.9018.0517.9817.8117.6327......233727.83263759.569790m 18.0417.3316.9316.5316.2615.9215.8715.6915.4715.3515.2315.2315.0615.0528......233730.15264600.387777m 17.8417.5117.4117.2317.0616.8816.8616.5716.5716.4716.4616.4716.2616.1529......233731.69265015.198381m 18.6917.9217.5117.0916.8816.5416.4416.3016.0815.9315.8215.7715.6315.5830......233733.73270137.1141327b 19.6919.3418.7918.2417.7317.5117.2216.9816.8516.6716.5116.4216.2416.2331......233735.21264856.0235169b 17.6017.2417.1616.9616.8116.6416.5816.2816.3116.1916.1816.1416.0015.9132......233738.11264910.149599m 19.4718.8718.5518.1417.9117.6017.4917.3717.1717.0217.0016.9216.7116.7633......233743.55270302.9818425b 17.2918.2017.8017.5917.2116.9516.9716.5816.5516.5616.3116.2616.1116.1034......233744.31264243.09...?0.0019.7519.2818.9118.5318.2818.1517.9217.7017.4817.3617.3617.1516.9035......233746.72265852.8011106m 18.0717.4516.9516.5616.3616.0315.8415.7115.5415.4115.2815.1715.0214.9736......233746.97264700.31...?19.2518.8218.3918.1217.7717.5917.5017.3017.1016.9516.8816.8916.7016.6537......233753.75270518.169898m 19.1018.4718.2017.8617.6917.4317.270.0016.7316.5816.5916.4916.2516.2138......233755.49270603.6710187m 18.6217.9717.5517.1516.9816.6416.4516.3116.1615.9915.8615.7615.6215.6039......233756.06271131.0737000b 20.6121.3120.9120.9220.7419.9819.6819.5019.4219.4118.8319.1518.6418.6340......233755.75271114.1737322b 19.8119.4018.8118.3217.8417.6317.3717.1017.0116.7816.6316.5016.4016.39T A B L E 2ÈC o n t i n u e dN o .R .A .(J 2000)D e c l .(J 2000)c z M b c d e f g h i j k m n o p (1)(2)(3)(4)(5)(6)(7)(8)(9)(10)(11)(12)(13)(14)(15)(16)(17)(18)(19)41......233756.22270412.3718429b 19.2618.8018.2017.6417.3917.1016.8816.7316.5416.3916.2016.1616.0615.8842......233756.81265402.3825676b 13.1612.5412.7511.6811.1311.0010.9111.0010.5610.4810.9011.0411.0711.1143......233757.94271553.2910211m 17.8517.1716.7316.3116.1415.7515.5315.3615.2415.0214.8414.7314.5714.5544......233758.06265732.09...?0.000.0020.6220.2319.9619.5519.5119.1518.9318.5718.7818.8218.420.0045......233758.91272250.698721m 18.1417.8917.8417.7117.5817.5117.3617.1117.2217.1217.0017.0116.9216.9746......233759.75264812.509410m 19.5718.8118.5318.2217.9717.7017.6017.4217.2717.1216.9917.0116.8816.8647......233800.97263451.5125915b 18.4818.0717.5317.1216.7416.4516.4316.1715.9515.8115.6915.7315.5815.4548......233802.29265833.82...?0.0019.4818.8118.5118.3617.9717.8217.7417.5317.4617.4717.4117.3317.2649......233802.32271210.4237540b 19.9719.3718.7418.1417.6517.4417.1316.9216.8316.5816.4416.2616.1516.1050......233803.13270523.5325797b 20.0319.6819.2418.7918.6518.3218.0917.9617.7917.5917.4317.4217.1717.3051......233805.02264611.548755m 18.8018.2517.9417.6517.3616.9816.8816.5916.4116.2516.1616.0415.8315.7552......233805.05263555.14...?19.7719.2918.9218.6318.2118.0518.0117.7717.6217.3917.3817.4017.2117.1353......233806.79264457.7510400m 20.1119.3218.8618.5418.2917.9517.9217.7517.5317.3717.3317.3617.1717.4354......233809.59265515.479801m 19.3318.9918.6018.1917.9917.6717.5317.3917.2017.0817.0616.8916.7416.6955......233810.04271208.687970m 18.1718.2718.2518.1617.6718.0918.0317.5517.8917.8217.8517.8417.750.0056......233810.35270151.488378m 19.0818.4017.9817.6217.4517.1116.9416.8116.6416.4916.3816.2916.1516.1357......233811.17263710.68...?18.7318.3718.2918.1617.9617.7917.8217.5617.4817.4417.4117.4217.3317.3158......233811.98263415.69...?19.1918.7218.5918.4318.2618.0518.1017.9117.5417.7417.6417.6517.6517.4859......233813.79272452.309285m 17.8617.1116.6416.1815.9915.6015.3415.1815.0414.8014.6514.5114.3714.3260......233814.40265803.919310m 19.3618.7518.3317.9317.7817.4117.2417.1216.9316.7716.7016.5716.4716.4361......233816.17264903.828752m 17.9217.2116.7316.3316.1115.7415.6615.5015.2815.1415.0714.9914.7914.8062......233816.33264222.529544m 0.0020.1019.7019.1218.5818.3618.2218.0117.8417.6117.6217.4417.3117.3263......233816.76265205.937800m 18.2317.9517.8617.7617.5617.4717.4117.1217.1217.0416.9716.9916.8116.7064......233817.28265542.939397m 18.9418.2417.8517.5117.3116.9716.8316.6816.4916.3616.2916.1816.0616.0465......233817.76265318.23...?18.4117.9517.5517.4217.1116.8116.8016.5016.5016.4116.2316.0515.8715.8566......233818.60265314.449348m 17.8417.1016.5916.2015.9815.6015.4815.2815.0914.9314.8114.7014.5314.4967......233818.74270208.549552m 18.4617.7417.2316.8216.6416.2616.0815.9415.7115.5815.4715.3315.1715.2068......233819.67264248.95...?20.0219.2818.9518.5618.3818.0018.0017.8317.6017.4617.4517.3717.2517.4269......233819.95265850.25...?19.7819.4119.2319.1819.0018.8618.7518.8218.6218.5518.9018.5718.980.0070......233820.85270304.5610111m 18.4517.7517.2216.7816.6116.2416.0615.9015.7115.5615.4215.3015.1515.1171......233821.44270302.26...?18.9218.4418.0417.7917.5517.2517.1816.8916.8516.7516.5516.4616.3416.3372......233821.01271815.769980m 18.6317.9217.4517.0416.8716.5116.2816.1515.9915.8115.6515.5715.4415.4173......233822.75271228.278572m 18.9918.2917.8417.4417.2716.9316.7116.5916.4216.2316.1016.0215.9115.8774......233822.89270930.879302m 17.7217.0016.5116.0915.9315.5615.3615.2015.0414.8614.7314.6114.4614.4575......233822.97271752.5737852b 19.5419.3318.8718.5318.1217.9417.6717.4917.3917.1717.0416.9616.8716.8076......233825.45270149.299532m 19.2318.5518.1517.8317.5517.1917.0916.8616.7516.6016.4916.3316.3016.2977......233826.94265908.0010774m 17.7417.0616.5516.1415.9415.5715.4215.2415.0714.9114.8014.6614.5014.4878......233826.98264324.30...?19.4218.9618.5618.3117.9717.7917.7117.5217.3417.1217.1517.0816.9216.8879......233827.19270939.10...?19.9719.3318.9218.5618.3418.0617.8917.7517.5817.4117.3417.2117.1217.2080......233827.25270527.107532m 18.4217.7617.3716.9916.8516.5116.3216.1916.0315.8415.7415.6715.5215.501722T A B L E 2ÈC o n t i n u e dN o .R .A .(J 2000)D e c l .(J 2000)c z M b c d e f g h i j k m n o p (1)(2)(3)(4)(5)(6)(7)(8)(9)(10)(11)(12)(13)(14)(15)(16)(17)(18)(19)81.......233828.72264908.419542m 17.4816.7616.2815.8815.6615.3115.2015.0514.8514.7014.6114.5214.3514.3982.......233829.27271226.328403m 19.8619.1118.7318.3418.1517.8317.6217.4917.3517.1517.0516.9516.8416.7783.......233829.30265845.229502m 17.6416.9216.4016.0015.8215.4315.2715.1014.9414.7714.6714.5214.3514.3484.......233829.36270225.3210183m 19.0118.4918.0917.8517.5317.1417.1216.8016.7616.6016.4516.3116.1816.1785.......233829.56270203.328104m 16.6915.9415.5415.2515.0014.6114.5414.2514.1814.0113.8413.7013.4913.4886.......233829.52270155.929060m 17.0716.2615.7415.3415.1614.7814.6014.3814.2214.0513.8913.7913.5713.6187.......233829.36270151.329252m 16.3715.5315.1314.7814.5414.1514.0513.7813.6813.5113.3413.2113.0213.0188.......233830.27263554.529395m 18.4217.9417.7417.5217.2517.0016.9916.7716.6416.5216.4116.3816.2816.2089.......233831.65272109.539984m 19.7019.1618.8118.4618.1517.8617.5817.3317.2216.9916.8816.7316.6016.5190.......233831.69270542.03...?19.5418.7318.1017.8117.7217.3317.1117.0416.9016.7416.6916.7516.6016.6391.......233831.36270540.33...?19.3018.2617.8617.6717.4817.0916.9416.8116.7016.5916.4516.5416.4016.3992.......233832.33265436.348270m 18.5317.9017.4117.0116.8416.4716.3516.2016.0015.8315.7815.6515.4915.5293.......233833.37270207.059828m 18.2517.5917.1216.7116.5416.1916.0115.8315.6415.4815.3815.2315.0515.0894.......233834.58265847.658515m 17.9317.2016.6616.2416.0915.7115.5415.3715.1914.9914.9314.7814.5814.5795.......233836.16272101.9736811b 19.3219.0118.4417.9017.4117.2316.8716.6916.5516.3416.2416.0615.9615.9996.......233836.37270148.378378m 18.0217.2416.7316.3116.1415.7615.5815.4015.2115.0214.9414.7814.6014.6397.......233837.15264318.075609f 0.0019.7719.3918.9518.4718.3018.1517.8717.6817.4317.4317.3017.1617.1198.......233838.91270042.299274m 17.6316.8716.4015.9815.8015.4415.2815.1014.9414.7714.6814.5414.3614.3999.......233838.29270037.389356m 17.8117.1316.7316.4416.1815.8115.7315.4715.4015.2315.0914.9214.7514.74100......233839.16270416.699443m 19.0218.3417.9317.5317.3817.0516.8816.7216.5916.4116.2916.2016.0416.06101......233841.21265621.20...?19.4219.0618.8518.5518.3118.1117.9617.7717.4117.5117.3917.3217.2017.07102......233841.85271256.118548m 18.8718.2417.7917.3817.2016.8616.6216.4916.3316.1516.0415.9115.7915.74103......233842.18270708.519607m 18.4017.6917.2016.7616.5816.2516.0015.8615.6815.4915.3715.2415.0815.06104......233842.43264625.419862m 16.1516.4116.0115.7215.4215.1215.0814.8014.7214.5914.4214.3314.1514.14105......233842.77270327.519983m 19.7218.9718.4518.1117.9217.6217.4417.2717.1416.9716.8416.7516.6516.62106......233843.23270232.429195m 19.0518.3117.8217.4117.2516.9116.7016.5716.3716.2216.1216.0015.8215.89107......233843.77271256.729279m 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17.3016.5516.0115.5715.3815.0114.7614.5914.4214.2114.0813.9313.7813.81117......233850.77270058.479970m 18.6917.9317.4817.1116.9516.6016.4116.2616.0815.9415.8615.7315.5715.61118......233852.60265623.589059m 19.1318.4918.0717.7317.5417.3017.0217.0316.6916.5416.5016.3816.2316.22119......233853.12270202.099940m 0.0019.6119.1818.7818.5418.2718.0717.9317.7717.5617.5017.4017.2817.37120......233854.05270245.899643m 18.5817.8917.3916.9916.8316.4916.2816.1415.9415.7715.6715.5615.3915.441723。