类星体的高分辨成像观测及其科学目标

王益萍国家天文台合作者：T.Yamada,I.Tanaka,M.Iye,T.Misawa,Y.Minowa，纪拓,田海俊,陈燕梅

等类星体的高分辨成像（AO）观测及其科学目标CHINA-AO2012

三峡大学，宜昌摘要1)高空间分辨率成像技术对天文研究的影响2）自适应光学系统（AO）简介3）类星体高分辨成像观测（AO）的科学目标a)类星体吸收线物理对应体的论证b)高红移类星体母星系的观测研究4）先遣观测结果和分析高分辨成像在天文研究上的主要应用：1）Planetaryscience:-asteroidsurfaces,satellitesurfaces,asteroidalmoon,moonsofgiantplanets….2)Solarphysics:-finestructuresandvarioussolarphenomena….3)Stellarastronomy:-youngbinarystars,stellarclusters,circumstellardisks,embeddedclustersetal.Faintcompanions:-veryfaintcompanionstonearbystars,browndwarfetc.5)Galacticandextragalactic:-QSOhostgalaxies,QALhostgalaxies,companiongalaxies,morphology,interactinggalaxies,thecoresofnearbygalaxies,Galacticcenter…影响天文成像质量的几大因素1）望远镜本身：光学系统，CCDetal.2)大气视宁度(seeing)大气湍流：1）星象抖动，星光闪烁；2）星象模糊

从而降低了望远镜的分辨本领和极限星等衍射极限：光学波段，台站seeing~1“，D=15cm,衍射极限~0.8”D=10米++，seeinglimited~1”Courtesy:LBTwebsite自适应光学（AO)—自动校正光学波前误差的技术BinaryHR1852,separationof0.”31,Takamietal.PASJ56,225(2004)AO观测简单流程：OptimizinganAOsystemOptimizetheAOsystemCredit:Brusaetal.StewardObs.?SubaruAO36,Takamietal.PASJ56,225(2004)AdaptiveOpticsincreasespeakintensityofapointsource,allowsastronomerstoperformaccuratemeasurementsontheimage,suchasphotometryandastrometry.Photocredit:LairdClose,CAAO,StewardObs.Credit:Marchettietal.2007High-zQSOiseasytodetect;QSOisbright,soabsorbersinfrontofthemcanbestudiedindetailthroughabsorptionlines+deepimaging.1)QSOaborptionlinesystemsGascontainingneutralHydrogen,heavyelements(C,Si,Mgetal.)LLSystemsareaclassofQALsystem.TheyaredefinedtobeopticallythickattheLymanLimit,whichgenerallyimpliesN(HI)>10^17cm^-2.Theyallshowmetals.2）重要性：Goodplacetostudygascyclingduringintensivegalaxyformationepoch(z~3)Fumagallietal.20121）适时性：Massivediskgalaxyathigh-z,Collapse?Merger?Coldstream?3）可行性：AO等高分辨成像技术+地面大望远镜P.Moller&S.J.Warren1998C.Churchill1999BVRIJHKsdeepimagingusingSubaruandHST:（Wangetal.2009)2”.4northoftheQSOsightline.Thecandidateisindicatedintheimage.2)impactparameterof~19.6kpc,ifatz~2.53.3)apparentK-magnitudem=21.91+/-0.26,aswellasaredcolorR-K>3.32”.4northoftheQSOsightline.Thecandidateisindicatedintheimage.2)impactparameterof~19.6kpc,ifatz~2.53.3)apparentK-magnitudem=21.91+/-0.26,aswellasaredcolorR-K>3.32”.4northoftheQSOsightline.Thecandidateisindicatedintheimage.2)impactparameterof~19.6kpc,ifatz~2.53.3)apparentK-magnitudem=21.91+/-0.26,aswellasaredcolorR-K>3.3IRCS+AOobservationofUM402atz~3Wangetal.2012submitted星系合并触发核区星暴和中心黑洞增长的演化模型巨黑洞哪来的？原料提供机制研究背景：模型和研究方法：主要结果：1）黑洞和母星系核球是共同演化的;2）中心星暴和AGN有一定的相关性。3)星系合并是触发核区剧烈星暴和巨黑洞形成的有效机制。统计上的意义Wang&Biermann1998;Wang&Biermann2000;Wangetal.2000;Wangetal.2003,20042)类星体母星系的观测，MBH–

Lhostrelation(KormendyandRichstone1995)高红移处还成立吗？星系合并—中心星暴/黑洞增长--早型星系/AGN中的“黑洞/核球”线性相关性模型的观测检验：

BHmassmeasurementsi)Keplerianrotation(inactivegalaxies)WatermaserHbeta,MgIIetal.ReveberationmappingVariabilityofAGNs………….2)Hostgalaxypropertiesi)spaceobservationii)AOimaging高光度(MB<-25)类星体数密度分布Boyleetal.2000红移z~2-3处的样本统计上具有重要意义！选源条件(IRCS+AO)：Guidestar:R<18,bestR=10-16Distanceofseparation:D<30”PSFcalibrationstar:closeenoughtotheQSO,similarmagnitude,similarguidestardistance,similardirectiontotheguidestar………...EmissionlinesHa,Hb,OII,OIIIshouldbeavoidedintheobservingbands.2”.4northoftheQSOsightline.Thecandidateisindicatedintheimage.2)impactparameterof~19.6kpc,ifatz~2.53.3)apparentK-magnitudem=21.91+/-0.26,aswellasaredcolorR-K>3.32”.4northoftheQSOsightline.Thecandidate