1 / 26

类星体的高分辨成像（ AO ）观测及其科学目标

CHINA-AO 2012 三峡大学，宜昌. 类星体的高分辨成像（ AO ）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. 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 ：.

pahana
Download Presentation

类星体的高分辨成像（ AO ）观测及其科学目标

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. CHINA-AO 2012 三峡大学，宜昌 类星体的高分辨成像（AO）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

  2. 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

  3. 高分辨成像在天文研究上的主要应用： • 1） Planetary science:- asteroid surfaces, satellite surfaces, asteroidal moon, moons of giant planets…. • 2) Solar physics:- fine structures and various solar phenomena…. • 3) Stellar astronomy:- young binary stars, stellar clusters, circumstellar disks, embedded clusters et al. • Faint companions:- very faint companions to nearby stars, brown dwarf etc. • 5) Galactic and extragalactic:- QSO host galaxies, QAL host galaxies, companion galaxies, morphology, interacting galaxies, the cores of nearby galaxies, Galactic center…

  4. 影响天文成像质量的几大因素 • 1）望远镜本身： 光学系统， CCD et al. • 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

  5. 衍射极限： 光学波段， 台站seeing ~ 1“， D=15cm , 衍射极限~0.8” D=10米++， seeing limited ~1” Courtesy: LBT website

  6. 自适应光学（AO)—自动校正光学波前误差的技术自适应光学（AO)—自动校正光学波前误差的技术 Binary HR 1852, separation of 0.”31, Takami et al. PASJ 56, 225 (2004)

  7. AO观测简单流程：

  8. Optimizing an AO system

  9. Optimize the AO system Subaru AO36, Takami et al. PASJ 56, 225(2004) Credit: Brusa et al. Steward Obs. ?

  10. Adaptive Optics increases peak intensity of a point source, allows astronomers to perform accurate measurements on the image, such as photometry and astrometry. Photo credit: Laird Close, CAAO, Steward Obs.

  11. Credit: Marchetti et al. 2007

  12. 1) QSO aborption line systems Gas containing neutral Hydrogen, heavy elements (C, Si, Mg et al.) • High-z QSO is easy to detect; • QSO is bright, so absorbers in front of them can be studied • in detail through absorption lines + deep imaging.

  13. LL Systems are a class of QAL system. They are defined to be optically thick at the Lyman Limit, which generally implies N(HI)> 10^17 cm^-2. They all show metals.

  14. Why high-z LLS sample ? 1）适时性： Massive disk galaxy at high-z, Collapse? Merger? Cold stream? 2）重要性： Good place to study gas cycling during intensive galaxy formation epoch (z~3) 3）可行性： AO等高分辨成像技术 +地面大望远镜 Fumagalli et al. 2012

  15. C. Churchill 1999 P. Moller & S.J. Warren 1998

  16. BVRIJHKs deep imaging using Subaru and HST: （Wang et al. 2009)

  17. IRCS+AO observation of UM402 at z~3 Wang et al. 2012 submitted • 2”.4 north of the QSO sightline. The candidate is indicated in the image. • 2) impact parameter of ~ 19.6 kpc, if at z~2.53. • 3) apparent K-magnitude m=21.91+/-0.26, as well as a red color R-K>3.3 • 2”.4 north of the QSO sightline. The candidate is indicated in the image. • 2) impact parameter of ~ 19.6 kpc, if at z~2.53. • 3) apparent K-magnitude m=21.91+/-0.26, as well as a red color R-K>3.3 • 2”.4 north of the QSO sightline. The candidate is indicated in the image. • 2) impact parameter of ~ 19.6 kpc, if at z~2.53. • 3) apparent K-magnitude m=21.91+/-0.26, as well as a red color R-K>3.3

  18. 2) 类星体母星系的观测，MBH –Lhost relation 星系合并触发核区星暴和中心黑洞增长的演化模型 Wang & Biermann 1998; Wang & Biermann 2000; Wang et al. 2000; Wang et al. 2003, 2004 研究背景： 模型和研究方法： 主要结果： 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 巨黑洞哪来的？ 原料提供机制 统计 上的 意义 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。 高红移处还成立吗？ (Kormendy and Richstone 1995)

  19. 模型的观测检验： • BH mass measurements • i) Keplerian rotation (inactive galaxies) • Water maser • Hbeta, MgII et al. • Reveberation mapping • Variability of AGNs…………. • 2) Host galaxy properties • i) space observation • ii) AO imaging

  20. 高光度(MB<-25)类星体数密度分布 红移z~2-3处的样本统计上具有重要意义！ Boyle et al. 2000

  21. 选源条件(IRCS+AO)： • Guide star : R<18, best R=10-16 • Distance of separation: D<30” • PSF calibration star: close enough to the QSO, similar magnitude, similar guide star distance, similar direction to the guide star ………... • Emission lines Ha, Hb, OII, OIII should be avoided in the observing bands.

  22. IRCS+AO observation of UM402 at z~3 Wang et al. 2012 submitted • 2”.4 north of the QSO sightline. The candidate is indicated in the image. • 2) impact parameter of ~ 19.6 kpc, if at z~2.53. • 3) apparent K-magnitude m=21.91+/-0.26, as well as a red color R-K>3.3 • 2”.4 north of the QSO sightline. The candidate is indicated in the image. • 2) impact parameter of ~ 19.6 kpc, if at z~2.53. • 3) apparent K-magnitude m=21.91+/-0.26, as well as a red color R-K>3.3

  23. 总结 • 高分辨成像（AO）将在类星体吸收线的物理对应体的认证工作中显示其重要性。 • 8-10米级望远镜+AO对红移z~2的类星体母星系的研究提供了可能性。

More Related