UV Emission Mapping for IGM & Nearby Galaxies Li Ji ( 纪丽 ) ji@pmo.ac.cn 中国科学院暗物质与空间天 文重点实验室 Key Laboratory of Dark Matter and Space Astronomy Chinese Academy of Sciences
Team in China Li Ji 1 on behalf of Jin Chang 1, Mingsheng Cai 1,Fuzhen Cheng 2, Jingquan Cheng 1, de Grijs, Richard 3, Taotao Fang 4, Longlong Feng 1,Yu Gao 1, Qiusheng Gu 5, Jianhua Guo 1, Bing Jiang 5, Shijun Lei 1, Zhiyuan Li 5, Jifeng Liu 6, Ping Ruan 7, Wenlei Shan 1,Qian Song 6, Q.Daniel Wang 5, Tinggui Wang 2, Sen Wang 6, Zhuangchun Wu 8, Shuinai Zhang 1, Xin Zhou 1 1 Purple Mountain Observatory, CAS, Nanjing, China 2 Dept. of Astronomy, University of Science and Technology of China, Hefei, China 3 Dept. The Kavli Institute for Astronomy & Astrophysics, Peking University, China 4 Dept. of Astronomy, Xiamen University, Xiamen, China 5 School of Astronomy &Space Science, Nanjing University, Nanjing, China 6 National Astronomical Observatories, CAS, Beijing, China 7 Xi an Institute of Optics and Precision Mechanics, CAS, Xi an, China 8 Nanjing University of Science and Technology, Nanjing, China
Cosmic Web credit: Suto et al. 2004 - the threads connecting galaxies & the large-scale structures of the Cosmic Web - Warm-hot Intergalactic Medium (WHIM)
Baryon density in the Universe credit: Nicastro et al. Science 2008 Fig. 1. Baryon density in the universe, at all redshifts, normalized to the cosmological mass density of baryons derived from cosmic microwave background (CMB) anisotropy measurements.
Measuring Cosmic Web credit: Cen & Ostriker (2006)
Existing Detections credit: Sembach et al. 2010 FUSE COS XMM-Newton 930-1180 Å 1140-1800 Å n 0.5 arcsec 1.5-170 Å 7-35 Å WHIM has to be detected in UV - Only absorption detections (FUSE, HST/COS) - Emission: Directly 3D (x,y,v) mapping
Nearby Galaxies M82 NGC1482 NGC253 edge-on galaxies with a range of starformation rates: (Strickland et al. 2004) - red: H - green: optical R band - blue: 0.3-2keV (soft X-ray) NGC3628 NGC3079 NGC4959 - Hot gas extending perpendicular to the major axes of the galaxies - No emission data for 1e5 K gas! NGC4631 NGC6503 NGC891 credit: Strickland et al. 2004
Scientific Examples Understand the galactic feedback is essential to the study of the galaxy formation & evolution credit: Cen & Ostriker 2006
Uniform Metallicities OVI CIV Simulations Predicts Simulation Metallicities OVI CIV WHIM gas. Finally, comparison of the two differ licity models shows that a larger fraction of emiss from gas on the IGM and cooling loci if we assume metallicity. This is a simple consequence of the m bution illustrated in Figure 4: metals tend to be centrated inside filaments, which are already relati emitters. A uniform metallicity thus decreases th betweenly filaments and voids. As mentioned above, nearly all the emission i is much less than the background z=0.15 and hence uno Figure 6 shows an example of what one could see (background-limited) observation. z =0.01 Figures 6a 6b sh of the universe with z ¼ 0:15, z ¼ 0:01, and (corresponding to a physical size 25 h 1 kpc). and 6b show the surface brightness of the O vi k1 tion assuming uniform and simulation metalliciti tively. Figures 6d and 6e show the same for the C transition. We include only those pixels with > 7 cm 2 s 1 Ly sr 1. Table 1 shows that this is a reason for the diffuse background for O vi k1032, assuming resolution P1 8. It is also compatible with the u credit: Furlanetto et al. 2004
Scientific Objectives Goal: first time 3D(x,y, v)-mapping the vicinities of nearby galaxies in 1e5 K - connections with cosmic web - feedback and accretions between galaxies & IGM - How WIHM distributed in Cosmic Web? filament? halo? - How does the outflow/inflow of hot gas affect the evolution of galaxies? - How does gas cool?
Other Possible Science Objectives - Atmospheres of (exo)planets e.g. Habitable exo-planets (Tian et al. 2013) Credit: Gudel, M.
'($)*&L,--,./-&,/&L"5N&8)7%5%/M#3&4$.M$)L-& UV in multi wavelength programs P0<Q<RG=& HESS/VERITAS/Cangaroo3 (Energy) Fermi Gamma-ray X-ray All-sky survey Gamma-ray satellite HXMT ASTRO-H/NuStar/ e-rosita/gems Chandra, XMM-Newton Suzaku Optical & infrared ASTRO-H is the observatory JWST Herschel High-resolution interferometer in the millimeter band. Radio 2008 DAMPE 2010 2012 ALMA 2014 (Year) 2016 Credit: Ohashi, T 2010, in Netherlands 2020
What do we have in China - PMO: Key Laboratory of Dark Matter & Space Astronomy DAMPE ( Launch in 2015) - NAO: Long Slit Spectrograph ( prototype, 3M USD, PI Sen Wang) - Team: -CAS: PMO,NAO,Xi an Institute of Optics & Precision Mechanics -Universities: USTC NJU XMU Tsinghua Univ.... -International Collaborations we anticipate collaborations from ( e.g. University of Leicester, UK ; De Paris Observatory, France etc.)
Team Members in China 课题主要参加人员 姓名 年龄 专业技术职务 学历 投入人年 课题中的分工 工作单位 高煜 50 研究员 博士 0.1 科学目标 紫金山天文台 冯珑珑 50 研究员 博士 0.1 科学目标数值模拟 紫金山天文台 蔡明生 47 研究员 博士 0.2 探测器 紫金山天文台 单文磊 41 研究员 博士 0.2 探测器 紫金山天文台 程景全 66 研究员 博士 0.2 望远镜设计 紫金山天文台 郭建华 33 副研究员 博士 0.2 控制系统 紫金山天文台 雷仕俊 38 助理研究员博士 0.3 科学目标模拟 紫金山天文台 张水乃 30 助理研究员博士 0.3 科学目标模拟 紫金山天文台 周鑫 31 助理研究员博士 0.3 科学目标模拟 紫金山天文台 王森 59 研究员 博士 0.2 光学工程 国家天文台 宋谦 48 研究员 博士 0.2 探测器 国家天文台 刘继峰 40 研究员 博士 0.2 科学目标 国家天文台 阮萍 48 研究员 博士 0.1 光学工程 中国科学院西安光学精密机械研究所 程福臻 71 教授 博士 0.1 科学目标 中国科技大学 王挺贵 48 教授 博士 0.2 科学目标 中国科技大学 顾秋生 45 教授 博士 0.2 科学目标 南京大学 李志远 36 教授 博士 0.2 科学目标 南京大学 姜冰 33 讲师 博士 0.3 科学目标 南京大学 方陶陶 43 教授 博士 0.2 科学目标数值模拟 厦门大学 - Science T. Wang, F. Cheng (USTC) Y. Gao, L. Ji, S. Zhang (PMO) Q. Wang, Q. Gu, Z. Li, B. Jiang (NJU) T. Fang (XMU) J. Liu (NAO), F. Tian (Tsinghua Univ.) de Grijs, R. (KIAA-PKU) -Simulations L. Feng, S. Lei, X., Zhou (PMO) -Optics design S. Wang (NAO), J. Cheng (PMO), P. Ruan (XIOPM) -Detector design W. Shan (PMO), Z. Wu (NUST), Q. Song (NAO) -Electronic System M. Cai, J. Guo, J. Chang (PMO)
UV Emission Mapping for IGM & Nearby Galaxies First look at accretion, feedback & WHIM Welcome you to join us! Li Ji ( 纪丽 ) ji@pmo.ac.cn