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,

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1 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

2 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

3 Cosmic Web credit: Suto et al the threads connecting galaxies & the large-scale structures of the Cosmic Web - Warm-hot Intergalactic Medium (WHIM)

4 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.

5 Measuring Cosmic Web credit: Cen & Ostriker (2006)

6 Existing Detections credit: Sembach et al FUSE COS XMM-Newton Å Å n 0.5 arcsec Å 7-35 Å WHIM has to be detected in UV - Only absorption detections (FUSE, HST/COS) - Emission: Directly 3D (x,y,v) mapping

7 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 NGC 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

8 Scientific Examples Understand the galactic feedback is essential to the study of the galaxy formation & evolution credit: Cen & Ostriker 2006

9 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

10 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?

11 Other Possible Science Objectives - Atmospheres of (exo)planets e.g. Habitable exo-planets (Tian et al. 2013) Credit: Gudel, M.

HESS/VERITAS/Cangaroo3 (Energy) Fermi Gamma-ray X-ray

e-rosita/gems Chandra, XMM-Newton Suzaku Optical &

High-resolution interferometer in the millimeter band.

12 '($)*&L,--,./-&,/&L"5N&8)7%5%/M#3&4$.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 ALMA 2014 (Year) 2016 Credit: Ohashi, T 2010, in Netherlands 2020

13 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.)

14 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)

15 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