[1] (TMT GMT JWST EUCLID ALMA SKA FAST LSST 21cm ) M σ [2 4] M σ 6 1/10 [5 7] X (recombination, z = ) 1/10 5 z = H 2 [8,9

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1 33 1 Vol. 33, No PROGRESS IN ASTRONOMY Feb., 2015 doi: /j.issn ,4 1,4,5,6 7 1,8 9 1, , ,12 8,13 1,4 14 8,15 1,4 9 1,4,5,6,8 ( Theoretisch-Physikalisches Institut, Friedrich-Schiller-Universität Jena, D Jena, Germany ) P A (XDA ) ( ) ( ) (Y3KF281CJ1) lau@amss.ac.cn

2 [1] (TMT GMT JWST EUCLID ALMA SKA FAST LSST 21cm ) M σ [2 4] M σ 6 1/10 [5 7] X (recombination, z = ) 1/10 5 z = H 2 [8,9] [10 12] [11 19] SDSS M ( 13 Ga) SDSS Gunn-Peterson z = 6 7 WMAP z = 16 z = 16 z = M (mini-quasars) [9,11 13,18,19]

3 1 61 H M [9] 10 4 M M [18,19] 1 3 [13 17] Hubble JWST ( ) 10 [20,21] [20,22,23] 1974 Hulse Taylor PSR B , [24,25] 1993 PSR J PSR J PSR J [26 28] [20]

4 62 33 h(t) = L L (15 Mpc) h [29] (ESA) [30 39] 10 ( 1 10 Hz) (1 10) km ( Hz) [20,38 40] (NASA) (ESA) LISA (Laser Interferometer Space Antenna) [37 39] 20 NASA LISA elisa (evolved LISA) [41,42] (the Gravitational Universe) (L3 mission) elisa 2034 LISA/eLISA LISA-Pathfinder 2015 LISA [43] 2050 [44] km (< Hz) (z 10) [45,46] elisa (1)

5 [20] [20] ( Hz) ( ) ( ) ( ) [20,39,41,42,45 48] ( ) ( ) ( ) [20] X 1 h

6 ( Hz) ( ) ( ) BBO DECIGO s [26 28,49] 10 [49] ( ) [50 52] LISA elisa ( )

7 1 65 [53 55] [45,52] ( ) 2.2 [21,42,45 48] (AGN) M σ ( Final Parsec )

8 66 33 [13 15,17,56] [21,57,58] ( 1 1 ) ( ) ( z > 10) [20,21] LISA/eLISA M [21,47,48,57,58] ( ) [45,46,59 61] 2.3 (Extreme Mass Ratio Inspirals, EMRI) ( ) (Innermost Stable Circular Orbit, ISCO) 1/10 6 EMRI [62 64] elisa 1 [62 67] EMRI EMRI EMRI EMRI

9 1 67 EMRI (z 0.1 1) EMRI ISCO Kerr EMRI [68 72] EMRI 17 Kerr EMRI [73 75] [68,76,77] EMRI ( M ) 2.4 X (Ultraluminous X-ray source, ULX) M Einstein X X J/s X X L X J/s X X L X < J/s ROAST Chandra X X M82 M15 NGC3628 ω [78 81] ULX ( 10 5 M ) ULX X ULX X ULX X M ULX ULX X ULX [82 86] ( ) [84 89] (Intermediate Mass Ratio Inspiral, IMRI)

10 68 33 IMRI ULX X XXM-Newton Hz 10 6 km ( ) [45,46,87 90] [89] IMRI IMRI EMRI IMRI IMRI [ ] s [20,99] BBO (Big Bang Observer) [100,101] DECIGO (Deci-Hertz Gravitational wave Observatory) [ ] ( )

11 1 69 LISA (elisa) 2.6 ( ) [44] [46] 3 [45,46] ( ) ( ) [39,40,46] LISA 2009 LISA km LISA [45] Peter Bender ALIA (Advanced LISA) [60,61] 0.01 Hz z = M [45] 0.1 pm [45] (20 30 a)

12 70 33 ( LISA/eLISA) 2 2 /km /W /m /pm Hz 1/2 /m s 2 Hz 1/ (ALIA) (> 1 mhz) ( ) (> 0.2 mhz) ( ) (> 0.1 mhz) (LISA) (> 0.1 mhz) (elisa) (> 0.1 mhz) 2 LISA 1 LISA Hz LISA elisa ( elisa LISA 3 [41] ) Hils Bender [51] Farmer Phinney [52] km 5 10 pm 10 pm km 3.2 LISA/eLISA ( ) ( )

13 1 71 [51, 52] 1 [20] ( ) 1:10 1:1000 IMRI 2 1:4 10 M M ( km 8 pm Hz 1/2 ) IMRI LISA 2 ( ) elisa (z > 10)

14 72 图2 天 文 学 进 展 33 卷 我国空间引力波探测任务预研究所建议的灵敏度设计在不同致密双星混淆噪声水平下对中等质量黑 洞相关的双黑洞绕转并合系统的平均探测范围 (a) 双中等质量黑洞并合系统 (质量比为 1:4) (b) 小黑洞 中等质量黑洞并合系统 (折合质量为 10 M ) km 臂长 即使在将任务测距精度放宽到 5 10 pm 的水平后 任务对中等质量双黑 洞目标波源的捕捉能力 (视野) 较之 LISA 等仍具有显著的提高 这个提高不仅是探测视野 任务对可探测到的波源也具有更好的信噪比和置信度水平 这在保证参数估计的准确度方面 是非常重要的 图 3 是 km 臂长设计对恒星质量黑洞 - 中等质量黑洞的 IMRI 并合波 源的信噪比等高线图 其中我们假设了折合质量仍然为 10M 图 4 图 5 是 km 臂 长设计对双中等质量黑洞并合系统的信噪比等高线图 分别考察质量比和红移对信噪比分布 的影响 这里的信噪比均指对波源位置 双星轨道倾角 极化平均过后的信噪比 我们假设 了对目标波源有 1 年连续的观测时间 这在空间引力波探测概念研究中是一个保守的假设 图 km 臂长的两种灵敏度设计对小黑洞 中等质量黑洞绕转并合系统 (折合质量为 10 M ) 的 单个迈克尔逊通道探测信噪比等高线图 (并合前 1 年的观测时间) (a) 5 pm Hz 1/2 (b) 8 pm Hz 1/2 双星背景噪声采用上限和下限估计的折中水平 3.3 基于冷暗物质模型的黑洞宇宙学成长并合模拟与探测率估计 在冷暗物质宇宙学模型暗物质晕等级成长的框架下 通过蒙特卡罗模拟实现暗物质晕的

15 km ( 1:1 1:10 ) ( 1 ) (a) 5 pm Hz 1/2 1:1 (b) 5 pm Hz 1/2 1:10 (c) 8 pm Hz 1/2 1:1 (d) 8 pm Hz 1/2 1:10 ( ) [13,14,17] ( z = 0 ) EPS ( Press-Schechter ) [10 13] z = 0 EPS ( EPS ) z = 0 (merger tree) ( )

16 km ( 1 ) (a) 5 pm Hz 1/2 z = 2 (b) 5 pm Hz 1/2 z = 6 (c) 5 pm Hz 1/2 z = 10 (d) 8 pm Hz 1/2 z = 2 (e) 8 pm Hz 1/2 z = 6 (f) 8 pm Hz 1/2 z = 10 LISA z = σ 150 M ( ) ( ) ( ) M σ

17 1 75 ( ) km/s 2000 km/s ( ) [105] [ ] MHD [ ] [ ] 6 MHD ( ) ( ) z = 0 2

18 z = 0 z = 0 6 ( z = 0 1 ) ( 7) IMRI

19 1期 龚雪飞 等 空间激光干涉引力波探测与早期宇宙结构形成 图7 图8 77 两种吸积机制下 红移 z = 0 处所观测到的黑洞并合率在不同质量区间随红移的分布 在所实现的宇宙学与天体物理模型下 预研究所建议的空间引力波探测任务设计对宇宙学双黑洞并 合事件的探测率

20 Hz IMRI [85 87] (1) n GC 8 h 3 Mpc 3 n YC 3 h 3 Mpc 3 h = H 0 /(100 km s 1 Mpc 1 ) h = 0.73 n C = 8 h 3 Mpc 3 (2) ν(m, µ, z) M µ a 1, ( ) [83 86] Pau Amaro-Seoane Pau Amaro-Seoane M 1 20 M IMRI 0.1 Ma LISA [86] (1 + z) (3) f(m) = f tot ln M max M min 1 M. M min M max 10 2 M 10 4 M f(m) = 0 f tot f tot = 0.1 [85,87] 10% M 3 1 IMRI

21 M 7 LISA elisa LISA elisa 2 ( 10 ) 3 IMRI km 1 2 pm Hz 1/ km 5 10 pm Hz 1/ LISA ( elisa) pm LISA Hz LISA elisa LISA/eLISA

22 80 33 [1] National Research Council. New Worlds, New Horizons in Astronomy and Astrophysics. Washington DC: The National Academies Press, 2010 [2] Ferrarese L, Merritt D. ApJ, 2000, 539: L9 [3] Gebhardt K, et al. ApJ, 2000, 539: L13 [4] Ferrarese L. ApJ, 2002, 578(1): 90 [5] Fan X, et al. ApJ, 2000, 122: 2833 [6] Fan X, et al. ApJ. 2000, 121: 54 [7] Fan X, et al. ApJ. 2004, 128: 515 [8] Madau P, Rees M J. ApJ, 2001, 551: L27 [9] Heger A, Woosley S E. ApJ, 2002, 567: 532 [10] Press W H, Schechter P. ApJ, 1974, 187: 425 [11] Lacey C, Cole S. MNRAS, 1993, 262: 627 [12] Cole S, et al. MNRAS, 2000, 319: 168 [13] Volonteri M, Haardt F, Madau P. ApJ, 2003, 582: 559 [14] Volonteri M, Haardt F, Madau P. ApJ, 2003, 593: 661 [15] Volonteri M, Madau P, Quataert E, et al. ApJ, 2005, 620: 69 [16] Volonteri M, Rees M J. ApJ, 2005, 633: 624 [17] Koushiappas S M, Zentner A R. ApJ, 2006, 639: 7 [18] Koushiappas S M, Bullock J S, Dekel A. MNRAS, 2004, 354: 292 [19] Begelman M C, Volonteri M, Rees M J. MNRAS, 2006, 370: 289 [20] Sathyaprakash B S, Schutz B F. Living Rev. Relativity, 2009, 12: 2 [21] Sesana A, Volonteri M, Haardt F. MNRAS, 2007, 377: 1711 [22] Misner C, Throne K, Wheeler J, eds. Gravitation. San Francisco: W H Freeman and Company [23] Thorne K. in Three Hundred Years of Gravitation. Hawking S K, Israel W, eds. Cambridge: Cambridge University Press, 1978 [24] Weisberg J M, Taylor J H, Fowler L A. Scientific American, 1981, 245: 74 [25] Taylor J H, Weisberg J M. ApJ, 1982, 253: 908 [26] Burgay M, et al. Nature, 2003, 426: 531 [27] Lyne A G, et al. Science, 2004, 303: 1153 [28] Antoniadis J, et al. Science, 2013, 340: 6131 [29] Saulson P R, ed. Fundamentalsa of Interferometric Gravitational Wave De- tectors. World Scientific, 1994 [30] [31] [32] [33] [34] [35] [36] [37] [38] Bender P, Brillet A, Ciufolini I, et al, eds. LISA pre-phase A report. Garching: Max-Planck-Institut fuer Quantenoptic, 1998 [39] LISA Yellow Book. ESA/SRE[2011]3, February 2011 [40],., 2013, 43: 415 [41] NGO Revealing a hidden Universe: opening a new chapter of discovery Assessment Study Report. ESA/SRE(2011)19 December 2011 [42] NGO White Paper: The Gravitational Universe A science theme addressed by the elisa mission observing the entire universe, 2013

23 1 81 [43] [44] Space Science and Technology in China: A Roadmap to 2050, Beijing: Science Press, 2010 [45] Gong X, et al. Class. Quantum Grav., 2011, 27: [46],. ( ), [47] Amaro-Seoane P, et al. elisa: Astrophysics and cosmology in the millihertz regime. Preprint arxiv: v1, 2012 [48] Amaro-Seoane P, et al. Low-frequency gravitational-wave science with elisa/ngo. Preprint arxiv: v1, 2012 [49] Marsh T R. Class. Quantum Grav., 2011, 28(9): [50] Nelemans G, et al. A&A, 2011, 368: 939 [51] Bender P L, Hils D. Class. Quantum Grav., 1997, 14: 1439 [52] Farmer A J, Phinney E S. MNRAS, 2003, 346: 1197 [53] Babak S, et al. Class. Quantum Grav., 2010, 27: [54] Baker J G, et al. Bulletin of the American Astronomical Society, 2010, 42: 574 [55] Blaut A, Babak S, Kr lak A. Phys. Rev. D, 2010, 81: [56] Berti E, Volonteri M. ApJ, 2008, 684: 822 [57] Alberto Sesana, Jonathan Gair, Emanuele Berti, et al. Phys. Rev. D, 2011, 83: [58] Jonathan R Gair, et al. Class. Quantum Grav., 2011, 28: [59] Bender P L, Begelman M C, Gair J R. Talk presented at the 8th International LISA Symposium. Stanford University: California, 2010 [60] Bender P L. Class. Quantum Grav., 2004, 21: S1203 [61] Bender P L, Begelman M C, eds. Trends in Space Science and Cosmic Vision (ESA SP-588) Noordwijk: ESA Publications Division, 2005: 33 [62] Amaro-Seoane P, et al. Class. Quantum Grav., 2007, 24: 113 [63] Miller M C, Freitag M, Hamilton D P, et al. ApJ, 2005, 631: L117 [64] Levin Y. MNRAS, 2007, 374: 515 [65] Hopman C. Class. Quantum Grav., 2009, 26: [66] Preto M, Amaro-Seoane P. ApJ, 2010, 708: L42 [67] Merritt D, Alexander T, Mikkola S, et al. Phys. Rev. D, 2011, 84: [68] Ryan F D. Phys. Rev. D, 1995, 52: 5707 [69] Ryan F D. Phys. Rev. D, 1997, 56: 1845 [70] Barack L, Cutler C. Phys. Rev. D, 2007, 75: [71] Finn L S, Thorne K S. Phys. Rev. D, 2000, 6212: [72] Drasco S. Class. Quantum Grav., 2006, 23: 769 [73] Cornish N J. Class. Quantum Grav., 2011, 28: [74] Gair J R, Porter E, Babak S, et al. Class. Quantum Grav., 2008, 25: [75] Babak S, et al. Class. Quantum Grav., 2010, 27: [76] Drasco S, Hughes S A. Phys. Rev. D, 2004, 69: [77] Barack L, Cutler C. Phys. Rev. D, 2007, 75: [78] Matsushita S, et al. ApJ, 2000, 545: L107 [79] Van der marel R P. Preprint arxiv:astro-ph/ v2, 2003 [80] Fabbiano G. Science, 2005, 307: 533 [81] Maccarone T J, Kundu A, Zepf S E, et al. Nature, 2007, 445: 183 [82] Portegies Zwart S F, McMillan S L W. ApJ, 2002, 576: 899 [83] Miller M C, Hamilton D P. MNRAS, 2002, 330: 232 [84] Miller M C. ApJ, 2002, 581: 438 [85] Miller M C, Colbert E J M. Int. J. Mod. Phys. D, 2004, 13: 1 [86] Miller M C. ApJ, 2005, 618: 426

24 82 33 [87] Will C M. ApJ, 2004, 611: 1080 [88] Konstantinidis S, Amaro-Seoane P, Kokkotas K D. Investigating the retention of intermediate-mass black holes in star clusters using N-body simulations Preprint arxiv: , 2011 [89] Mandel I, Gair J. Class. Quantum Grav., 2009, 26: [90] Gair J R, Mandel I, Miller M C, et al. General Relativity and Gravitation, 2011, 43: 485 [91] Huerta E A, Gair J. Phys. Rev. D, 2011, 84: [92] Huerta E A, Gair J, Brown D. Preprint arxiv: v2, 2011 [93] Lousto C O, Zlochower Y. Phys. Rev. D, 2009, 79: [94] Gonzalez J A, Sperhake U, Brugmann B. Phys. Rev. D, 2009, 79: [95] Lousto C O, Nakano H, Zlochower Y, et al. Phys. Rev. Lett., 2010, 104: [96] Lousto C O, Zlochower Y. Phys. Rev. Lett., 2011, 106: [97] Lousto C, Nakano H, Ziochower Y, et al. Phys. Rev. D, 2010, 82: [98] Han W, Cao Z. Phys. Rev. D, 2011, 84: [99] Binsetruy P, Bohse A, Caprini C, et al. Cosmology Astropart. Phys., : 027 [100] Phinney S, et al, eds. The Big Bang Observer: direct detection of gravita- tional waves from the birth of the Universe to the present. NASA Mission Concept Study, 2004 [101] Crowder J, Cornish N. Phys. Rev. D, 2005, 72: [102] Seto N, Kawamura S, Nakamura T. Phys. Rev. Lett., 2011, 87: [103] Asto S, et al. Jour. of Physics: Conf. Series, 2008, 120: [104] Ando M, et al. Class. Quantum Grav., 2011, 27: [105] Shakura N I, Sunyaev R A. A&A, 1973, 24: 337 [106] King A R, et al. MNRAS, 2005, 363: 49 [107] King A R, Pringle J E. MNRAS, 2006, 373(1): L90 [108] King A R, Pringle J E, Hofmann J A. MNRAS, 2008, 385(3): 1621 [109] Lodato G, Pringle J E. MNRAS, (3): 1196 [110] Gammie C F, Shapiro S L, McKinney J C. ApJ, 2004, 602(1): 312 [111] Shapiro S L. ApJ, 2005, 620(1): 59 [112] Croom S M, et al. MNRAS, 2004, 349(4): 1397 [113] Yuan Y F. Astrophysics of Compact Objects. US: AIP, 2011: 369 [114],. :, 2012, 42: 1256 [115] Ajith P, et al. Phys. Rev. D, 2008, 77: [116] Ajith P, et al. Preprint arxiv: , 2009 Laser Interferometric Gravitational Wave Detection in Space and Structure Formation in the Early Universe GONG Xue-fei 1, XU Sheng-nian 1, YUAN Ye-fei 2, BAI Shan 3, BIAN Xing 1,4, CAO Zhou-jian 1,4,5,6, CHEN Ge-rui 7, DONG Peng 1,8, GAO Tian-shu 9, GAO Wei 1,4, HUANG Shuang-lin 9, LIU Ying 4,10, LUO Zi-ren 11, SHAO Ming-xue 8,12, SUN Bao-san 8,13, TANG Wen-lin 1,4, Yu Pin 14, XU Peng 8,15, ZANG Yun-long 1,4, ZHANG Hai-peng 9, LAU Yun-kau 1,4,5,6,8 (1. Academy of Mathematics and Systems Science, Chinese Academy of Sciences, Beijing , China; 2. University of Science and Technology of China, Department of Astronomy, Hefei ,

25 1 83 China; 3. Theoretisch-Physikalisches Institut, Friedrich-Schiller-Universität Jena, D Jena, Germany; 4. University of Chinese Academy of Sciences, Beijing , China; 5. State Key Laboratory of Scientific and Engineering Computing, Academy of Mathematics and Systems Science, Chinese Academy of Sciences, Beijing , China; 6. State Key Laboratory of Theoretical Physics, Institute of Theoretical Physics, Chinese Academy of Sciences, Beijing , China; 7. Beijing University of Technology, College of Applied Sciences, Beijing , China; 8. Morningside Center of Mathematics, Chinese Academy of Sciences, Beijing , China; 9. Capital Normal University, Beijing , China; 10. Henan University, Department of Mathematics, Kaifeng , China; 11. Institute of Mechanics, Chinese Academy of Sciences, Beijing , China; 12. Henan Polytechnic University, Jiaozuo, Henan , China; 13. Huazhong University of Science and Technology, School of Physics, Wuhan , China; 14. Tshinghua University, Mathematical Sciences Center, Beijing , China; 15. Institute of Theoretical Physics, Chinese Academy of Sciences, Beijing , China) Abstract: In this article, we report on the feasibility study of gravitational wave detection in space commissioned by the Chinese Academy of Sciences. We consider the relative merits between scientific significance and viability in technologies of a few representative mission options. The primary science driver is targeted at the detection of mergers of intermediate to super massive binary black holes in the structure assembly history as well as in dense stellar environments within our local Universe. By striking a balance between science and technological feasibility, a preliminary mission design is put forward for future Chinese gravitational wave detection mission alternative to elisa. Our study indicates that, with suitable design of baseline parameters of a mission, gravitational wave detection in space holds the promise of being a new observation window to the structure formation stage at early Universe and shed light on certain outstanding issues, among which are the evolution of PopIII stars after the dark age, the co-evolution of galaxies and their central black holes, etc. Key words: gravitational wave; ΛCDM hierarchical structure formation picture; intermediate mass black hole; binary black hole coalescence