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Galaxy Co-Evolution with Black Holes Dark Energy and Gravitational-Wave (GW) Detection

Galaxy Co-Evolution with Black Holes Dark Energy and Gravitational-Wave (GW) Detection. 倪维斗 W.-T. Ni Center for Gravitation and Cosmology Department of Physics, National Tsing Hua University, Hsinchu and Shanghai United Center for Astrophysics, Shanghai Normal University, Shanghai

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Galaxy Co-Evolution with Black Holes Dark Energy and Gravitational-Wave (GW) Detection

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  1. Galaxy Co-Evolution with Black Holes Dark Energy and Gravitational-Wave(GW) Detection 倪维斗W.-T. Ni Center for Gravitation and Cosmology Department of Physics, National Tsing Hua University, Hsinchu and Shanghai United Center for Astrophysics, Shanghai Normal University, Shanghai weitou@gmail.com Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  2. Outline • Introduction–GWDetection • Black hole co-evolution with galaxies • Pulsar timing arrays (PTA’s) as very low frequency GW detectors • Space GW detectors LISA, ASTROD-GW, DECIGO, Big Bang Observer • DarkEnergy,Inflation,Discussion and outlook Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  3. Gravitational Wave Detection • Explore fundamental physics and cosmology； • As a tool to study Astronomy and Astrophysics Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  4. The effect of a plus-polarized/cross-polarized gravitational wave on a ring of particles plus-polarized cross-polarized Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  5. Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  6. Complete GW Classificationhttp://astrod.wikispaces.com/file/view/GW-classification.pdf (Modern Physics Letters A 25 [2010] pp. 922-935; arXiv:1003.3899v1 [astro-ph.CO]) Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  7. 0.1mHz-1 Hz ~10Hz-kHz Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  8. LIGO staff installing a mode-matching mirror and suspension into a vacuum chamber during the construction of LIGO Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  9. LIGO instrumental sensitivity for science runs S1 (2002) to S5 (present) in units of gravitational-wave strain per Hz1/2 as a function of frequency Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  10. Experimental Layout of LFF Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  11. Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  12. In addition to adLIGO and adVirgo, LCGT construction started this yearLedbyICRR(KajitaandKuroda) ChineseParticipants TsingHuaU. W-TNi,H-HMei CMS,ITRI S-sPan,S-RChen BeijingN.U. ZZhu TsinghuaU. JCao USTC YZhang ShanghaiN.U. W-TNi,PXi, XZhai Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  13. Second Generation Detectors • AdLIGO 10 times enhancement in strain sensitivity  10 times reach in distance  1000 times in volume (2015+) GW detection from ns-ns merging: 1 per 10-20 yrs  50-100 per year • AdVIRGO (2015+) • LCGT (Started construction, June, 2010) • AIGO, INDIGO  meeting in Perth, Feb. 2010 meeting in Delhi, Feb. 2011 Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  14. Complete GW Classification (I) • Ultra high frequency band (above 1 THz): Detection methods include Terahertz resonators, optical resonators, and ingenious methods to be invented. • Very high frequency band (100 kHz – 1 THz): Microwave resonator/wave guide detectors, optical interferometers and Gaussian beam detectors are sensitive to this band. • High frequency band (10 Hz – 100 kHz): Low-temperature resonators and laser-interferometric ground detectors are most sensitive to this band. • Middle frequency band (0.1 Hz – 10 Hz): Space interferometric detectors of short armlength (1000-100000 km). • Low frequency band (100 nHz – 0.1 Hz): Laser-interferometer space detectors are most sensitive to this band. Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  15. Complete GW Classification (II) • Very low frequency band (300 pHz – 100 nHz): Pulsar timing observations are most sensitive to this band. • Ultra low frequency band (10 fHz – 300 pHz): Astrometry of quasar proper motions are most sensitive to this band. • Extremely low (Hubble) frequency band（1 aHz – 10 fHz): Cosmic microwave background experiments are most sensitive to this band. • Beyond Hubble frequency band (below 1 aHz): Inflationary cosmological models give strengths of GWs in this band. They may be verified indirectly through the verifications of inflationary cosmological models. Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  16. ASTROD-GW has the best sensitivity in the 100 nHz – 1 mHz band and fills the gap ASTROD-GW Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  17. FAST IJMPD,inpress,2011 Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  18. Figure New demonstrator with complete mechanisms at Miyun station. Figure Sketch of the cabin suspension system. Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  19. GuoShou-JinTelescope(LAMOST)andGuoShou-Jin:Shou-ShiLi,1280NathanSivin:GrantingtheSeasons,Springer2009GuoShou-JinTelescope(LAMOST)andGuoShou-Jin:Shou-ShiLi,1280NathanSivin:GrantingtheSeasons,Springer2009 Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  20. Massive Black Hole Systems: Massive BH Mergers &Extreme Mass Ratio Mergers (EMRIs) Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  21. Nature, Jan. 20, 2011 Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  22. LISA LISA consists of a fleet of 3 spacecraft 20º behind earth in solar orbit keeping a triangular configuration of nearly equal sides (5 × 106 km). Mapping the space-time outside super-massive black holes by measuring the capture of compact objects set the LISA requirement sensitivity between 10-2-10-3 Hz. To measure the properties of massive black hole binaries also requires good sensitivity down at least to 10-4 Hz. (2020) Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  23. Primordial Black Holes • Planck Mass BHs (formed at the Planck epoch) to solar mass (M⊙) BHs (formed at the QCD phase transition) up to 105M⊙ BHs • Physical or Astrophysical Constraints (i) BH mass < 5 x 1014 g: already evaporated due to Hawking radiation; (ii) BH mass about 1015 g: contribution to matter density less than 10-8 (constraints from diffuse gamma ray background; (iii) BH mass below about 103 (constraints from microlensing and CMB distorsions) Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  24. Remnants of massive single stars as a function of initial metallicity (y-axis; qualitatively) and initial mass (x-axis) Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  25. BH Coevolution with galaxies • S. Sesana, A. Vecchio and C. N. Colacino, Mon. Not. R. Astron. Soc.390, 192-209 (2008). • S. Sesana, A. Vecchio and M. Volonteri, Mon. Not. R. Astron. Soc.394, 2255-2265 (2009). Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  26. Models of formation of massive black hole binary systems (1) • (i) the VHM model (Volonteri, Haardt & Madau 2003), • (ii) the KBD model (Koushiappas, Bullock & Dekel 2004), • (iii) the BVRhf model (Begelman, Volonteri & Rees 2006) and • (iv) the VHMhopk model. • In these scenarios, seed black holes are massive (M ∼ 104 M⊙) as in the case of KBD and BVRhf, or light (M ∼ 102 M⊙), as prescribed by VHM; seed black holes are abundant (VHM, KBD) or just a few (BVRhf). • The VHMhopk model assumes essentially the same assembly history of the VHM model, but with a somewhat different accretion prescription (Volonteri, Salvaterra & Haardt 2006). Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  27. Models of formation of massive black hole binary systems (2) • the merger hierarchy of 220 dark matter halos in the mass range 1011 − 1015 M⊙ up to z = 20 (Volonteri, Haardt & Madau 2003), then populating the halos with seed black holes and following their evolution to the present time. • For each of the 220 halos all the coalescence events happening during the cosmic history are collected. The outputs are then weighted using the EPS (Extended Press-Schechter) halo mass function and integrated over the observable volume shell at every redshift to obtain numerically the coalescence rate of MBHBs as a function of black hole masses and redshift. • the outcome of this procedure is the numerical distribution d3N/dzdMdt. Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  28. Characteristic GW amplitude hc from massive black hole binaries, the thick line shows hc produced in a specific Monte-Carlo realization. (thin line) the prediction yielded by the semi-analytical approach. The observation time is T = 5 yr Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  29. A candidate sub-parsec supermassive binary blackhole system (Nature 2009) Todd A. Boroson & Tod R. Lauer (dubious from more recent GMRT observation) • quasar SDSS J153636.221 044127.0 separated in velocity by 3,500 km/s. • A binary system of two black holes, having masses of 10^7.3 and 10^8.9 solar masses • Separated by 0.1 parsec with an orbital period of 100 years. Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  30. Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  31. LISA LISA consists of a fleet of 3 spacecraft 20º behind earth in solar orbit keeping a triangular configuration of nearly equal sides (5 × 106 km). Mapping the space-time outside super-massive black holes by measuring the capture of compact objects set the LISA requirement sensitivity between 10-2-10-3 Hz. To measure the properties of massive black hole binaries also requires good sensitivity down at least to 10-4 Hz. (2020) Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  32. One Science Goal of LISA Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  33. Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  34. Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  35. Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  36. LISA Instrument & Sciencecraft Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  37. LISA Pathfinder • Paul McNamara for the LPF Team • LISA Pathfinder Project Scientist • GWADW • 10th - 15th May 2009 Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  38. Drag-free AOC requirements • Atmospheric (terrestrial) air column exclude a resolution of better than 1 mm • This reduces demands on drag-free AOC by orders of magnitude • Nevertheless, drag-free AOC is needed for geodesic orbit integration. Thruster requirements Proof mass-S/C coupling Control loopgain Thrust noise Proof mass Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  39. LISA Pathfinder in Assembly Clean Room Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  40. Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  41. Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  42. Complete GW Classificationhttp://astrod.wikispaces.com/file/view/GW-classification.pdf (Modern Physics Letters A 25 [2010] pp. 922-935; arXiv:1003.3899v1 [astro-ph.CO]) Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  43. Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  44. NANOGrav and PTA expectations Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  45. Demorest et al white paper Summary • Given sufficient resources, we expect to detect GWs through the IPTA within the next five years. • We also expect to gain new astrophysical insight on the detected sources and, for the first time, characterize the universe in this completely new regime. • The international effort is well on its way to achieving its goals. With sustained effort, and sufficient resources, this work is poised to offer a new window into the Universe by 2020. Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  46. probing the black hole co-evolution with galaxies Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  47. ASTROD-GW has the best sensitivity in the 100 nHz – 1 mHz band and fills the gap ASTROD-GW Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  48. S/C 1 (L4) 60 地球 (L3) S/C 2 L1 L2 60 S/C 3 (L5) ASTROD-GW Mission Orbit • Considering the requirement for optimizing GW detection while keeping the armlength, mission orbit design uses nearly equal arms. • 3 S/C are near Sun-Earth Lagrange points L3、L4、L5，forming a nearly equilateral trianglewith armlength260 million km（1.732AU）. • 3 S/C ranging interferometrically to each other. Earth Sun Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  49. Weak-Light Phase Locking • To 2pWA.-C. Liao, W.-T. Ni and J.-T. Shy, On the study of weak-light phase-locking for laser astrodynamical missions, Publications of the Yunnan Observatory 2002, 88-100 (2002). • To 40 fWG. J. Dick, M., D. Strekalov, K. Birnbaum, and N. Yu, IPN Progress Report42-175 (2008). Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

  50. Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni

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