1. Documents pour LISA : LISA Science case Science Requirement Document LISA-France, LAPP, 1er février 2007 Pierre Binétruy http://www.lisa-science.org/resources/talks-articles/science

2. LISA Science Case Goal: present to an educated reader (typically a member of a committee such as BEPAC) the science case of LISA. Contributors and editors: John Baker (GSFC), Pete Bender (U. of Colorado), Pierre Binetruy (APC - Paris), Joan Centrella (GSFC), Teviet Creighton (JPL), Jeff Crowder (JPL), Curt Cutler (JPL), Karsten Danzman (U. of Hannover and A.E.I.), Steve Drasco (JPL), Lee S. Finn (U. of Pennsylvania), Craig Hogan (U. of Washington), Cole Miller (U. of Maryland), Milos Miloslavljevic (U. of Texas, Austin), Gijs Nelemans (Radboud University Nijmegen), Sterl Phinney (Caltech), Tom Prince (Caltech/JPL), Bonny Schumaker (JPL), Bernard Schutz (A.E.I.), Michele Vallisneri (JPL), Marta Volonteri (Univ. of Michigan) and Karen Willacy (JPL).

3. LISA Science Case Goal: present to an educated reader (typically a member of a committee such as BEPAC) the science case of LISA. Contributors and editors: John Baker (GSFC), Pete Bender (U. of Colorado), Pierre Binetruy (APC - Paris), Joan Centrella (GSFC), Teviet Creighton (JPL), Jeff Crowder (JPL), Curt Cutler (JPL), Karsten Danzman (U. of Hannover and A.E.I.), Steve Drasco (JPL), Lee S. Finn (U. of Pennsylvania), Craig Hogan (U. of Washington), Cole Miller (U. of Maryland), Milos Miloslavljevic (U. of Texas, Austin), Gijs Nelemans (Radboud University Nijmegen), Sterl Phinney (Caltech), Tom Prince (Caltech/JPL), Bonny Schumaker (JPL), Bernard Schutz (A.E.I.), Michele Vallisneri (JPL), Marta Volonteri (Univ. of Michigan) and Karen Willacy (JPL).

4. Executive Summary 1.Gravitational Waves: An Overview 2. LISA Mission Overview 3.Black Hole Astrophysics: Massive Black Holes in Galactic Nuclei 4.Black Hole Physics: Confronting General Relativity with Precision Measurements of Strong Gravity 5.Precision Cosmometry and Cosmology 6.Ultra-compact binaries 7.New Physics and the Early Universe 8.LISA and the Key Questions of Astronomy and Physics List of contents

5. Executive Summary 1.Gravitational Waves: An Overview 2. LISA Mission Overview 3.Black Hole Astrophysics: Massive Black Holes in Galactic Nuclei 4.Black Hole Physics: Confronting General Relativity with Precision Measurements of Strong Gravity 5.Precision Cosmometry and Cosmology 6.Ultra-compact binaries 7.New Physics and the Early Universe 8.LISA and the Key Questions of Astronomy and Physics

6. Key science questions When did the massive black holes in galactic nuclei form, and how did they grow? What fraction of proto-galaxies contained massive black holes in their cores, as a function of redshift? What are the mass and spin distributions of the supermassive black holes in galactic nuclei? What is the role of black hole mergers in early hierarchical structure assembly? What are dynamics of stars near massive black holes in galactic nuclei? Key science questions When did the massive black holes in galactic nuclei form, and how did they grow? What fraction of proto-galaxies contained massive black holes in their cores, as a function of redshift? What are the mass and spin distributions of the supermassive black holes in galactic nuclei? What is the role of black hole mergers in early hierarchical structure assembly? What are dynamics of stars near massive black holes in galactic nuclei?

7. 1% duty cycle Characteristic time for BH in AGN to increase their mass by accretion: t ~  Mc 2 / L Edd ~ 4 10 7 (  / 0.1) yr ~ t universe /100 at redshift z ~ 1  efficiency of radiation production  Expect BH present in galaxies are active 1% of the time

8. The coupled evolution of galaxies and their nuclear BH M BH in M  galaxy bulge velocity dispersion  (  depth of gravit. Potential well)

9. Mass density of local BH  BH = 2 to 5 10 5 M  Mpc -3  BH ~ 3.5 10 5 (  / 0.1) -1 M  Mpc -3 Increase in density of BH if total energy in AGN was produced by accretion Most comes from BH of mass between 10 8 and 10 9 M  Supermassive BH growing by accretion? Smaller ones by merger?

10. Growth and merger history of massive black holes Merger rate : 1 per year (10 10 galaxies seen by HST have fossile evidence of a merger since z=1 i.e. 10 10 years)

12. Stellar captures and the dynamics of galactic nuclei EMRI events e.g. diffusion of stars through 2-body collisions  (S/M 2 ) ~ 10 -4

13. Executive Summary 1.Gravitational Waves: An Overview 2. LISA Mission Overview 3.Black Hole Astrophysics: Massive Black Holes in Galactic Nuclei 4.Black Hole Physics: Confronting General Relativity with Precision Measurements of Strong Gravity 5.Precision Cosmometry and Cosmology 6.Ultra-compact binaries 7.New Physics and the Early Universe 8.LISA and the Key Questions of Astronomy and Physics List of contents

14. Key Science Questions Is the strong field gravity correctly described by GR? Are the massive dark central objects in galaxies really black holes? Key Science Questions Is the strong field gravity correctly described by GR? Are the massive dark central objects in galaxies really black holes?

15. M 1 = M 2 = 2 10 5 M , z=5

16. Merger stage S/N

17. EMRI : precision probes of Kerr spacetimes

18. Executive Summary 1.Gravitational Waves: An Overview 2. LISA Mission Overview 3.Black Hole Astrophysics: Massive Black Holes in Galactic Nuclei 4.Black Hole Physics: Confronting General Relativity with Precision Measurements of Strong Gravity 5.Precision Cosmometry and Cosmology 6.Ultra-compact binaries 7.New Physics and the Early Universe 8.LISA and the Key Questions of Astronomy and Physics List of contents

19. Key science questions What is the nature of dark energy? What is the global geometry of the Universe? What is the Hubble constant? Key science questions What is the nature of dark energy? What is the global geometry of the Universe? What is the Hubble constant?

20. Inspiral phase Key parameter : chirp mass M = (m 1 m 2 ) 3/5 (m 1 + m 2 ) 1/5 (z) (1+z)

21. Inspiral phase Key parameter : chirp mass M = (m 1 m 2 ) 3/5 (m 1 + m 2 ) 1/5 (z) (1+z) Binary system : L = -- M R 2 + --  r 2 + G ---- MM r 11 22 R=r1+r2r=r1-r2R=r1+r2r=r1-r2.. Defining r =  1/2 r, the relative motion depnds on the mass only through: ^ M = (  3 M 2 ) 1/5

22. Inspiral phase Key parameter : chirp mass M = (m 1 m 2 ) 3/5 (m 1 + m 2 ) 1/5 (z) (1+z)

23. Inspiral phase Key parameter : chirp mass M = (m 1 m 2 ) 3/5 (m 1 + m 2 ) 1/5 Amplitude of the gravitational wave: h(t) = F (angles) cos  (t) M (z) 5/3 f(t) 2/3 dLdL Luminosity distance frequency f(t) = d  /2  dt (z) (1+z)

24. Inspiral phase Key parameter : chirp mass M = (m 1 m 2 ) 3/5 (m 1 + m 2 ) 1/5 Amplitude of the gravitational wave: h(t) = F (angles) cos  (t) M (z) 5/3 f(t) 2/3 dLdL Luminosity distancepoorly known in the case of LISA  ~ 10 arcmin1 Hz SNRf GW (z) (1+z)

25. z = 1, m 1 = 10 5 M , m 2 = 6.10 5 M   (arcminutes)  d L /d L 3° 5% Holz & Hughes

26. Using the electromagnetic counterpart Allows both a measure of the direction and of the redshift Holz and Hughes  d L /d L 0.5%

27. 3000 supernovae 100 SMBH sources

28. Executive Summary 1.Gravitational Waves: An Overview 2. LISA Mission Overview 3.Black Hole Astrophysics: Massive Black Holes in Galactic Nuclei 4.Black Hole Physics: Confronting General Relativity with Precision Measurements of Strong Gravity 5.Precision Cosmometry and Cosmology 6.Ultra-compact binaries 7.New Physics and the Early Universe 8.LISA and the Key Questions of Astronomy and Physics

29. Key science questions Is general relativity the correct theory of gravitation? Is there a large population of ultra-compact binaries in the Galaxy? How did compact binaries form and what is the outcome of a common-envelope phase? What is the nature of the fundamental physical interactions in compact binaries? How are the compact binaries distributed in the Galaxy and what does that tell us about the formation and evolution of the Galaxy? Key science questions Is general relativity the correct theory of gravitation? Is there a large population of ultra-compact binaries in the Galaxy? How did compact binaries form and what is the outcome of a common-envelope phase? What is the nature of the fundamental physical interactions in compact binaries? How are the compact binaries distributed in the Galaxy and what does that tell us about the formation and evolution of the Galaxy?

30. AM CVn systems Ultra-compact X-ray sources Neutron star binaries resolved WD binaries average WD binary bkgd S/N = 5 S/N = 1 NS WD

31. Several thousands WD binaries individually detected (d< 100 kpc) Several millions unresolved form a background. Period less than 20 minutes

32. Verification binaries

33. Studying the astrophysics of compact binaries using LISA physics of tidal interaction physics of mass-tranfer stability double WD mergers neutron star and BH binaries millisecond X-ray pulsars

34. Executive Summary 1.Gravitational Waves: An Overview 2. LISA Mission Overview 3.Black Hole Astrophysics: Massive Black Holes in Galactic Nuclei 4.Black Hole Physics: Confronting General Relativity with Precision Measurements of Strong Gravity 5.Precision Cosmometry and Cosmology 6.Ultra-compact binaries 7.New Physics and the Early Universe 8.LISA and the Key Questions of Astronomy and Physics

35. Key science questions Is there a first-order phase transition at or beyond TeV energies? Are there extra dimensions at the submillimeter scale? Do stable superstrings exist, and can they be blown up to form cosmic strings? What was the quantum state of the Universe at or before the Big Bang? How did inflation end? Were there violent events in the early Universe that left no relic trace in conventional particles and fields? Key science questions Is there a first-order phase transition at or beyond TeV energies? Are there extra dimensions at the submillimeter scale? Do stable superstrings exist, and can they be blown up to form cosmic strings? What was the quantum state of the Universe at or before the Big Bang? How did inflation end? Were there violent events in the early Universe that left no relic trace in conventional particles and fields?

36. Gravitons of frequency f * produced at temperature T * are observed at a redshifted frequency f = 1.65 10 -7 Hz --- ( ----- ) ( ---- )  1T*T* 1GeV g*g* 100 1/6 At production * =  H * -1 (or f * = H * /  ) Horizon length Wavelength

37. for  =1  GW = --- -------- d  GW d logf cc 1,  c = 3H 0 /(8  G N ) Gravitons produced at the electroweak phase transition would be observed in the LISA window.

38. But are gravitons produced in sufficient numbers at the electroweak phase transition? If the transition is first order, nucleation of true vacuum bubbles inside the false vacuum Collision of bubbles and turbulence  production of gravitational waves

40. 1.Understand the formation of massive black holes 1.1. Search for a population of seed black holes at early epochs. 1.2. Search for remnants of the first (Pop III) stars through observation of intermediate mass black hole captures, also at later epochs. 2. Trace the growth and merger history of massive black holes and their host galaxies 2.1. Determine the relative importance of different black hole growth mechanisms as a function of redshift. 2.2. Determine the merger history of two black holes before the era of the earliest known quasars (z ~ 6). 2.3. Determine the merger history of two black holes at later epochs (z < 6). 3. Explore stellar populations and dynamics in galactic nuclei 3.1. Characterize the immediate environment of MBHs in z < 1 galactic nuclei from EMRI capture signals. 3.2. Study intermediate-mass black holes from their capture signals. 3.3. Improve our understanding of stars and gas in the vicinity of Galactic black holes using coordinated gravitational and electromagnetic observations. Science objectives

41. 4.Survey compact stellar-mass binaries and study the structure of the Galaxy 4.1. Elucidate the formation and evolution of Galactic stellar-mass binaries: constrain the diffuse extragalactic foreground. 4.2. Determine the spatial distribution of stellar mass binaries in the Milky Way and environs. 4.3. Improve our understanding of white dwarfs, their masses, and their interactions in binaries and enable combined gravitational and electromagnetic observations. 5. Confront General Relativity with observations 5.1. Detect gravitational waves directly and measure their properties precisely. 5.2. Test whether the central massive objects in galactic nuclei are the black holes of general relativity. 5.3. Make precision tests of dynamical strong-field gravity. 6.Probe new physics and cosmology with gravitational waves 6.1. Study cosmic expansion history, geometry and dark energy using precise gravitationally calibrated distances in cases where redshifts are measured. 6.2. Measure the spectrum of, or set bounds on, cosmological backgrounds. 6.3. Search for burst events from cosmic string cusps. 7. Search for unforeseen sources of gravitational waves

42. 4.1 Understand the formation and growth of massive black holes 4.2 Trace the birth and evolution of galaxies 4.3 Explore stellar populations and their dynamics in galactic nuclei 4.4 Survey compact stellar-mass binaries and study the morphology of the Galaxy 4.5 Confront general relativity with observations 4.6 Probe the early universe 4.7 Search for new phenomena Science objectives proposed

43. 4.1 Understand the formation of massive black holes 4.2 Trace the growth and merger history of massive black holes and their co-evolution with galaxies 4.3 Explore stellar populations and their dynamics in galactic nuclei 4.4 Survey compact stellar-mass binaries and study the structure of the Galaxy 4.5 Confront general relativity with observations 4.6 Probe the early universe 4.7 Search for new phenomena New science objectives

44. 4.1 Understand the formation of massive black holes 4.1.1. Search for the earliest massive black holes and elucidate their formation mechanism 4.1.2. Search for the remnants of the first (Pop III) star formation through observation of intermediate-mass black hole capture

45. 4.2 Trace the growth and merger history of massive black holes and their co-evolution with galaxies 4.2.1. Determine the relative importance of different growth mechanisms as a function of redshift 4.2.2 Determine the merger history of small black holes (MBHs ~10 4 to 3 10 5 M  ) in the era of formation of the first galaxies (6<z<30) 4.2.3 Determine the merger history of black holes (MBH's 3~10 5 to 10 7 M  ) in established galaxies (z<6)

46. 4.3 Explore stellar populations and their dynamics in galactic nuclei 4.3.1 Characterize the immediate environment of MBHs in z<1 galactic nuclei from EMRI capture signals (was 4.2.1) 4.3.2 Study intermediate-mass black holes, and gather evidence about Pop III star formation, from IMRI capture signals

47. 4.3 Explore stellar populations and dynamics in galactic nuclei 4.3.1 Characterize the immediate environment of MBHs in z<1 galactic nuclei from EMRI capture signals 4.3.2 Study intermediate-mass black holes from their capture signals 4.3.3 Improve our understanding of stars and gas in the vicinity of massive black holes using coordinated gravitational and electromagnetic observations

48. 4.4 Survey compact stellar-mass binaries and study the morphology of the Galaxy 4.4.1 Elucidate the evolutionary history of galactic and extragalactic stellar-mass binaries (was 5.4.2) 4.4.2 Determine the spatial distribution of stellar mass binaries in the Milky Way, satellite galaxies and globular clusters 4.4.3 Improve our understanding of white dwarfs, their masses, and their interactions in binaries using coordinated gravitational and electromagnetic observations (was A&A 5.b)

49. 4.4 Survey compact stellar-mass binaries and study the structure of the Galaxy 4.4.1 Elucidate the formation and evolution of Galactic stellar-mass binaries; constrain the diffuse extragalactic background 4.4.2 Determine the spatial distribution of stellar mass binaries in the Milky Way and environs. 4.4.3 Improve our understanding of white dwarfs, their masses, and their interactions in binaries using coordinated gravitational and electromagnetic observations

50. 4.5 Confront general relativity with observations 4.5.1 Detect gravitational waves directly and explore their properties 4.5.2 Make precision tests of strong-field gravity 4.5.3 Verify that the central massive objects in galactic nuclei are Kerr black holes (was 4.2.2)

51. 4.5 Confront general relativity with observations 4.5.1 Detect gravitational waves directly and measure their properties precisely 4.5.2. Test to high accuracy whether the central massive objects in galactic nuclei are the black holes of general relativity 4.5.3 Make precision tests of dynamical strong-field gravity

52. 4.6 Probe the early universe 4.6.1 Enable studies of the expansion history of the universe using precise gravitationally calibrated distances to objects where a host galaxy has been identified (was A&A5a and P&C3a) 4.6.2 Detect or set bounds on cosmological backgrounds 4.7 Search for new phenomena

53. 4.6 Probe the early universe 4.6.1 Precisely measure gravitationally calibrated luminosity distances for precision cosmology when redshifts can be determined 4.6.2 Detect or set bounds on cosmological backgrounds 4.7 Search for new phenomena

54. Science requirement document

55. Changes of Quantitative Requirements between SRD v3 and ScRD v4i

57. Intermediate frequency requirements No substantial differences between 0.1 and 50 mHz

58. Low frequency requirements v3: Lowest frequency requirement is 0.03 mHz v4i: Lowest frequency requirement is 0.1 mHz 0.03 mHz v3: 2.6 x 10 -16 Hz -1/2 v4i: Goal at 3 x 10 -16 Hz -1/2 0.1 mHz v3: 3.9 x 10 -17 Hz -1/2 v4i: 3.9 x 10 -17 Hz -1/2 Strain sensitivity

59. High frequency requirements v3: Highest frequency requirement is 1 Hz v4i: Highest frequency requirement is 0.05 Hz 50 mHz v3: No requirement v4i: 6.5 x 10 -20 Hz -1/2 100 mHz v3: 7.5 x 10 -20 Hz -1/2 v4i: 8 x 10 -20 Hz -1/2 (calculation needed; discovery potential) 1 Hz v3: 7.5 x 10 -19 Hz -1/2 v4i: Goal : 1.5 x 10 -18 Hz -1/2

60. 4) Arm Configuration v3: 3 arm configuration required v4i: No requirement, rather a goal of 6 links 5) Mission Lifetime Unchanged: Both have 5 year requirement 6) Data Availability v3: 4 days uninterrupted around merger time w/ 2 weeks notice v4i: 4 days uninterrupted around merger time w/ 2 weeks notice 7)Minimum Requirements Unchanged Other Requirements

61. 0.03 mHz 0.1 mHz 0.5 mHz 1.0 mHz 5 mHz 10 mHz 50 mHz 100 mHz 1 Hz v3 2.6 (4) 3.9 (3) 4.3 (2) 3.0 (1) 1.11.3None7.57.5 (1) v4i None3.9 (3) None3.2 (1) 1.11.36.5None Summary Table of Strain Sensitivity (units of 10 -20 Hz -1/2 & e.g. 2.6(4) = 2.6 x 10 4 )