1. Quantum vacuum in cosmology

2. What is the vacuum in cosmology ?

3. Vacuum in cosmology state of the Universe in absence of matter and radiation ? state of the Universe in absence of matter and radiation ? gravity + scalar field gravity + scalar field characterized by mean fields and fluctuations characterized by mean fields and fluctuations no time translation invariance no time translation invariance no conserved energy, state of minimal energy not meaningful no conserved energy, state of minimal energy not meaningful attractor of time evolution attractor of time evolution

4. vacuum in cosmology = (space averaged ) state of Universe vacuum is quantum object and not “empty” vacuum is quantum object and not “empty”

5. Three questions Can we observe quantum vacuum properties in cosmology ? Can we compute quantum vacuum properties in gravity ? What is the role of scale symmetry and its spontaneous breaking ? What is the role of scale symmetry and its spontaneous breaking ?

6. Does inflation allow us to observe quantum vacuum properties ?

7. correlation function for different initial conditions correlation function for different initial conditions u = k η no loss of memory at horizon crossing at horizon crossing ( u = -1 )

8. inflation processes fluctuations fluctuations are not “ generated “ during inflation fluctuations are not “ generated “ during inflation every statistical system has fluctuations every statistical system has fluctuations fluctuations already present at “beginning” of inflation ( or at extremely early stages if inflation lasts from the infinite past ) fluctuations already present at “beginning” of inflation ( or at extremely early stages if inflation lasts from the infinite past ) fluctuations get processed by scale violating effects from inflaton potential near horizon crossing fluctuations get processed by scale violating effects from inflaton potential near horizon crossing

9. memory of initial spectrum

10. equilibration ? for interacting theories : there could be processes that bring arbitrary initial fluctuations close to universal form for interacting theories : there could be processes that bring arbitrary initial fluctuations close to universal form no such loss of memory found within present approximations no such loss of memory found within present approximations equilibration time will be very long since interactions are tiny equilibration time will be very long since interactions are tiny

11. scalar correlation function

12. correlation function from quantum effective action no operators needed no operators needed no explicit construction of vacuum state no explicit construction of vacuum state no distinction between quantum and classical fluctuations no distinction between quantum and classical fluctuations one relevant quantity : correlation function one relevant quantity : correlation function

13. quantum theory as functional integral background geometry given by vierbein or metric homogeneous and isotropic cosmology M:E:

14. quantum effective action quantum effective action exact field equation exact propagator equation

15. correlation function and quantum effective action

16. propagator equation for interacting scalar field in homogeneous and isotropic cosmology G

17. general solution and mode functions

18. Bunch – Davies vacuum α = 1, ζ = 0 for all k

19. initial conditions β 2 + γ 2 = 4 ζ ζ* mixed state : positive probabilities p i

20. absence of loss of memory of initial correlations each k-mode has three each k-mode has three free integration constants !

21. memory of initial spectrum α = 1 + A p example : spectral index :

22. predictivity of inflation ? initial spectrum at beginning of inflation : gets only processed by inflaton potential initial spectrum at beginning of inflation : gets only processed by inflaton potential small tilt in initial spectrum is not distinguishable from small scale violation due to inflaton potential small tilt in initial spectrum is not distinguishable from small scale violation due to inflaton potential long duration of inflation before horizon crossing of observable modes : one sees UV-tail of initial spectrum. long duration of inflation before horizon crossing of observable modes : one sees UV-tail of initial spectrum. If flat, predictivity retained ! If flat, predictivity retained !

23. vacuum in cosmology simply the ( averaged ) state of the Universe result of time evolution minimal “particle number” ? depends on definition of particle number as observable

24. Can we compute the vacuum for gravity ?

25. Can we compute the quantum effective action ?

26. Functional renormalization : Exact renormalization group equation M.Reuter+… for gravity

27. flowing action Wikipedia

28. asymptotic safety for gravity ? S. Weinberg, M. Reuter, …

29. Dilaton quantum gravity Functional renormalization flow, with truncation :

30. Functional renormalization equations Percacci, Narain

31. Fixed point for large scalar field This fixed point describes already realistic gravity ! Limit k → 0 can be taken !

32. Fixed point for large scalar field

33. Vicinity of fixed point solution : Cosmology with dynamical dark energy ! Cosmological constant vanishes asymptotically !

34. asymptotically vanishing cosmological „constant“ What matters : Ratio of potential divided by fourth power of Planck mass What matters : Ratio of potential divided by fourth power of Planck mass vanishes for χ → ∞ ! vanishes for χ → ∞ ! similar for mass term :

35. How well motivated are guesses on the “natural value” of the cosmological constant ?

36. Quantum fluctuations induce cosmological constant

37. Same argument leads to very different physical effects when applied in different frames V / M 4 or

38. small dimensionless number ? needs two intrinsic mass scales needs two intrinsic mass scales V and M ( cosmological constant and Planck mass ) V and M ( cosmological constant and Planck mass ) variable Planck mass moving to infinity, with fixed V: ratio vanishes asymptotically ! variable Planck mass moving to infinity, with fixed V: ratio vanishes asymptotically !

39. How well motivated are guesses on the “natural values” of masses and couplings ?

40. properties of fixed points will not be seen by naïve order of magnitude estimates

41. Scale symmetry and its spontaneous breaking

42. Crossover in quantum gravity

43. Approximate scale symmetry near fixed points UV : approximate scale invariance of primordial fluctuation spectrum from inflation cosmon is pseudo Goldstone boson of IR : cosmon is pseudo Goldstone boson of spontaneously broken scale symmetry, spontaneously broken scale symmetry, tiny mass, tiny mass, responsible for dynamical Dark Energy

44. Asymptotic safety if UV fixed point exists : quantum gravity is non-perturbatively renormalizable ! S. Weinberg, M. Reuter

45. Quantum scale symmetry quantum fluctuations violate scale symmetry quantum fluctuations violate scale symmetry running dimensionless couplings running dimensionless couplings at fixed points, scale symmetry is exact ! at fixed points, scale symmetry is exact ! scale symmetry includes gravity ( different from approximate scale symmetry of particle physics with fixed Planck mass ) scale symmetry includes gravity ( different from approximate scale symmetry of particle physics with fixed Planck mass )

46. Cosmological solution : crossover from UV to IR fixed point Dimensionless functions Dimensionless functions depend only on ratio μ/χ. depend only on ratio μ/χ. IR: μ→0, χ→∞ IR: μ→0, χ→∞ UV: μ→∞, χ→0 UV: μ→∞, χ→0 Cosmology makes crossover between fixed points by variation of χ.

47. Variable Gravity quantum effective action, variation yields field equations

48. Variable Gravity Variable Gravity Scalar field coupled to gravity Scalar field coupled to gravity Effective Planck mass depends on scalar field Effective Planck mass depends on scalar field Simple quadratic scalar potential involves intrinsic mass μ Simple quadratic scalar potential involves intrinsic mass μ Nucleon and electron mass proportional to dynamical Planck mass Nucleon and electron mass proportional to dynamical Planck mass Neutrino mass has different dependence on scalar field Neutrino mass has different dependence on scalar field

49. Kinetial B : Crossover between two fixed points m : scale of crossover can be exponentially larger than intrinsic scale μ running coupling obeys flow equation

50. Cosmological solution scalar field χ vanishes in the infinite past scalar field χ vanishes in the infinite past scalar field χ diverges in the infinite future scalar field χ diverges in the infinite future

51. Sonntagszeitung Zürich, Laukenmann Strange evolution of Universe

52. Model is compatible with present observations Together with variation of neutrino mass over electron mass in present cosmological epoch : model is compatible with all present observations

53. Do we know that the Universe expands ? instead of redshift due to expansion : smaller frequencies have been emitted in the past, because electron mass was smaller ! smaller frequencies have been emitted in the past, because electron mass was smaller !

54. What is increasing ? Ratio of distance between galaxies over size of atoms ! atom size constant : expanding geometry alternative : shrinking size of atoms

55. conclusions from variable gravity Big bang singularity is artefact Big bang singularity is artefact of inappropriate choice of field variables – of inappropriate choice of field variables – no physical singularity no physical singularity Quantum gravity is obervable in Quantum gravity is obervable in dynamics of present Universe dynamics of present Universe

56. No tiny dimensionless parameters ( except gauge hierarchy ) one mass scale one mass scale one time scale μ -1 = 10 10 yr one time scale μ -1 = 10 10 yr Planck mass does not appear as parameter Planck mass does not appear as parameter Planck mass grows large dynamically Planck mass grows large dynamically μ = 2  10 -33 eV

57. Slow Universe Asymptotic solution in freeze frame : Expansion or shrinking always slow, characteristic time scale of the order of the age of the characteristic time scale of the order of the age of the Universe : t ch ~ μ -1 ~ 10 billion years ! Universe : t ch ~ μ -1 ~ 10 billion years ! Hubble parameter of the order of present Hubble parameter for all times, including inflation and big bang ! parameter for all times, including inflation and big bang ! Slow increase of particle masses ! μ = 2  10 -33 eV

58. asymptotically vanishing cosmological „constant“ What matters : Ratio of potential divided by fourth power of Planck mass What matters : Ratio of potential divided by fourth power of Planck mass vanishes for χ → ∞ ! vanishes for χ → ∞ !

59. Quintessence Dynamical dark energy, Dynamical dark energy, generated by scalar field (cosmon ) generated by scalar field (cosmon ) C.Wetterich,Nucl.Phys.B302(1988)668, 24.9.87 P.J.E.Peebles,B.Ratra,ApJ.Lett.325(1988)L17, 20.10.87

60. Prediction : homogeneous dark energy influences recent cosmology - of same order as dark matter - Original models do not fit the present observations …. modifications …. modifications ( different growth of neutrino mass ) ( different growth of neutrino mass )

61. Cosmon inflation Unified picture of inflation and dynamical dark energy Cosmon and inflaton are the same scalar field

62. Anomalous dimension determines spectrum of primordial fluctuations

63. relation between n and r r = 8.19 ( 1 – n ) - 0.1365

64. Compatibility with observations and possible tests Realistic inflation model: Realistic inflation model: n = 0.97, r = 0.1 n = 0.97, r = 0.1 Almost same prediction for radiation, matter, and Dark Energy domination as Λ CDM Almost same prediction for radiation, matter, and Dark Energy domination as Λ CDM Presence of small fraction of Early Dark Energy Presence of small fraction of Early Dark Energy Large neutrino lumps Large neutrino lumps

65. Second stage of crossover from SM to IR from SM to IR in sector Beyond Standard Model in sector Beyond Standard Model affects neutrino masses first ( seesaw or cascade mechanism ) affects neutrino masses first ( seesaw or cascade mechanism )

66. Varying particle masses at onset of second crossover All particle masses except for neutrinos are proportional to χ. All particle masses except for neutrinos are proportional to χ. Ratios of particle masses remain constant. Ratios of particle masses remain constant. Compatibility with observational bounds on time dependence of particle mass ratios. Compatibility with observational bounds on time dependence of particle mass ratios. Neutrino masses show stronger increase with χ, such that ratio neutrino mass over electron mass grows. Neutrino masses show stronger increase with χ, such that ratio neutrino mass over electron mass grows.

67. connection between dark energy and neutrino properties present equation of state given by neutrino mass ! present dark energy density given by neutrino mass = 1.27 L.Amendola, M.Baldi, …

68. Oscillating neutrino lumps Y.Ayaita, M.Weber,… Ayaita, Baldi, Fuehrer, Puchwein,…

69. Evolution of dark energy similar to ΛCDM

70. Simplicity simple description of all cosmological epochs natural incorporation of Dark Energy : inflation inflation Early Dark Energy Early Dark Energy present Dark Energy dominated epoch present Dark Energy dominated epoch

71. conclusions crossover in quantum gravity is reflected in crossover in cosmology crossover in quantum gravity is reflected in crossover in cosmology quantum gravity becomes testable by cosmology quantum gravity becomes testable by cosmology quantum gravity plays a role not only for primordial cosmology quantum gravity plays a role not only for primordial cosmology crossover scenario explains different cosmological epochs crossover scenario explains different cosmological epochs simple model is compatible with present observations simple model is compatible with present observations no more parameters than ΛCDM : tests possible no more parameters than ΛCDM : tests possible

72. end

73. conclusions (2) Variable gravity cosmologies can give a simple and realistic description of Universe Variable gravity cosmologies can give a simple and realistic description of Universe Compatible with tests of equivalence principle and bounds on variation of fundamental couplings if nucleon and electron masses are proportional to variable Planck mass Compatible with tests of equivalence principle and bounds on variation of fundamental couplings if nucleon and electron masses are proportional to variable Planck mass Different cosmon dependence of neutrino mass can explain why Universe makes a transition to Dark Energy domination now Different cosmon dependence of neutrino mass can explain why Universe makes a transition to Dark Energy domination now characteristic signal : neutrino lumps characteristic signal : neutrino lumps

74. propagator equation in homogeneous and isotropic cosmology η > η’ : G > = G s + G a

75. evolution equation for equal time correlation function massless scalar in de Sitter space : u = k η

76. Amplitude of density fluctuations small because of logarithmic running near UV fixed point ! N : number of e – foldings at horizon crossing

77. Einstein frame Weyl scaling maps variable gravity model to Universe with fixed masses and standard expansion history. Weyl scaling maps variable gravity model to Universe with fixed masses and standard expansion history. Standard gravity coupled to scalar field. Standard gravity coupled to scalar field. Only neutrino masses are growing. Only neutrino masses are growing.

78. Einstein frame Weyl scaling : Weyl scaling : effective action in Einstein frame :

79. Field relativity : different pictures of cosmology same physical content can be described by different pictures same physical content can be described by different pictures related by field – redefinitions, e.g. Weyl scaling, conformal scaling of metric related by field – redefinitions, e.g. Weyl scaling, conformal scaling of metric which picture is usefull ? which picture is usefull ?

80. Primordial flat frame Minkowski space in infinite past Minkowski space in infinite past absence of any singularity absence of any singularity geodesic completeness geodesic completeness

81. Eternal Universe solution valid back to the infinite past in physical time no singularity physical time to infinite past is infinite Asymptotic solution in freeze frame :

82. Physical time field equation for scalar field mode determine physical time by counting number of oscillations m=0

83. Big bang singularity in Einstein frame is field singularity ! choice of frame with constant particle masses is not well suited if physical masses go to zero !

84. Origin of mass UV fixed point : scale symmetry unbroken UV fixed point : scale symmetry unbroken all particles are massless all particles are massless IR fixed point : scale symmetry spontaneously broken, IR fixed point : scale symmetry spontaneously broken, massive particles, massless dilaton massive particles, massless dilaton crossover : explicit mass scale μ or m important crossover : explicit mass scale μ or m important SM fixed point : approximate scale symmetry spontaneously broken, massive particles, almost massless cosmon, tiny cosmon potential SM fixed point : approximate scale symmetry spontaneously broken, massive particles, almost massless cosmon, tiny cosmon potential

85. Hot plasma ? Temperature in radiation dominated Universe : T ~ χ ½ smaller than today Temperature in radiation dominated Universe : T ~ χ ½ smaller than today Ratio temperature / particle mass : T /m p ~ χ - ½ larger than today Ratio temperature / particle mass : T /m p ~ χ - ½ larger than today T/m p counts ! This ratio decreases with time. T/m p counts ! This ratio decreases with time. Nucleosynthesis, CMB emission as in standard cosmology ! Nucleosynthesis, CMB emission as in standard cosmology !

86. Infinite past : slow inflation σ = 2 : field equations solution

87. First step of crossover ends inflation induced by crossover in B induced by crossover in B after crossover B changes only very slowly after crossover B changes only very slowly

88. Scaling solutions near SM fixed point ( approximation for constant B ) Different scaling solutions for radiation domination and matter domination

89. Radiation domination Universe shrinks ! K = B - 6 solution exists for B < 1 or K< -5

90. Varying particle masses near SM fixed point All particle masses are proportional to χ. All particle masses are proportional to χ. ( scale symmetry ) ( scale symmetry ) Ratios of particle masses remain constant. Ratios of particle masses remain constant. Compatibility with observational bounds on time dependence of particle mass ratios. Compatibility with observational bounds on time dependence of particle mass ratios.

91. Scaling of particle masses mass of electron or nucleon is proportional to variable Planck mass χ ! effective potential for Higgs doublet h

92. cosmon coupling to matter q χ =-(ρ-3p)/χ F = χ 2

93. Matter domination Universe shrinks ! solution exists for B < 4/3, K = B - 6

94. Early Dark Energy Energy density in radiation increases, proportional to cosmon potential fraction in early dark energy observation requires B < 0.02 ( at CMB emission ) or m

95. Dark Energy domination neutrino masses scale differently from electron mass new scaling solution. not yet reached. at present : transition period

96. Infrared fixed point μ→ 0 μ→ 0 B→ 0 B→ 0 no intrinsic mass scale no intrinsic mass scale scale symmetry scale symmetry

97. Ultraviolet fixed point μ→ ∞ μ→ ∞ kinetial diverges kinetial diverges scale symmetry with anomalous dimension σ scale symmetry with anomalous dimension σ

98. Renormalized field at UV fixed point no mass scale deviation from fixed point vanishes for μ→ ∞ 1 < σ < 2