Grc talk revised
- 1. Observational Constraints on the Primordial Curvature Power Spectrum Dr. Razieh Emami Meibody Prof. George F. Smoot (IAS) Hong Kong University of Science and Technology Nazarbayev University Astana Kazakhstan Paris Center for Cosmological Physics (PCCP) Université Sorbonne Paris Cité - Université Paris Diderot – APC Berkeley Center for Cosmological Physics LBNL & Physics Department University of California， Berkeley Based on : arXiv:1705.09924, R. Emami, George F. Smoot
- 2. CMB TEMPERATURE FLUCTUATION OBSERVATIONS PROVIDE A PRECISE MEASUREMENT OF THE PRIMORDIAL POWER SPECTRUM ON LARGE SCALES, CORRESPONDING TO WAVENUMBERS 10−3 MPC−1 <K< 0.1 MPC−1 LSS: LUMINOUS RED GALAXIES AND GALAXY CLUSTERS PROBE THE MATTER POWER SPECTRUM ON OVERLAPPING SCALES (0.02 MPC−1 <K< 0.7 MPC−1, WHILE THE LYMAN-ALPHA FOREST REACHES SLIGHTLY SMALLER SCALES (0.3 MPC−1 <K< 3 MPC−1; THE PRIMORDIAL POWER SPECTRUM IS NEARLY SCALE-INVARIANT WITH AN AMPLITUDE CLOSE TO 2 × 10−9. STRONGLY SUPPORT INFLATION AND MOTIVATE US TO OBTAIN OBSERVATIONS AND CONSTRAINTS REACHING TO SMALLER SCALES ON THE PRIMORDIAL CURVATURE POWER SPECTRUM AND BY IMPLICATION ON INFLATION. THE CMB & INFLATIONARY COSMOLOGY
- 3. Outline: A quick introduction to Primordial Black Hole (PBH) as the Dark matter, Observational Constraints on the primordial power-spectrum from PBHs, An introduction to Ultra Compact Mini-Halos (UCMH) Observational Constraints on the primordial power-spectrum from UCMH, Constraining the Dark Matter mass fraction for PBHs and UCMHs
- 4. “An Introduction to Primordial Black Holes (PBH)”
- 6. OBSERVATIONAL LIMITS ON COMPACT OBJECTS AS FRACTION OF DARK MATTER N S-CFLH R M ACH O ERO S ER I I D F FI RAS W M AP PBH Log (M/MSun) S. Blinnikov, A. Dolgov, N.K. Poraykoe, and K.Postnov arXiv:1611.00541 fDM
- 7. DARK MATTER MASS FRACTION LIMITS 1016 1026 1036 1046 10- 7 10- 5 0.001 0.100 10- 17 10- 7 103 1013 M/g f M/M⊙ 11 KEG F WD NS ML E WB mLQ LSS WMAP FIRAS DF Primordial Black Holes as Dark Matter arXiv:1607.06077 Bernard Carr, Florian Kuhnel, Marit Sandstad 10 20 50 100 0.001 0.005 0.010 0.050 M/M⊙ 11 f Primoridial Black Holes (PBH) Produced via: Running mass inflation blue and axion-like curvatron red
- 8. Planck Evaporation FL HSC NS EROS CMBanisotropy BBN - 20 - 15 - 10 - 5 0 5 - 10 - 8 - 6 - 4 - 2 0 log10(M/M⊙ ) log10(ρPBH/ρDM) arXiv:1706.03746: Primordial black holes from inflat Bernard Carr, Tommi Tenkanen, Vi
- 9. Planck Evaporation FL WD K HSC NS EROS M WB SegIEriII - 15 - 10 - 5 0 - 3.0 - 2.5 - 2.0 - 1.5 - 1.0 - 0.5 0.0 log10(Mc /M⊙ ) log10fPBH monochromatic arXiv:1705.05567 [ Primordial black hole constraints for extended mass functions Bernard Carr, Martti Raidal, Tommi Tenkanen, Ville Vaskonen, Hardi Veermäe
- 10. - 15 - 10 - 5 0 - 3.0 - 2.5 - 2.0 - 1.5 - 1.0 - 0.5 0.0 log10(Mc /M⊙ ) log10fPBH lognormal, σ=2
- 11. If the density perturbations at the stage of the horizon re-entry exceeds a threshold value, of order one, the gravity on that region will overcome the repulsive pressure and that area would be subjected to collapse and will form PBH. Assuming that at every epoch, the mass of the PBH is a fixed fraction, 𝑓 𝑀, of the horizon mass, we have, Initial abundance of PBHs is given by: (Current) fraction of the mass of Milky Way halo in PBHs:
- 12. For this purpose, we first figure out the observational constraints on the initial abundance of PBH. Then using the following formula, we could calculate the constraints on the primordial power-spectrum:
- 13. Constraints on the initial PBHs abundance, bPBH
- 14. The “Current” constraints on the primordial power-spectrum PBH decay vacuum instability
- 15. The “Futuristic” constraints on the primordial power-spectrum
- 16. “An Introduction to UCMHs” (Ultra Compact Mini-Halo objects)
- 17. UCMHs are dense dark matter structures, which can be formed from the larger over density perturbations right after the matter-radiation equality. Density perturbations of the order though its exact number is scale dependent as we will point it out in what follows, can collapse prior or right after the matter-radiation equality and therefore seed the formation of UCMHs. The Mass fraction of UCMHs is given by:
- 18. As for the PBHs, we first figure out the observational constraints on the initial abundance of UCMHs. Then, using the following formula, we calculate the constraints on the primordial power-spectrum: Unlike to the case of the PBHs, though, the minimal threshold for the over-density may be scale-dependent.
- 19. constraints on the initial UCMHs abundance, 𝛽 𝑈𝐶𝑀𝐻
- 20. The observational constraints on the primordial power-spectrum
- 21. LACK OF UCMH OBJECTS IMPLIES LIMITS ON PBH •LACK OF UCHM OBJECTS OBSERVATIONS IMPLIES STRONG LIMIT ON THE PRIMORDIAL POWER SPECTRUM •IF THE PPS IS GAUSSIAN, THEN ESSENTIALLY NO FLUCTUATIONS OF STRENGTH TO PRODUCE PBH •IN THE RANGE 1 < K < 106 MPC-1 OR IN ABOUT 1 MSUN < MPBH < 1016 MSUN •THE PERTURBATION SPECTRUM WOULD HAVE TO BE NON-GAUSSIAN WITH A TINY FEATURE AT HIGH CURVATURE TO MAKE PBH
- 22. “Combined Constraints on the Primordial Power Spectrum from PBH as well as the UCMHs”
- 24. PBH decay vacuum instability
- 25. Conclusion : Introduced PBH and UCMHs as two examples of compact objects, Presented the observational constraints on the primordial power- spectrum from both of PBHs and UCMHs, Planck mass PBH decay and vacuum instability all leading to constraints on primordial perturbations and thus Inflation Finally, combining the constraints discussed the PBH abundance from the constraints coming from the UCMHs. Thanks so much for your attention!
Editor's Notes
- #8: Constraints on f(M) for a variety of effects including evaporation (magenta), dynamical red, lensing (cyan), large scale structure (green) and accretion (orange) effects associated with PBHs. The effects are extragalactic γ-rays from evaporation (EG) [11], femtolensing of γ-ray bursts (F) [187], white-dwarf explosions (WD) [188], neutron-star capture (NS) [36], Kepler microlensing of stars (K) [189], MACHO/EROS/OGLE microlensing of stars (ML) [27] and quasar microlensing (broken line) (ML) [191], survival of a star cluster in Eridanus II (E) [190], wide-binary disruption (WB) [37], dynamical friction on halo objects (DF) [33], millilensing of quasars (mLQ) [32], generation of large-scale structure through Poisson fluctuations (LSS) [14], and accretion effects (WMAP, FIRAS) [15]. Only the strongest constraint is usually included in each mass range, but the accretion limits are shown with broken lines since they are are highly model-dependent. Where a constraint depends on some extra parameter which is not well-known, we use a typical value. Most constraints cut off at high M due to the incredulity limit. See the original references for more accurate forms of these constraints.
- #10: Constraints from different observations on the fraction of PBH DM, fPBH ≡ ΩPBH/ΩDM, as a function of the PBH mass Mc, assuming a monochromatic mass function. The purple region on the left is excluded by evaporations [8], the red region by femtolensing of gamma-ray bursts (FL) [40], the brown region by neutron star capture (NS) for different values of the dark matter density in the cores of globular clusters [41], the green region by white dwarf explosions (WD) [42], the blue, violet, yellow and purple regions by the microlensing results from Subaru (HSC) [43], Kepler (K) [44], EROS [45] and MACHO (M) [46], respectively. The dark blue, orange, red and green regions on the right are excluded by Planck data [36], survival of stars in Segue I (Seg I) [47] and Eridanus II (Eri II) [48], and the distribution of wide binaries (WB) [49], respectively. The black dashed and solid lines show, respectively, the combined constraint with and without the constraints depicted by the colored dashed lines.