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Primordial Black Holes As a Dark Matter Candidate Primordial black holes as a dark matter candidate Ranjan Laha Theoretical Physics Department, CERN Contents • Primordial black hole introduction • Primordial black hole constraints (a) from evaporation (b) from lensing (c) from gravitational waves (d) from dynamical effects (e) from accretion • Future of primordial black hole detection • Conclusions Ranjan Laha <latexit sha1_base64="Cin7YGCoXXynkKwTRwcOVCyCl3E=">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</latexit> <latexit sha1_base64="Om0WqQlKGr6DbfSSqF7tB4Q5gHE=">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</latexit> Primordial black holes Primordial Black Holes What are primordial black holes? Primordial black holes are exotic compact objects which can form in the early Universe due to large density perturbations (numerous formation models) and/ or due to new physics (Zel’dovich and Novikov PrimordialAstron. Zhu, 1966, HawkingBlack MNRAS Holes 1971, Carr (PBHs) and Hawking could MNRAS 1974, form Chapline in Nat.the 1975 early and many others; Shandera, Jeong, and Gebhardt 1802.08206 PRL and Kouvaris, Tinyakov, and8 Tytgat 1804.06740 PRL ) Universe ( z<latexit sha1_base64="l3bkAcTGOF9hOY91kzgf/vspFVQ=">AAAB8XicbZDLSsNAFIZPvNZ6q7p0M1gEVyURweKq4MZlBXvBNpbJ9CQdOpmEmYlQQ9/CjQtF3Po27nwbp5eFtv4w8PGfc5hz/iAVXBvX/XZWVtfWNzYLW8Xtnd29/dLBYVMnmWLYYIlIVDugGgWX2DDcCGynCmkcCGwFw+tJvfWISvNE3plRin5MI8lDzqix1v0T6UYR8dyHaq9UdivuVGQZvDmUYa56r/TV7Scsi1EaJqjWHc9NjZ9TZTgTOC52M40pZUMaYceipDFqP59uPCan1umTMFH2SUOm7u+JnMZaj+LAdsbUDPRibWL+V+tkJqz6OZdpZlCy2UdhJohJyOR80ucKmREjC5QpbnclbEAVZcaGVLQheIsnL0PzvOJZvr0o167mcRTgGE7gDDy4hBrcQB0awEDCM7zCm6OdF+fd+Zi1rjjzmSP4I+fzB9yCj7E=</latexit> 10 ) from large over-densities 15 t MPBH 10 23 g (for PBHs formed in the early Universe) ⇡ 10− s Mass roughly given✓ by mass◆ inside horizon at time of formation: Primordial black holes can have a wide range[Green of masses & Liddle, andastro-ph/9901268 can form ]the entire dark matter density of the Universe Fig. courtesy: Kavanagh GW4FP 2019 M 17 15 13 11 9 7 5 3 1 1 3 5 10− 10− 10− 10− 10− 10− 10− 10− 10− 10 10 10 30g 57 1018 1020 10122M 1024 2 101026 10kg28 110.301 101032 GeV1034 1036 1038 ⇡ ⇥ ⇡ ⇥ Primordial black holes can have a log-normaleV mass function or a power law mass function1051 10and53 can1055 have10 a57 wide1059 range1061 of spins1063 1065 1067 1069 1071 Ranjan Laha [Zel’dovich & Novikov (1967), Hawking (1971), Carr & Hawking (1974), Carr (1975)] Bradley J. Kavanagh (GRAPPA, Amsterdam) Hearing the sirens of the early Universe: PBHs & GWs 3 Primordial black hole (PBH)dark matter MPBH/M⊙ 10-17 10-15 10-13 10-11 10-9 10-7 10-5 10-3 10-1 101 103 100 SN Kepler Mass range where PBHs can lensing K - form the entire dark matter density MACHO/EROS/OGLE -1 10 SUPER Subaru O2 result INTEGRAL O1 result 10-2 PBH UF dwarf f fPBH = fraction of the dark matter in the form of PBHs Planck 10-3 (collisional ionization) IGRB VOYAGER Global constraints on primordial black hole dark matter Dasgupta, Laha, and Ray 1912.01014 10-4 1015 1016 1017 1018 1019 1020 1021 1022 1023 1024 1025 1026 1027 1028 1029 1030 1031 1032 1033 1034 1035 1036 1037 MPBH [g] Multiple constraints exist over wide range of masses (all of these are not shown for clarity) I will discuss some of these constraints in the following slides (individual references later) Ranjan Laha Microlensing Dynamical effects stars, supernovae, quasars dwarf galaxies, wide binary stars Accretion Evaporation CMB, radio & X-ray Primordialgamma-rays black holes constraints from evaporation Constraints Emission of particles PBH Pic. courtesy: Green 2019 talk Ranjan Laha Effects on stars Mergers white dwarf explosions gravitational waves [Initially all constraints assume a delta-function PBH mass function.] Evaporation of low-mass primordial black holes Black holes evaporate to produce Standard Model particles and can have observable consequences S. W. Hawking, Nature 248 10 (1974) 30–31. Temperature of 10 kg S. W. Hawking,, Commun. Math. the black hole T =1.06 GeV Phys. 43 (1975) 199–220. BH M <latexit sha1_base64="kSiwPun7pNtLwxV3vISsvovV7fI=">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</latexit> ✓ BH ◆ Dimensionless absorption probability Mass of the black hole for the emitted species dN Γ 1 s = s dt dE 2⇡ exp(E/T ) ( 1)2s <latexit sha1_base64="AIIAaVlZMSdpwxKIcVwwxgwOE4A=">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</latexit> Z BH − − Evaporation energy spectrum of Page PRD 16, 8, 2402 – 2411, 1977 particle of spin s<latexit sha1_base64="d0SkknmjHALu9tUEssf1X4Gl4nQ=">AAAB6HicbVDJSgNBEK2JW4xb1KOXxiB4CjMqLregF48JmAWSIfR0apI2PQvdPUII+QIvHhTx6id582/smQyixgcFj/eqqKrnxYIrbdufVmFpeWV1rbhe2tjc2t4p7+61VJRIhk0WiUh2PKpQ8BCbmmuBnVgiDTyBbW98k/rtB5SKR+GdnsToBnQYcp8zqo3UUP1yxa7aGcgicXJSgRz1fvmjN4hYEmComaBKdR071u6USs2ZwFmplyiMKRvTIXYNDWmAyp1mh87IkVEGxI+kqVCTTP05MaWBUpPAM50B1SP110vF/7xuov1Ld8rDONEYsvkiPxFERyT9mgy4RKbFxBDKJDe3EjaikjJtsillIVylOP9+eZG0TqrOafW0cVapXedxFOEADuEYHLiAGtxCHZrAAOERnuHFureerFfrbd5asPKZffgF6/0L922NLg==</latexit> from a non- spinning black hole Low-mass primordial black holes and photons Primordial black holes can evaporate to produce photons The photons can contribute to the cosmic photon background The isotropic gamma-ray background and the cosmic MeV background has been used to constrain the density of primordial black holes The constraint can be derived by either assuming astrophysical contribution(s) to the photon background or by assuming no modeling (to derive a more conservative limit) 100 FERMI Dirac − 1 FERMI σ =0.1 10− − FERMI σ =0.5 − 10 2 FERMI σ =1.0 − − 3 10− DM ⇢ 4 / 10 − Auffinger, Arbey, PBH and Silk 1906.04750 Ballesteros etal. ⇢ 5 10− + = Bulge e Dirac 1906.10113 − f 6 Bulge e+ σ =0.1 10− − Bulge e+ σ =0.5 − 7 Voyager 1 e+ Dirac 10− − Voyager 1 e+ σ =0.1 − 10 8 Voyager 1 e+ σ =0.5 − − Voyager 1 e+ σ =1.0 10 9 − − 1015 1016 1017 1018 M (g) Low-mass primordial black holes and Galactic Center 511 keV line 0 Low-mass primordial black holes can 10 evaporate to produce e<latexit sha1_base64="mcNP4nkOiAaDWkppRm0QWNHSFpA=">AAAB7HicbVBNS8NAEJ3Ur1q/qh69LBbBU0mqoMeiF48VTFtoY9lsJ+3SzSbsboRS+hu8eFDEqz/Im//GbZuDtj4YeLw3w8y8MBVcG9f9dgpr6xubW8Xt0s7u3v5B+fCoqZNMMfRZIhLVDqlGwSX6hhuB7VQhjUOBrXB0O/NbT6g0T+SDGacYxHQgecQZNVby8bGbxr1yxa26c5BV4uWkAjkavfJXt5+wLEZpmKBadzw3NcGEKsOZwGmpm2lMKRvRAXYslTRGHUzmx07JmVX6JEqULWnIXP09MaGx1uM4tJ0xNUO97M3E/7xOZqLrYMJlmhmUbLEoygQxCZl9TvpcITNibAllittbCRtSRZmx+ZRsCN7yy6ukWat6F9Xa/WWlfpPHUYQTOIVz8OAK6nAHDfCBAYdneIU3RzovzrvzsWgtOPnMMfyB8/kDyzaOrA==</latexit> ± pairs Cosmic rays rays − CMB Iso 1.5 kpc −1 10 NFW 1.5 kpc gamma The positrons will lose energy, become non- Iso 3 kpc NFW 3 kpc relativistic, and annihilate with the ambient Cosmic rays DM electrons to produce photons f 10−2 Galactic Center observations reveal an Laha 1906.09994 PRL intense flux of 511 keV photons produced Monochromatic by unknown source(s) (talk to R. Crocker and J. Knodlseder for more details about modeling and observation) 10−3 1013 1014 MPBH (kg) Requiring that the positrons from primordial Similar results in DeRocco and Graham 1906.07740 PRL black hole evaporation do not overshoot the positron luminosity produces the strongest These positron measurements can limit on their abundance with masses also be used to constrain spinning between ~ 1013 kg to 1014 kg primordial black hole dark matter (Dasgupta, Laha, and Ray 1912.01014) Microlensing Dynamical effects stars, supernovae, quasars dwarf galaxies, wide binary stars Primordial black holes constraints from lensing Source Pic. courtesy: Green 2019 talk Exotic compact object Observer Ranjan Laha Accretion Evaporation CMB, radio & X-ray gamma-rays Constraints Effects on stars Mergers white dwarf explosions gravitational
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