Primordial Black Holes as Dark Matter: Almost All or Almost Nothing

Lacki, Brian C.; Beacom, J. F.

doi:10.1088/2041-8205/720/1/l67

Cited by 125 publications

(139 citation statements)

References 39 publications

(52 reference statements)

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“…It has been argued that PBHs can also seed the formation of minihalos [6,11,12], and the resulting gamma-ray emission (assuming that the remainder of the dark matter is in the form of WIMPs) leads to constraints on the abundance of PBHs [13], however we do not pursue that possibility here.…”

Section: Ucmh Formation and Gamma-ray Emissionmentioning

confidence: 99%

Gamma rays from ultracompact minihalos: Potential constraints on the primordial curvature perturbation

Josan¹,

Green²

2010

Phys. Rev. D

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Ultracompact minihalos (UCMHs) are dense dark matter structures which can form from large density perturbations shortly after matter-radiation equality. If dark matter is in the form of Weakly Interacting Massive Particles (WIMPs), then UCMHs may be detected via their gamma-ray emission. We investigate how the Fermi satellite could constrain the abundance of UCMHs and place limits on the power spectrum of the primordial curvature perturbation. Detection by Fermi would put a lower limit on the UCMH halo fraction. The smallest detectable halo fraction, fUCMH > ∼ 10 −7 , is for MUCMH ∼ 10 3 M⊙. If gamma-ray emission from UCMHs is not detected, an upper limit can be placed on the halo fraction. The bound is tightest, fUCMH < ∼ 10 −5 , for MUCMH ∼ 10 5 M⊙. The resulting upper limit on the power spectrum of the primordial curvature perturbation in the event of non-detection is in the range PR < ∼ 10 −6.5 − 10 −6 on scales k ∼ 10 1 − 10 6 Mpc −1 . This is substantially tighter than the existing constraints from primordial black hole formation on these scales, however it assumes that dark matter is in the form of WIMPs and UCMHs are not disrupted during the formation of the Milky Way halo.

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Section: Ucmh Formation and Gamma-ray Emissionmentioning

confidence: 99%

Gamma rays from ultracompact minihalos: Potential constraints on the primordial curvature perturbation

Josan¹,

Green²

2010

Phys. Rev. D

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“…PBHs can themselves represent dark matter (DM) [18] if they are formed in sufficiently large quantities, but they can also serve as seeds for the formation of DM clumps [19][20][21][22][23][24]. Secondary accretion (generally, this mechanism was developed in cold DM onto a PBH [25], when DM flows toward the PBH and is virialized at some radius to form a halo, is usually considered in investigating DM clumps around PBHs.…”

Section: Introductionmentioning

confidence: 99%

“…Calculations [23] and [24] assumed the density profile in the central region of a clump to be close to ρ ∝ r −3/2 , while [26] considered power-law profiles ρ ∝ r −α with α = 1.5 − 3. The annihilation of DM in density cusps around black holes was considered in [27], [28], [29], and new gamma-ray constraints were obtained.…”

Section: Introductionmentioning

confidence: 99%

Dark matter density spikes around primordial black holes

Eroshenko

2016

Astron. Lett.

129

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We show that density spikes begin to form from dark matter particles around primordial black holes immediately after their formation at the radiation-dominated cosmological stage. This follows from the fact that in the thermal velocity distribution of particles there are particles with low velocities that remain in finite orbits around black holes and are not involved in the cosmological expansion. The accumulation of such particles near black holes gives rise to density spikes. These spikes are considerably denser than those that are formed later by the mechanism of secondary accretion. The density spikes must be bright gamma-ray sources. Comparison of the calculated signal from particle annihilation with the Fermi-LAT data constrains the present-day cosmological density parameter for primordial black holes with masses MBH ≥ 10 −8 M⊙ from above by values from ΩBH ≤ 1 to ΩBH ≤ 10 −8 , depending on MBH. These constraints are several orders of magnitude more stringent than other known constraints.

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“…In particular, an early period of matter domination could amplify the primordial inflationary seeds leading to the formation of halos or mini-halos, objects which can be in principle observable and detectable [8,9,[13][14][15].…”

Section: Discussionmentioning

confidence: 99%

“…In particular, this feature may be important for a Dark Matter Halo to collapse shortly after matterradiation equality forming an ultracompact minihalo, which are excellent indirect detection targets [8,9] and attractive for lensing prospects [10].…”

Section: Perturbations and Structure Formationmentioning

confidence: 99%

Structure formation during an early period of matter domination

Barenboim

Rasero

2014

J. High Energ. Phys.

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In this work we show that modifying the thermal history of the Universe by including an early period of matter domination can lead to the formation of astronomical objects. However, the survival of these objects can only be possible if the dominating matter decays to a daughter particle which is not only almost degenerate with the parent particle but also has an open annihilation channel. This requirement translates in an upper bound for the coupling of such a channel and makes the early structure formation viable.

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Primordial Black Holes as Dark Matter: Almost All or Almost Nothing

Cited by 125 publications

References 39 publications

Gamma rays from ultracompact minihalos: Potential constraints on the primordial curvature perturbation

Gamma rays from ultracompact minihalos: Potential constraints on the primordial curvature perturbation

Dark matter density spikes around primordial black holes

Structure formation during an early period of matter domination

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