Constraining Primordial Black Hole Abundance with the Galactic 511 keV Line

DeRocco, William; Graham, Peter W.

doi:10.1103/physrevlett.123.251102

Cited by 149 publications

(124 citation statements)

References 56 publications

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“…4, where we see that INTEGRAL can rule out PBHs composing the entirety of the DM for masses up to M PBH ¼ 1.2 × 10 17 g, providing the strongest constraint to date. Our result improves upon that obtained through the flux of electron-positron pairs in the Galaxy, which would then annihilate and emit a line at 511 keV [56][57][58] (this constraint depends on the dark matter profile at the Galactic Center and the propagation distance of low-energy positrons). Additionally, our constraint is tighter than CMB limits [62] (see also Ref.…”

Section: B Ultralight Pbhssupporting

confidence: 78%

“…Instead, a promising avenue consists of searching for the radiation from ultralight PBHs as they Hawking evaporate [46][47][48][49][50]. Previous works have searched for Hawking-evaporating PBHs through electron-positron pairs [51][52][53][54][55][56][57][58], extra-Galactic gamma rays [59][60][61], and the CMB [62][63][64][65]. These studies have ruled out PBHs as the entirety of the DM for M PBH ≲ 10 17 g. Here we search for gamma rays from PBHs in the DM halo around the Milky Way (MW), which would appear as a modified blackbody spectrum in the INTEGRAL data.…”

Section: Introductionmentioning

confidence: 99%

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INTEGRALconstraints on primordial black holes and particle dark matter

2020

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The International Gamma-Ray Astrophysics Laboratory (INTEGRAL) satellite has yielded unprecedented measurements of the soft gamma-ray spectrum of our Galaxy. Here we use those measurements to set constraints on dark matter (DM) that decays or annihilates into photons with energies E ≈ 0.02-2 MeV. First, we revisit the constraints on particle DM that decays or annihilates to photon pairs. In particular, for decaying DM, we find that previous limits were overstated by roughly an order of magnitude. Our new, conservative analysis finds that the DM lifetime must satisfy τ ≳ 5 × 10 26 s × ðm χ =MeVÞ −1 for DM masses m χ ¼ 0.054-3.6 MeV. For MeV-scale DM that annihilates into photons INTEGRAL sets the strongest constraints to date. Second, we target ultralight primordial black holes (PBHs) through their Hawking radiation. This makes them appear as decaying DM with a photon spectrum peaking at E ≈ 5.77=ð8πGM PBH Þ, for a PBH of mass M PBH. We use the INTEGRAL data to demonstrate that, at 95% C.L., PBHs with masses less than 1.2 × 10 17 g cannot comprise all of the DM, setting the tightest bound to date on ultralight PBHs.

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Section: B Ultralight Pbhssupporting

confidence: 78%

Section: Introductionmentioning

confidence: 99%

INTEGRALconstraints on primordial black holes and particle dark matter

2020

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“…Positrons produced by PBHs will also annihilate and contribute to the flux of the 511 keV line [177]. The SPI/INTEGRAL limits on this line lead to limits on the PBH fraction which are similar to the gamma-ray limit for 10 16 g M PBH 10 17 g [158,159]. There are somewhat tighter constraints (that exclude f PBH = 1 up to M PBH ≈ 2 × 10 17 g) from INTEGRAL measurements of the Galactic diffuse flux in the MeV range [160].…”

Section: Evaporationmentioning

confidence: 96%

Primordial black holes as a dark matter candidate

Green

Kavanagh

2021

J. Phys. G: Nucl. Part. Phys.

509

406

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The detection of gravitational waves from mergers of tens of Solar mass black hole binaries has led to a surge in interest in primordial black holes (PBHs) as a dark matter candidate. We aim to provide a (relatively) concise overview of the status of PBHs as a dark matter candidate, circa Summer 2020. First we review the formation of PBHs in the early Universe, focussing mainly on PBHs formed via the collapse of large density perturbations generated by inflation. Then we review the various current and future constraints on the present day abundance of PBHs. We conclude with a discussion of the key open questions in this field.

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“…The lifetime of PBHs with masses less than 2.5 × 10 −19 M ⊙ (3.5 × 10 −19 M ⊙ ) for nonrotating (maximally rotating) black holes is less than the age of the Universe and it cannot contribute to the DM density [51][52][53][54]. The leading constraints on low-mass PBHs arise from the observation of photons [8,55,56], cosmic rays [9], and the 511 keV gamma-ray line [57,58]. Astrophysical observations of neutrinos have been used to constrain particle DM [59,60] and here we study its implications for PBHs.…”

mentioning

confidence: 99%

Neutrino and Positron Constraints on Spinning Primordial Black Hole Dark Matter

2020

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Primordial black holes can have substantial spin-a fundamental property that has a strong effect on its evaporation rate. We conduct a comprehensive study of the detectability of primordial black holes with non-negligible spin, via the searches for the neutrinos and positrons in the MeV energy range. Diffuse supernova neutrino background searches and observation of the 511 keV gamma-ray line from positrons in the Galactic center set competitive constraints. Spinning primordial black holes are probed up to a slightly higher mass range compared to nonspinning ones. Our constraint using neutrinos is slightly weaker than that due to the diffuse gamma-ray background, but complementary and robust. Our positron constraints are typically weaker in the lower mass range and stronger in the higher mass range for the spinning primordial black holes compared to the nonspinning ones. They are generally stronger than those derived from the diffuse gamma-ray measurements for primordial black holes having masses greater than a few ×10 16 g.

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Constraining Primordial Black Hole Abundance with the Galactic 511 keV Line

Cited by 149 publications

References 56 publications

INTEGRALconstraints on primordial black holes and particle dark matter

INTEGRALconstraints on primordial black holes and particle dark matter

Primordial black holes as a dark matter candidate

Neutrino and Positron Constraints on Spinning Primordial Black Hole Dark Matter

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