{"paper":{"title":"In-depth analysis of the clustering of dark matter particles around primordial black holes. Part III: CMB constraints","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"Even a tiny fraction of primordial black holes can force co-existing thermal dark matter particles to annihilate far more slowly than usual, as shown by CMB data analysis.","cross_cats":["hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Julien Lavalle, Pierre Salati, Vivian Poulin","submitted_at":"2026-04-20T09:30:49Z","abstract_excerpt":"In a mixed dark matter scenario in which primordial black holes (PBHs) would co-exist with thermally produced self-annihilating particles, one expects the former to be surrounded by extremely dense halos made of the latter, built up during radiation domination. Here, as a continuation of previous work, we derive observational limits on such a scenario from a full statistical analysis of cosmic microwave background (CMB) data. We quantify how a tiny fraction $\\fbh$ of PBHs could restrict the parameter space available to thermal particle dark matter, limiting the $s$-wave annihilation cross sect"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"we derive observational limits on such a scenario from a full statistical analysis of cosmic microwave background (CMB) data. We quantify how a tiny fraction f_BH of PBHs could restrict the parameter space available to thermal particle dark matter, limiting the s-wave annihilation cross section to values ≲ 10^{-30} cm³/s (mχ/100 GeV) (f_BH/10^{-6})^{-3} if PBHs are typically heavier than ∼10^{-10} M_⊙","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"The assumption that PBHs are surrounded by extremely dense halos of self-annihilating particles built up during radiation domination, as modeled in prior parts of this work series.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"CMB data limits the s-wave annihilation cross section of thermal dark matter particles to ≲ 10^{-30} cm³/s scaled by PBH fraction and mass for PBHs heavier than ~10^{-10} solar masses.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"Even a tiny fraction of primordial black holes can force co-existing thermal dark matter particles to annihilate far more slowly than usual, as shown by CMB data analysis.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"b3c0f428dd3e61e6f82478abf52f1905f937e7509e5f9a69239d442a77a113cc"},"source":{"id":"2604.18007","kind":"arxiv","version":1},"verdict":{"id":"f986e4da-d8bb-4d1f-bb5e-26d48f412e18","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-10T04:07:10.789751Z","strongest_claim":"we derive observational limits on such a scenario from a full statistical analysis of cosmic microwave background (CMB) data. We quantify how a tiny fraction f_BH of PBHs could restrict the parameter space available to thermal particle dark matter, limiting the s-wave annihilation cross section to values ≲ 10^{-30} cm³/s (mχ/100 GeV) (f_BH/10^{-6})^{-3} if PBHs are typically heavier than ∼10^{-10} M_⊙","one_line_summary":"CMB data limits the s-wave annihilation cross section of thermal dark matter particles to ≲ 10^{-30} cm³/s scaled by PBH fraction and mass for PBHs heavier than ~10^{-10} solar masses.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"The assumption that PBHs are surrounded by extremely dense halos of self-annihilating particles built up during radiation domination, as modeled in prior parts of this work series.","pith_extraction_headline":"Even a tiny fraction of primordial black holes can force co-existing thermal dark matter particles to annihilate far more slowly than usual, as shown by CMB data analysis."},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2604.18007/integrity.json","findings":[],"available":true,"detectors_run":[{"name":"doi_compliance","ran_at":"2026-05-20T04:32:40.701771Z","status":"completed","version":"1.0.0","findings_count":0}],"snapshot_sha256":"aea73470b0fd5fc18eafd9c9838503f94deb4ffa86e3f67a05a526dc74ce95f7"},"references":{"count":76,"sample":[{"doi":"","year":null,"title":"P. J. E. Peebles,Primeval adiabatic perturbations - effect of massive neutrinos,ApJ258(July,","work_id":"34f3af29-9f6b-4eb2-af24-c5647deb7727","ref_index":1,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":1996,"title":"Supersymmetric Dark Matter","work_id":"99ed5a80-a296-49ed-a4a4-69fe2d18a215","ref_index":2,"cited_arxiv_id":"hep-ph/9506380","is_internal_anchor":false},{"doi":"","year":2010,"title":"Dark Matter Candidates from Particle Physics and Methods of Detection","work_id":"41aa3f7d-d51d-47ac-ae55-7153be74cec8","ref_index":3,"cited_arxiv_id":"1003.0904","is_internal_anchor":false},{"doi":"","year":2024,"title":"M. Cirelli, A. Strumia and J. Zupan,Dark matter,arXiv e-prints(June, 2024) arXiv:2406.01705, [2406.01705]","work_id":"37c4bfed-9b75-43f4-96fe-1b75751acf8f","ref_index":4,"cited_arxiv_id":"2406.01705","is_internal_anchor":true},{"doi":"","year":1967,"title":"Y. B. Zel’dovich and I. D. Novikov,The hypothesis of cores retarded during expansion and the – 32 – hot cosmological model,Soviet Ast.10(Feb., 1967) 602","work_id":"5c21852c-7778-492a-a543-e747cd619a40","ref_index":5,"cited_arxiv_id":"","is_internal_anchor":false}],"resolved_work":76,"snapshot_sha256":"b580a61eefdc69186ac60ca9bde1383256d34db595544bb33742be71c53549f8","internal_anchors":14},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}