{"paper":{"title":"Intermediate-Mass Black Holes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"Dynamical and accretion signatures indicate that most galaxies with masses 10^9 to 10^10 solar masses contain black holes below 10^5 solar masses, while no solid detections exist in globular clusters.","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Jay Strader, Jenny E. Greene, Luis C. Ho","submitted_at":"2019-11-21T18:59:59Z","abstract_excerpt":"We describe ongoing searches for intermediate-mass black holes with M_BH ~ 100-10^5 M_sun. We review a range of search mechanisms, both dynamical and those that rely on accretion signatures. We find that dynamical and accretion signatures alike point to a high fraction of 10^9-10^10 M_sun galaxies hosting black holes with M_BH<10^5 M_sun. In contrast, there are no solid detections of black holes in globular clusters. There are few observational constraints on black holes in any environment with M_BH ~ 100-10^4 M_sun. Considering low-mass galaxies with dynamical black hole masses and constraini"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"We find that dynamical and accretion signatures alike point to a high fraction of 10^9-10^10 M_sun galaxies hosting black holes with M_BH<10^5 M_sun. In contrast, there are no solid detections of black holes in globular clusters.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"The interpretation that non-detections in globular clusters reflect true absence rather than observational limits or selection effects, and that the observed scatter in the M_BH-sigma relation is driven by a broad range in black hole mass and occupation fraction.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"A literature review finds that a high fraction of low-mass galaxies host intermediate-mass black holes below 100,000 solar masses, with no solid detections in globular clusters and the black hole mass-stellar velocity dispersion relation extending unbroken to lower masses despite large scatter.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"Dynamical and accretion signatures indicate that most galaxies with masses 10^9 to 10^10 solar masses contain black holes below 10^5 solar masses, while no solid detections exist in globular clusters.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"fb4bc8a6488ff10077adef584122dd1658442e73ef4e551e5c866379c5ba80cc"},"source":{"id":"1911.09678","kind":"arxiv","version":2},"verdict":{"id":"43bf1f3b-bc82-4c0f-90ef-793d000ff064","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-17T10:31:43.458368Z","strongest_claim":"We find that dynamical and accretion signatures alike point to a high fraction of 10^9-10^10 M_sun galaxies hosting black holes with M_BH<10^5 M_sun. In contrast, there are no solid detections of black holes in globular clusters.","one_line_summary":"A literature review finds that a high fraction of low-mass galaxies host intermediate-mass black holes below 100,000 solar masses, with no solid detections in globular clusters and the black hole mass-stellar velocity dispersion relation extending unbroken to lower masses despite large scatter.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"The interpretation that non-detections in globular clusters reflect true absence rather than observational limits or selection effects, and that the observed scatter in the M_BH-sigma relation is driven by a broad range in black hole mass and occupation fraction.","pith_extraction_headline":"Dynamical and accretion signatures indicate that most galaxies with masses 10^9 to 10^10 solar masses contain black holes below 10^5 solar masses, while no solid detections exist in globular clusters."},"references":{"count":300,"sample":[{"doi":"","year":2009,"title":"Abadi MG, Navarro JF, Steinmetz M. 2009. 691:L63--L66","work_id":"fc6c7018-b56c-45c6-b509-b240be83c041","ref_index":1,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2018,"title":"Abbate F, Possenti A, Ridolfi A, Freire PCC, Camilo F, et al. 2018. 481:627--638","work_id":"28c161e7-be56-45d5-ac4b-cb042ecc9fe1","ref_index":2,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2018,"title":"Afanasiev AV, Chilingarian IV, Mieske S, Voggel KT, Picotti A, et al. 2018. 477:4856--4865","work_id":"d6d7340b-5575-4cbc-ae50-5d433ac8bb27","ref_index":3,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2018,"title":"Ahn CP, Seth AC, Cappellari M, Krajnovi \\'c D, Strader J, et al. 2018. 858:102","work_id":"2f8e762d-c13d-44de-adf5-68389b446931","ref_index":4,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2017,"title":"Ahn CP, Seth AC, den Brok M, Strader J, Baumgardt H, et al. 2017. 839:72","work_id":"3b7f4af1-e799-4c70-9a0a-1ef477fc6274","ref_index":5,"cited_arxiv_id":"","is_internal_anchor":false}],"resolved_work":300,"snapshot_sha256":"3719b0ab76e9d0f8664fd88ec8d4d020ba91f7fb93e70e3c8405541d93eb0f01","internal_anchors":2},"formal_canon":{"evidence_count":2,"snapshot_sha256":"6c092f8c92764b8e4ae4f558506be0fd13f6c7c253438bc612aa3bec4b6b3617"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}