{"schema":"pubphys.bundle/1","record":{"author":{"account_ref":null,"orcid":null},"builds_on":[],"content_schema":"pubphys.content.revision/1","content_sha256":"6f2adb9543b73b69bd3a58cbfb9f47ad17f4a16022dccaa129a30a084be03464","created":"2026-10-15T23:43:22Z","files":[],"origin":{"assisted_by":[],"kind":"seed"},"parents":["ce59fb6cd812fc05906d0c60a71c75ea22bc686bcf38e7c3ef7010834d98ee7b","ff2e1233e790554ae8919aa8b59cf43552508a5d54741b831c0fad63057b0db6"],"salt":"7825e7a16fbdc3e3d2e4bb76aa631cdc83648e7a73a595adb5d738d25faefeaa","schema":"pubphys.record/2","site":"pubphys.com","target":null,"type":"revision"},"content":{"answer_type":"identification","assisted_by":[],"external_id":"astro.compact-binary-origins.mass-peak-35","kind":"phenomenon","literature_status":"contested","n":"2","parents":[],"plain":"Merging black holes pile up near 35 solar masses, more than a smooth distribution would give; this could mark the pile-up just below the pair-instability gap or a feature of one formation route.","posed_since":"2021","precise":"Population analyses of LIGO-Virgo-KAGRA catalogs find a peak near $35\\,M_{\\mathrm{sun}}$ in the primary-mass distribution, below the $\\sim 40\\text{ to }50\\,M_{\\mathrm{sun}}$ where standard pulsational pair-instability models put the pile-up. Determine whether the peak is the pair-instability pile-up shifted by nuclear-rate or wind physics, a signature of a channel such as globular-cluster dynamics, or a core-collapse fallback feature. Answer: an identification that predicts the peak location, width and any redshift dependence.","problem_ref":"ff2e1233e790554ae8919aa8b59cf43552508a5d54741b831c0fad63057b0db6","references":"","settled_by":"Measurement of the peak location versus redshift and spin with a catalog of order $10^{3}$ events, compared with channel predictions.","status_note":"","title":"What produces the excess of merging black holes near 35 solar 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