{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2015:NB3ZMQ6PYBC6QQEEAHA4CPCDXO","short_pith_number":"pith:NB3ZMQ6P","schema_version":"1.0","canonical_sha256":"68779643cfc045e8408401c1c13c43bb868352c4ba220012fd7c9aee6a183ddf","source":{"kind":"arxiv","id":"1504.05591","version":1},"attestation_state":"computed","paper":{"title":"The splashback radius as a physical halo boundary and the growth of halo mass","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Andrey Kravtsov, Benedikt Diemer, Surhud More","submitted_at":"2015-04-21T20:01:40Z","abstract_excerpt":"The boundaries of cold dark matter halos are commonly defined to enclose a density contrast $\\Delta$ relative to a reference (mean or critical) density. We argue that a more physical boundary of halos is the radius at which accreted matter reaches its first orbital apocenter after turnaround. This splashback radius, $R_{sp}$, manifests itself as a sharp density drop in the halo outskirts, at a location that depends upon the mass accretion rate. We present calibrations of $R_{sp}$ and the enclosed mass, $M_{sp}$, as a function of the accretion rate and alternatively peak height. We find that $R"},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":false,"formal_links_present":false},"canonical_record":{"source":{"id":"1504.05591","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2015-04-21T20:01:40Z","cross_cats_sorted":[],"title_canon_sha256":"61dc526b83851ac84a5bea2d96799948684b0973643197f60f6999d72dfe63f1","abstract_canon_sha256":"1c97f1889a566e83a2229afcccd9ef0724fa712b3fa29500978b4f034a7a5c3c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:33:43.493419Z","signature_b64":"D43KX/663HB7uqfHZ5IenG2LFVAwWG7LVitWY0543djUqnynYmiX+ntshUeP+4IbT20BsviELkLjjuDur69sCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"68779643cfc045e8408401c1c13c43bb868352c4ba220012fd7c9aee6a183ddf","last_reissued_at":"2026-05-18T01:33:43.492944Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:33:43.492944Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The splashback radius as a physical halo boundary and the growth of halo mass","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Andrey Kravtsov, Benedikt Diemer, Surhud More","submitted_at":"2015-04-21T20:01:40Z","abstract_excerpt":"The boundaries of cold dark matter halos are commonly defined to enclose a density contrast $\\Delta$ relative to a reference (mean or critical) density. We argue that a more physical boundary of halos is the radius at which accreted matter reaches its first orbital apocenter after turnaround. This splashback radius, $R_{sp}$, manifests itself as a sharp density drop in the halo outskirts, at a location that depends upon the mass accretion rate. We present calibrations of $R_{sp}$ and the enclosed mass, $M_{sp}$, as a function of the accretion rate and alternatively peak height. We find that $R"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1504.05591","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"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"},"aliases":[{"alias_kind":"arxiv","alias_value":"1504.05591","created_at":"2026-05-18T01:33:43.493010+00:00"},{"alias_kind":"arxiv_version","alias_value":"1504.05591v1","created_at":"2026-05-18T01:33:43.493010+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1504.05591","created_at":"2026-05-18T01:33:43.493010+00:00"},{"alias_kind":"pith_short_12","alias_value":"NB3ZMQ6PYBC6","created_at":"2026-05-18T12:29:32.376354+00:00"},{"alias_kind":"pith_short_16","alias_value":"NB3ZMQ6PYBC6QQEE","created_at":"2026-05-18T12:29:32.376354+00:00"},{"alias_kind":"pith_short_8","alias_value":"NB3ZMQ6P","created_at":"2026-05-18T12:29:32.376354+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.16483","citing_title":"The limits of feedback from active galactic nuclei","ref_index":67,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/NB3ZMQ6PYBC6QQEEAHA4CPCDXO","json":"https://pith.science/pith/NB3ZMQ6PYBC6QQEEAHA4CPCDXO.json","graph_json":"https://pith.science/api/pith-number/NB3ZMQ6PYBC6QQEEAHA4CPCDXO/graph.json","events_json":"https://pith.science/api/pith-number/NB3ZMQ6PYBC6QQEEAHA4CPCDXO/events.json","paper":"https://pith.science/paper/NB3ZMQ6P"},"agent_actions":{"view_html":"https://pith.science/pith/NB3ZMQ6PYBC6QQEEAHA4CPCDXO","download_json":"https://pith.science/pith/NB3ZMQ6PYBC6QQEEAHA4CPCDXO.json","view_paper":"https://pith.science/paper/NB3ZMQ6P","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1504.05591&json=true","fetch_graph":"https://pith.science/api/pith-number/NB3ZMQ6PYBC6QQEEAHA4CPCDXO/graph.json","fetch_events":"https://pith.science/api/pith-number/NB3ZMQ6PYBC6QQEEAHA4CPCDXO/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/NB3ZMQ6PYBC6QQEEAHA4CPCDXO/action/timestamp_anchor","attest_storage":"https://pith.science/pith/NB3ZMQ6PYBC6QQEEAHA4CPCDXO/action/storage_attestation","attest_author":"https://pith.science/pith/NB3ZMQ6PYBC6QQEEAHA4CPCDXO/action/author_attestation","sign_citation":"https://pith.science/pith/NB3ZMQ6PYBC6QQEEAHA4CPCDXO/action/citation_signature","submit_replication":"https://pith.science/pith/NB3ZMQ6PYBC6QQEEAHA4CPCDXO/action/replication_record"}},"created_at":"2026-05-18T01:33:43.493010+00:00","updated_at":"2026-05-18T01:33:43.493010+00:00"}