{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:3SXWLAPSG5QJWWL2LVFVXJFPL7","short_pith_number":"pith:3SXWLAPS","schema_version":"1.0","canonical_sha256":"dcaf6581f237609b597a5d4b5ba4af5fe2d53e4214109442fb90e7b774338bbf","source":{"kind":"arxiv","id":"1810.07055","version":2},"attestation_state":"computed","paper":{"title":"The optimal gravitational softening length for cosmological N-body simulations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"Liang Gao, Ming Li, Shihong Liao, Tianchi Zhang","submitted_at":"2018-10-16T14:53:49Z","abstract_excerpt":"Gravitational softening length is one of the key parameters to properly set up a cosmological $N$-body simulation. In this paper, we perform a large suit of high-resolution $N$-body simulations to revise the optimal softening scheme proposed by Power et al. (P03). Our finding is that P03 optimal scheme works well but is over conservative. Using smaller softening lengths than that of P03 can achieve higher spatial resolution and numerically convergent results on both circular velocity and density profiles. However using an over small softening length overpredicts matter density at the inner mos"},"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":"1810.07055","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2018-10-16T14:53:49Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"9cbcea517b4bab2c7b14dbcc92ef5bdb5bd58064f47a4929d8344952a0748a4e","abstract_canon_sha256":"b3499763ba8b87f48669d2f35a24e6ddadc745761103905080326338330d8c67"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:44:02.756704Z","signature_b64":"EfHNZd51Y+ycxXs2vyel97WGztxg31F/iP32vpBPQ+RTomFPetRUHuWkT/o1Dt6eRmK0P5hQPSCibHyJxrAqDw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"dcaf6581f237609b597a5d4b5ba4af5fe2d53e4214109442fb90e7b774338bbf","last_reissued_at":"2026-05-17T23:44:02.756112Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:44:02.756112Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The optimal gravitational softening length for cosmological N-body simulations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"Liang Gao, Ming Li, Shihong Liao, Tianchi Zhang","submitted_at":"2018-10-16T14:53:49Z","abstract_excerpt":"Gravitational softening length is one of the key parameters to properly set up a cosmological $N$-body simulation. In this paper, we perform a large suit of high-resolution $N$-body simulations to revise the optimal softening scheme proposed by Power et al. (P03). Our finding is that P03 optimal scheme works well but is over conservative. Using smaller softening lengths than that of P03 can achieve higher spatial resolution and numerically convergent results on both circular velocity and density profiles. However using an over small softening length overpredicts matter density at the inner mos"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1810.07055","kind":"arxiv","version":2},"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":"1810.07055","created_at":"2026-05-17T23:44:02.756198+00:00"},{"alias_kind":"arxiv_version","alias_value":"1810.07055v2","created_at":"2026-05-17T23:44:02.756198+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1810.07055","created_at":"2026-05-17T23:44:02.756198+00:00"},{"alias_kind":"pith_short_12","alias_value":"3SXWLAPSG5QJ","created_at":"2026-05-18T12:32:05.422762+00:00"},{"alias_kind":"pith_short_16","alias_value":"3SXWLAPSG5QJWWL2","created_at":"2026-05-18T12:32:05.422762+00:00"},{"alias_kind":"pith_short_8","alias_value":"3SXWLAPS","created_at":"2026-05-18T12:32:05.422762+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":3,"sample":[{"citing_arxiv_id":"2607.06933","citing_title":"Constructing a Mock Galaxy Catalog for the All-sky SPECtroscopic Survey of Nearby Galaxies (A-SPEC) Using the Machine-assisted Semi-Simulation Model","ref_index":134,"is_internal_anchor":true},{"citing_arxiv_id":"2605.15310","citing_title":"Introducing the Lumina project: large-volume radiation-hydrodynamic simulations of the epochs of hydrogen and helium reionization","ref_index":220,"is_internal_anchor":true},{"citing_arxiv_id":"2601.19812","citing_title":"An essential building block for cosmological zoom-in perturbation theory","ref_index":27,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/3SXWLAPSG5QJWWL2LVFVXJFPL7","json":"https://pith.science/pith/3SXWLAPSG5QJWWL2LVFVXJFPL7.json","graph_json":"https://pith.science/api/pith-number/3SXWLAPSG5QJWWL2LVFVXJFPL7/graph.json","events_json":"https://pith.science/api/pith-number/3SXWLAPSG5QJWWL2LVFVXJFPL7/events.json","paper":"https://pith.science/paper/3SXWLAPS"},"agent_actions":{"view_html":"https://pith.science/pith/3SXWLAPSG5QJWWL2LVFVXJFPL7","download_json":"https://pith.science/pith/3SXWLAPSG5QJWWL2LVFVXJFPL7.json","view_paper":"https://pith.science/paper/3SXWLAPS","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1810.07055&json=true","fetch_graph":"https://pith.science/api/pith-number/3SXWLAPSG5QJWWL2LVFVXJFPL7/graph.json","fetch_events":"https://pith.science/api/pith-number/3SXWLAPSG5QJWWL2LVFVXJFPL7/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/3SXWLAPSG5QJWWL2LVFVXJFPL7/action/timestamp_anchor","attest_storage":"https://pith.science/pith/3SXWLAPSG5QJWWL2LVFVXJFPL7/action/storage_attestation","attest_author":"https://pith.science/pith/3SXWLAPSG5QJWWL2LVFVXJFPL7/action/author_attestation","sign_citation":"https://pith.science/pith/3SXWLAPSG5QJWWL2LVFVXJFPL7/action/citation_signature","submit_replication":"https://pith.science/pith/3SXWLAPSG5QJWWL2LVFVXJFPL7/action/replication_record"}},"created_at":"2026-05-17T23:44:02.756198+00:00","updated_at":"2026-05-17T23:44:02.756198+00:00"}