{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2007:OFO3ULCITPY6362GJHHCJI235Y","short_pith_number":"pith:OFO3ULCI","schema_version":"1.0","canonical_sha256":"715dba2c489bf1edfb4649ce24a35bee3380c79d4cbde851c09342c10698f79e","source":{"kind":"arxiv","id":"0708.1949","version":2},"attestation_state":"computed","paper":{"title":"Cold Dark Matter Substructure and Galactic Disks I: Morphological Signatures of Hierarchical Satellite Accretion","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Andrew R. Zentner (KICP/U.Chicago), Andrey V. Kravtsov (KICP/U.Chicago), James S. Bullock (UC Irvine), Leonidas A. Moustakas (JPL/Caltech), Stelios Kazantzidis (KIPAC/Stanford)","submitted_at":"2007-08-15T19:13:07Z","abstract_excerpt":"(Abridged) We conduct a series of high-resolution, dissipationless N-body simulations to investigate the cumulative effect of substructure mergers onto thin disk galaxies in the context of the LCDM paradigm of structure formation. Our simulation campaign is based on a hybrid approach. Substructure properties are culled directly from cosmological simulations of galaxy-sized cold dark matter (CDM) halos. In contrast to what can be inferred from statistics of the present-day substructure populations, accretions of massive subhalos onto the central regions of host halos, where the galactic disk re"},"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":"0708.1949","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph","submitted_at":"2007-08-15T19:13:07Z","cross_cats_sorted":[],"title_canon_sha256":"ec08159c50333f1d6705ad7edc3126371a95c82477f76aa8c0a3fcca87e3551b","abstract_canon_sha256":"e2f33b15ececc39e5053c171b6c5ef0def927f3a38610b50d6ffa853acce8b55"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T17:20:26.306850Z","signature_b64":"Mh3bgES3MLe9UNX3oRLZZYEyc2mJCbOlPnRWUo+yxkB5rZK7u6ySoSnUfbswBd5cH36yFWnkwz0NYdVAe0xoAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"715dba2c489bf1edfb4649ce24a35bee3380c79d4cbde851c09342c10698f79e","last_reissued_at":"2026-07-04T17:20:26.306427Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T17:20:26.306427Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Cold Dark Matter Substructure and Galactic Disks I: Morphological Signatures of Hierarchical Satellite Accretion","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Andrew R. Zentner (KICP/U.Chicago), Andrey V. Kravtsov (KICP/U.Chicago), James S. Bullock (UC Irvine), Leonidas A. Moustakas (JPL/Caltech), Stelios Kazantzidis (KIPAC/Stanford)","submitted_at":"2007-08-15T19:13:07Z","abstract_excerpt":"(Abridged) We conduct a series of high-resolution, dissipationless N-body simulations to investigate the cumulative effect of substructure mergers onto thin disk galaxies in the context of the LCDM paradigm of structure formation. Our simulation campaign is based on a hybrid approach. Substructure properties are culled directly from cosmological simulations of galaxy-sized cold dark matter (CDM) halos. In contrast to what can be inferred from statistics of the present-day substructure populations, accretions of massive subhalos onto the central regions of host halos, where the galactic disk re"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0708.1949","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/0708.1949/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"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":"0708.1949","created_at":"2026-07-04T17:20:26.306487+00:00"},{"alias_kind":"arxiv_version","alias_value":"0708.1949v2","created_at":"2026-07-04T17:20:26.306487+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0708.1949","created_at":"2026-07-04T17:20:26.306487+00:00"},{"alias_kind":"pith_short_12","alias_value":"OFO3ULCITPY6","created_at":"2026-07-04T17:20:26.306487+00:00"},{"alias_kind":"pith_short_16","alias_value":"OFO3ULCITPY6362G","created_at":"2026-07-04T17:20:26.306487+00:00"},{"alias_kind":"pith_short_8","alias_value":"OFO3ULCI","created_at":"2026-07-04T17:20:26.306487+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2606.30752","citing_title":"Wrinkles in Time. II. Stellar Age Trends in Kinematic Signatures from Transient Spiral Structure","ref_index":41,"is_internal_anchor":true},{"citing_arxiv_id":"2606.27480","citing_title":"Self-interacting dark matter promotes bar formation in disk galaxies","ref_index":66,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/OFO3ULCITPY6362GJHHCJI235Y","json":"https://pith.science/pith/OFO3ULCITPY6362GJHHCJI235Y.json","graph_json":"https://pith.science/api/pith-number/OFO3ULCITPY6362GJHHCJI235Y/graph.json","events_json":"https://pith.science/api/pith-number/OFO3ULCITPY6362GJHHCJI235Y/events.json","paper":"https://pith.science/paper/OFO3ULCI"},"agent_actions":{"view_html":"https://pith.science/pith/OFO3ULCITPY6362GJHHCJI235Y","download_json":"https://pith.science/pith/OFO3ULCITPY6362GJHHCJI235Y.json","view_paper":"https://pith.science/paper/OFO3ULCI","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0708.1949&json=true","fetch_graph":"https://pith.science/api/pith-number/OFO3ULCITPY6362GJHHCJI235Y/graph.json","fetch_events":"https://pith.science/api/pith-number/OFO3ULCITPY6362GJHHCJI235Y/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/OFO3ULCITPY6362GJHHCJI235Y/action/timestamp_anchor","attest_storage":"https://pith.science/pith/OFO3ULCITPY6362GJHHCJI235Y/action/storage_attestation","attest_author":"https://pith.science/pith/OFO3ULCITPY6362GJHHCJI235Y/action/author_attestation","sign_citation":"https://pith.science/pith/OFO3ULCITPY6362GJHHCJI235Y/action/citation_signature","submit_replication":"https://pith.science/pith/OFO3ULCITPY6362GJHHCJI235Y/action/replication_record"}},"created_at":"2026-07-04T17:20:26.306487+00:00","updated_at":"2026-07-04T17:20:26.306487+00:00"}