{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:LGDBH27U3HUB4NFT7UGJ2KZF6S","short_pith_number":"pith:LGDBH27U","schema_version":"1.0","canonical_sha256":"598613ebf4d9e81e34b3fd0c9d2b25f4ab7fad674414a394df27196364513a0e","source":{"kind":"arxiv","id":"1701.03526","version":2},"attestation_state":"computed","paper":{"title":"The Relationship between Galaxy and Dark Matter Halo Size from z~3 to the present","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Adriano Fontana, Anton M. Koekemoer, Arjen van der Wel, Avishai Dekel, David Koo, Edward N. Taylor, Joel R. Primack, Paola Santini, Peter Behroozi, P.G. P\\'erez-Gonz\\'alez, Rachel S. Somerville, S. M. Faber, Viraj Pandya","submitted_at":"2017-01-12T22:48:08Z","abstract_excerpt":"We explore empirical constraints on the statistical relationship between the radial size of galaxies and the radius of their host dark matter halos from $z\\sim 0.1$--3 using the GAMA and CANDELS surveys. We map dark matter halo mass to galaxy stellar mass using relationships from abundance matching, applied to the Bolshoi-Planck dissipationless N-body simulation. We define SRHR$\\equiv r_e/R_h$ as the ratio of galaxy radius to halo virial radius, and SRHR$\\lambda \\equiv r_e/(\\lambda R_h)$ as the ratio of galaxy radius to halo spin parameter times halo radius. At $z\\sim 0.1$, we find an average "},"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":"1701.03526","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2017-01-12T22:48:08Z","cross_cats_sorted":[],"title_canon_sha256":"159de922354595c4635a24102891375675c4a1f2daa8e6bc875f4c032f3d4eb4","abstract_canon_sha256":"b7c097e5cfc551dc0866e133777b3eea338cb825934f0ac51a34da5347410d42"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:29:31.108047Z","signature_b64":"IESW+Td4YTv3mLQs+ixnROpHm2bVDKnD/58zj5RVNUpE45U3nyLOil+uuFSojoLuLwsgHPZ4yUZU4tYJYcqPDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"598613ebf4d9e81e34b3fd0c9d2b25f4ab7fad674414a394df27196364513a0e","last_reissued_at":"2026-05-18T00:29:31.107556Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:29:31.107556Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Relationship between Galaxy and Dark Matter Halo Size from z~3 to the present","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Adriano Fontana, Anton M. Koekemoer, Arjen van der Wel, Avishai Dekel, David Koo, Edward N. Taylor, Joel R. Primack, Paola Santini, Peter Behroozi, P.G. P\\'erez-Gonz\\'alez, Rachel S. Somerville, S. M. Faber, Viraj Pandya","submitted_at":"2017-01-12T22:48:08Z","abstract_excerpt":"We explore empirical constraints on the statistical relationship between the radial size of galaxies and the radius of their host dark matter halos from $z\\sim 0.1$--3 using the GAMA and CANDELS surveys. We map dark matter halo mass to galaxy stellar mass using relationships from abundance matching, applied to the Bolshoi-Planck dissipationless N-body simulation. We define SRHR$\\equiv r_e/R_h$ as the ratio of galaxy radius to halo virial radius, and SRHR$\\lambda \\equiv r_e/(\\lambda R_h)$ as the ratio of galaxy radius to halo spin parameter times halo radius. At $z\\sim 0.1$, we find an average "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1701.03526","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":"1701.03526","created_at":"2026-05-18T00:29:31.107615+00:00"},{"alias_kind":"arxiv_version","alias_value":"1701.03526v2","created_at":"2026-05-18T00:29:31.107615+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1701.03526","created_at":"2026-05-18T00:29:31.107615+00:00"},{"alias_kind":"pith_short_12","alias_value":"LGDBH27U3HUB","created_at":"2026-05-18T12:31:28.150371+00:00"},{"alias_kind":"pith_short_16","alias_value":"LGDBH27U3HUB4NFT","created_at":"2026-05-18T12:31:28.150371+00:00"},{"alias_kind":"pith_short_8","alias_value":"LGDBH27U","created_at":"2026-05-18T12:31:28.150371+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2411.13484","citing_title":"The Impact of Galaxy-halo Size Relations on Galaxy Clustering Signals","ref_index":7,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/LGDBH27U3HUB4NFT7UGJ2KZF6S","json":"https://pith.science/pith/LGDBH27U3HUB4NFT7UGJ2KZF6S.json","graph_json":"https://pith.science/api/pith-number/LGDBH27U3HUB4NFT7UGJ2KZF6S/graph.json","events_json":"https://pith.science/api/pith-number/LGDBH27U3HUB4NFT7UGJ2KZF6S/events.json","paper":"https://pith.science/paper/LGDBH27U"},"agent_actions":{"view_html":"https://pith.science/pith/LGDBH27U3HUB4NFT7UGJ2KZF6S","download_json":"https://pith.science/pith/LGDBH27U3HUB4NFT7UGJ2KZF6S.json","view_paper":"https://pith.science/paper/LGDBH27U","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1701.03526&json=true","fetch_graph":"https://pith.science/api/pith-number/LGDBH27U3HUB4NFT7UGJ2KZF6S/graph.json","fetch_events":"https://pith.science/api/pith-number/LGDBH27U3HUB4NFT7UGJ2KZF6S/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/LGDBH27U3HUB4NFT7UGJ2KZF6S/action/timestamp_anchor","attest_storage":"https://pith.science/pith/LGDBH27U3HUB4NFT7UGJ2KZF6S/action/storage_attestation","attest_author":"https://pith.science/pith/LGDBH27U3HUB4NFT7UGJ2KZF6S/action/author_attestation","sign_citation":"https://pith.science/pith/LGDBH27U3HUB4NFT7UGJ2KZF6S/action/citation_signature","submit_replication":"https://pith.science/pith/LGDBH27U3HUB4NFT7UGJ2KZF6S/action/replication_record"}},"created_at":"2026-05-18T00:29:31.107615+00:00","updated_at":"2026-05-18T00:29:31.107615+00:00"}