{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:LBXMV7JMMBLK2IKAMAZ5IKUG3A","short_pith_number":"pith:LBXMV7JM","schema_version":"1.0","canonical_sha256":"586ecafd2c6056ad21406033d42a86d8212a9804ff8b9c34a8b7e1bcd951f28a","source":{"kind":"arxiv","id":"1707.03397","version":2},"attestation_state":"computed","paper":{"title":"First results from the IllustrisTNG simulations: matter and galaxy clustering","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"2), (2) Heidelberg University, (3) MPIA, (4) MPA, (5) Harvard-CfA, (6) MIT, (7) CCA, 8), (8) Columbia University), Annalisa Pillepich (3), Dylan Nelson (4), Federico Marinacci (6), Jill Naiman (5) ((1) HITS, Lars Hernquist (5), Mark Vogelsberger (6), Paul Torrey (6), Rainer Weinberger (1), R\\\"udiger Pakmor (1), Shy Genel (7, Volker Springel (1","submitted_at":"2017-07-11T18:00:01Z","abstract_excerpt":"Hydrodynamical simulations of galaxy formation have now reached sufficient volume to make precision predictions for clustering on cosmologically relevant scales. Here we use our new IllustrisTNG simulations to study the non-linear correlation functions and power spectra of baryons, dark matter, galaxies and haloes over an exceptionally large range of scales. We find that baryonic effects increase the clustering of dark matter on small scales and damp the total matter power spectrum on scales up to k ~ 10 h/Mpc by 20%. The non-linear two-point correlation function of the stellar mass is close t"},"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":"1707.03397","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2017-07-11T18:00:01Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"7cadb1e352e322a513e33c1ef955ddb44e740183e048c5de7b47ec5016bcb9ed","abstract_canon_sha256":"5c8b46e7eab11b91e833b19877386573535baef477cb79d69017b6b7ec3e4281"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:23:45.569573Z","signature_b64":"WfxBtv2QmEZ5LAa+dyA1E8x3JmbUUrqS6jiGpGDWfFa8wXoBZIMIIb5+ER5PL6/m71AsGBRukzNWfzVjgfhqAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"586ecafd2c6056ad21406033d42a86d8212a9804ff8b9c34a8b7e1bcd951f28a","last_reissued_at":"2026-05-18T00:23:45.569110Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:23:45.569110Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"First results from the IllustrisTNG simulations: matter and galaxy clustering","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"2), (2) Heidelberg University, (3) MPIA, (4) MPA, (5) Harvard-CfA, (6) MIT, (7) CCA, 8), (8) Columbia University), Annalisa Pillepich (3), Dylan Nelson (4), Federico Marinacci (6), Jill Naiman (5) ((1) HITS, Lars Hernquist (5), Mark Vogelsberger (6), Paul Torrey (6), Rainer Weinberger (1), R\\\"udiger Pakmor (1), Shy Genel (7, Volker Springel (1","submitted_at":"2017-07-11T18:00:01Z","abstract_excerpt":"Hydrodynamical simulations of galaxy formation have now reached sufficient volume to make precision predictions for clustering on cosmologically relevant scales. Here we use our new IllustrisTNG simulations to study the non-linear correlation functions and power spectra of baryons, dark matter, galaxies and haloes over an exceptionally large range of scales. We find that baryonic effects increase the clustering of dark matter on small scales and damp the total matter power spectrum on scales up to k ~ 10 h/Mpc by 20%. The non-linear two-point correlation function of the stellar mass is close t"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1707.03397","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":"1707.03397","created_at":"2026-05-18T00:23:45.569177+00:00"},{"alias_kind":"arxiv_version","alias_value":"1707.03397v2","created_at":"2026-05-18T00:23:45.569177+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1707.03397","created_at":"2026-05-18T00:23:45.569177+00:00"},{"alias_kind":"pith_short_12","alias_value":"LBXMV7JMMBLK","created_at":"2026-05-18T12:31:28.150371+00:00"},{"alias_kind":"pith_short_16","alias_value":"LBXMV7JMMBLK2IKA","created_at":"2026-05-18T12:31:28.150371+00:00"},{"alias_kind":"pith_short_8","alias_value":"LBXMV7JM","created_at":"2026-05-18T12:31:28.150371+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":8,"internal_anchor_count":5,"sample":[{"citing_arxiv_id":"2605.23006","citing_title":"\\texttt{calypso}: a Parameter-Conditioned Stochastic Surrogate Model for Circumbinary Accretion Time-Series","ref_index":290,"is_internal_anchor":true},{"citing_arxiv_id":"1907.02977","citing_title":"Realistic simulations of galaxy formation in f(R) modified gravity","ref_index":36,"is_internal_anchor":true},{"citing_arxiv_id":"2605.18975","citing_title":"Bulgeless Evolution And the Rise of Discs (BEARD) III. A numerical simulation view of satellites around Milky-Way analogues","ref_index":94,"is_internal_anchor":true},{"citing_arxiv_id":"2512.07396","citing_title":"Phase-space perturbation theory for cosmic large-scale structure","ref_index":3,"is_internal_anchor":true},{"citing_arxiv_id":"2605.13472","citing_title":"First Light And Reionization Epoch Simulations (FLARES) XXI: The UV Indices of Galaxies in the Early Universe","ref_index":86,"is_internal_anchor":true},{"citing_arxiv_id":"2604.26022","citing_title":"Secondary Dependence of Baryonic Effects on the Density Profile of Dark Matter Halos","ref_index":17,"is_internal_anchor":false},{"citing_arxiv_id":"2604.08647","citing_title":"Bypassed Core Formation in Milky Way-Mass SIDM Halos: Implications for the Local Group Past-Pericenter Scenario","ref_index":74,"is_internal_anchor":false},{"citing_arxiv_id":"2605.01963","citing_title":"Constraints on Halo Gas Profiles from Joint kSZ and Galaxy Clustering Analysis of ACT DR6 and CMASS","ref_index":24,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/LBXMV7JMMBLK2IKAMAZ5IKUG3A","json":"https://pith.science/pith/LBXMV7JMMBLK2IKAMAZ5IKUG3A.json","graph_json":"https://pith.science/api/pith-number/LBXMV7JMMBLK2IKAMAZ5IKUG3A/graph.json","events_json":"https://pith.science/api/pith-number/LBXMV7JMMBLK2IKAMAZ5IKUG3A/events.json","paper":"https://pith.science/paper/LBXMV7JM"},"agent_actions":{"view_html":"https://pith.science/pith/LBXMV7JMMBLK2IKAMAZ5IKUG3A","download_json":"https://pith.science/pith/LBXMV7JMMBLK2IKAMAZ5IKUG3A.json","view_paper":"https://pith.science/paper/LBXMV7JM","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1707.03397&json=true","fetch_graph":"https://pith.science/api/pith-number/LBXMV7JMMBLK2IKAMAZ5IKUG3A/graph.json","fetch_events":"https://pith.science/api/pith-number/LBXMV7JMMBLK2IKAMAZ5IKUG3A/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/LBXMV7JMMBLK2IKAMAZ5IKUG3A/action/timestamp_anchor","attest_storage":"https://pith.science/pith/LBXMV7JMMBLK2IKAMAZ5IKUG3A/action/storage_attestation","attest_author":"https://pith.science/pith/LBXMV7JMMBLK2IKAMAZ5IKUG3A/action/author_attestation","sign_citation":"https://pith.science/pith/LBXMV7JMMBLK2IKAMAZ5IKUG3A/action/citation_signature","submit_replication":"https://pith.science/pith/LBXMV7JMMBLK2IKAMAZ5IKUG3A/action/replication_record"}},"created_at":"2026-05-18T00:23:45.569177+00:00","updated_at":"2026-05-18T00:23:45.569177+00:00"}