{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:EMRRW5LFXBAHIUODZNFPEEJUSZ","short_pith_number":"pith:EMRRW5LF","schema_version":"1.0","canonical_sha256":"23231b7565b8407451c3cb4af211349667cbcccf33bb9b562abc8cc3b6f57406","source":{"kind":"arxiv","id":"1607.03486","version":2},"attestation_state":"computed","paper":{"title":"Simulating galaxy formation with black hole driven thermal and kinetic feedback","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Annalisa Pillepich, Dylan Nelson, Federico Marinacci, Jill Naiman, Lars Hernquist, Mark Vogelsberger, Paul Torrey, Rainer Weinberger, R\\\"udiger Pakmor, Shy Genel, Volker Springel","submitted_at":"2016-07-12T20:00:00Z","abstract_excerpt":"The inefficiency of star formation in massive elliptical galaxies is widely believed to be caused by the interactions of an active galactic nucleus (AGN) with the surrounding gas. Achieving a sufficiently rapid reddening of moderately massive galaxies without expelling too many baryons has however proven difficult for hydrodynamical simulations of galaxy formation, prompting us to explore a new model for the accretion and feedback effects of supermassive black holes. For high accretion rates relative to the Eddington limit, we assume that a fraction of the accreted rest mass energy heats the s"},"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":"1607.03486","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2016-07-12T20:00:00Z","cross_cats_sorted":[],"title_canon_sha256":"f24ea168ba344aae23e6c4d79c20c65f58e7c3027187459a97a084daecb4579b","abstract_canon_sha256":"c50a2068f3a4cc2208e6c835a31dee35dc1ef8ec3b4f7555fab466e9eafbbda6"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T21:45:03.319588Z","signature_b64":"blJicEkla28tEClcUUuzqa93fZID5A1j8QTtL+sysXT2CAvYcFiAASZoq33uQkBP6g3oDs+DxVvUrdLhnTLKAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"23231b7565b8407451c3cb4af211349667cbcccf33bb9b562abc8cc3b6f57406","last_reissued_at":"2026-07-04T21:45:03.319094Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T21:45:03.319094Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Simulating galaxy formation with black hole driven thermal and kinetic feedback","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Annalisa Pillepich, Dylan Nelson, Federico Marinacci, Jill Naiman, Lars Hernquist, Mark Vogelsberger, Paul Torrey, Rainer Weinberger, R\\\"udiger Pakmor, Shy Genel, Volker Springel","submitted_at":"2016-07-12T20:00:00Z","abstract_excerpt":"The inefficiency of star formation in massive elliptical galaxies is widely believed to be caused by the interactions of an active galactic nucleus (AGN) with the surrounding gas. Achieving a sufficiently rapid reddening of moderately massive galaxies without expelling too many baryons has however proven difficult for hydrodynamical simulations of galaxy formation, prompting us to explore a new model for the accretion and feedback effects of supermassive black holes. For high accretion rates relative to the Eddington limit, we assume that a fraction of the accreted rest mass energy heats the s"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1607.03486","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/1607.03486/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":"1607.03486","created_at":"2026-07-04T21:45:03.319150+00:00"},{"alias_kind":"arxiv_version","alias_value":"1607.03486v2","created_at":"2026-07-04T21:45:03.319150+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1607.03486","created_at":"2026-07-04T21:45:03.319150+00:00"},{"alias_kind":"pith_short_12","alias_value":"EMRRW5LFXBAH","created_at":"2026-07-04T21:45:03.319150+00:00"},{"alias_kind":"pith_short_16","alias_value":"EMRRW5LFXBAHIUOD","created_at":"2026-07-04T21:45:03.319150+00:00"},{"alias_kind":"pith_short_8","alias_value":"EMRRW5LF","created_at":"2026-07-04T21:45:03.319150+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":64,"internal_anchor_count":49,"sample":[{"citing_arxiv_id":"2607.07793","citing_title":"Tracing black hole and galaxy growth across environments since cosmic noon","ref_index":15,"is_internal_anchor":true},{"citing_arxiv_id":"2606.26234","citing_title":"Lyman-Alpha Forest and its Cross-Correlation with High-Redshift Galaxies in Effective Field Theory at the Field Level","ref_index":68,"is_internal_anchor":true},{"citing_arxiv_id":"2605.00349","citing_title":"A Universal Dance of Galactic Disks: Ubiquitous Precession and Its Implications","ref_index":61,"is_internal_anchor":true},{"citing_arxiv_id":"2606.09616","citing_title":"Blowing star formation away in AGN hosts (BAH) -- V: The Feeding-Feedback Cycle in local AGNs as revealed by their stellar populations","ref_index":110,"is_internal_anchor":true},{"citing_arxiv_id":"2606.27426","citing_title":"Too shy to spin? Cosmic wallflowers as proto-globular clusters","ref_index":288,"is_internal_anchor":true},{"citing_arxiv_id":"2605.31077","citing_title":"Super-Eddington accretion of black holes in early nuclear bursts gives birth to Little Red Dots","ref_index":62,"is_internal_anchor":true},{"citing_arxiv_id":"2606.02688","citing_title":"NOEMA$^\\rm{3D}$: A deep view of cold gas flows in a barred spiral galaxy at $z\\sim1$","ref_index":6,"is_internal_anchor":true},{"citing_arxiv_id":"2606.05355","citing_title":"Bulk vs. turbulent motions at the centres of galaxy clusters: AGN-driven turbulence according to TNG-Cluster","ref_index":94,"is_internal_anchor":true},{"citing_arxiv_id":"2606.05006","citing_title":"A Measurement of the Thermal and Ionization State of the IGM at $z < 0.5$","ref_index":119,"is_internal_anchor":true},{"citing_arxiv_id":"2606.10038","citing_title":"Learning the Universe with the 2nd Generation of CAMELS: Varying 35 parameters of the IllustrisTNG model in (50Mpc/h)^3 boxes","ref_index":96,"is_internal_anchor":true},{"citing_arxiv_id":"2606.10036","citing_title":"Learning the Universe at High Redshifts: Impact of Accretion Modeling on Early Black Hole Growth","ref_index":95,"is_internal_anchor":true},{"citing_arxiv_id":"2606.09616","citing_title":"Blowing star formation away in AGN hosts (BAH) -- V: The Feeding-Feedback Cycle in local AGNs as revealed by their stellar populations","ref_index":110,"is_internal_anchor":true},{"citing_arxiv_id":"2606.09817","citing_title":"Satellite compaction pathways: environmental drivers shaping dwarf galaxy corpulence in the TNG50 simulation","ref_index":4,"is_internal_anchor":true},{"citing_arxiv_id":"2606.10022","citing_title":"Learning the Universe with PRFM-vol: Introducing a new subgrid model for star formation in cosmological simulations","ref_index":52,"is_internal_anchor":true},{"citing_arxiv_id":"2606.09997","citing_title":"A universal model for the accretion rates and formation times of dark matter halos","ref_index":108,"is_internal_anchor":true},{"citing_arxiv_id":"2606.10020","citing_title":"The Manticore Project II: Bayesian digital twins of cosmic structure across the SDSS and BOSS volumes","ref_index":147,"is_internal_anchor":true},{"citing_arxiv_id":"2606.12511","citing_title":"Unification models of Active Galactic Nuclei","ref_index":231,"is_internal_anchor":true},{"citing_arxiv_id":"2606.12851","citing_title":"Supermassive Black Hole Assembly from Heavy Seeds with Dynamical Friction in the BRAHMA Simulations: Implications for JWST, LISA, and the Local Universe","ref_index":135,"is_internal_anchor":true},{"citing_arxiv_id":"2606.18352","citing_title":"TNG SAM: Bridging Hydrodynamical Complexity and Semi-Analytic Efficiency to Model Galaxy Formation","ref_index":25,"is_internal_anchor":true},{"citing_arxiv_id":"2606.18082","citing_title":"Variability in Cosmological Hydrodynamical Simulations: how Stochastic Processes, Numerical Effects, and Reproducibility Limits impact Predictability","ref_index":117,"is_internal_anchor":true},{"citing_arxiv_id":"2606.18382","citing_title":"The Lumina Project: Intergalactic Clumping and Recombination Sinks","ref_index":61,"is_internal_anchor":true},{"citing_arxiv_id":"2606.19099","citing_title":"IllustrisTNG50 angular momentum maps: tracing the morpho-kinematic evolution of galaxies","ref_index":8,"is_internal_anchor":true},{"citing_arxiv_id":"2606.20175","citing_title":"A Consistent Comparison of Intracluster Light Assembly in Simulations I. Redshift Evolution and Progenitor Galaxies","ref_index":146,"is_internal_anchor":true},{"citing_arxiv_id":"2606.23798","citing_title":"The PICO-Cluster Project: presenting the galaxy cluster sample and studying magnetic field growth, Faraday rotation and Braginskii heating","ref_index":227,"is_internal_anchor":true},{"citing_arxiv_id":"2606.27182","citing_title":"Forward-modelling the Tolman and distance-duality tests with IllustrisTNG","ref_index":47,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/EMRRW5LFXBAHIUODZNFPEEJUSZ","json":"https://pith.science/pith/EMRRW5LFXBAHIUODZNFPEEJUSZ.json","graph_json":"https://pith.science/api/pith-number/EMRRW5LFXBAHIUODZNFPEEJUSZ/graph.json","events_json":"https://pith.science/api/pith-number/EMRRW5LFXBAHIUODZNFPEEJUSZ/events.json","paper":"https://pith.science/paper/EMRRW5LF"},"agent_actions":{"view_html":"https://pith.science/pith/EMRRW5LFXBAHIUODZNFPEEJUSZ","download_json":"https://pith.science/pith/EMRRW5LFXBAHIUODZNFPEEJUSZ.json","view_paper":"https://pith.science/paper/EMRRW5LF","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1607.03486&json=true","fetch_graph":"https://pith.science/api/pith-number/EMRRW5LFXBAHIUODZNFPEEJUSZ/graph.json","fetch_events":"https://pith.science/api/pith-number/EMRRW5LFXBAHIUODZNFPEEJUSZ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/EMRRW5LFXBAHIUODZNFPEEJUSZ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/EMRRW5LFXBAHIUODZNFPEEJUSZ/action/storage_attestation","attest_author":"https://pith.science/pith/EMRRW5LFXBAHIUODZNFPEEJUSZ/action/author_attestation","sign_citation":"https://pith.science/pith/EMRRW5LFXBAHIUODZNFPEEJUSZ/action/citation_signature","submit_replication":"https://pith.science/pith/EMRRW5LFXBAHIUODZNFPEEJUSZ/action/replication_record"}},"created_at":"2026-07-04T21:45:03.319150+00:00","updated_at":"2026-07-04T21:45:03.319150+00:00"}