{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2007:M6NO33CSO2LXM72DQWB2ALUXO4","short_pith_number":"pith:M6NO33CS","schema_version":"1.0","canonical_sha256":"679aedec527697767f438583a02e97771f20facceb90b5f39cf529e696c3e1a3","source":{"kind":"arxiv","id":"0711.4803","version":1},"attestation_state":"computed","paper":{"title":"Stellar Feedback in Dwarf Galaxy Formation","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"H. M. P. Couchman, James Wadsley, Sergey Mashchenko","submitted_at":"2007-11-29T19:31:38Z","abstract_excerpt":"Dwarf galaxies pose significant challenges for cosmological models. In particular, current models predict a dark matter density that is divergent at the center, in sharp contrast with observations which indicate an approximately constant central density core. Energy feedback, from supernova explosions and stellar winds, has been proposed as a major factor shaping the evolution of dwarf galaxies. We present detailed cosmological simulations with sufficient resolution both to model the relevant physical processes and to directly assess the impact of stellar feedback on observable properties of d"},"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":"0711.4803","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2007-11-29T19:31:38Z","cross_cats_sorted":[],"title_canon_sha256":"0f306e1c3544cfdac9b9abd118ac653b8748b79bf32108bb53b5ffc6ee56986d","abstract_canon_sha256":"6be5405cc99df46d5d63861d806629d3662919c5537ebb0a8d02d91d247deb60"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T17:06:59.889484Z","signature_b64":"W4M5lbOhvdDI7b9zPkq4XW8lpQocwuJLZWSrBflDO35Lrcsd/F29c6I5plpr2bek4QWEJCS9PM+B2+tHL74qBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"679aedec527697767f438583a02e97771f20facceb90b5f39cf529e696c3e1a3","last_reissued_at":"2026-07-04T17:06:59.889059Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T17:06:59.889059Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Stellar Feedback in Dwarf Galaxy Formation","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"H. M. P. Couchman, James Wadsley, Sergey Mashchenko","submitted_at":"2007-11-29T19:31:38Z","abstract_excerpt":"Dwarf galaxies pose significant challenges for cosmological models. In particular, current models predict a dark matter density that is divergent at the center, in sharp contrast with observations which indicate an approximately constant central density core. Energy feedback, from supernova explosions and stellar winds, has been proposed as a major factor shaping the evolution of dwarf galaxies. We present detailed cosmological simulations with sufficient resolution both to model the relevant physical processes and to directly assess the impact of stellar feedback on observable properties of d"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0711.4803","kind":"arxiv","version":1},"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/0711.4803/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":"0711.4803","created_at":"2026-07-04T17:06:59.889119+00:00"},{"alias_kind":"arxiv_version","alias_value":"0711.4803v1","created_at":"2026-07-04T17:06:59.889119+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0711.4803","created_at":"2026-07-04T17:06:59.889119+00:00"},{"alias_kind":"pith_short_12","alias_value":"M6NO33CSO2LX","created_at":"2026-07-04T17:06:59.889119+00:00"},{"alias_kind":"pith_short_16","alias_value":"M6NO33CSO2LXM72D","created_at":"2026-07-04T17:06:59.889119+00:00"},{"alias_kind":"pith_short_8","alias_value":"M6NO33CS","created_at":"2026-07-04T17:06:59.889119+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":3,"sample":[{"citing_arxiv_id":"2606.08628","citing_title":"Thermal emission from dark matter-heated neutron stars in the Galactic Center","ref_index":48,"is_internal_anchor":true},{"citing_arxiv_id":"2606.00221","citing_title":"It's Not Just Star Formation: A trend of low dark matter densities in the Andromeda dwarf galaxy system","ref_index":156,"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":209,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/M6NO33CSO2LXM72DQWB2ALUXO4","json":"https://pith.science/pith/M6NO33CSO2LXM72DQWB2ALUXO4.json","graph_json":"https://pith.science/api/pith-number/M6NO33CSO2LXM72DQWB2ALUXO4/graph.json","events_json":"https://pith.science/api/pith-number/M6NO33CSO2LXM72DQWB2ALUXO4/events.json","paper":"https://pith.science/paper/M6NO33CS"},"agent_actions":{"view_html":"https://pith.science/pith/M6NO33CSO2LXM72DQWB2ALUXO4","download_json":"https://pith.science/pith/M6NO33CSO2LXM72DQWB2ALUXO4.json","view_paper":"https://pith.science/paper/M6NO33CS","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0711.4803&json=true","fetch_graph":"https://pith.science/api/pith-number/M6NO33CSO2LXM72DQWB2ALUXO4/graph.json","fetch_events":"https://pith.science/api/pith-number/M6NO33CSO2LXM72DQWB2ALUXO4/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/M6NO33CSO2LXM72DQWB2ALUXO4/action/timestamp_anchor","attest_storage":"https://pith.science/pith/M6NO33CSO2LXM72DQWB2ALUXO4/action/storage_attestation","attest_author":"https://pith.science/pith/M6NO33CSO2LXM72DQWB2ALUXO4/action/author_attestation","sign_citation":"https://pith.science/pith/M6NO33CSO2LXM72DQWB2ALUXO4/action/citation_signature","submit_replication":"https://pith.science/pith/M6NO33CSO2LXM72DQWB2ALUXO4/action/replication_record"}},"created_at":"2026-07-04T17:06:59.889119+00:00","updated_at":"2026-07-04T17:06:59.889119+00:00"}