{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:PP4FU3S7NH7GHOA4VYMJQVO6CJ","short_pith_number":"pith:PP4FU3S7","schema_version":"1.0","canonical_sha256":"7bf85a6e5f69fe63b81cae189855de1265ef21b7ccd202969e44395792abbe2d","source":{"kind":"arxiv","id":"1608.01327","version":2},"attestation_state":"computed","paper":{"title":"NIHAO XI: Formation of Ultra-Diffuse Galaxies by outflows","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Aaron A. Dutton (NYUAD), Andrea V. Macci\\`o (NYUAD), Arianna Di Cintio (DARK), Aura C. Obreja (NYUAD), Avishai Dekel (HUJI), Chris B. Brook (UAM)","submitted_at":"2016-08-03T20:04:58Z","abstract_excerpt":"We address the origin of Ultra-Diffuse Galaxies (UDGs), which have stellar masses typical of dwarf galaxies but effective radii of Milky Way-sized objects. Their formation mechanism, and whether they are failed $\\rm L_{\\star}$ galaxies or diffuse dwarfs, are challenging issues. Using zoom-in cosmological simulations from the NIHAO project, we show that UDG analogues form naturally in medium-mass haloes due to episodes of gas outflows associated with star formation. The simulated UDGs live in isolated haloes of masses $10^{10-11}\\rm M_{\\odot}$, have stellar masses of $10^{7-8.5}\\rm M_{\\odot}$, "},"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":"1608.01327","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2016-08-03T20:04:58Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"3e37eece6e14c99d26e90a740fc326529d3ee8a792e3f7a321e8d17e236b545d","abstract_canon_sha256":"57edc594ee6cd9382c26c1d9b1524185775a1afadaa176204b304174e1dc595c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:55:12.800053Z","signature_b64":"2GFsV7LJ/2gVsKCi3kmc8CheM41MbJP5xoXp5xZyuj5eMcr4ZGBqWhfg/h5i6HOS8ruUstNuS0bbQmuNrUREDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7bf85a6e5f69fe63b81cae189855de1265ef21b7ccd202969e44395792abbe2d","last_reissued_at":"2026-05-18T00:55:12.799475Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:55:12.799475Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"NIHAO XI: Formation of Ultra-Diffuse Galaxies by outflows","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Aaron A. Dutton (NYUAD), Andrea V. Macci\\`o (NYUAD), Arianna Di Cintio (DARK), Aura C. Obreja (NYUAD), Avishai Dekel (HUJI), Chris B. Brook (UAM)","submitted_at":"2016-08-03T20:04:58Z","abstract_excerpt":"We address the origin of Ultra-Diffuse Galaxies (UDGs), which have stellar masses typical of dwarf galaxies but effective radii of Milky Way-sized objects. Their formation mechanism, and whether they are failed $\\rm L_{\\star}$ galaxies or diffuse dwarfs, are challenging issues. Using zoom-in cosmological simulations from the NIHAO project, we show that UDG analogues form naturally in medium-mass haloes due to episodes of gas outflows associated with star formation. The simulated UDGs live in isolated haloes of masses $10^{10-11}\\rm M_{\\odot}$, have stellar masses of $10^{7-8.5}\\rm M_{\\odot}$, "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1608.01327","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":"1608.01327","created_at":"2026-05-18T00:55:12.799569+00:00"},{"alias_kind":"arxiv_version","alias_value":"1608.01327v2","created_at":"2026-05-18T00:55:12.799569+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1608.01327","created_at":"2026-05-18T00:55:12.799569+00:00"},{"alias_kind":"pith_short_12","alias_value":"PP4FU3S7NH7G","created_at":"2026-05-18T12:30:39.010887+00:00"},{"alias_kind":"pith_short_16","alias_value":"PP4FU3S7NH7GHOA4","created_at":"2026-05-18T12:30:39.010887+00:00"},{"alias_kind":"pith_short_8","alias_value":"PP4FU3S7","created_at":"2026-05-18T12:30:39.010887+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":4,"sample":[{"citing_arxiv_id":"2504.02476","citing_title":"Globular cluster distributions as a dynamical probe of dark matter","ref_index":65,"is_internal_anchor":true},{"citing_arxiv_id":"2605.21598","citing_title":"Advancing the detection of low surface brightness galaxies. I. ATTILA: multi-tAsking deTecTIon tool for Lsb gAlaxies","ref_index":183,"is_internal_anchor":true},{"citing_arxiv_id":"2605.17253","citing_title":"HI Observations of Baryon-Dominated Dwarf Galaxy Candidates","ref_index":138,"is_internal_anchor":true},{"citing_arxiv_id":"2605.13842","citing_title":"From DES to KiDS: Domain adaptation for cross-survey detection of low-surface-brightness galaxies","ref_index":212,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/PP4FU3S7NH7GHOA4VYMJQVO6CJ","json":"https://pith.science/pith/PP4FU3S7NH7GHOA4VYMJQVO6CJ.json","graph_json":"https://pith.science/api/pith-number/PP4FU3S7NH7GHOA4VYMJQVO6CJ/graph.json","events_json":"https://pith.science/api/pith-number/PP4FU3S7NH7GHOA4VYMJQVO6CJ/events.json","paper":"https://pith.science/paper/PP4FU3S7"},"agent_actions":{"view_html":"https://pith.science/pith/PP4FU3S7NH7GHOA4VYMJQVO6CJ","download_json":"https://pith.science/pith/PP4FU3S7NH7GHOA4VYMJQVO6CJ.json","view_paper":"https://pith.science/paper/PP4FU3S7","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1608.01327&json=true","fetch_graph":"https://pith.science/api/pith-number/PP4FU3S7NH7GHOA4VYMJQVO6CJ/graph.json","fetch_events":"https://pith.science/api/pith-number/PP4FU3S7NH7GHOA4VYMJQVO6CJ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/PP4FU3S7NH7GHOA4VYMJQVO6CJ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/PP4FU3S7NH7GHOA4VYMJQVO6CJ/action/storage_attestation","attest_author":"https://pith.science/pith/PP4FU3S7NH7GHOA4VYMJQVO6CJ/action/author_attestation","sign_citation":"https://pith.science/pith/PP4FU3S7NH7GHOA4VYMJQVO6CJ/action/citation_signature","submit_replication":"https://pith.science/pith/PP4FU3S7NH7GHOA4VYMJQVO6CJ/action/replication_record"}},"created_at":"2026-05-18T00:55:12.799569+00:00","updated_at":"2026-05-18T00:55:12.799569+00:00"}