{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:MZFTYS644UZ3QADIYH22L77EWP","short_pith_number":"pith:MZFTYS64","schema_version":"1.0","canonical_sha256":"664b3c4bdce533b80068c1f5a5ffe4b3ef084d25ad05227b93fbd6b9a47cef3e","source":{"kind":"arxiv","id":"1705.05845","version":2},"attestation_state":"computed","paper":{"title":"Galaxy Formation with BECDM: I. Turbulence and relaxation of idealised haloes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"(2) MIT, (3) UC Irvine (4) University of Iceland (5) UT Austin), Anastasia Fialkov (1), Jesus Zavala (4), Lars Hernquist (1) ((1) Harvard, Mark Vogelsberger (2), Michael Boylan-Kolchin (5), Philip Mocz (1), Victor Robles (3)","submitted_at":"2017-05-16T18:00:07Z","abstract_excerpt":"We present a theoretical analysis of some unexplored aspects of relaxed Bose-Einstein condensate dark matter (BECDM) haloes. This type of ultralight bosonic scalar field dark matter is a viable alternative to the standard cold dark matter (CDM) paradigm, as it makes the same large-scale predictions as CDM and potentially overcomes CDM's small-scale problems via a galaxy-scale de Broglie wavelength. We simulate BECDM halo formation through mergers, evolved under the Schr\\\"odinger-Poisson equations. The formed haloes consist of a soliton core supported against gravitational collapse by the quant"},"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":"1705.05845","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2017-05-16T18:00:07Z","cross_cats_sorted":[],"title_canon_sha256":"62ddb58fbdd7339d76d311ca947ff2e20c55e38c244f2cdb3af44d6c30dc6aa9","abstract_canon_sha256":"2267e2901bc0172cc070d3f2f113942f3f746415075c4bcb3c8f2a7d1b857304"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:32:43.140347Z","signature_b64":"C8ZkaOapq+aAjB926tbtkAZ2alehjyJeZ+ZZ8hPIMI5ON/OQ0HTiKsW6zXgH0zaqeu33mrajyk7GfNv5+q6PBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"664b3c4bdce533b80068c1f5a5ffe4b3ef084d25ad05227b93fbd6b9a47cef3e","last_reissued_at":"2026-05-18T00:32:43.139652Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:32:43.139652Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Galaxy Formation with BECDM: I. Turbulence and relaxation of idealised haloes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"(2) MIT, (3) UC Irvine (4) University of Iceland (5) UT Austin), Anastasia Fialkov (1), Jesus Zavala (4), Lars Hernquist (1) ((1) Harvard, Mark Vogelsberger (2), Michael Boylan-Kolchin (5), Philip Mocz (1), Victor Robles (3)","submitted_at":"2017-05-16T18:00:07Z","abstract_excerpt":"We present a theoretical analysis of some unexplored aspects of relaxed Bose-Einstein condensate dark matter (BECDM) haloes. This type of ultralight bosonic scalar field dark matter is a viable alternative to the standard cold dark matter (CDM) paradigm, as it makes the same large-scale predictions as CDM and potentially overcomes CDM's small-scale problems via a galaxy-scale de Broglie wavelength. We simulate BECDM halo formation through mergers, evolved under the Schr\\\"odinger-Poisson equations. The formed haloes consist of a soliton core supported against gravitational collapse by the quant"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1705.05845","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":"1705.05845","created_at":"2026-05-18T00:32:43.139750+00:00"},{"alias_kind":"arxiv_version","alias_value":"1705.05845v2","created_at":"2026-05-18T00:32:43.139750+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1705.05845","created_at":"2026-05-18T00:32:43.139750+00:00"},{"alias_kind":"pith_short_12","alias_value":"MZFTYS644UZ3","created_at":"2026-05-18T12:31:31.346846+00:00"},{"alias_kind":"pith_short_16","alias_value":"MZFTYS644UZ3QADI","created_at":"2026-05-18T12:31:31.346846+00:00"},{"alias_kind":"pith_short_8","alias_value":"MZFTYS64","created_at":"2026-05-18T12:31:31.346846+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":4,"sample":[{"citing_arxiv_id":"2605.23206","citing_title":"Yukawa-Screened Bose-Star Condensation","ref_index":43,"is_internal_anchor":true},{"citing_arxiv_id":"2605.22901","citing_title":"A No-Go Theorem for the Mass-Radius Relation of Solitons","ref_index":15,"is_internal_anchor":true},{"citing_arxiv_id":"2406.13394","citing_title":"Gravitational Wave Birefringence from Fuzzy Dark Matter","ref_index":57,"is_internal_anchor":true},{"citing_arxiv_id":"2603.06329","citing_title":"Effects of Self-Interaction and of an Ideal Gas in Binary Mergers of Bosonic Dark Matter Cores","ref_index":8,"is_internal_anchor":true},{"citing_arxiv_id":"2604.26393","citing_title":"Tidal Heating of Stellar Clusters in Fuzzy Dark Matter Halos","ref_index":15,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/MZFTYS644UZ3QADIYH22L77EWP","json":"https://pith.science/pith/MZFTYS644UZ3QADIYH22L77EWP.json","graph_json":"https://pith.science/api/pith-number/MZFTYS644UZ3QADIYH22L77EWP/graph.json","events_json":"https://pith.science/api/pith-number/MZFTYS644UZ3QADIYH22L77EWP/events.json","paper":"https://pith.science/paper/MZFTYS64"},"agent_actions":{"view_html":"https://pith.science/pith/MZFTYS644UZ3QADIYH22L77EWP","download_json":"https://pith.science/pith/MZFTYS644UZ3QADIYH22L77EWP.json","view_paper":"https://pith.science/paper/MZFTYS64","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1705.05845&json=true","fetch_graph":"https://pith.science/api/pith-number/MZFTYS644UZ3QADIYH22L77EWP/graph.json","fetch_events":"https://pith.science/api/pith-number/MZFTYS644UZ3QADIYH22L77EWP/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/MZFTYS644UZ3QADIYH22L77EWP/action/timestamp_anchor","attest_storage":"https://pith.science/pith/MZFTYS644UZ3QADIYH22L77EWP/action/storage_attestation","attest_author":"https://pith.science/pith/MZFTYS644UZ3QADIYH22L77EWP/action/author_attestation","sign_citation":"https://pith.science/pith/MZFTYS644UZ3QADIYH22L77EWP/action/citation_signature","submit_replication":"https://pith.science/pith/MZFTYS644UZ3QADIYH22L77EWP/action/replication_record"}},"created_at":"2026-05-18T00:32:43.139750+00:00","updated_at":"2026-05-18T00:32:43.139750+00:00"}