{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:A7PWOK6TT7XEGAUJPONTW4X3YN","short_pith_number":"pith:A7PWOK6T","schema_version":"1.0","canonical_sha256":"07df672bd39fee4302897b9b3b72fbc34259b189630db106f398483ad3c371f6","source":{"kind":"arxiv","id":"2507.00705","version":1},"attestation_state":"computed","paper":{"title":"Ultralight fuzzy dark matter review","license":"http://creativecommons.org/licenses/by-sa/4.0/","headline":"","cross_cats":["astro-ph.GA","hep-ph","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"Andrew Eberhardt, Elisa G. M. Ferreira","submitted_at":"2025-07-01T12:04:24Z","abstract_excerpt":"Ultralight dark matter refers to the lightest potential dark matter candidates. We will focus on the mass range that has been studied using astrophysical and cosmological observations, corresponding to a mass $10^{-24} \\, \\mathrm{eV} \\lesssim m \\lesssim 10^{-18} \\, \\mathrm{eV}$. We will discuss the motivations for this mass range. The most studied model in this range corresponds to a minimally coupled, single, classical, spin-0 field comprising all dark matter. However, the work exploring extensions of this model (for example, higher spin, self-coupled, multiple field, and mixed models) will b"},"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":"2507.00705","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by-sa/4.0/","primary_cat":"astro-ph.CO","submitted_at":"2025-07-01T12:04:24Z","cross_cats_sorted":["astro-ph.GA","hep-ph","hep-th"],"title_canon_sha256":"2afb0b943bfe2bc4e334d194c2b2511137e4b675d432fd2f167b74f4c83745d2","abstract_canon_sha256":"8bdff9d4e91eb0aba1c1708e5ceb8765989d4592ba4d91e56b1498de08d4b0b3"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T11:30:13.254486Z","signature_b64":"xGuK6QvAmDEEybAPD1iIjo4Py25AZ8x3Msoc8qXV1IIL7rbaCGlRYnbU6BZ+KUwt7/LoLUHTc6cHOM875S3EBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"07df672bd39fee4302897b9b3b72fbc34259b189630db106f398483ad3c371f6","last_reissued_at":"2026-07-05T11:30:13.253744Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T11:30:13.253744Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Ultralight fuzzy dark matter review","license":"http://creativecommons.org/licenses/by-sa/4.0/","headline":"","cross_cats":["astro-ph.GA","hep-ph","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"Andrew Eberhardt, Elisa G. M. Ferreira","submitted_at":"2025-07-01T12:04:24Z","abstract_excerpt":"Ultralight dark matter refers to the lightest potential dark matter candidates. We will focus on the mass range that has been studied using astrophysical and cosmological observations, corresponding to a mass $10^{-24} \\, \\mathrm{eV} \\lesssim m \\lesssim 10^{-18} \\, \\mathrm{eV}$. We will discuss the motivations for this mass range. The most studied model in this range corresponds to a minimally coupled, single, classical, spin-0 field comprising all dark matter. However, the work exploring extensions of this model (for example, higher spin, self-coupled, multiple field, and mixed models) will b"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2507.00705","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/2507.00705/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":"2507.00705","created_at":"2026-07-05T11:30:13.253841+00:00"},{"alias_kind":"arxiv_version","alias_value":"2507.00705v1","created_at":"2026-07-05T11:30:13.253841+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2507.00705","created_at":"2026-07-05T11:30:13.253841+00:00"},{"alias_kind":"pith_short_12","alias_value":"A7PWOK6TT7XE","created_at":"2026-07-05T11:30:13.253841+00:00"},{"alias_kind":"pith_short_16","alias_value":"A7PWOK6TT7XEGAUJ","created_at":"2026-07-05T11:30:13.253841+00:00"},{"alias_kind":"pith_short_8","alias_value":"A7PWOK6T","created_at":"2026-07-05T11:30:13.253841+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":15,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.10055","citing_title":"Identical Bosons, large occupation numbers and classical field description","ref_index":8,"is_internal_anchor":false},{"citing_arxiv_id":"2606.06969","citing_title":"Lyman-$\\alpha$ forest constraints on pure and mixed fuzzy dark matter","ref_index":20,"is_internal_anchor":false},{"citing_arxiv_id":"2607.00072","citing_title":"Precision Solar System Dynamics for Ultralight Dark Matter Search","ref_index":13,"is_internal_anchor":false},{"citing_arxiv_id":"2606.07008","citing_title":"Macroscopic Quantum Interference in Dark Matter Wave Scattering with MICROSCOPE","ref_index":14,"is_internal_anchor":false},{"citing_arxiv_id":"2605.22685","citing_title":"Dwarf Galaxy Constraints on Interacting Fermionic Dark Matter","ref_index":10,"is_internal_anchor":false},{"citing_arxiv_id":"2510.15046","citing_title":"Multi-species Dark Matter with Warmth and Randomness","ref_index":29,"is_internal_anchor":false},{"citing_arxiv_id":"2510.17977","citing_title":"Growth of Structure in Multi-species Wave Dark Matter","ref_index":11,"is_internal_anchor":false},{"citing_arxiv_id":"2605.17211","citing_title":"Constraints on Self-Interacting Fuzzy Dark Matter from the Stellar Kinematics of the Dwarf Galaxy Leo II","ref_index":6,"is_internal_anchor":false},{"citing_arxiv_id":"2509.23231","citing_title":"Fuzzy dark matter simulations","ref_index":50,"is_internal_anchor":false},{"citing_arxiv_id":"2510.02130","citing_title":"In-situ globular clusters in alternative dark matter Milky Way galaxies: a first approach to fuzzy and core-like dark matter theories","ref_index":21,"is_internal_anchor":false},{"citing_arxiv_id":"2511.04400","citing_title":"Artificial Precision Polarization Array: Sensitivity for the axion-like dark matter with clock satellites","ref_index":17,"is_internal_anchor":false},{"citing_arxiv_id":"2511.10617","citing_title":"Dark Matter from Holography","ref_index":7,"is_internal_anchor":false},{"citing_arxiv_id":"2602.11512","citing_title":"Stone Skipping Black Holes in Ultralight Dark Matter Solitons","ref_index":21,"is_internal_anchor":false},{"citing_arxiv_id":"2605.11071","citing_title":"Time-dependent signals of new physics at the LHC","ref_index":5,"is_internal_anchor":false},{"citing_arxiv_id":"2605.11600","citing_title":"A Reusable Hierarchical Framework for Joint Inference of Ultralight-Dark-Matter Mass and Core-Halo Scaling","ref_index":7,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/A7PWOK6TT7XEGAUJPONTW4X3YN","json":"https://pith.science/pith/A7PWOK6TT7XEGAUJPONTW4X3YN.json","graph_json":"https://pith.science/api/pith-number/A7PWOK6TT7XEGAUJPONTW4X3YN/graph.json","events_json":"https://pith.science/api/pith-number/A7PWOK6TT7XEGAUJPONTW4X3YN/events.json","paper":"https://pith.science/paper/A7PWOK6T"},"agent_actions":{"view_html":"https://pith.science/pith/A7PWOK6TT7XEGAUJPONTW4X3YN","download_json":"https://pith.science/pith/A7PWOK6TT7XEGAUJPONTW4X3YN.json","view_paper":"https://pith.science/paper/A7PWOK6T","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2507.00705&json=true","fetch_graph":"https://pith.science/api/pith-number/A7PWOK6TT7XEGAUJPONTW4X3YN/graph.json","fetch_events":"https://pith.science/api/pith-number/A7PWOK6TT7XEGAUJPONTW4X3YN/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/A7PWOK6TT7XEGAUJPONTW4X3YN/action/timestamp_anchor","attest_storage":"https://pith.science/pith/A7PWOK6TT7XEGAUJPONTW4X3YN/action/storage_attestation","attest_author":"https://pith.science/pith/A7PWOK6TT7XEGAUJPONTW4X3YN/action/author_attestation","sign_citation":"https://pith.science/pith/A7PWOK6TT7XEGAUJPONTW4X3YN/action/citation_signature","submit_replication":"https://pith.science/pith/A7PWOK6TT7XEGAUJPONTW4X3YN/action/replication_record"}},"created_at":"2026-07-05T11:30:13.253841+00:00","updated_at":"2026-07-05T11:30:13.253841+00:00"}