{"work":{"id":"3bc0d074-1f4f-4d3e-89b5-918a814fc688","openalex_id":null,"doi":null,"arxiv_id":"astro-ph/0003365","raw_key":null,"title":"Cold and Fuzzy Dark Matter","authors":null,"authors_text":"W","year":2000,"venue":"astro-ph","abstract":"Cold dark matter (CDM) models predict small-scale structure in excess of observations of the cores and abundance of dwarf galaxies. These problems might be solved, and the virtues of CDM models retained, even without postulating {\\it ad hoc} dark matter particle or field interactions, if the dark matter is composed of ultra-light scalar particles (m ~ 10^{-22}eV), initially in a (cold) Bose-Einstein condensate, similar to axion dark matter models. The wave properties of the dark matter stabilize gravitational collapse providing halo cores and sharply suppressing small-scale linear power.","external_url":"https://arxiv.org/abs/astro-ph/0003365","cited_by_count":null,"metadata_source":"pith","metadata_fetched_at":"2026-05-25T04:30:19.556391+00:00","pith_arxiv_id":"astro-ph/0003365","created_at":"2026-05-09T05:50:27.818479+00:00","updated_at":"2026-06-05T21:23:00.469572+00:00","title_quality_ok":false,"display_title":"Cold and Fuzzy Dark Matter","render_title":"Cold and Fuzzy Dark Matter"},"hub":{"state":{"work_id":"3bc0d074-1f4f-4d3e-89b5-918a814fc688","tier":"hub","tier_reason":"10+ Pith inbound or 1,000+ external citations","pith_inbound_count":27,"external_cited_by_count":null,"distinct_field_count":3,"first_pith_cited_at":"2019-07-12T11:38:03+00:00","last_pith_cited_at":"2026-05-22T03:48:41+00:00","author_build_status":"not_needed","summary_status":"needed","contexts_status":"needed","graph_status":"needed","ask_index_status":"not_needed","reader_status":"not_needed","recognition_status":"not_needed","updated_at":"2026-06-06T19:30:54.762290+00:00","tier_text":"hub"},"tier":"hub","role_counts":[{"context_role":"background","n":14}],"polarity_counts":[{"context_polarity":"background","n":14}],"runs":{},"summary":{},"graph":{},"authors":[]}}