{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:L46MSEQSP46EMQHMGM7NY2YEUE","short_pith_number":"pith:L46MSEQS","schema_version":"1.0","canonical_sha256":"5f3cc912127f3c4640ec333edc6b04a118058430c2963edfdadbe4923611ff6f","source":{"kind":"arxiv","id":"2208.03282","version":2},"attestation_state":"computed","paper":{"title":"Constraining bosonic asymmetric dark matter with neutron star mass-radius measurements","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"","cross_cats":["hep-ph","nucl-th"],"primary_cat":"astro-ph.HE","authors_text":"Anna Watts, Chanda Prescod-Weinstein, Geert Raaijmakers, Nathan Rutherford","submitted_at":"2022-08-05T17:11:30Z","abstract_excerpt":"Neutron stars can accumulate asymmetric dark matter (ADM) in their interiors, which affects the neutron star's measurable properties and makes compact objects prime targets to search for ADM. In this work, we use Bayesian inference to explore potential neutron star mass-radius measurements, from current and future x-ray telescopes, to constrain the bosonic ADM parameters for the case where bosonic ADM has accumulated in the neutron star interior. We find that the current uncertainties in the baryonic equation of state do not allow for constraints on the ADM parameter space to be made. However,"},"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":"2208.03282","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2022-08-05T17:11:30Z","cross_cats_sorted":["hep-ph","nucl-th"],"title_canon_sha256":"6f568f401fe470671ac0ed3c897be3d66513138644c4659eeb9ec739a1ab8e24","abstract_canon_sha256":"fd9b91e073d7c6b17ccda26c96d663fdee15c92538536ac78f10fbbe1bde1a59"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T06:16:46.957762Z","signature_b64":"MVY+hb9PyCpoPzGr8N9p+yN5iFzrFoT4aP14P/XT8xaTjcnVJ/mrVK7LZ28lVfnspFc5G217rp6QMerjBxkbDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"5f3cc912127f3c4640ec333edc6b04a118058430c2963edfdadbe4923611ff6f","last_reissued_at":"2026-07-05T06:16:46.957349Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T06:16:46.957349Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Constraining bosonic asymmetric dark matter with neutron star mass-radius measurements","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"","cross_cats":["hep-ph","nucl-th"],"primary_cat":"astro-ph.HE","authors_text":"Anna Watts, Chanda Prescod-Weinstein, Geert Raaijmakers, Nathan Rutherford","submitted_at":"2022-08-05T17:11:30Z","abstract_excerpt":"Neutron stars can accumulate asymmetric dark matter (ADM) in their interiors, which affects the neutron star's measurable properties and makes compact objects prime targets to search for ADM. In this work, we use Bayesian inference to explore potential neutron star mass-radius measurements, from current and future x-ray telescopes, to constrain the bosonic ADM parameters for the case where bosonic ADM has accumulated in the neutron star interior. We find that the current uncertainties in the baryonic equation of state do not allow for constraints on the ADM parameter space to be made. However,"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2208.03282","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2208.03282/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":"2208.03282","created_at":"2026-07-05T06:16:46.957402+00:00"},{"alias_kind":"arxiv_version","alias_value":"2208.03282v2","created_at":"2026-07-05T06:16:46.957402+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2208.03282","created_at":"2026-07-05T06:16:46.957402+00:00"},{"alias_kind":"pith_short_12","alias_value":"L46MSEQSP46E","created_at":"2026-07-05T06:16:46.957402+00:00"},{"alias_kind":"pith_short_16","alias_value":"L46MSEQSP46EMQHM","created_at":"2026-07-05T06:16:46.957402+00:00"},{"alias_kind":"pith_short_8","alias_value":"L46MSEQS","created_at":"2026-07-05T06:16:46.957402+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.27456","citing_title":"The crust of dark-matter admixed neutron stars: bulk properties and torsional oscillations","ref_index":14,"is_internal_anchor":false},{"citing_arxiv_id":"2503.19691","citing_title":"Strongly Interacting Dark Matter admixed Neutron Stars","ref_index":95,"is_internal_anchor":false},{"citing_arxiv_id":"2511.07567","citing_title":"Dark Matter Heating in Evolving Proto-Neutron Stars: A Two-Fluid Approach","ref_index":70,"is_internal_anchor":false},{"citing_arxiv_id":"2604.04560","citing_title":"Neutron star with dark matter using vector portal","ref_index":15,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/L46MSEQSP46EMQHMGM7NY2YEUE","json":"https://pith.science/pith/L46MSEQSP46EMQHMGM7NY2YEUE.json","graph_json":"https://pith.science/api/pith-number/L46MSEQSP46EMQHMGM7NY2YEUE/graph.json","events_json":"https://pith.science/api/pith-number/L46MSEQSP46EMQHMGM7NY2YEUE/events.json","paper":"https://pith.science/paper/L46MSEQS"},"agent_actions":{"view_html":"https://pith.science/pith/L46MSEQSP46EMQHMGM7NY2YEUE","download_json":"https://pith.science/pith/L46MSEQSP46EMQHMGM7NY2YEUE.json","view_paper":"https://pith.science/paper/L46MSEQS","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2208.03282&json=true","fetch_graph":"https://pith.science/api/pith-number/L46MSEQSP46EMQHMGM7NY2YEUE/graph.json","fetch_events":"https://pith.science/api/pith-number/L46MSEQSP46EMQHMGM7NY2YEUE/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/L46MSEQSP46EMQHMGM7NY2YEUE/action/timestamp_anchor","attest_storage":"https://pith.science/pith/L46MSEQSP46EMQHMGM7NY2YEUE/action/storage_attestation","attest_author":"https://pith.science/pith/L46MSEQSP46EMQHMGM7NY2YEUE/action/author_attestation","sign_citation":"https://pith.science/pith/L46MSEQSP46EMQHMGM7NY2YEUE/action/citation_signature","submit_replication":"https://pith.science/pith/L46MSEQSP46EMQHMGM7NY2YEUE/action/replication_record"}},"created_at":"2026-07-05T06:16:46.957402+00:00","updated_at":"2026-07-05T06:16:46.957402+00:00"}