{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:KGGDBGQM3MOCPL3YAZDAQJ4QXR","short_pith_number":"pith:KGGDBGQM","schema_version":"1.0","canonical_sha256":"518c309a0cdb1c27af780646082790bc5f326bda48446f17844be69694311ee9","source":{"kind":"arxiv","id":"1811.03627","version":1},"attestation_state":"computed","paper":{"title":"Low-mass halo perturbations in strong gravitational lenses at redshift z$\\sim$0.5 are consistent with CDM","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"E. Ritondale, G. Despali, J. P. McKean, L. V. E Koopmans, M. W. Auger, S. Vegetti","submitted_at":"2018-11-08T19:00:01Z","abstract_excerpt":"We use a sample of 17 strong gravitational lens systems from the BELLS GALLERY survey to quantify the amount of low-mass dark matter haloes within the lensing galaxies and along their lines of sight, and to constrain the properties of dark matter. Based on a detection criterion of 10$\\sigma$, we report no significant detection in any of the lenses. Using the sensitivity function at the 10-$\\sigma$ level, we have calculated the predicted number of detectable cold dark matter (CDM) line-of-sight haloes to be $\\mu_{l} = 1.17\\pm1.08$, in agreement with our null detection. Assuming a detection sens"},"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":"1811.03627","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2018-11-08T19:00:01Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"f336e3e5570e614f4ae2ec4fc8ed3079e42675a2fbb9d395046ac8dc9131cd86","abstract_canon_sha256":"bbe19fe4f3a99f861accdb39f66b1d4919932e7ac596d7a712b5084143b964b8"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:53:24.580851Z","signature_b64":"8lgDC0WCMUHdOvFhBkwnUygE7YA/qEOP0FCFEH8D8GngqhkU8d9EAHwshNb12g0KQx+2inqtRVS8fjuBSfpIAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"518c309a0cdb1c27af780646082790bc5f326bda48446f17844be69694311ee9","last_reissued_at":"2026-05-17T23:53:24.580136Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:53:24.580136Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Low-mass halo perturbations in strong gravitational lenses at redshift z$\\sim$0.5 are consistent with CDM","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"E. Ritondale, G. Despali, J. P. McKean, L. V. E Koopmans, M. W. Auger, S. Vegetti","submitted_at":"2018-11-08T19:00:01Z","abstract_excerpt":"We use a sample of 17 strong gravitational lens systems from the BELLS GALLERY survey to quantify the amount of low-mass dark matter haloes within the lensing galaxies and along their lines of sight, and to constrain the properties of dark matter. Based on a detection criterion of 10$\\sigma$, we report no significant detection in any of the lenses. Using the sensitivity function at the 10-$\\sigma$ level, we have calculated the predicted number of detectable cold dark matter (CDM) line-of-sight haloes to be $\\mu_{l} = 1.17\\pm1.08$, in agreement with our null detection. Assuming a detection sens"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1811.03627","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":""},"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":"1811.03627","created_at":"2026-05-17T23:53:24.580241+00:00"},{"alias_kind":"arxiv_version","alias_value":"1811.03627v1","created_at":"2026-05-17T23:53:24.580241+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1811.03627","created_at":"2026-05-17T23:53:24.580241+00:00"},{"alias_kind":"pith_short_12","alias_value":"KGGDBGQM3MOC","created_at":"2026-05-18T12:32:33.847187+00:00"},{"alias_kind":"pith_short_16","alias_value":"KGGDBGQM3MOCPL3Y","created_at":"2026-05-18T12:32:33.847187+00:00"},{"alias_kind":"pith_short_8","alias_value":"KGGDBGQM","created_at":"2026-05-18T12:32:33.847187+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.21212","citing_title":"Detection of a dark matter subhalo in the strongly lensed system PJ011646","ref_index":72,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/KGGDBGQM3MOCPL3YAZDAQJ4QXR","json":"https://pith.science/pith/KGGDBGQM3MOCPL3YAZDAQJ4QXR.json","graph_json":"https://pith.science/api/pith-number/KGGDBGQM3MOCPL3YAZDAQJ4QXR/graph.json","events_json":"https://pith.science/api/pith-number/KGGDBGQM3MOCPL3YAZDAQJ4QXR/events.json","paper":"https://pith.science/paper/KGGDBGQM"},"agent_actions":{"view_html":"https://pith.science/pith/KGGDBGQM3MOCPL3YAZDAQJ4QXR","download_json":"https://pith.science/pith/KGGDBGQM3MOCPL3YAZDAQJ4QXR.json","view_paper":"https://pith.science/paper/KGGDBGQM","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1811.03627&json=true","fetch_graph":"https://pith.science/api/pith-number/KGGDBGQM3MOCPL3YAZDAQJ4QXR/graph.json","fetch_events":"https://pith.science/api/pith-number/KGGDBGQM3MOCPL3YAZDAQJ4QXR/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/KGGDBGQM3MOCPL3YAZDAQJ4QXR/action/timestamp_anchor","attest_storage":"https://pith.science/pith/KGGDBGQM3MOCPL3YAZDAQJ4QXR/action/storage_attestation","attest_author":"https://pith.science/pith/KGGDBGQM3MOCPL3YAZDAQJ4QXR/action/author_attestation","sign_citation":"https://pith.science/pith/KGGDBGQM3MOCPL3YAZDAQJ4QXR/action/citation_signature","submit_replication":"https://pith.science/pith/KGGDBGQM3MOCPL3YAZDAQJ4QXR/action/replication_record"}},"created_at":"2026-05-17T23:53:24.580241+00:00","updated_at":"2026-05-17T23:53:24.580241+00:00"}