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Buder, J. A. Brevik, J. Connors, J. E. Tolan, J. Grayson, J. J. Bock, J. Kang, J. M. Kovac, J. P. Filippin, J. P. Kaufman, J. Willmert, K. D. Alexander, K. D. Irwin, K. G. Megerian, K. L. Thompson, K. S. Karkare, K. W. Yoon, L. Duband, M. Halpern, M. Lueker, R. Bowens-Rubin, R. O'Brient, R. Schwarz, R. V. Sudiwala, R. W. Aikin, R. W. Ogburn IV, S. A. Kernasovskiy, S. Fliescher, S. Harrison, S. J. Benton, S. Kefeli, S. R. Hildebrandt, S. Richter, The Keck Array, T. Namikawa, V. Buza, W. L. K. Wu, Z. Ahmed, Z. K. Staniszewski","submitted_at":"2016-06-06T22:52:58Z","abstract_excerpt":"We present measurements of polarization lensing using the 150 GHz maps which include all data taken by the BICEP2 & Keck Array CMB polarization experiments up to and including the 2014 observing season (BK14). Despite their modest angular resolution ($\\sim 0.5^\\circ$), the excellent sensitivity ($\\sim 3\\mu$K-arcmin) of these maps makes it possible to directly reconstruct the lensing potential using only information at larger angular scales ($\\ell\\leq 700$). From the auto-spectrum of the reconstructed potential we measure an amplitude of the spectrum to be $A^{\\phi\\phi}_{\\rm L}=1.15\\pm 0.36$ (P"},"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":"1606.01968","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2016-06-06T22:52:58Z","cross_cats_sorted":[],"title_canon_sha256":"452185232bebbd37ec7e0f7099741e65220b656ec3b2ff5283e96843e8f3d48f","abstract_canon_sha256":"af815379500f0cb0a109a546f86f6dad02c0318d6e60f2d5efee951ed59fcff5"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:53:08.097592Z","signature_b64":"57qb6E212UEQ/IrBhGFB62tiD9RVXvCSYTxKrRT0NEBUygKV5Yl4QGdZmOTUlYXWVanTnzmVSLbF0VVl+DEXCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c7971a62a390468a2f4a4e764cfb362efba0aa91341c2d1d7e7ee3d2f76850e4","last_reissued_at":"2026-05-18T00:53:08.097093Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:53:08.097093Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"BICEP2 / Keck Array VIII: Measurement of gravitational lensing from large-scale B-mode polarization","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. C. Weber, A. D. Turner, A. G. Vieregg, A. Orlando, B. G. Keating, BICEP2 Collaborations: P. A. R. Ade, B. P. Crill, B. Steinbach, C. A. Bischoff, C. B. Netterfield, C. D. Sheehy, C. Dvorkin, C. L. Kuo, C. L. Wong, C. Pryke, C. Tucker, D. Barkats, D. V. Wiebe, E. Bullock, E. Karpel, E. M. Leitch, G. C. Hilton, G. P. Teply, H. Hui, H. T. Nguyen, I. Buder, J. A. Brevik, J. Connors, J. E. Tolan, J. Grayson, J. J. Bock, J. Kang, J. M. Kovac, J. P. Filippin, J. P. Kaufman, J. Willmert, K. D. Alexander, K. D. Irwin, K. G. Megerian, K. L. Thompson, K. S. Karkare, K. W. Yoon, L. Duband, M. Halpern, M. Lueker, R. Bowens-Rubin, R. O'Brient, R. Schwarz, R. V. Sudiwala, R. W. Aikin, R. W. Ogburn IV, S. A. Kernasovskiy, S. Fliescher, S. Harrison, S. J. Benton, S. Kefeli, S. R. Hildebrandt, S. Richter, The Keck Array, T. Namikawa, V. Buza, W. L. K. Wu, Z. Ahmed, Z. K. Staniszewski","submitted_at":"2016-06-06T22:52:58Z","abstract_excerpt":"We present measurements of polarization lensing using the 150 GHz maps which include all data taken by the BICEP2 & Keck Array CMB polarization experiments up to and including the 2014 observing season (BK14). Despite their modest angular resolution ($\\sim 0.5^\\circ$), the excellent sensitivity ($\\sim 3\\mu$K-arcmin) of these maps makes it possible to directly reconstruct the lensing potential using only information at larger angular scales ($\\ell\\leq 700$). From the auto-spectrum of the reconstructed potential we measure an amplitude of the spectrum to be $A^{\\phi\\phi}_{\\rm L}=1.15\\pm 0.36$ (P"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1606.01968","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":"1606.01968","created_at":"2026-05-18T00:53:08.097170+00:00"},{"alias_kind":"arxiv_version","alias_value":"1606.01968v2","created_at":"2026-05-18T00:53:08.097170+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1606.01968","created_at":"2026-05-18T00:53:08.097170+00:00"},{"alias_kind":"pith_short_12","alias_value":"Y6LRUYVDSBDI","created_at":"2026-05-18T12:30:53.716459+00:00"},{"alias_kind":"pith_short_16","alias_value":"Y6LRUYVDSBDIUL2K","created_at":"2026-05-18T12:30:53.716459+00:00"},{"alias_kind":"pith_short_8","alias_value":"Y6LRUYVD","created_at":"2026-05-18T12:30:53.716459+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2605.23489","citing_title":"A comparison between Galactic magnetic field models and polarized synchrotron emission with C-BASS at 4.76 GHz and S-PASS at 2.3 GHz","ref_index":48,"is_internal_anchor":true},{"citing_arxiv_id":"2304.05202","citing_title":"The Atacama Cosmology Telescope: A Measurement of the DR6 CMB Lensing Power Spectrum and its Implications for Structure Growth","ref_index":20,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/Y6LRUYVDSBDIUL2KJZ3EZ6ZWF3","json":"https://pith.science/pith/Y6LRUYVDSBDIUL2KJZ3EZ6ZWF3.json","graph_json":"https://pith.science/api/pith-number/Y6LRUYVDSBDIUL2KJZ3EZ6ZWF3/graph.json","events_json":"https://pith.science/api/pith-number/Y6LRUYVDSBDIUL2KJZ3EZ6ZWF3/events.json","paper":"https://pith.science/paper/Y6LRUYVD"},"agent_actions":{"view_html":"https://pith.science/pith/Y6LRUYVDSBDIUL2KJZ3EZ6ZWF3","download_json":"https://pith.science/pith/Y6LRUYVDSBDIUL2KJZ3EZ6ZWF3.json","view_paper":"https://pith.science/paper/Y6LRUYVD","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1606.01968&json=true","fetch_graph":"https://pith.science/api/pith-number/Y6LRUYVDSBDIUL2KJZ3EZ6ZWF3/graph.json","fetch_events":"https://pith.science/api/pith-number/Y6LRUYVDSBDIUL2KJZ3EZ6ZWF3/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/Y6LRUYVDSBDIUL2KJZ3EZ6ZWF3/action/timestamp_anchor","attest_storage":"https://pith.science/pith/Y6LRUYVDSBDIUL2KJZ3EZ6ZWF3/action/storage_attestation","attest_author":"https://pith.science/pith/Y6LRUYVDSBDIUL2KJZ3EZ6ZWF3/action/author_attestation","sign_citation":"https://pith.science/pith/Y6LRUYVDSBDIUL2KJZ3EZ6ZWF3/action/citation_signature","submit_replication":"https://pith.science/pith/Y6LRUYVDSBDIUL2KJZ3EZ6ZWF3/action/replication_record"}},"created_at":"2026-05-18T00:53:08.097170+00:00","updated_at":"2026-05-18T00:53:08.097170+00:00"}