{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:KKXY46SBCHF7FRCZ6CAZ7U4IN4","short_pith_number":"pith:KKXY46SB","schema_version":"1.0","canonical_sha256":"52af8e7a4111cbf2c459f0819fd3886f0d75a7adef2c0c3f5383ccc9e7e73700","source":{"kind":"arxiv","id":"1409.4804","version":2},"attestation_state":"computed","paper":{"title":"VLT/X-shooter spectroscopy of the afterglow of the Swift GRB 130606A: Chemical abundances and reionisation at $z\\sim6$","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"A. De Cia, A. de Ugarte Postigo, A. J. Levan, B. Milvang-Jensen, C. Ledoux, D. Malesani, D. Xu, G. Tagliaferri, H. Flores, J. Datson, J. Hjorth, J.-K. Krogager, J. P. U. Fynbo, J. Sollerman, K. Mikkelsen, K. Wiersema, L. Kaper, M. Sparre, N. Aghanim, N. R. Tanvir, O. E. Hartoog, P. Goldoni, P. Jakobsson, P. M{\\o}ller, P. M. Vreeswijk, R. Salinas, S. Covino, S. D. Vergani, T. Goto, T. Kr\\\"uhler, V. D'Elia","submitted_at":"2014-09-16T21:05:32Z","abstract_excerpt":"The reionisation of the Universe is thought to have ended around z~6, as inferred from spectroscopy of distant bright background sources, such as quasars (QSO) and gamma-ray burst (GRB) afterglows. Furthermore, spectroscopy of a GRB afterglow provides insight in its host galaxy, which is often too dim and distant to study otherwise. We present the high S/N VLT/X-shooter spectrum of GRB130606A at z=5.913. We aim to measure the degree of ionisation of the IGM between 5.02<z<5.84 and to study the chemical abundance pattern and dust content of its host galaxy. We measured the flux decrement due to"},"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":"1409.4804","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2014-09-16T21:05:32Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"a3323dc9ed32aa7eb6d9fd998fc561c31ccd720ca4b4aa05d965bd2238dd5980","abstract_canon_sha256":"c831d8f66d95e0025dd5b224ab18bc61211c06eadb66ed97b19148e4206ed58b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:34:50.892061Z","signature_b64":"Gr2k4Sa/VQMKyEvqAM4qTY3tvPgVXLGHTM0z38oFm1RwRpmnxuANuugwHA34bE2BKownM0mt4aaAS93O4xDDAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"52af8e7a4111cbf2c459f0819fd3886f0d75a7adef2c0c3f5383ccc9e7e73700","last_reissued_at":"2026-05-18T01:34:50.891524Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:34:50.891524Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"VLT/X-shooter spectroscopy of the afterglow of the Swift GRB 130606A: Chemical abundances and reionisation at $z\\sim6$","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"A. De Cia, A. de Ugarte Postigo, A. J. Levan, B. Milvang-Jensen, C. Ledoux, D. Malesani, D. Xu, G. Tagliaferri, H. Flores, J. Datson, J. Hjorth, J.-K. Krogager, J. P. U. Fynbo, J. Sollerman, K. Mikkelsen, K. Wiersema, L. Kaper, M. Sparre, N. Aghanim, N. R. Tanvir, O. E. Hartoog, P. Goldoni, P. Jakobsson, P. M{\\o}ller, P. M. Vreeswijk, R. Salinas, S. Covino, S. D. Vergani, T. Goto, T. Kr\\\"uhler, V. D'Elia","submitted_at":"2014-09-16T21:05:32Z","abstract_excerpt":"The reionisation of the Universe is thought to have ended around z~6, as inferred from spectroscopy of distant bright background sources, such as quasars (QSO) and gamma-ray burst (GRB) afterglows. Furthermore, spectroscopy of a GRB afterglow provides insight in its host galaxy, which is often too dim and distant to study otherwise. We present the high S/N VLT/X-shooter spectrum of GRB130606A at z=5.913. We aim to measure the degree of ionisation of the IGM between 5.02<z<5.84 and to study the chemical abundance pattern and dust content of its host galaxy. We measured the flux decrement due to"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1409.4804","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":"1409.4804","created_at":"2026-05-18T01:34:50.891596+00:00"},{"alias_kind":"arxiv_version","alias_value":"1409.4804v2","created_at":"2026-05-18T01:34:50.891596+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1409.4804","created_at":"2026-05-18T01:34:50.891596+00:00"},{"alias_kind":"pith_short_12","alias_value":"KKXY46SBCHF7","created_at":"2026-05-18T12:28:35.611951+00:00"},{"alias_kind":"pith_short_16","alias_value":"KKXY46SBCHF7FRCZ","created_at":"2026-05-18T12:28:35.611951+00:00"},{"alias_kind":"pith_short_8","alias_value":"KKXY46SB","created_at":"2026-05-18T12:28:35.611951+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/KKXY46SBCHF7FRCZ6CAZ7U4IN4","json":"https://pith.science/pith/KKXY46SBCHF7FRCZ6CAZ7U4IN4.json","graph_json":"https://pith.science/api/pith-number/KKXY46SBCHF7FRCZ6CAZ7U4IN4/graph.json","events_json":"https://pith.science/api/pith-number/KKXY46SBCHF7FRCZ6CAZ7U4IN4/events.json","paper":"https://pith.science/paper/KKXY46SB"},"agent_actions":{"view_html":"https://pith.science/pith/KKXY46SBCHF7FRCZ6CAZ7U4IN4","download_json":"https://pith.science/pith/KKXY46SBCHF7FRCZ6CAZ7U4IN4.json","view_paper":"https://pith.science/paper/KKXY46SB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1409.4804&json=true","fetch_graph":"https://pith.science/api/pith-number/KKXY46SBCHF7FRCZ6CAZ7U4IN4/graph.json","fetch_events":"https://pith.science/api/pith-number/KKXY46SBCHF7FRCZ6CAZ7U4IN4/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/KKXY46SBCHF7FRCZ6CAZ7U4IN4/action/timestamp_anchor","attest_storage":"https://pith.science/pith/KKXY46SBCHF7FRCZ6CAZ7U4IN4/action/storage_attestation","attest_author":"https://pith.science/pith/KKXY46SBCHF7FRCZ6CAZ7U4IN4/action/author_attestation","sign_citation":"https://pith.science/pith/KKXY46SBCHF7FRCZ6CAZ7U4IN4/action/citation_signature","submit_replication":"https://pith.science/pith/KKXY46SBCHF7FRCZ6CAZ7U4IN4/action/replication_record"}},"created_at":"2026-05-18T01:34:50.891596+00:00","updated_at":"2026-05-18T01:34:50.891596+00:00"}