{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:MASPEHL7KKZCDXRUUCPLIWSEFB","short_pith_number":"pith:MASPEHL7","schema_version":"1.0","canonical_sha256":"6024f21d7f52b221de34a09eb45a44287809e4a8274df6eec7442a473a5bccf2","source":{"kind":"arxiv","id":"1402.4026","version":1},"attestation_state":"computed","paper":{"title":"VLT/X-shooter spectroscopy of the GRB 120327A afterglow","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","astro-ph.GA"],"primary_cat":"astro-ph.HE","authors_text":"A. de Ugarte Postigo, A. J. Castro-Tirado, C. Ledoux, D. J. Watson, D. Malesani, D. Xu, E. Pian, F. Calura, F. Matteucci R. Sanchez-Ramirez, G. Tagliaferri, J. Gorosabel, J. P. U. Fynbo, L. Kaper, N. Tanvir, O. E. Hartoog, P. Goldoni, S. Covino, S. D. Vergani, S. Piranomonte, S. Savaglio, T. Munoz-Darias, V. D'Elia","submitted_at":"2014-02-17T15:14:12Z","abstract_excerpt":"We present a study of the environment of the Swift long gamma-ray burst GRB 120327A at z ~2.8 through optical spectroscopy of its afterglow. We analyzed medium-resolution, multi-epoch spectroscopic observations (~7000 - 12000, corresponding to ~ 15 - 23 km/s, S/N = 15- 30 and wavelength range 3000-25000AA) of the optical afterglow of GRB 120327A, taken with X-shooter at the VLT 2.13 and 27.65 hr after the GRB trigger. The first epoch spectrum shows that the ISM in the GRB host galaxy at z = 2.8145 is extremely rich in absorption features, with three components contributing to the line profiles"},"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":"1402.4026","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2014-02-17T15:14:12Z","cross_cats_sorted":["astro-ph.CO","astro-ph.GA"],"title_canon_sha256":"3fe61bda7aa38d2b2175d7fecc17f5996fa4a508ebd1ae675853b914cc21d5c8","abstract_canon_sha256":"539a505107a2b0b7611919e3f2fa9453ff1686fa964dc25119aa1d61e1339f03"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:54:47.967615Z","signature_b64":"4uANiaLevkSmRZUtBrKLCDjfoWLz6dWS1tIKFngXOnMJlmG/yamZVhneRXfI/6agUjAh4hZ/US8ZHleg03deBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"6024f21d7f52b221de34a09eb45a44287809e4a8274df6eec7442a473a5bccf2","last_reissued_at":"2026-05-18T02:54:47.967199Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:54:47.967199Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"VLT/X-shooter spectroscopy of the GRB 120327A afterglow","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","astro-ph.GA"],"primary_cat":"astro-ph.HE","authors_text":"A. de Ugarte Postigo, A. J. Castro-Tirado, C. Ledoux, D. J. Watson, D. Malesani, D. Xu, E. Pian, F. Calura, F. Matteucci R. Sanchez-Ramirez, G. Tagliaferri, J. Gorosabel, J. P. U. Fynbo, L. Kaper, N. Tanvir, O. E. Hartoog, P. Goldoni, S. Covino, S. D. Vergani, S. Piranomonte, S. Savaglio, T. Munoz-Darias, V. D'Elia","submitted_at":"2014-02-17T15:14:12Z","abstract_excerpt":"We present a study of the environment of the Swift long gamma-ray burst GRB 120327A at z ~2.8 through optical spectroscopy of its afterglow. We analyzed medium-resolution, multi-epoch spectroscopic observations (~7000 - 12000, corresponding to ~ 15 - 23 km/s, S/N = 15- 30 and wavelength range 3000-25000AA) of the optical afterglow of GRB 120327A, taken with X-shooter at the VLT 2.13 and 27.65 hr after the GRB trigger. The first epoch spectrum shows that the ISM in the GRB host galaxy at z = 2.8145 is extremely rich in absorption features, with three components contributing to the line profiles"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1402.4026","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":"1402.4026","created_at":"2026-05-18T02:54:47.967262+00:00"},{"alias_kind":"arxiv_version","alias_value":"1402.4026v1","created_at":"2026-05-18T02:54:47.967262+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1402.4026","created_at":"2026-05-18T02:54:47.967262+00:00"},{"alias_kind":"pith_short_12","alias_value":"MASPEHL7KKZC","created_at":"2026-05-18T12:28:38.356838+00:00"},{"alias_kind":"pith_short_16","alias_value":"MASPEHL7KKZCDXRU","created_at":"2026-05-18T12:28:38.356838+00:00"},{"alias_kind":"pith_short_8","alias_value":"MASPEHL7","created_at":"2026-05-18T12:28:38.356838+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2506.13851","citing_title":"Interstellar dust production, destruction and effects of dust depletion in galaxies","ref_index":121,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/MASPEHL7KKZCDXRUUCPLIWSEFB","json":"https://pith.science/pith/MASPEHL7KKZCDXRUUCPLIWSEFB.json","graph_json":"https://pith.science/api/pith-number/MASPEHL7KKZCDXRUUCPLIWSEFB/graph.json","events_json":"https://pith.science/api/pith-number/MASPEHL7KKZCDXRUUCPLIWSEFB/events.json","paper":"https://pith.science/paper/MASPEHL7"},"agent_actions":{"view_html":"https://pith.science/pith/MASPEHL7KKZCDXRUUCPLIWSEFB","download_json":"https://pith.science/pith/MASPEHL7KKZCDXRUUCPLIWSEFB.json","view_paper":"https://pith.science/paper/MASPEHL7","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1402.4026&json=true","fetch_graph":"https://pith.science/api/pith-number/MASPEHL7KKZCDXRUUCPLIWSEFB/graph.json","fetch_events":"https://pith.science/api/pith-number/MASPEHL7KKZCDXRUUCPLIWSEFB/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/MASPEHL7KKZCDXRUUCPLIWSEFB/action/timestamp_anchor","attest_storage":"https://pith.science/pith/MASPEHL7KKZCDXRUUCPLIWSEFB/action/storage_attestation","attest_author":"https://pith.science/pith/MASPEHL7KKZCDXRUUCPLIWSEFB/action/author_attestation","sign_citation":"https://pith.science/pith/MASPEHL7KKZCDXRUUCPLIWSEFB/action/citation_signature","submit_replication":"https://pith.science/pith/MASPEHL7KKZCDXRUUCPLIWSEFB/action/replication_record"}},"created_at":"2026-05-18T02:54:47.967262+00:00","updated_at":"2026-05-18T02:54:47.967262+00:00"}