{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:2VL44EBTL6VNW3S2KNK4PXNCVP","short_pith_number":"pith:2VL44EBT","schema_version":"1.0","canonical_sha256":"d557ce10335faadb6e5a5355c7dda2abcf6bc9637fad66fafb33e9771fb0cdf6","source":{"kind":"arxiv","id":"1802.05720","version":2},"attestation_state":"computed","paper":{"title":"Obscured star-formation in bright z ~ 7 Lyman-break galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"D.J.McLeod, J.S.Dunlop, N.Bourne, R.A.A.Bowler, R.J.McLure","submitted_at":"2018-02-15T19:00:02Z","abstract_excerpt":"We present Atacama Large Millimeter/Submillimeter Array observations of the rest-frame far-infrared (FIR) dust continuum emission of six bright Lyman-break galaxies (LBGs) at $z \\simeq 7$. One LBG is detected ($5.2\\sigma$ at peak emission), while the others remain individually undetected at the $3\\sigma$ level. The average FIR luminosity of the sample is found to be $L_{\\rm FIR} \\simeq 2 \\times 10^{11}\\,{\\rm L}_{\\odot}$, corresponding to an obscured star-formation rate (SFR) that is comparable to that inferred from the unobscured UV emission. In comparison to the infrared excess (IRX$\\,=L_{\\rm"},"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":"1802.05720","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2018-02-15T19:00:02Z","cross_cats_sorted":[],"title_canon_sha256":"38946ca65df70311556b093dc93397b1bfdbb52f22631c377dc670da8b66ea30","abstract_canon_sha256":"b2c0e5944a2d96cf174e1920e5e6ed173290928d2d030cd9a38bb55239ce8d60"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:06:40.668086Z","signature_b64":"m/h5rEaa/MSTgeWxPlRXwB1GJj+HoZYZBq6I2ZaEWGCn1kI8EX+LvmuJNU3ZW5TOgIcodjmCUsnnZlsnkfh9BA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d557ce10335faadb6e5a5355c7dda2abcf6bc9637fad66fafb33e9771fb0cdf6","last_reissued_at":"2026-05-18T00:06:40.667597Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:06:40.667597Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Obscured star-formation in bright z ~ 7 Lyman-break galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"D.J.McLeod, J.S.Dunlop, N.Bourne, R.A.A.Bowler, R.J.McLure","submitted_at":"2018-02-15T19:00:02Z","abstract_excerpt":"We present Atacama Large Millimeter/Submillimeter Array observations of the rest-frame far-infrared (FIR) dust continuum emission of six bright Lyman-break galaxies (LBGs) at $z \\simeq 7$. One LBG is detected ($5.2\\sigma$ at peak emission), while the others remain individually undetected at the $3\\sigma$ level. The average FIR luminosity of the sample is found to be $L_{\\rm FIR} \\simeq 2 \\times 10^{11}\\,{\\rm L}_{\\odot}$, corresponding to an obscured star-formation rate (SFR) that is comparable to that inferred from the unobscured UV emission. In comparison to the infrared excess (IRX$\\,=L_{\\rm"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1802.05720","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":"1802.05720","created_at":"2026-05-18T00:06:40.667668+00:00"},{"alias_kind":"arxiv_version","alias_value":"1802.05720v2","created_at":"2026-05-18T00:06:40.667668+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1802.05720","created_at":"2026-05-18T00:06:40.667668+00:00"},{"alias_kind":"pith_short_12","alias_value":"2VL44EBTL6VN","created_at":"2026-05-18T12:32:02.567920+00:00"},{"alias_kind":"pith_short_16","alias_value":"2VL44EBTL6VNW3S2","created_at":"2026-05-18T12:32:02.567920+00:00"},{"alias_kind":"pith_short_8","alias_value":"2VL44EBT","created_at":"2026-05-18T12:32:02.567920+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.13472","citing_title":"First Light And Reionization Epoch Simulations (FLARES) XXI: The UV Indices of Galaxies in the Early Universe","ref_index":94,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/2VL44EBTL6VNW3S2KNK4PXNCVP","json":"https://pith.science/pith/2VL44EBTL6VNW3S2KNK4PXNCVP.json","graph_json":"https://pith.science/api/pith-number/2VL44EBTL6VNW3S2KNK4PXNCVP/graph.json","events_json":"https://pith.science/api/pith-number/2VL44EBTL6VNW3S2KNK4PXNCVP/events.json","paper":"https://pith.science/paper/2VL44EBT"},"agent_actions":{"view_html":"https://pith.science/pith/2VL44EBTL6VNW3S2KNK4PXNCVP","download_json":"https://pith.science/pith/2VL44EBTL6VNW3S2KNK4PXNCVP.json","view_paper":"https://pith.science/paper/2VL44EBT","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1802.05720&json=true","fetch_graph":"https://pith.science/api/pith-number/2VL44EBTL6VNW3S2KNK4PXNCVP/graph.json","fetch_events":"https://pith.science/api/pith-number/2VL44EBTL6VNW3S2KNK4PXNCVP/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/2VL44EBTL6VNW3S2KNK4PXNCVP/action/timestamp_anchor","attest_storage":"https://pith.science/pith/2VL44EBTL6VNW3S2KNK4PXNCVP/action/storage_attestation","attest_author":"https://pith.science/pith/2VL44EBTL6VNW3S2KNK4PXNCVP/action/author_attestation","sign_citation":"https://pith.science/pith/2VL44EBTL6VNW3S2KNK4PXNCVP/action/citation_signature","submit_replication":"https://pith.science/pith/2VL44EBTL6VNW3S2KNK4PXNCVP/action/replication_record"}},"created_at":"2026-05-18T00:06:40.667668+00:00","updated_at":"2026-05-18T00:06:40.667668+00:00"}