{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:OKL4TUMZKEY6TXNC5FG6KK75K3","short_pith_number":"pith:OKL4TUMZ","schema_version":"1.0","canonical_sha256":"7297c9d1995131e9dda2e94de52bfd56d8e9b6ca2770b36ccc039dd1546d15f3","source":{"kind":"arxiv","id":"1707.02980","version":1},"attestation_state":"computed","paper":{"title":"Dust Properties of [CII] Detected z $\\sim$ 5.5 Galaxies: New HST/WFC3 Near-IR Observations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Andreas L. Faisst, Caitlin M. Casey, Dominik A. Riechers, Ivana Bari\\v{s}i\\'c, Jeyhan S. Kartaltepe, Kevin C. Cooke, Nick Z. Scoville, Peter L. Capak, Riccardo Pavesi, Vernesa Smol\\v{c}i\\'c","submitted_at":"2017-07-10T18:00:00Z","abstract_excerpt":"We examine the rest-frame ultra-violet (UV) properties of 10 [CII]$\\lambda158\\,{\\rm \\mu m}$$-$detected galaxies at $z\\sim5.5$ in COSMOS using new HST/WFC3 near-infrared imaging. Together with pre-existing $158\\,{\\rm \\mu m}-$continuum and [CII] line measurements by ALMA, we study their dust attenuation properties on the IRX-$\\beta$ diagram, which connects the total dust emission ($\\propto$ IRX=log($L_{FIR}/L_{1600}$)) to the line-of-sight dust column ($\\propto\\beta$). We find systematically bluer UV continuum spectral slopes ($\\beta$) compared to previous low-resolution ground-based measurement"},"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":"1707.02980","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2017-07-10T18:00:00Z","cross_cats_sorted":[],"title_canon_sha256":"5dd874e30f41e61ad779eaf2843e7639fb7c8c807947a23a2ef386373358700e","abstract_canon_sha256":"bde610b4d5fa057dedacf752072166fda279b0e8014a2b579d4c1249a2d70522"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:37:18.137188Z","signature_b64":"ilTjJCnAwL0iXCuuOUMLEXvdFkX/WCnTn+I/fPD5zcQfm4SyzgkDSUUujayI6zLVbvpupNqXaSLg9uoMmMJ7Cw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7297c9d1995131e9dda2e94de52bfd56d8e9b6ca2770b36ccc039dd1546d15f3","last_reissued_at":"2026-05-18T00:37:18.136653Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:37:18.136653Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Dust Properties of [CII] Detected z $\\sim$ 5.5 Galaxies: New HST/WFC3 Near-IR Observations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Andreas L. Faisst, Caitlin M. Casey, Dominik A. Riechers, Ivana Bari\\v{s}i\\'c, Jeyhan S. Kartaltepe, Kevin C. Cooke, Nick Z. Scoville, Peter L. Capak, Riccardo Pavesi, Vernesa Smol\\v{c}i\\'c","submitted_at":"2017-07-10T18:00:00Z","abstract_excerpt":"We examine the rest-frame ultra-violet (UV) properties of 10 [CII]$\\lambda158\\,{\\rm \\mu m}$$-$detected galaxies at $z\\sim5.5$ in COSMOS using new HST/WFC3 near-infrared imaging. Together with pre-existing $158\\,{\\rm \\mu m}-$continuum and [CII] line measurements by ALMA, we study their dust attenuation properties on the IRX-$\\beta$ diagram, which connects the total dust emission ($\\propto$ IRX=log($L_{FIR}/L_{1600}$)) to the line-of-sight dust column ($\\propto\\beta$). We find systematically bluer UV continuum spectral slopes ($\\beta$) compared to previous low-resolution ground-based measurement"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1707.02980","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":"1707.02980","created_at":"2026-05-18T00:37:18.136745+00:00"},{"alias_kind":"arxiv_version","alias_value":"1707.02980v1","created_at":"2026-05-18T00:37:18.136745+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1707.02980","created_at":"2026-05-18T00:37:18.136745+00:00"},{"alias_kind":"pith_short_12","alias_value":"OKL4TUMZKEY6","created_at":"2026-05-18T12:31:34.259226+00:00"},{"alias_kind":"pith_short_16","alias_value":"OKL4TUMZKEY6TXNC","created_at":"2026-05-18T12:31:34.259226+00:00"},{"alias_kind":"pith_short_8","alias_value":"OKL4TUMZ","created_at":"2026-05-18T12:31:34.259226+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":69,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/OKL4TUMZKEY6TXNC5FG6KK75K3","json":"https://pith.science/pith/OKL4TUMZKEY6TXNC5FG6KK75K3.json","graph_json":"https://pith.science/api/pith-number/OKL4TUMZKEY6TXNC5FG6KK75K3/graph.json","events_json":"https://pith.science/api/pith-number/OKL4TUMZKEY6TXNC5FG6KK75K3/events.json","paper":"https://pith.science/paper/OKL4TUMZ"},"agent_actions":{"view_html":"https://pith.science/pith/OKL4TUMZKEY6TXNC5FG6KK75K3","download_json":"https://pith.science/pith/OKL4TUMZKEY6TXNC5FG6KK75K3.json","view_paper":"https://pith.science/paper/OKL4TUMZ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1707.02980&json=true","fetch_graph":"https://pith.science/api/pith-number/OKL4TUMZKEY6TXNC5FG6KK75K3/graph.json","fetch_events":"https://pith.science/api/pith-number/OKL4TUMZKEY6TXNC5FG6KK75K3/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/OKL4TUMZKEY6TXNC5FG6KK75K3/action/timestamp_anchor","attest_storage":"https://pith.science/pith/OKL4TUMZKEY6TXNC5FG6KK75K3/action/storage_attestation","attest_author":"https://pith.science/pith/OKL4TUMZKEY6TXNC5FG6KK75K3/action/author_attestation","sign_citation":"https://pith.science/pith/OKL4TUMZKEY6TXNC5FG6KK75K3/action/citation_signature","submit_replication":"https://pith.science/pith/OKL4TUMZKEY6TXNC5FG6KK75K3/action/replication_record"}},"created_at":"2026-05-18T00:37:18.136745+00:00","updated_at":"2026-05-18T00:37:18.136745+00:00"}