{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:37BSCOLNRAYZDQTSPTZ6IFXR7Z","short_pith_number":"pith:37BSCOLN","schema_version":"1.0","canonical_sha256":"dfc321396d883191c2727cf3e416f1fe53c2a9ed2cc4efb381fd326912863d92","source":{"kind":"arxiv","id":"1608.02587","version":2},"attestation_state":"computed","paper":{"title":"Nebular Emission Line Ratios in z~2-3 Star-Forming Galaxies with KBSS-MOSFIRE: Exploring the Impact of Ionization, Excitation, and Nitrogen-to-Oxygen Ratio","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Allison L. Strom, Charles C. Steidel, Gwen C. Rudie, Max Pettini, Naveen A. Reddy, Ryan F. Trainor","submitted_at":"2016-08-08T20:00:02Z","abstract_excerpt":"We present a detailed study of the rest-optical (3600-7000 Angstrom) nebular spectra of ~380 star-forming galaxies at z~2-3 obtained with Keck/MOSFIRE as part of the Keck Baryonic Structure Survey (KBSS). The KBSS-MOSFIRE sample is representative of star-forming galaxies at these redshifts, with stellar masses M*=10^9-10^11.5 M_sun and star formation rates SFR=3-1000 M_sun/yr. We focus on robust measurements of many strong diagnostic emission lines for individual galaxies: [O II]3727,3729, [Ne III]3869, H-beta, [O III]4960,5008, [N II]6549,6585, H-alpha, and [S II]6718,6732. Comparisons with o"},"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":"1608.02587","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2016-08-08T20:00:02Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"a424f989e10731c3f6ccc6396f7b4117dac80d3815f0ec944b60f6f2055701b4","abstract_canon_sha256":"974deccfcb2daeacac1ef3aacccb3e3c010803e6424ed8943a33c6899737a8d8"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:50:19.538576Z","signature_b64":"KLkDLSQfCcYG27fwzZOez0WHgtsQ0eCMyNaCHljntzVE3g2vIwWy4pQWnP8VNtC1mtjIjV+sHmDAw63kMPvVAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"dfc321396d883191c2727cf3e416f1fe53c2a9ed2cc4efb381fd326912863d92","last_reissued_at":"2026-05-18T00:50:19.538001Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:50:19.538001Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Nebular Emission Line Ratios in z~2-3 Star-Forming Galaxies with KBSS-MOSFIRE: Exploring the Impact of Ionization, Excitation, and Nitrogen-to-Oxygen Ratio","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Allison L. Strom, Charles C. Steidel, Gwen C. Rudie, Max Pettini, Naveen A. Reddy, Ryan F. Trainor","submitted_at":"2016-08-08T20:00:02Z","abstract_excerpt":"We present a detailed study of the rest-optical (3600-7000 Angstrom) nebular spectra of ~380 star-forming galaxies at z~2-3 obtained with Keck/MOSFIRE as part of the Keck Baryonic Structure Survey (KBSS). The KBSS-MOSFIRE sample is representative of star-forming galaxies at these redshifts, with stellar masses M*=10^9-10^11.5 M_sun and star formation rates SFR=3-1000 M_sun/yr. We focus on robust measurements of many strong diagnostic emission lines for individual galaxies: [O II]3727,3729, [Ne III]3869, H-beta, [O III]4960,5008, [N II]6549,6585, H-alpha, and [S II]6718,6732. Comparisons with o"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1608.02587","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":"1608.02587","created_at":"2026-05-18T00:50:19.538108+00:00"},{"alias_kind":"arxiv_version","alias_value":"1608.02587v2","created_at":"2026-05-18T00:50:19.538108+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1608.02587","created_at":"2026-05-18T00:50:19.538108+00:00"},{"alias_kind":"pith_short_12","alias_value":"37BSCOLNRAYZ","created_at":"2026-05-18T12:29:55.572404+00:00"},{"alias_kind":"pith_short_16","alias_value":"37BSCOLNRAYZDQTS","created_at":"2026-05-18T12:29:55.572404+00:00"},{"alias_kind":"pith_short_8","alias_value":"37BSCOLN","created_at":"2026-05-18T12:29:55.572404+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.20590","citing_title":"Spider-Webb: enhanced star formation in low-mass galaxies within the Spiderweb protocluster revealed by JWST Pa$\\beta$ narrow-band imaging","ref_index":104,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/37BSCOLNRAYZDQTSPTZ6IFXR7Z","json":"https://pith.science/pith/37BSCOLNRAYZDQTSPTZ6IFXR7Z.json","graph_json":"https://pith.science/api/pith-number/37BSCOLNRAYZDQTSPTZ6IFXR7Z/graph.json","events_json":"https://pith.science/api/pith-number/37BSCOLNRAYZDQTSPTZ6IFXR7Z/events.json","paper":"https://pith.science/paper/37BSCOLN"},"agent_actions":{"view_html":"https://pith.science/pith/37BSCOLNRAYZDQTSPTZ6IFXR7Z","download_json":"https://pith.science/pith/37BSCOLNRAYZDQTSPTZ6IFXR7Z.json","view_paper":"https://pith.science/paper/37BSCOLN","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1608.02587&json=true","fetch_graph":"https://pith.science/api/pith-number/37BSCOLNRAYZDQTSPTZ6IFXR7Z/graph.json","fetch_events":"https://pith.science/api/pith-number/37BSCOLNRAYZDQTSPTZ6IFXR7Z/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/37BSCOLNRAYZDQTSPTZ6IFXR7Z/action/timestamp_anchor","attest_storage":"https://pith.science/pith/37BSCOLNRAYZDQTSPTZ6IFXR7Z/action/storage_attestation","attest_author":"https://pith.science/pith/37BSCOLNRAYZDQTSPTZ6IFXR7Z/action/author_attestation","sign_citation":"https://pith.science/pith/37BSCOLNRAYZDQTSPTZ6IFXR7Z/action/citation_signature","submit_replication":"https://pith.science/pith/37BSCOLNRAYZDQTSPTZ6IFXR7Z/action/replication_record"}},"created_at":"2026-05-18T00:50:19.538108+00:00","updated_at":"2026-05-18T00:50:19.538108+00:00"}