{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:JJSMDQ7IF7JV7A3WVCDJXBGZBU","short_pith_number":"pith:JJSMDQ7I","schema_version":"1.0","canonical_sha256":"4a64c1c3e82fd35f8376a8869b84d90d3bc6b297302eb7be9c376af5270716c0","source":{"kind":"arxiv","id":"1602.06983","version":1},"attestation_state":"computed","paper":{"title":"Simulated stellar kinematics studies of high-redshift galaxies with the HARMONI Integral Field Spectrograph","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.GA","authors_text":"2, (2) ESO, 3) ((1) University of Oxford, (3) University of Hertfordshire), B. H\\\"aussler (1, F. Clarke (1), J. Devriendt (1), K. O'Brien (1), M. Tecza (1), N. Thatte (1), R.C.W. Houghton (1), Santiago, S. Kendrew (1), S. Zieleniewski (1)","submitted_at":"2016-02-22T22:00:10Z","abstract_excerpt":"We present a study into the capabilities of integrated and spatially resolved integral field spectroscopy of galaxies at z=2-4 with the future HARMONI spectrograph for the European Extremely Large Telescope (E-ELT) using the simulation pipeline, HSIM. We focus particularly on the instrument's capabilities in stellar absorption line integral field spectroscopy, which will allow us to study the stellar kinematics and stellar population characteristics. Such measurements for star-forming and passive galaxies around the peak star formation era will provide a critical insight into the star formatio"},"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":"1602.06983","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2016-02-22T22:00:10Z","cross_cats_sorted":["astro-ph.IM"],"title_canon_sha256":"353c553d96ea9da390816bc147d90d29871dca2afcaf24c8ab75b02455ff1e06","abstract_canon_sha256":"7ab4608184bfd26dd0c9061b485f8c03dfe92bbbc389e1a19dc075b22e1e18ec"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:18:28.875340Z","signature_b64":"+OVy4Ipu4putr8kZPet4iUZb7VRclcJ00WAn5/U1/iSHGNfce+6cZd7C0LvTaTIhPC5QeRUBjFj/Xr1pV0X0Dg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"4a64c1c3e82fd35f8376a8869b84d90d3bc6b297302eb7be9c376af5270716c0","last_reissued_at":"2026-05-18T01:18:28.874714Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:18:28.874714Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Simulated stellar kinematics studies of high-redshift galaxies with the HARMONI Integral Field Spectrograph","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.GA","authors_text":"2, (2) ESO, 3) ((1) University of Oxford, (3) University of Hertfordshire), B. H\\\"aussler (1, F. Clarke (1), J. Devriendt (1), K. O'Brien (1), M. Tecza (1), N. Thatte (1), R.C.W. Houghton (1), Santiago, S. Kendrew (1), S. Zieleniewski (1)","submitted_at":"2016-02-22T22:00:10Z","abstract_excerpt":"We present a study into the capabilities of integrated and spatially resolved integral field spectroscopy of galaxies at z=2-4 with the future HARMONI spectrograph for the European Extremely Large Telescope (E-ELT) using the simulation pipeline, HSIM. We focus particularly on the instrument's capabilities in stellar absorption line integral field spectroscopy, which will allow us to study the stellar kinematics and stellar population characteristics. Such measurements for star-forming and passive galaxies around the peak star formation era will provide a critical insight into the star formatio"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1602.06983","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":"1602.06983","created_at":"2026-05-18T01:18:28.874807+00:00"},{"alias_kind":"arxiv_version","alias_value":"1602.06983v1","created_at":"2026-05-18T01:18:28.874807+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1602.06983","created_at":"2026-05-18T01:18:28.874807+00:00"},{"alias_kind":"pith_short_12","alias_value":"JJSMDQ7IF7JV","created_at":"2026-05-18T12:30:25.849896+00:00"},{"alias_kind":"pith_short_16","alias_value":"JJSMDQ7IF7JV7A3W","created_at":"2026-05-18T12:30:25.849896+00:00"},{"alias_kind":"pith_short_8","alias_value":"JJSMDQ7I","created_at":"2026-05-18T12:30:25.849896+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/JJSMDQ7IF7JV7A3WVCDJXBGZBU","json":"https://pith.science/pith/JJSMDQ7IF7JV7A3WVCDJXBGZBU.json","graph_json":"https://pith.science/api/pith-number/JJSMDQ7IF7JV7A3WVCDJXBGZBU/graph.json","events_json":"https://pith.science/api/pith-number/JJSMDQ7IF7JV7A3WVCDJXBGZBU/events.json","paper":"https://pith.science/paper/JJSMDQ7I"},"agent_actions":{"view_html":"https://pith.science/pith/JJSMDQ7IF7JV7A3WVCDJXBGZBU","download_json":"https://pith.science/pith/JJSMDQ7IF7JV7A3WVCDJXBGZBU.json","view_paper":"https://pith.science/paper/JJSMDQ7I","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1602.06983&json=true","fetch_graph":"https://pith.science/api/pith-number/JJSMDQ7IF7JV7A3WVCDJXBGZBU/graph.json","fetch_events":"https://pith.science/api/pith-number/JJSMDQ7IF7JV7A3WVCDJXBGZBU/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/JJSMDQ7IF7JV7A3WVCDJXBGZBU/action/timestamp_anchor","attest_storage":"https://pith.science/pith/JJSMDQ7IF7JV7A3WVCDJXBGZBU/action/storage_attestation","attest_author":"https://pith.science/pith/JJSMDQ7IF7JV7A3WVCDJXBGZBU/action/author_attestation","sign_citation":"https://pith.science/pith/JJSMDQ7IF7JV7A3WVCDJXBGZBU/action/citation_signature","submit_replication":"https://pith.science/pith/JJSMDQ7IF7JV7A3WVCDJXBGZBU/action/replication_record"}},"created_at":"2026-05-18T01:18:28.874807+00:00","updated_at":"2026-05-18T01:18:28.874807+00:00"}