{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:2VJI4QEFCXH4SMYCKAWLXC74PY","short_pith_number":"pith:2VJI4QEF","schema_version":"1.0","canonical_sha256":"d5528e408515cfc93302502cbb8bfc7e18b6f003f6d60d9cf971e21b642ad64c","source":{"kind":"arxiv","id":"2412.07835","version":1},"attestation_state":"computed","paper":{"title":"Baryonic Ecosystem in Galaxies (BEINGMgII). Host Galaxies of Ultra-strong MgII Absorbers in Subaru Hyper Suprime-Cam Survey","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"C\\'eline P\\'eroux, Hassen M. Yesuf, Luis C. Ho, Matteo Fossati, Michele Fumagalli, Ravi Joshi (IIA), Reena Chaudhary, Sarbeswar Das","submitted_at":"2024-12-10T19:00:01Z","abstract_excerpt":"We study the galaxies hosting ultra-strong MgII (USMgII) absorbers at small impact parameters of $\\sim$2\" (5 - 20 kpc), spanning a redshift range of $0.4 \\le z \\le 1.7$, using deep, high-resolution images from Hyper Suprime-Cam Subaru Strategic Survey and spectra from SDSS survey. From a total of 418 USMgII absorbers with $W_{2796}\\ \\ge 3 \\mathring{A}$, along 412 quasar sightlines, we detect 50 galaxies based on [O II] $\\lambda\\lambda$3727,3729 nebular emission detected at $\\ge 2\\sigma$ level. Utilizing the [O II] emission from the stacked spectrum and employing the best-fit galaxy SED templat"},"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":"2412.07835","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.GA","submitted_at":"2024-12-10T19:00:01Z","cross_cats_sorted":[],"title_canon_sha256":"b8116964d7409c5a9f6bbb45f121b4f75d54dd93bbe13b6381e6b4f3467306a4","abstract_canon_sha256":"6853af8b736d084f0df0c7289562708fe5e0fa8f34130bd698870e9ce585550c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T09:47:39.890543Z","signature_b64":"YZ5YR5unOoA6S54CFusN2YmiqrgE0cJSQR/cbJQCfoYRnzbv5r26stkAWdmL3SfqcRLdtZgiDorGEaDKebytCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d5528e408515cfc93302502cbb8bfc7e18b6f003f6d60d9cf971e21b642ad64c","last_reissued_at":"2026-07-05T09:47:39.890062Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T09:47:39.890062Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Baryonic Ecosystem in Galaxies (BEINGMgII). Host Galaxies of Ultra-strong MgII Absorbers in Subaru Hyper Suprime-Cam Survey","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"C\\'eline P\\'eroux, Hassen M. Yesuf, Luis C. Ho, Matteo Fossati, Michele Fumagalli, Ravi Joshi (IIA), Reena Chaudhary, Sarbeswar Das","submitted_at":"2024-12-10T19:00:01Z","abstract_excerpt":"We study the galaxies hosting ultra-strong MgII (USMgII) absorbers at small impact parameters of $\\sim$2\" (5 - 20 kpc), spanning a redshift range of $0.4 \\le z \\le 1.7$, using deep, high-resolution images from Hyper Suprime-Cam Subaru Strategic Survey and spectra from SDSS survey. From a total of 418 USMgII absorbers with $W_{2796}\\ \\ge 3 \\mathring{A}$, along 412 quasar sightlines, we detect 50 galaxies based on [O II] $\\lambda\\lambda$3727,3729 nebular emission detected at $\\ge 2\\sigma$ level. Utilizing the [O II] emission from the stacked spectrum and employing the best-fit galaxy SED templat"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2412.07835","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2412.07835/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"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":"2412.07835","created_at":"2026-07-05T09:47:39.890121+00:00"},{"alias_kind":"arxiv_version","alias_value":"2412.07835v1","created_at":"2026-07-05T09:47:39.890121+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2412.07835","created_at":"2026-07-05T09:47:39.890121+00:00"},{"alias_kind":"pith_short_12","alias_value":"2VJI4QEFCXH4","created_at":"2026-07-05T09:47:39.890121+00:00"},{"alias_kind":"pith_short_16","alias_value":"2VJI4QEFCXH4SMYC","created_at":"2026-07-05T09:47:39.890121+00:00"},{"alias_kind":"pith_short_8","alias_value":"2VJI4QEF","created_at":"2026-07-05T09:47:39.890121+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2605.05650","citing_title":"Differences between emission and absorption tracers of spatially resolved outflows in clumpy z ~ 0.1 star-forming galaxies","ref_index":199,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/2VJI4QEFCXH4SMYCKAWLXC74PY","json":"https://pith.science/pith/2VJI4QEFCXH4SMYCKAWLXC74PY.json","graph_json":"https://pith.science/api/pith-number/2VJI4QEFCXH4SMYCKAWLXC74PY/graph.json","events_json":"https://pith.science/api/pith-number/2VJI4QEFCXH4SMYCKAWLXC74PY/events.json","paper":"https://pith.science/paper/2VJI4QEF"},"agent_actions":{"view_html":"https://pith.science/pith/2VJI4QEFCXH4SMYCKAWLXC74PY","download_json":"https://pith.science/pith/2VJI4QEFCXH4SMYCKAWLXC74PY.json","view_paper":"https://pith.science/paper/2VJI4QEF","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2412.07835&json=true","fetch_graph":"https://pith.science/api/pith-number/2VJI4QEFCXH4SMYCKAWLXC74PY/graph.json","fetch_events":"https://pith.science/api/pith-number/2VJI4QEFCXH4SMYCKAWLXC74PY/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/2VJI4QEFCXH4SMYCKAWLXC74PY/action/timestamp_anchor","attest_storage":"https://pith.science/pith/2VJI4QEFCXH4SMYCKAWLXC74PY/action/storage_attestation","attest_author":"https://pith.science/pith/2VJI4QEFCXH4SMYCKAWLXC74PY/action/author_attestation","sign_citation":"https://pith.science/pith/2VJI4QEFCXH4SMYCKAWLXC74PY/action/citation_signature","submit_replication":"https://pith.science/pith/2VJI4QEFCXH4SMYCKAWLXC74PY/action/replication_record"}},"created_at":"2026-07-05T09:47:39.890121+00:00","updated_at":"2026-07-05T09:47:39.890121+00:00"}