{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:PJCPJZCUE6IAHYPKFYREUJMO7W","short_pith_number":"pith:PJCPJZCU","schema_version":"1.0","canonical_sha256":"7a44f4e454279003e1ea2e224a258efd8f6588457bbbaaa759e68a158382f2be","source":{"kind":"arxiv","id":"1412.3116","version":2},"attestation_state":"computed","paper":{"title":"Constraining the Milky Way's Hot Gas Halo with OVII and OVII Emission Lines","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Joel N. Bregman, Matthew J. Miller","submitted_at":"2014-12-09T21:02:41Z","abstract_excerpt":"The Milky Way hosts a hot ($\\approx 2 \\times 10^6$ K), diffuse, gaseous halo based on detections of z = 0 OVII and OVIII absorption lines in quasar spectra and emission lines in blank-sky spectra. Here we improve constraints on the structure of the hot gas halo by fitting a radial model to a much larger sample of OVII and OVIII emission line measurements from XMM-Newton EPIC-MOS spectra compared to previous studies ($\\approx$ 650 sightlines). We assume a modified $\\beta$-model for the halo density distribution and a constant-density Local Bubble from which we calculate emission to compare with"},"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":"1412.3116","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2014-12-09T21:02:41Z","cross_cats_sorted":[],"title_canon_sha256":"e2a9ae6bbe775c121fe7a21bf19e96d02aa7a5f594aebb8b4ee749f682a21d42","abstract_canon_sha256":"11b3eb9f9e782c0c7ba8b949caed6bb155912e4bff6fa71d6eef2c76dcde3560"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:41:20.275154Z","signature_b64":"VX5B5VwdWzZmK1cKlxv01zv++OuE8GEbeB+ICgFDCAqKWZZ/UT5WJXXTbAXJ04G1osQfAgH4UgNEPti/k/ZzBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7a44f4e454279003e1ea2e224a258efd8f6588457bbbaaa759e68a158382f2be","last_reissued_at":"2026-05-18T01:41:20.274640Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:41:20.274640Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Constraining the Milky Way's Hot Gas Halo with OVII and OVII Emission Lines","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Joel N. Bregman, Matthew J. Miller","submitted_at":"2014-12-09T21:02:41Z","abstract_excerpt":"The Milky Way hosts a hot ($\\approx 2 \\times 10^6$ K), diffuse, gaseous halo based on detections of z = 0 OVII and OVIII absorption lines in quasar spectra and emission lines in blank-sky spectra. Here we improve constraints on the structure of the hot gas halo by fitting a radial model to a much larger sample of OVII and OVIII emission line measurements from XMM-Newton EPIC-MOS spectra compared to previous studies ($\\approx$ 650 sightlines). We assume a modified $\\beta$-model for the halo density distribution and a constant-density Local Bubble from which we calculate emission to compare with"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1412.3116","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":"1412.3116","created_at":"2026-05-18T01:41:20.274719+00:00"},{"alias_kind":"arxiv_version","alias_value":"1412.3116v2","created_at":"2026-05-18T01:41:20.274719+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1412.3116","created_at":"2026-05-18T01:41:20.274719+00:00"},{"alias_kind":"pith_short_12","alias_value":"PJCPJZCUE6IA","created_at":"2026-05-18T12:28:43.426989+00:00"},{"alias_kind":"pith_short_16","alias_value":"PJCPJZCUE6IAHYPK","created_at":"2026-05-18T12:28:43.426989+00:00"},{"alias_kind":"pith_short_8","alias_value":"PJCPJZCU","created_at":"2026-05-18T12:28:43.426989+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2606.10712","citing_title":"DIffuse X-ray Explorer (DIXE): Sky Survey Strategy and Collimator Response Demodulation","ref_index":36,"is_internal_anchor":true},{"citing_arxiv_id":"2602.00226","citing_title":"Nested Fermi and eROSITA bubbles require very similar $\\sim10^{56}$ erg collimated Galactic-center outbursts; their asymmetry indicates an eastern density gradient","ref_index":26,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/PJCPJZCUE6IAHYPKFYREUJMO7W","json":"https://pith.science/pith/PJCPJZCUE6IAHYPKFYREUJMO7W.json","graph_json":"https://pith.science/api/pith-number/PJCPJZCUE6IAHYPKFYREUJMO7W/graph.json","events_json":"https://pith.science/api/pith-number/PJCPJZCUE6IAHYPKFYREUJMO7W/events.json","paper":"https://pith.science/paper/PJCPJZCU"},"agent_actions":{"view_html":"https://pith.science/pith/PJCPJZCUE6IAHYPKFYREUJMO7W","download_json":"https://pith.science/pith/PJCPJZCUE6IAHYPKFYREUJMO7W.json","view_paper":"https://pith.science/paper/PJCPJZCU","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1412.3116&json=true","fetch_graph":"https://pith.science/api/pith-number/PJCPJZCUE6IAHYPKFYREUJMO7W/graph.json","fetch_events":"https://pith.science/api/pith-number/PJCPJZCUE6IAHYPKFYREUJMO7W/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/PJCPJZCUE6IAHYPKFYREUJMO7W/action/timestamp_anchor","attest_storage":"https://pith.science/pith/PJCPJZCUE6IAHYPKFYREUJMO7W/action/storage_attestation","attest_author":"https://pith.science/pith/PJCPJZCUE6IAHYPKFYREUJMO7W/action/author_attestation","sign_citation":"https://pith.science/pith/PJCPJZCUE6IAHYPKFYREUJMO7W/action/citation_signature","submit_replication":"https://pith.science/pith/PJCPJZCUE6IAHYPKFYREUJMO7W/action/replication_record"}},"created_at":"2026-05-18T01:41:20.274719+00:00","updated_at":"2026-05-18T01:41:20.274719+00:00"}