{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2007:IDHJKIEKN3ZL3A4MZ52OGO5FP5","short_pith_number":"pith:IDHJKIEK","schema_version":"1.0","canonical_sha256":"40ce95208a6ef2bd838ccf74e33ba57f5ac04e094d2373919e5d92757f69fcf9","source":{"kind":"arxiv","id":"astro-ph/0702087","version":1},"attestation_state":"computed","paper":{"title":"Clear anti-correlation between luminosity and high energy cutoff in the low/hard state of the black hole candidate GX339-4","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Atsumasa Yoshida, Hajime Inoue, Kazutaka Yamaoka, Koji Saito, Tadayasu Dotani, Takehiro G. Miyakawa","submitted_at":"2007-02-03T03:32:05Z","abstract_excerpt":"We have analyzed the 171 RXTE data sets of the black hole candidate GX 339-4 in the low/hard state during its 1996--2005 outburst. All the broadband spectra were successfully modeled by a simple analytic model, power-law with an exponential cutoff. The obtained energy cutoff($E_{\\rm{cut}}$) is distributed over 50--300 keV, and the photon index over 1.4-1.6. We found a clear correlation ($E_{\\rm{cut}}$ is proportional to $L^{-0.75 \\pm 0.04}$) between luminosity in 2-200 keV (L) and $E_{\\rm{cut}}$ when L is larger than 5$\\times 10^{37}$ erg $s^{-1}$, while $E_{\\rm{cut}}$ is almost constant at 20"},"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":"astro-ph/0702087","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2007-02-03T03:32:05Z","cross_cats_sorted":[],"title_canon_sha256":"8bd61c790dc645e3026249341e69e2d0166af780ba6f6d898ea65dba66848c01","abstract_canon_sha256":"9e6a9db9e7fa6c1367c664e2adb24a8b6b035c935575454880efcdd2ef8fb16b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:16:34.117694Z","signature_b64":"djCGOzLg6aAy/4N5jlBFuKOux3vFtnP48/gLa5QcNWpKBiOGZW/C2t4PfkIPockQu7ULXFxh2+XU+gJsSGrTCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"40ce95208a6ef2bd838ccf74e33ba57f5ac04e094d2373919e5d92757f69fcf9","last_reissued_at":"2026-07-04T15:16:34.117151Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:16:34.117151Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Clear anti-correlation between luminosity and high energy cutoff in the low/hard state of the black hole candidate GX339-4","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Atsumasa Yoshida, Hajime Inoue, Kazutaka Yamaoka, Koji Saito, Tadayasu Dotani, Takehiro G. Miyakawa","submitted_at":"2007-02-03T03:32:05Z","abstract_excerpt":"We have analyzed the 171 RXTE data sets of the black hole candidate GX 339-4 in the low/hard state during its 1996--2005 outburst. All the broadband spectra were successfully modeled by a simple analytic model, power-law with an exponential cutoff. The obtained energy cutoff($E_{\\rm{cut}}$) is distributed over 50--300 keV, and the photon index over 1.4-1.6. We found a clear correlation ($E_{\\rm{cut}}$ is proportional to $L^{-0.75 \\pm 0.04}$) between luminosity in 2-200 keV (L) and $E_{\\rm{cut}}$ when L is larger than 5$\\times 10^{37}$ erg $s^{-1}$, while $E_{\\rm{cut}}$ is almost constant at 20"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0702087","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/astro-ph/0702087/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":"astro-ph/0702087","created_at":"2026-07-04T15:16:34.117219+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0702087v1","created_at":"2026-07-04T15:16:34.117219+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0702087","created_at":"2026-07-04T15:16:34.117219+00:00"},{"alias_kind":"pith_short_12","alias_value":"IDHJKIEKN3ZL","created_at":"2026-07-04T15:16:34.117219+00:00"},{"alias_kind":"pith_short_16","alias_value":"IDHJKIEKN3ZL3A4M","created_at":"2026-07-04T15:16:34.117219+00:00"},{"alias_kind":"pith_short_8","alias_value":"IDHJKIEK","created_at":"2026-07-04T15:16:34.117219+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2605.19473","citing_title":"Radio-X-ray Time Lags in GX 339-4: Probing Magnetic Field Transport in Black Hole Accretion","ref_index":144,"is_internal_anchor":true},{"citing_arxiv_id":"2605.19473","citing_title":"Radio-X-ray Time Lags in GX 339-4: Probing Magnetic Field Transport in Black Hole Accretion","ref_index":144,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/IDHJKIEKN3ZL3A4MZ52OGO5FP5","json":"https://pith.science/pith/IDHJKIEKN3ZL3A4MZ52OGO5FP5.json","graph_json":"https://pith.science/api/pith-number/IDHJKIEKN3ZL3A4MZ52OGO5FP5/graph.json","events_json":"https://pith.science/api/pith-number/IDHJKIEKN3ZL3A4MZ52OGO5FP5/events.json","paper":"https://pith.science/paper/IDHJKIEK"},"agent_actions":{"view_html":"https://pith.science/pith/IDHJKIEKN3ZL3A4MZ52OGO5FP5","download_json":"https://pith.science/pith/IDHJKIEKN3ZL3A4MZ52OGO5FP5.json","view_paper":"https://pith.science/paper/IDHJKIEK","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0702087&json=true","fetch_graph":"https://pith.science/api/pith-number/IDHJKIEKN3ZL3A4MZ52OGO5FP5/graph.json","fetch_events":"https://pith.science/api/pith-number/IDHJKIEKN3ZL3A4MZ52OGO5FP5/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/IDHJKIEKN3ZL3A4MZ52OGO5FP5/action/timestamp_anchor","attest_storage":"https://pith.science/pith/IDHJKIEKN3ZL3A4MZ52OGO5FP5/action/storage_attestation","attest_author":"https://pith.science/pith/IDHJKIEKN3ZL3A4MZ52OGO5FP5/action/author_attestation","sign_citation":"https://pith.science/pith/IDHJKIEKN3ZL3A4MZ52OGO5FP5/action/citation_signature","submit_replication":"https://pith.science/pith/IDHJKIEKN3ZL3A4MZ52OGO5FP5/action/replication_record"}},"created_at":"2026-07-04T15:16:34.117219+00:00","updated_at":"2026-07-04T15:16:34.117219+00:00"}