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The plasma is characterized by an electron temperature of 0.49$^{+0.08}_{-0.06}$ keV with subsolar abundances for O (0.58$^{+0.06}_{-0.05}$ solar value) and Fe (0.72$^{+0.06}_{-0.05}$ solar value) and slightly overabundance for Mg (1.23$^{+0.14}_{-0.14}$ solar value). It seems that the central X-ray emission originate"},"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":"1507.02788","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2015-07-10T06:46:18Z","cross_cats_sorted":[],"title_canon_sha256":"1106c7207619bd9f70c6cfb120aeedd0ae4e673545691653680da94eb866f310","abstract_canon_sha256":"2ebefb58d381ec241130ace5b20ee534b142b02beaf5d8489aca231d6985e376"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:36:47.662899Z","signature_b64":"JPBh1pS7FrLiQKPYOcvKYRpRyM4PjkGT3Byj58so/EJeMxMEgSvN/Zpq70qS1oi1sX8W36nAiiuwYQ3+RHdIBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"497948e72574c18ea82fb1274e6f5409896d654b0b594e18ce1fdb5b11d1f599","last_reissued_at":"2026-05-18T01:36:47.662363Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:36:47.662363Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Suzaku observation and distance of supernova remnant G332.5-5.6","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"D. Wu, H. Zhu, W. W. Tian","submitted_at":"2015-07-10T06:46:18Z","abstract_excerpt":"We analyze the Suzaku XIS data of the central region of supernova remnant G332.5-5.6. The X-ray data are well described by a single non-equilibrium ionization thermal model, {\\tt vnei}, with an absorbing hydrogen column density of 1.4$^{+0.4}_{-0.1}$ $\\times$ 10$^{21}$ cm$^{-2}$. The plasma is characterized by an electron temperature of 0.49$^{+0.08}_{-0.06}$ keV with subsolar abundances for O (0.58$^{+0.06}_{-0.05}$ solar value) and Fe (0.72$^{+0.06}_{-0.05}$ solar value) and slightly overabundance for Mg (1.23$^{+0.14}_{-0.14}$ solar value). 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