{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2013:KZUANF7QS67MMPZGLBZI23KWRE","short_pith_number":"pith:KZUANF7Q","schema_version":"1.0","canonical_sha256":"56680697f097bec63f2658728d6d568937ae1ec3ffd2cbd2f5ec91576acee48e","source":{"kind":"arxiv","id":"1309.1371","version":1},"attestation_state":"computed","paper":{"title":"Revealing the cold dust in low-metallicity environments: I - Photometry analysis of the Dwarf Galaxy Survey with Herschel","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. Boselli, A. R\\'emy-Ruyer, C.D. Wilson, D. Cormier, F. Galliano, G. J. Bendo, H. Roussel, I. De Looze, L. Ciesla, L. Spinoglio, M. Baes, M. Boquien, M. Galametz, M. J. Barlow, M. Pohlen, M. Sauvage, M. Vaccari, M. W. L. Smith, O. {\\L}. Karczewski, P. Panuzzo, R. Wu, S.C. Madden, S. Hony, the Herschel-SAG2 consortium, V. Lebouteiller","submitted_at":"2013-09-05T15:18:48Z","abstract_excerpt":"We present new photometric data from our Herschel Key Programme, the Dwarf Galaxy Survey (DGS), dedicated to the observation of the gas and dust in 48 low-metallicity environments. They were observed with PACS and SPIRE onboard Herschel at 70,100,160,250,350, and 500 microns. We focus on a systematic comparison of the derived FIR properties (FIR luminosity, dust mass, dust temperature and emissivity index) with more metal-rich galaxies and investigate the detection of a potential submm excess. The data reduction method is adapted for each galaxy to derive the most reliable photometry from the "},"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":"1309.1371","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2013-09-05T15:18:48Z","cross_cats_sorted":[],"title_canon_sha256":"1dcbcc4ab8b2f3516536c6f4bc5ad0edfa356d1de71677455dd66e39fd6f041a","abstract_canon_sha256":"5a457909bd4692250f228274bbba748e226e687af73a92709155aaffe9aec613"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T03:13:33.375335Z","signature_b64":"DOZZdNa2EPDMpPUwcFp7495hkjTw5mVNMPdSQN5l501cpnFpxEHGrTACEtugDkc/niENjX80EkrKZd/92ZK2CQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"56680697f097bec63f2658728d6d568937ae1ec3ffd2cbd2f5ec91576acee48e","last_reissued_at":"2026-05-18T03:13:33.374673Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T03:13:33.374673Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Revealing the cold dust in low-metallicity environments: I - Photometry analysis of the Dwarf Galaxy Survey with Herschel","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. Boselli, A. R\\'emy-Ruyer, C.D. Wilson, D. Cormier, F. Galliano, G. J. Bendo, H. Roussel, I. De Looze, L. Ciesla, L. Spinoglio, M. Baes, M. Boquien, M. Galametz, M. J. Barlow, M. Pohlen, M. Sauvage, M. Vaccari, M. W. L. Smith, O. {\\L}. Karczewski, P. Panuzzo, R. Wu, S.C. Madden, S. Hony, the Herschel-SAG2 consortium, V. Lebouteiller","submitted_at":"2013-09-05T15:18:48Z","abstract_excerpt":"We present new photometric data from our Herschel Key Programme, the Dwarf Galaxy Survey (DGS), dedicated to the observation of the gas and dust in 48 low-metallicity environments. They were observed with PACS and SPIRE onboard Herschel at 70,100,160,250,350, and 500 microns. We focus on a systematic comparison of the derived FIR properties (FIR luminosity, dust mass, dust temperature and emissivity index) with more metal-rich galaxies and investigate the detection of a potential submm excess. The data reduction method is adapted for each galaxy to derive the most reliable photometry from the "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1309.1371","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":"1309.1371","created_at":"2026-05-18T03:13:33.374769+00:00"},{"alias_kind":"arxiv_version","alias_value":"1309.1371v1","created_at":"2026-05-18T03:13:33.374769+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1309.1371","created_at":"2026-05-18T03:13:33.374769+00:00"},{"alias_kind":"pith_short_12","alias_value":"KZUANF7QS67M","created_at":"2026-05-18T12:27:51.066281+00:00"},{"alias_kind":"pith_short_16","alias_value":"KZUANF7QS67MMPZG","created_at":"2026-05-18T12:27:51.066281+00:00"},{"alias_kind":"pith_short_8","alias_value":"KZUANF7Q","created_at":"2026-05-18T12:27:51.066281+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/KZUANF7QS67MMPZGLBZI23KWRE","json":"https://pith.science/pith/KZUANF7QS67MMPZGLBZI23KWRE.json","graph_json":"https://pith.science/api/pith-number/KZUANF7QS67MMPZGLBZI23KWRE/graph.json","events_json":"https://pith.science/api/pith-number/KZUANF7QS67MMPZGLBZI23KWRE/events.json","paper":"https://pith.science/paper/KZUANF7Q"},"agent_actions":{"view_html":"https://pith.science/pith/KZUANF7QS67MMPZGLBZI23KWRE","download_json":"https://pith.science/pith/KZUANF7QS67MMPZGLBZI23KWRE.json","view_paper":"https://pith.science/paper/KZUANF7Q","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1309.1371&json=true","fetch_graph":"https://pith.science/api/pith-number/KZUANF7QS67MMPZGLBZI23KWRE/graph.json","fetch_events":"https://pith.science/api/pith-number/KZUANF7QS67MMPZGLBZI23KWRE/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/KZUANF7QS67MMPZGLBZI23KWRE/action/timestamp_anchor","attest_storage":"https://pith.science/pith/KZUANF7QS67MMPZGLBZI23KWRE/action/storage_attestation","attest_author":"https://pith.science/pith/KZUANF7QS67MMPZGLBZI23KWRE/action/author_attestation","sign_citation":"https://pith.science/pith/KZUANF7QS67MMPZGLBZI23KWRE/action/citation_signature","submit_replication":"https://pith.science/pith/KZUANF7QS67MMPZGLBZI23KWRE/action/replication_record"}},"created_at":"2026-05-18T03:13:33.374769+00:00","updated_at":"2026-05-18T03:13:33.374769+00:00"}