{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2026:EX74RWKPAMM7EYYD3RYOWKG3B4","short_pith_number":"pith:EX74RWKP","schema_version":"1.0","canonical_sha256":"25ffc8d94f0319f26303dc70eb28db0f0a0cad72788ae98cced7e254beb66f1e","source":{"kind":"arxiv","id":"2604.09875","version":3},"attestation_state":"computed","paper":{"title":"Galactic Archaeology with the Subaru `\\=Onohi`ula Prime Focus Spectrograph Strategic Program","license":"http://creativecommons.org/licenses/by/4.0/","headline":"A Subaru PFS survey will model density profiles of six dwarf galaxies using 18,000 stars to test if they show cold dark matter cusps or alternative cores.","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"Alexander S. Szalay, Ana L. Chies-Santos, Andrew P. Cooper, Carrie Filion, Chiaki Kobayashi, Dafa Wardana, Elisa G. M. Ferreira, Evan N. Kirby, Federico Sestito, Gang Zhao, Itsuki Ogami, Ivanna Escala, Jihye Hong, Jingkun Zhao, Judith G. Cohen, Keyi Ding, Kohei Hayashi, Kyosuke Sato, L\\'aszl\\'o Dobos, Lauren Henderson, Magda Arnaboldi, Masashi Chiba, Miho N. Ishigaki, Mohammad K. Mardini, Nicolas Martin, Nicole L. Klock-Miranda, Ortwin Gerhard, Pete B. Kuzma, Rin Miyazaki Sakurako Okamoto, Rohan Pattnaik, Roman Gerasimov, Rosemary F. G. Wyse, Ryo Ishikawa, Ryota Ikeda, Shunichi Horigome, Souradeep Bhattacharya, Takanobu Kirihara, Tam\\'as Budav\\'ari, Viska Wei, Wenbo Wu, Xiangwei Zhang, Xianhao Ye, Xiaosheng Zhao, Xinfeng Xu, Yohei Miki, Yoshihisa Suzuki, Yutaka Hirai, Yutaka Komiyama, Zhenyu Wu, Zhuohan Li","submitted_at":"2026-04-10T20:04:44Z","abstract_excerpt":"The recently commissioned Subaru `\\=Onohi`ula Prime Focus Spectrograph (PFS) will obtain spectra from nearly 2,400 fibers that cover 1.24 square degrees. The 360 night Subaru Strategic Program for PFS is dedicating approximately one-third of its allocation (130 nights) to study the structure and evolution of galaxies in the Local Group. This Galactic Archaeological survey has three pillars. (1) We will determine whether the mass density profiles of dwarf galaxies are consistent with cusps, as expected for cold dark matter, or cores, as expected from alternative dark matter theories or baryonic"},"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":"2604.09875","kind":"arxiv","version":3},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.GA","submitted_at":"2026-04-10T20:04:44Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"c2bb3ba8dd43095dce870e040e5cf1a7c2f09bb4d08532fba409234f663702b1","abstract_canon_sha256":"79c0ecdb19cce9f28eac654d31f6f05d30ddfe9a67b18687e5278dcc6f3cb9bc"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-01T00:17:11.391094Z","signature_b64":"kREM7dX800Lh+sRaC/dhd0oEcbrT300108PWSYLcy7AZtFN1s4I/wWPfbjyy2dkfhT17ooaNahTxcfFImtf4CQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"25ffc8d94f0319f26303dc70eb28db0f0a0cad72788ae98cced7e254beb66f1e","last_reissued_at":"2026-07-01T00:17:11.390600Z","signature_status":"signed_v1","first_computed_at":"2026-07-01T00:17:11.390600Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Galactic Archaeology with the Subaru `\\=Onohi`ula Prime Focus Spectrograph Strategic Program","license":"http://creativecommons.org/licenses/by/4.0/","headline":"A Subaru PFS survey will model density profiles of six dwarf galaxies using 18,000 stars to test if they show cold dark matter cusps or alternative cores.","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"Alexander S. Szalay, Ana L. Chies-Santos, Andrew P. Cooper, Carrie Filion, Chiaki Kobayashi, Dafa Wardana, Elisa G. M. Ferreira, Evan N. Kirby, Federico Sestito, Gang Zhao, Itsuki Ogami, Ivanna Escala, Jihye Hong, Jingkun Zhao, Judith G. Cohen, Keyi Ding, Kohei Hayashi, Kyosuke Sato, L\\'aszl\\'o Dobos, Lauren Henderson, Magda Arnaboldi, Masashi Chiba, Miho N. Ishigaki, Mohammad K. Mardini, Nicolas Martin, Nicole L. Klock-Miranda, Ortwin Gerhard, Pete B. Kuzma, Rin Miyazaki Sakurako Okamoto, Rohan Pattnaik, Roman Gerasimov, Rosemary F. G. Wyse, Ryo Ishikawa, Ryota Ikeda, Shunichi Horigome, Souradeep Bhattacharya, Takanobu Kirihara, Tam\\'as Budav\\'ari, Viska Wei, Wenbo Wu, Xiangwei Zhang, Xianhao Ye, Xiaosheng Zhao, Xinfeng Xu, Yohei Miki, Yoshihisa Suzuki, Yutaka Hirai, Yutaka Komiyama, Zhenyu Wu, Zhuohan Li","submitted_at":"2026-04-10T20:04:44Z","abstract_excerpt":"The recently commissioned Subaru `\\=Onohi`ula Prime Focus Spectrograph (PFS) will obtain spectra from nearly 2,400 fibers that cover 1.24 square degrees. The 360 night Subaru Strategic Program for PFS is dedicating approximately one-third of its allocation (130 nights) to study the structure and evolution of galaxies in the Local Group. This Galactic Archaeological survey has three pillars. (1) We will determine whether the mass density profiles of dwarf galaxies are consistent with cusps, as expected for cold dark matter, or cores, as expected from alternative dark matter theories or baryonic"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"We will determine whether the mass density profiles of dwarf galaxies are consistent with cusps, as expected for cold dark matter, or cores, as expected from alternative dark matter theories or baryonic feedback.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"That the planned samples of 18,000 dwarf galaxy members and 30,000 M31 halo stars will be sufficient to reliably model full line-of-sight velocity and abundance distributions beyond tidal radii without significant contamination or selection biases.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"The PFS Galactic Archaeology survey will observe thousands of stars in Local Group systems to measure density profiles in dwarfs and compare assembly histories of M31 and the Milky Way.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"A Subaru PFS survey will model density profiles of six dwarf galaxies using 18,000 stars to test if they show cold dark matter cusps or alternative cores.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"926c15ee12cd47933eb850fa626f14fbce8329045d6fb887311d496db3eab769"},"source":{"id":"2604.09875","kind":"arxiv","version":3},"verdict":{"id":"9a6fbbd2-5b26-46f2-be6a-c0ab63d4f5a1","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-10T16:51:28.951771Z","strongest_claim":"We will determine whether the mass density profiles of dwarf galaxies are consistent with cusps, as expected for cold dark matter, or cores, as expected from alternative dark matter theories or baryonic feedback.","one_line_summary":"The PFS Galactic Archaeology survey will observe thousands of stars in Local Group systems to measure density profiles in dwarfs and compare assembly histories of M31 and the Milky Way.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"That the planned samples of 18,000 dwarf galaxy members and 30,000 M31 halo stars will be sufficient to reliably model full line-of-sight velocity and abundance distributions beyond tidal radii without significant contamination or selection biases.","pith_extraction_headline":"A Subaru PFS survey will model density profiles of six dwarf galaxies using 18,000 stars to test if they show cold dark matter cusps or alternative cores."},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2604.09875/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":"2604.09875","created_at":"2026-07-01T00:17:11.390657+00:00"},{"alias_kind":"arxiv_version","alias_value":"2604.09875v3","created_at":"2026-07-01T00:17:11.390657+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2604.09875","created_at":"2026-07-01T00:17:11.390657+00:00"},{"alias_kind":"pith_short_12","alias_value":"EX74RWKPAMM7","created_at":"2026-07-01T00:17:11.390657+00:00"},{"alias_kind":"pith_short_16","alias_value":"EX74RWKPAMM7EYYD","created_at":"2026-07-01T00:17:11.390657+00:00"},{"alias_kind":"pith_short_8","alias_value":"EX74RWKP","created_at":"2026-07-01T00:17:11.390657+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.02480","citing_title":"The Merger-Driven Origin of the Vast Extended Stellar Disc Around the Andromeda Galaxy","ref_index":128,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/EX74RWKPAMM7EYYD3RYOWKG3B4","json":"https://pith.science/pith/EX74RWKPAMM7EYYD3RYOWKG3B4.json","graph_json":"https://pith.science/api/pith-number/EX74RWKPAMM7EYYD3RYOWKG3B4/graph.json","events_json":"https://pith.science/api/pith-number/EX74RWKPAMM7EYYD3RYOWKG3B4/events.json","paper":"https://pith.science/paper/EX74RWKP"},"agent_actions":{"view_html":"https://pith.science/pith/EX74RWKPAMM7EYYD3RYOWKG3B4","download_json":"https://pith.science/pith/EX74RWKPAMM7EYYD3RYOWKG3B4.json","view_paper":"https://pith.science/paper/EX74RWKP","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2604.09875&json=true","fetch_graph":"https://pith.science/api/pith-number/EX74RWKPAMM7EYYD3RYOWKG3B4/graph.json","fetch_events":"https://pith.science/api/pith-number/EX74RWKPAMM7EYYD3RYOWKG3B4/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/EX74RWKPAMM7EYYD3RYOWKG3B4/action/timestamp_anchor","attest_storage":"https://pith.science/pith/EX74RWKPAMM7EYYD3RYOWKG3B4/action/storage_attestation","attest_author":"https://pith.science/pith/EX74RWKPAMM7EYYD3RYOWKG3B4/action/author_attestation","sign_citation":"https://pith.science/pith/EX74RWKPAMM7EYYD3RYOWKG3B4/action/citation_signature","submit_replication":"https://pith.science/pith/EX74RWKPAMM7EYYD3RYOWKG3B4/action/replication_record"}},"created_at":"2026-07-01T00:17:11.390657+00:00","updated_at":"2026-07-01T00:17:11.390657+00:00"}