{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:DRJRWUITMKO5V3ICFTBXG5EYU3","short_pith_number":"pith:DRJRWUIT","schema_version":"1.0","canonical_sha256":"1c531b5113629ddaed022cc3737498a6c72dfde565cad0fccc6eab17464fb57a","source":{"kind":"arxiv","id":"1606.07448","version":1},"attestation_state":"computed","paper":{"title":"IMF shape constraints from stellar populations and dynamics from CALIFA","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"A. Gallazzi, A. Vazdekis, B. Husemann, B. Ziegler, C.J. Walcher, D. Mast, F. La Barbera, G. van de Ven, I. Mart\\'in-Navarro, J. Bland-Hawthorn, J. Falc\\'on-Barroso, J. Mendez-Abreu, L. Galbany, L. Zhu, M. Lyubenova, P. S\\'anchez-Bl\\'azquez, R. A. Marino, R.C.E. van den Bosch, R.F.P. Peletier, R. Garc\\'ia-Benito, R. Gonz\\'alez Delgado, S.C. Trager, S.F. S\\'anchez, S. Zibetti, the CALIFA collaboration","submitted_at":"2016-06-23T20:00:07Z","abstract_excerpt":"In this letter we describe how we use stellar dynamics information to constrain the shape of the stellar IMF in a sample of 27 early-type galaxies from the CALIFA survey. We obtain dynamical and stellar mass-to-light ratios, $\\Upsilon_\\mathrm{dyn}$ and $\\Upsilon_{\\ast}$, over a homogenous aperture of 0.5~$R_{e}$. We use the constraint $\\Upsilon_\\mathrm{dyn} \\ge \\Upsilon_{\\ast}$ to test two IMF shapes within the framework of the extended MILES stellar population models. We rule out a single power law IMF shape for 75% of the galaxies in our sample. Conversely, we find that a double power law IM"},"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":"1606.07448","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2016-06-23T20:00:07Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"1a4cb6d40db1e5370ea80b8f46806a155b62b67f604628144d6783d760a65a21","abstract_canon_sha256":"fc93119361de12c93a79f85ca2ecfd34004dad4bf5b1031f072057249c9d62b5"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:02:38.636027Z","signature_b64":"TpILshKYXe39Ys7sOlqoU6nmDGoyLA7s6n7oeP3cy940XTVnO+iURnn4LyoqR6TgPXjXtE9qCq0769nhPHdfCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"1c531b5113629ddaed022cc3737498a6c72dfde565cad0fccc6eab17464fb57a","last_reissued_at":"2026-05-18T01:02:38.635291Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:02:38.635291Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"IMF shape constraints from stellar populations and dynamics from CALIFA","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"A. Gallazzi, A. Vazdekis, B. Husemann, B. Ziegler, C.J. Walcher, D. Mast, F. La Barbera, G. van de Ven, I. Mart\\'in-Navarro, J. Bland-Hawthorn, J. Falc\\'on-Barroso, J. Mendez-Abreu, L. Galbany, L. Zhu, M. Lyubenova, P. S\\'anchez-Bl\\'azquez, R. A. Marino, R.C.E. van den Bosch, R.F.P. Peletier, R. Garc\\'ia-Benito, R. Gonz\\'alez Delgado, S.C. Trager, S.F. S\\'anchez, S. Zibetti, the CALIFA collaboration","submitted_at":"2016-06-23T20:00:07Z","abstract_excerpt":"In this letter we describe how we use stellar dynamics information to constrain the shape of the stellar IMF in a sample of 27 early-type galaxies from the CALIFA survey. We obtain dynamical and stellar mass-to-light ratios, $\\Upsilon_\\mathrm{dyn}$ and $\\Upsilon_{\\ast}$, over a homogenous aperture of 0.5~$R_{e}$. We use the constraint $\\Upsilon_\\mathrm{dyn} \\ge \\Upsilon_{\\ast}$ to test two IMF shapes within the framework of the extended MILES stellar population models. We rule out a single power law IMF shape for 75% of the galaxies in our sample. Conversely, we find that a double power law IM"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1606.07448","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":"1606.07448","created_at":"2026-05-18T01:02:38.635433+00:00"},{"alias_kind":"arxiv_version","alias_value":"1606.07448v1","created_at":"2026-05-18T01:02:38.635433+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1606.07448","created_at":"2026-05-18T01:02:38.635433+00:00"},{"alias_kind":"pith_short_12","alias_value":"DRJRWUITMKO5","created_at":"2026-05-18T12:30:12.583610+00:00"},{"alias_kind":"pith_short_16","alias_value":"DRJRWUITMKO5V3IC","created_at":"2026-05-18T12:30:12.583610+00:00"},{"alias_kind":"pith_short_8","alias_value":"DRJRWUIT","created_at":"2026-05-18T12:30:12.583610+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/DRJRWUITMKO5V3ICFTBXG5EYU3","json":"https://pith.science/pith/DRJRWUITMKO5V3ICFTBXG5EYU3.json","graph_json":"https://pith.science/api/pith-number/DRJRWUITMKO5V3ICFTBXG5EYU3/graph.json","events_json":"https://pith.science/api/pith-number/DRJRWUITMKO5V3ICFTBXG5EYU3/events.json","paper":"https://pith.science/paper/DRJRWUIT"},"agent_actions":{"view_html":"https://pith.science/pith/DRJRWUITMKO5V3ICFTBXG5EYU3","download_json":"https://pith.science/pith/DRJRWUITMKO5V3ICFTBXG5EYU3.json","view_paper":"https://pith.science/paper/DRJRWUIT","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1606.07448&json=true","fetch_graph":"https://pith.science/api/pith-number/DRJRWUITMKO5V3ICFTBXG5EYU3/graph.json","fetch_events":"https://pith.science/api/pith-number/DRJRWUITMKO5V3ICFTBXG5EYU3/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/DRJRWUITMKO5V3ICFTBXG5EYU3/action/timestamp_anchor","attest_storage":"https://pith.science/pith/DRJRWUITMKO5V3ICFTBXG5EYU3/action/storage_attestation","attest_author":"https://pith.science/pith/DRJRWUITMKO5V3ICFTBXG5EYU3/action/author_attestation","sign_citation":"https://pith.science/pith/DRJRWUITMKO5V3ICFTBXG5EYU3/action/citation_signature","submit_replication":"https://pith.science/pith/DRJRWUITMKO5V3ICFTBXG5EYU3/action/replication_record"}},"created_at":"2026-05-18T01:02:38.635433+00:00","updated_at":"2026-05-18T01:02:38.635433+00:00"}