{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:SWMNF4TK7HEWD7GP6LUO76AFK5","short_pith_number":"pith:SWMNF4TK","schema_version":"1.0","canonical_sha256":"9598d2f26af9c961fccff2e8eff805574d0e0c9654a0f69e0235ca39ba2f9de8","source":{"kind":"arxiv","id":"1804.08359","version":2},"attestation_state":"computed","paper":{"title":"A catalogue of masses, structural parameters and velocity dispersion profiles of 112 Milky Way globular clusters","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"H. Baumgardt, M. Hilker","submitted_at":"2018-04-23T12:19:05Z","abstract_excerpt":"We have determined masses, stellar mass functions and structural parameters of 112 Milky Way globular clusters by fitting a large set of N-body simulations to their velocity dispersion and surface density profiles. The velocity dispersion profiles were calculated based on a combination of more than 15,000 high-precision radial velocities which we derived from archival ESO/VLT and Keck spectra together with ~20,000 published radial velocities from the literature. Our fits also include the stellar mass functions of the globular clusters, which are available for 47 clusters in our sample, allowin"},"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":"1804.08359","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2018-04-23T12:19:05Z","cross_cats_sorted":[],"title_canon_sha256":"a9b2e24ff65c1767acd413931f24a08da247bc9d9c1ec7d3950b46d929f7e654","abstract_canon_sha256":"0f2916db564ad5d6c8886dbfdf790cca7c412091f8399289bc0bedd67e270212"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:11:56.922139Z","signature_b64":"ZvGrEu7gGho50vcrLb51CtlHRuFR6/Bf2onLymNewer7XYNjhHomi1RZ4XwblKFb5ixYu0t/LWm+PAaZtGLxBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"9598d2f26af9c961fccff2e8eff805574d0e0c9654a0f69e0235ca39ba2f9de8","last_reissued_at":"2026-05-18T00:11:56.921507Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:11:56.921507Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A catalogue of masses, structural parameters and velocity dispersion profiles of 112 Milky Way globular clusters","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"H. Baumgardt, M. Hilker","submitted_at":"2018-04-23T12:19:05Z","abstract_excerpt":"We have determined masses, stellar mass functions and structural parameters of 112 Milky Way globular clusters by fitting a large set of N-body simulations to their velocity dispersion and surface density profiles. The velocity dispersion profiles were calculated based on a combination of more than 15,000 high-precision radial velocities which we derived from archival ESO/VLT and Keck spectra together with ~20,000 published radial velocities from the literature. Our fits also include the stellar mass functions of the globular clusters, which are available for 47 clusters in our sample, allowin"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1804.08359","kind":"arxiv","version":2},"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":"1804.08359","created_at":"2026-05-18T00:11:56.921634+00:00"},{"alias_kind":"arxiv_version","alias_value":"1804.08359v2","created_at":"2026-05-18T00:11:56.921634+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1804.08359","created_at":"2026-05-18T00:11:56.921634+00:00"},{"alias_kind":"pith_short_12","alias_value":"SWMNF4TK7HEW","created_at":"2026-05-18T12:32:53.628368+00:00"},{"alias_kind":"pith_short_16","alias_value":"SWMNF4TK7HEWD7GP","created_at":"2026-05-18T12:32:53.628368+00:00"},{"alias_kind":"pith_short_8","alias_value":"SWMNF4TK","created_at":"2026-05-18T12:32:53.628368+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":12,"internal_anchor_count":9,"sample":[{"citing_arxiv_id":"2607.08376","citing_title":"Multiple populations along the asymptotic giant branch: a Gaia+APOGEE study of 22 Galactic globular clusters","ref_index":3,"is_internal_anchor":true},{"citing_arxiv_id":"2606.31531","citing_title":"Probing globular clusters parameters through gravitational wave lensing with stellar-mass black hole binaries","ref_index":38,"is_internal_anchor":true},{"citing_arxiv_id":"2605.28716","citing_title":"Eccentric and unbound compact binaries in the LIGO-Virgo-KAGRA catalog: parameter estimation and waveform systematics with SEOBNRv6EHM","ref_index":165,"is_internal_anchor":true},{"citing_arxiv_id":"2606.27426","citing_title":"Too shy to spin? Cosmic wallflowers as proto-globular clusters","ref_index":264,"is_internal_anchor":true},{"citing_arxiv_id":"2606.12605","citing_title":"Feedback-Free Star Formation in Clusters within a Galaxy Simulated at High Resolution in Cosmic Dawn","ref_index":13,"is_internal_anchor":true},{"citing_arxiv_id":"2606.20979","citing_title":"Globular Clusters in the Time of the JWST. I. Survey Design and First Results on Multiple Populations and Beyond","ref_index":11,"is_internal_anchor":true},{"citing_arxiv_id":"2606.24824","citing_title":"Solving Inverse Problems of Chaotic Systems with Bidirectional Conditional Flow Matching","ref_index":84,"is_internal_anchor":true},{"citing_arxiv_id":"2605.21593","citing_title":"Predicting intermediate-mass black hole formation in star clusters with machine learning","ref_index":73,"is_internal_anchor":true},{"citing_arxiv_id":"2603.07481","citing_title":"New Way to Date Globular Clusters: Brown Dwarf Cooling Sequences","ref_index":130,"is_internal_anchor":true},{"citing_arxiv_id":"2604.22441","citing_title":"How lonely are the Binary Compact Objects Detected by the LIGO-Virgo-KAGRA Collaboration?","ref_index":67,"is_internal_anchor":false},{"citing_arxiv_id":"2604.04546","citing_title":"Recoil kicks from binary black hole mergers in GWTC catalogs: implications for retention and hierarchical mergers","ref_index":92,"is_internal_anchor":false},{"citing_arxiv_id":"2604.13930","citing_title":"Bayesian Analysis of Gravitational Wave Microlensing Effects from Galactic Double White Dwarfs","ref_index":53,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/SWMNF4TK7HEWD7GP6LUO76AFK5","json":"https://pith.science/pith/SWMNF4TK7HEWD7GP6LUO76AFK5.json","graph_json":"https://pith.science/api/pith-number/SWMNF4TK7HEWD7GP6LUO76AFK5/graph.json","events_json":"https://pith.science/api/pith-number/SWMNF4TK7HEWD7GP6LUO76AFK5/events.json","paper":"https://pith.science/paper/SWMNF4TK"},"agent_actions":{"view_html":"https://pith.science/pith/SWMNF4TK7HEWD7GP6LUO76AFK5","download_json":"https://pith.science/pith/SWMNF4TK7HEWD7GP6LUO76AFK5.json","view_paper":"https://pith.science/paper/SWMNF4TK","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1804.08359&json=true","fetch_graph":"https://pith.science/api/pith-number/SWMNF4TK7HEWD7GP6LUO76AFK5/graph.json","fetch_events":"https://pith.science/api/pith-number/SWMNF4TK7HEWD7GP6LUO76AFK5/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/SWMNF4TK7HEWD7GP6LUO76AFK5/action/timestamp_anchor","attest_storage":"https://pith.science/pith/SWMNF4TK7HEWD7GP6LUO76AFK5/action/storage_attestation","attest_author":"https://pith.science/pith/SWMNF4TK7HEWD7GP6LUO76AFK5/action/author_attestation","sign_citation":"https://pith.science/pith/SWMNF4TK7HEWD7GP6LUO76AFK5/action/citation_signature","submit_replication":"https://pith.science/pith/SWMNF4TK7HEWD7GP6LUO76AFK5/action/replication_record"}},"created_at":"2026-05-18T00:11:56.921634+00:00","updated_at":"2026-05-18T00:11:56.921634+00:00"}