{"paper":{"title":"New Relationships between Galaxy Properties and Host Halo Mass, and the Role of Feedbacks in Galaxy Formation","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"1), 3), A. Lapi (1), F. Shankar (1, G. de Zotti (2, Italy;2-INAF-Padova, Italy;3-Ohio State University), L. Danese (1) (1-SISSA/ISAS, P. Salucci (1), Trieste","submitted_at":"2006-01-25T18:01:57Z","abstract_excerpt":"We present new relationships between halo masses M_h and several galaxy properties, including r*-band luminosities L_r, stellar (M_star) and baryonic masses, stellar velocity dispersions (sigma), and black hole masses (M_BH). Approximate analytic expressions are given. In the galaxy halo mass range 3*10^(10) M_sun <= M_h <= 3*10^(13) M_sun the M_h-L_r, M_star-M_h, and M_BH-M_h are well represented by a double power law, with a break at M_h_break~3*10^(11) M_sun, corresponding to a mass in stars M_star~ 1.2*10^(10) M_sun, to a r*-band luminosity L_r~ 5*10^9 L_sun, to a stellar velocity dispersi"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0601577","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"}