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Berger, J. Ramos, L. Rodet, L. Weber, M. Bonnefoy, M. Feldt, M. Janson, M. Langlois, M. Meyer, M. Samland, P. Delorme, R. Gratton, R. Ligi, R. Rigal, R. Roelfsema, S. Desidera, S. Durkan, S. Lacour, S. Messina, S. Peretti, S. Udry, T. Henning, T. Schmidt, W. Brandner","submitted_at":"2018-06-14T12:02:33Z","abstract_excerpt":"Evolutionary models are widely used to infer the mass of stars, brown dwarfs, and giant planets. Their predictions are thought to be less reliable at young ages ($<$ 200 Myr) and in the low-mass regime ($\\mathrm{<1~M_{\\odot}}$). GJ 2060 AB and TWA 22 AB are two rare astrometric M-dwarf binaries respectively members of the AB Doradus and Beta Pictoris moving groups. As their dynamical mass can be measured within a few years, they can be used to calibrate the evolutionary tracks and set new constraints on the age of young moving groups. We find a total mass of $\\mathrm{0.18\\pm 0.02~M_\\odot}$ for"},"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":"1806.05491","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2018-06-14T12:02:33Z","cross_cats_sorted":["astro-ph.EP"],"title_canon_sha256":"ce94301eb5cb5cf4f741ad48e39f0251d6dc4b4466d882a0b9f054866eed07ae","abstract_canon_sha256":"3995953c24353b4b644fe2d30ff96d73f65e367a9385ed96438769bb09d9422f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:03:46.627217Z","signature_b64":"d6n1ReTjFILL/RcCaZH3IOccEs/ZMZH+ih3XkXLXWvC06PVP8LS9hRUhyRj6mhMHDw60dLgo/3+7vw+T/QE5Dg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"eed1445f60eb640bc4c25219a4f9e6776e934b16344381b6f44c27263bbfe437","last_reissued_at":"2026-05-18T00:03:46.626540Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:03:46.626540Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Dynamical masses of M-dwarf binaries in young moving groups: I - The case of TWA 22 and GJ 2060","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.EP"],"primary_cat":"astro-ph.SR","authors_text":"A. Bazzon, A. Boccaletti, A. Delboulbe, A. Grandjean, A.-L. Maire, A-M Lagrange, A. Pavlov, A. Vigan, B. Biller, C. Bergfors, D. Homeier, D. Maurel, D. Mesa, D. Segransan, E. Stadler, F. Allard, F. Menard, G. Chauvin, G. Salter, H. Beust, J.-B. Le Bouquin, J. E. Schlieder, J. Girard, J. Hagelberg, J. Lannier, J.-L. Beuzit, J.-L. Monin, J.-P. Berger, J. Ramos, L. Rodet, L. Weber, M. Bonnefoy, M. Feldt, M. Janson, M. Langlois, M. Meyer, M. Samland, P. Delorme, R. Gratton, R. Ligi, R. Rigal, R. Roelfsema, S. Desidera, S. Durkan, S. Lacour, S. Messina, S. Peretti, S. Udry, T. Henning, T. Schmidt, W. Brandner","submitted_at":"2018-06-14T12:02:33Z","abstract_excerpt":"Evolutionary models are widely used to infer the mass of stars, brown dwarfs, and giant planets. Their predictions are thought to be less reliable at young ages ($<$ 200 Myr) and in the low-mass regime ($\\mathrm{<1~M_{\\odot}}$). 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