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MAE Publications and Papers

Sibley School of Mechanical and Aerospace Engineering

New article: Dynamical Mass Measurement of the Young Spectroscopic Binary V343 Normae AaAb Resolved with the Gemini Planet Imager

Article:  Nielsen, EL; De Rosa, RJ; Wang, J; Rameau, J; Song, I; Graham, JR; Macintosh, B; Ammons, M; Bailey, VP; Barman, TS; Bulger, J; Chilcote, JK; Cotten, T; Doyon, R; Duchene, G; Fitzgerald, MP; Follette, KB; Greenbaum, AZ; Hibon, P; Hung, LW; Ingraham, P; Kalas, P; Konopacky, QM; Larkin, JE; Maire, J; Marchis, F; Marley, MS; Marois, C; Metchev, S; Millar-Blanchaer, MA; Oppenheimer, R; Palmer, DW; Patience, J; Perrin, MD; Poyneer, LA; Pueyo, L; Rajan, A; Rantakyro, FT; Savransky, D; Schneider, AC; Sivaramakrishnan, A; Soummer, R; Thomas, S; Wallace, JK; Ward-Duong, K; Wiktorowicz, SJ; Wolff, SG; “Dynamical Mass Measurement of the Young Spectroscopic Binary V343 Normae AaAb Resolved with the Gemini Planet Imager”, Astonomical Journal, 152 (6)


Abstract:  We present new spatially resolved astrometry and photometry from the Gemini Planet Imager of the inner binary of the young multiple star system V343 Normae, which is a member of the beta Pictoris (beta Pic) moving group. V343 Normae comprises a K0 and mid-M star in a similar to 4.5 year orbit (AaAb) and a wide 10 ” M5 companion (B). By combining these data with archival astrometry and radial velocities we fit the orbit and measure individual masses for both components of M-Aa = 1.10+/- 0.10M(circle dot) and M-Ab= 0.290 +/- 0.018 M-circle dot. Comparing to theoretical isochrones, we find good agreement for the measured masses and JHK band magnitudes of the two components consistent with the age of the beta Pic moving group. We derive a model-dependent age for the beta Pic moving group of 26 +/- 3 Myr by combining our results for V343 Normae with literature measurements for GJ. 3305, which is another group member with resolved binary components

Funding Acknowledgement:  NSF [AST-0909188, AST-1313718, AST-1411868, AST-141378, NNX11AF74G, DGE-1232825]; NASA [NNX15AD95G/NEXSS, NNX11AD21G, NNX14AJ80G]; Fonds de Recherche du Quebec; U.S. Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; National Sciences and Engineering Research Council of Canada; JPL Research and Technology Grant

Funding Text:  We thank the anonymous referee for helpful comments that improved the quality of this work. These results are based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the National Science Foundation (NSF) on behalf of the Gemini partnership: the NSF (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. Supported by NSF grants AST-0909188 and AST-1313718 (RJDR, JRG, JJW, TME, PGK), AST-1411868 (BM, KF, JLP, AR, KWD), AST-141378 (PA, GD, MPF), NNX11AF74G (AZG, AS), and DGE-1232825 (AZG). Supported by NASA grants NNX15AD95G/NEXSS and NNX11AD21G (RJDR, JRG, JJW, TME, PGK), and NNX14 AJ80G (ELN, SCB, BM, FM, MP). J.R., R.D., and D.L. acknowledge support from the Fonds de Recherche du Quebec. Portions of this work were performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344 (SMA). B.G. and M.J.G. acknowledge support from the National Sciences and Engineering Research Council of Canada. G.V. acknowledges a JPL Research and Technology Grant for improvements to the GPI CAL system.

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