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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 731610.0, MPI für Astronomie / Publikationen_mpia
SEEDS direct Imaging of the RV-detected companion to V450 Andromedae, and characterization of the system
Authors:Hełminiak, K. G.; Kuzuhara, M.; Mede, K.; Brandt, T. D.; Kandori, R.; Suenaga, T.; Kusakabe, N.; Narita, N.; Carson, J. C.; Currie, T.; Kudo, T.; Hashimoto, J.; Abe, L.; Akiyama, E.; Brandner, W.; Feldt, M.; Goto, M.; Grady, C. A.; Guyon, O.; Hayano, Y.; Hayashi, M.; Hayashi, S. S.; Henning, T.; Hodapp, K. W.; Ishii, M.; Iye, M.; Janson, M.; Knapp, G. R.; Kwon, J.; Matsuo, T.; McElwain, M. W.; Miyama, S.; Morino, J. -. I.; Moro-Martin, A.; Nishimura, T.; Ryu, T.; Pyo, T. -. S.; Serabyn, E.; Suto, H.; Suzuki, R.; Takahashi, Y. H.; Takami, M.; Takato, N.; Terada, H.; Thalmann, C.; Turner, E. L.; Watanabe, M.; Wisniewski, J.; Yamada, T.; Takami, H.; Usuda, T.; Tamura, M.
Date of Publication (YYYY-MM-DD):2016
Title of Journal:The Astrophysical Journal
Issue / Number:1
Start Page:id. 33 (13 pp)
Audience:Not Specified
Abstract / Description:We report the direct imaging detection of a low-mass companion to a young, moderately active star V450 And, that was previously identified with the radial velocity (RV) method. The companion was found in high-contrast images obtained with the Subaru Telescope equipped with the HiCIAO camera and AO188 adaptive optics system. From the public ELODIE and SOPHIE archives we extracted available high-resolution spectra and RV measurements, along with RVs from the Lick planet search program. We combined our multi-epoch astrometry with these archival, partially unpublished RVs, and found that the companion is a low-mass star, not a brown dwarf, as previously suggested. We found the best-fitting dynamical masses to be {m}1={1.141}-0.091+0.037 and {m}2={0.279}-0.020+0.023 {M}ȯ . We also performed spectral analysis of the SOPHIE spectra with the iSpec code. Hipparcos time-series photometry shows a periodicity of P = 5.743 day, which is also seen in the SOPHIE spectra as an RV modulation of the star A. We interpret it as being caused by spots on the stellar surface, and the star to be rotating with the given period. From the rotation and level of activity, we found that the system is {380}-100+220 Myr old, consistent with an isochrone analysis ({220}-90+2120 Myr). This work may serve as a test case for future studies of low-mass stars, brown dwarfs, and exoplanets by combination of RV and direct imaging data.
Free Keywords:binaries: spectroscopic; binaries: visual; stars: imaging; stars: individual: V450 And; stars: low-mass
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0004-637X %R 10.3847/0004-637X/832/1/33
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