MagAO IMAGING OF LONG-PERIOD OBJECTS (MILO). I. A BENCHMARK M DWARF COMPANION EXCITING A MASSIVE PLANET AROUND THE SUN-LIKE STAR HD 7449

作者：Rodigas Timothy J^*; Arriagada Pamela; Faherty Jackie; Anglada Escude Guillem; Kaib Nathan; Butler R Paul; Shectman Stephen; Weinberger Alycia; Males Jared R; Morzinski Katie M; Close Laird M; Hinz Philip M; Crane Jeffrey D; Thompson Ian; Teske Johanna; Diaz Matias; Minniti Dante; Lopez Morales Mercedes; Adams Fred C; Boss Alan P

来源：Astrophysical Journal, 2016, 818(2): 106.

DOI：10.3847/0004-637X/818/2/106

• binaries: general
• instrumentation: adaptive optics
• planetary systems
• stars: individual (HD 7449)
• techniques: high angular resolution
• techniques: radial velocities

We present high-contrast Magellan adaptive optics images of HD 7449, a Sun-like star with one planet and a long-term radial velocity (RV) trend. We unambiguously detect the source of the long-term trend from 0.6-2.15 mu m. at a separation of similar to 0.'' 54. We use the object's colors and spectral energy distribution to show that it is most likely an M4-M5 dwarf (mass similar to 0.1-0.2 M-circle dot) at the same distance as the primary and is therefore likely bound. We also present new RVs measured with the Magellan/MIKE and Planet Finder Spectrograph spectrometers and compile these with archival data from CORALIE and HARPS. We use a new Markov chain Monte Carlo procedure to constrain both the mass (>0.17 M-circle dot at 99% confidence) and semimajor axis (similar to 18 AU) of the M dwarf companion (HD 7449B). We also refine the parameters of the known massive planet (HD 7449Ab), finding that its minimum mass is 1.09(-0.19)(+0.52) M-J, its semimajor axis is 2.33(-0.02)(+0.01) AU, and its eccentricity is 0.8(-0.06)(+0.08). We use N-body simulations to constrain the eccentricity of HD 7449B to less than or similar to 0.5. The M dwarf may be inducing Kozai oscillations on the planet, explaining its high eccentricity. If this is the case and its orbit was initially circular, the mass of the planet would need to be less than or similar to 1.5 M-J. This demonstrates that strong constraints on known planets can be made using direct observations of otherwise undetectable long-period companions.