42 research outputs found
A Planetary Companion to the Intermediate-Mass Giant HD 100655
A precise radial velocity survey conducted by a Korean-Japanese planet search
program revealed a planetary companion around the intermediate-mass clump giant
HD 100655. The radial velocity of the star exhibits a periodic Keplerian
variation with a period, semi-amplitude and eccentricity of 157.57 d, 35.2 m
s^-1 and 0.085, respectively. Adopting an estimated stellar mass of 2.4 M_Sun,
we confirmed the presence of a planetary companion with a semi-major axis of
0.76 AU and a minimum mass of 1.7 M_Jup. The planet is the lowest-mass planet
yet discovered around clump giants with masses greater than 1.9 M_Sun.Comment: 17 pages, 8 figures, accepted for publication in PAS
Korean-Japanese Planet Search Program: Substellar Companions around Intermediate-Mass Giants
A Korean-Japanese planet search program has been carried out using the 1.8m
telescope at Bohyunsan Optical Astronomy Observatory (BOAO) in Korea, and the
1.88m telescope at Okayama Astrophysical Observatory (OAO) in Japan to search
for planets around intermediate-mass giant stars. The program aims to show the
properties of planetary systems around such stars by precise Doppler survey of
about 190 G or K type giants together with collaborative surveys of the
East-Asian Planet Search Network. So far, we detected two substellar companions
around massive intermediate-mass giants in the Korean-Japanese planet search
program. One is a brown dwarf-mass companion with 37.6
orbiting a giant HD 119445 with 3.9 , which is the most massive
brown dwarf companion among those found around intermediate-mass giants. The
other is a planetary companion with 1.8 orbiting a giant star
with 2.4 , which is the lowest-mass planetary companion among those
detected around giant stars with 1.9 . Plotting these systems on
companion mass vs. stellar mass diagram, there seem to exist two unpopulated
regions of substellar companions around giants with 1.5--3 and
planetary companions orbiting giants with 2.4--4 . The existence of
these possible unpopulated regions supports a current characteristic view that
more massive substellar companions tend to exist around more massive stars.Comment: 8 pages, 3 figures, Part of PlanetsbeyondMS/2010 proceedings
http://arxiv.org/html/1011.660
Substellar Companions to Evolved Intermediate-Mass Stars: HD 145457 and HD 180314
We report the detections of two substellar companions orbiting around evolved
intermediate-mass stars from precise Doppler measurements at Subaru Telescope
and Okayama Astrophysical Observatory. HD 145457 is a K0 giant with a mass of
1.9 M_sun and has a planet of minimum mass m_2sini=2.9 M_J orbiting with period
of P=176 d and eccentricity of e=0.11. HD 180314 is also a K0 giant with 2.6
M_sun and hosts a substellar companion of m_2sin i=22 M_J, which falls in
brown-dwarf mass regime, in an orbit with P=396 d and e=0.26. HD 145457 b is
one of the innermost planets and HD 180314 b is the seventh candidate of
brown-dwarf-mass companion found around intermediate-mass evolved stars.Comment: 16 pages, 4 figures, accepted for publication in PAS
Planetary Companions to Evolved Intermediate-Mass Stars: 14 Andromedae, 81 Ceti, 6 Lyncis, and HD 167042
We report on the detection of four extrasolar planets orbiting evolved
intermediate-mass stars from a precise Doppler survey of G and K giants at
Okayama Astrophysical Observatory. All of the host stars are considered to be
formerly early F-type or A-type dwarfs when they were on the main sequence. 14
And (K0 III) is a clump giant with a mass of 2.2 M_solar and has a planet of
minimum mass m_2sin i=4.8 M_Jup in a nearly circular orbit with a 186 day
period. This is one of the innermost planets around evolved intermediate-mass
stars and such planets have only been discovered in clump giants. 81 Cet (G5
III) is a clump giant with 2.4 M_solar hosting a planet of m_2sin i=5.3 M_Jup
in a 953 day orbit with an eccentricity of e=0.21. 6 Lyn (K0 IV) is a less
evolved subgiant with 1.7 M_solar and has a planet of m_2sin i=2.4 M_Jup in a
899 day orbit with e=0.13. HD 167042 (K1 IV) is also a less evolved star with
1.5 M_solar hosting a planet of m_2sin i=1.6 M_Jup in a 418 day orbit with
e=0.10. This planet was independently announced by Johnson et al. (2008, ApJ,
675, 784). All of the host stars have solar or sub-solar metallicity, which
supports the lack of metal-rich tendency in planet-harboring giants in contrast
to the case of dwarfs.Comment: 23 pages, 6 figures, accepted for publication in PAS
Detection of a low-eccentricity and super-massive planet to the subgiant HD 38801
We report the detection of a large mass planet orbiting around the K0
metal-rich subgiant HD38801 () by precise radial velocity (RV)
measurements from the Subaru Telescope and the Keck Telescope. The star has a
mass of and metallicity of [Fe/H]= +0.26. The RV variations are
consistent with a circular orbit with a period of 696.0 days and a velocity
semiamplitude of 200.0\mps, which yield a minimum-mass for the companion of
10.7\mjup and semimajor axis of 1.71 AU. Such super-massive objects with very
low-eccentricities and hundreds of days period are uncommon among the ensemble
of known exoplanets
Five Intermediate-Period Planets from the N2K Sample
We report the detection of five Jovian mass planets orbiting high metallicity
stars. Four of these stars were first observed as part of the N2K program and
exhibited low RMS velocity scatter after three consecutive observations.
However, follow-up observations over the last three years now reveal the
presence of longer period planets with orbital periods ranging from 21 days to
a few years. HD 11506 is a G0V star with a planet of \msini = 4.74 \mjup in a
3.85 year orbit. HD 17156 is a G0V star with a 3.12 \mjup planet in a 21.2 day
orbit. The eccentricity of this orbit is 0.67, one of the highest known for a
planet with a relatively short period. The orbital period for this planet
places it in a region of parameter space where relatively few planets have been
detected. HD 125612 is a G3V star with a planet of \msini = 3.5 \mjup in a 1.4
year orbit. HD 170469 is a G5IV star with a planet of \msini = 0.67 \mjup in a
3.13 year orbit. HD 231701 is an F8V star with planet of 1.08 \mjup in a 142
day orbit. All of these stars have supersolar metallicity. Three of the five
stars were observed photometrically but showed no evidence of brightness
variability. A transit search conducted for HD 17156 was negative but covered
only 25% of the search space and so is not conclusive.Comment: 13 pages, 9 figures, accepted ApJ Resubmitted here with some
additional data, modified Keplerian orbit
A Substellar Companion to the Intermediate-Mass Giant 11 Com
We report the detection of a substellar companion orbiting the
intermediate-mass giant star 11 Com (G8 III). Precise Doppler measurements of
the star from Xinglong station and Okayama Astrophysical Observatory (OAO)
revealed Keplerian velocity variations with an orbital period of 326.03 +/-
0.32 days, a semiamplitude of 302.8 +/- 2.6 m/s, and an eccentricity of 0.231
+/- 0.005. Adopting a stellar mass of 2.7 +/- 0.3 M_solar, the minimum mass of
the companion is 19.4 +/- 1.5 M_Jup, well above the deuterium burning limit,
and the semimajor axis is 1.29 +/- 0.05 AU. This is the first result from the
joint planet search program between China and Japan aiming at revealing
statistics of substellar companions around intermediate-mass giants. 11 Com b
emerged from 300 targets of the planet search program at OAO. The current
detection rate of a brown dwarf candidate seems to be comparable to that around
solar-type stars within orbital separations of 3 AU.Comment: 19 pages, 4 figures, accepted by Ap
A Massive Substellar Companion to the Massive Giant HD 119445
We detected a brown dwarf-mass companion around the intermediate-mass giant
star HD 119445 (G6III) using the Doppler technique. This discovery is the first
result from a Korean-Japanese planet search program based on precise radial
velocity measurements. The radial velocity of this star exhibits a periodic
Keplerian variation with a period, semi-amplitude and eccentricity of 410.2
days, 413.5 m/s and 0.082, respectively. Adopting a stellar mass of 3.9
M_solar, we were able to confirm the presence of a massive substellar companion
with a semimajor axis of 1.71 AU and a minimum mass of 37.6 M_Jup, which falls
in the middle of the brown dwarf-mass region. This substellar companion is the
most massive ever discovered within 3 AU of a central intermediate-mass star.
The host star also ranks among the most massive stars with substellar
companions ever detected by the Doppler technique. This result supports the
current view of substellar systems that more massive substellar companions tend
to exist around more massive stars, and may further constrain substellar system
formation mechanisms.Comment: 17 pages, 5 figures, PASJ accepte