J/ApJ/821/89 12yrs of radial velocity obs. of exoplanet systems (Bryan+, 2016)
Statistics of long period gas giant planets in known planetary systems.
Bryan M.L., Knutson H.A., Howard A.W., Ngo H., Batygin K., Crepp J.R.,
Fulton B.J., Hinkley S., Isaacson H., Johnson J.A., Marcy G.W., Wright J.T.
<Astrophys. J., 821, 89-89 (2016)>
=2016ApJ...821...89B 2016ApJ...821...89B (SIMBAD/NED BibCode)
ADC_Keywords: Radial velocities ; Stars, double and multiple
Keywords: methods: statistical; techniques: radial velocities; planetary systems
Abstract:
We conducted a Doppler survey at Keck combined with NIRC2 K-band
adaptive optics (AO) imaging to search for massive, long-period
companions to 123 known exoplanet systems with one or two planets
detected using the radial velocity (RV) method. Our survey is
sensitive to Jupiter-mass planets out to 20au for a majority of stars
in our sample, and we report the discovery of eight new long-period
planets, in addition to 20 systems with statistically significant RV
trends that indicate the presence of an outer companion beyond 5AU. We
combine our RV observations with AO imaging to determine the range of
allowed masses and orbital separations for these companions, and
account for variations in our sensitivity to companions among stars in
our sample. We estimate the total occurrence rate of companions in our
sample to be 52±5% over the range 1-20MJup and 5-20AU. Our data
also suggest a declining frequency for gas giant planets in these
systems beyond 3-10AU, in contrast to earlier studies that found a
rising frequency for giant planets in the range 0.01-3AU. This
suggests either that the frequency of gas giant planets peaks between
3 and 10 AU, or that outer companions in these systems have a
different semi-major axis distribution than the overall population of
gas giant planets. Our results also suggest that hot gas giants may be
more likely to have an outer companion than cold gas giants. We find
that planets with an outer companion have higher average
eccentricities than their single counterparts, suggesting that
dynamical interactions between planets may play an important role in
these systems.
Description:
RV measurements were made at Keck Observatory as part of more than a
dozen PI-led programs falling under the umbrella of the California
Planet Survey (CPS; Howard et al. 2010ApJ...721.1467H 2010ApJ...721.1467H). We observed
each target star using HIRES. While the majority of the RV data used
in this study (spanning 1996 Jul to 2015 Feb) were published in
previous papers, we also obtained new observations that extend these
published baselines by up to 12 years.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 95 123 Radial velocity observations
table4.dat 29 333 RVs for systems with new planets: HD 156279,
HD 33142, GJ 317, HD 95089, HD 4203, HD 99706,
HD 102329, HD 116029
refs.dat 66 47 References
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See also:
J/ApJ/806/60 : Radial velocities of 70 Vir (HD117176) (Kane+, 2015)
J/ApJ/805/175 : Keck and APF radial velocities of HD7924 (Fulton+, 2015)
J/A+A/558/A106 : Chemical abundances for 83 transit hosts (Mortier+, 2013)
J/A+A/549/A109 : HARPS XXXI. The M-dwarf sample (Bonfils+, 2013)
J/ApJ/761/46 : HD 37605 radial velocities and photometry (Wang+, 2012)
J/ApJ/757/18 : RVs for 16 hot Jupiter host stars (Albrecht+, 2012)
J/A+A/545/A55 : Exoplanets. Radial velocities of 5 stars (Boisse+, 2012)
J/A+A/538/A113 : Exoplanets. Radial velocities of eight stars (Diaz+ 2012)
J/A+A/535/A54 : HARPS search for extra-solar planets. XXIX (Segransan+, 2011)
J/A+A/534/A58 : HD20794, HD85512, HD192310 HARPS RVs (Pepe+, 2011)
J/PASP/123/412 : Exoplanet Orbit Database (Wright+, 2011)
J/A+A/527/A63 : RVs of 7 new HARPS planetary systems (Moutou+, 2011)
J/ApJ/727/117 : RVs of four exoplanet candidates (Meschiari+, 2011)
J/ApJ/725/875 : Chromospheric activity for CPS stars (Isaacson+, 2010)
J/A+A/511/A54 : Magnetic cycles & radial-velocity for 8 stars (Santos+, 2010)
J/A+A/503/601 : HD 17156 transit photometry + radial vel. (Barbieri+, 2009)
J/ApJS/182/97 : Radial velocities of multi-planet systems (Wittenmyer+, 2009)
J/A+A/498/L5 : Photometry and spectroscopy of HD 80606b (Moutou+, 2009)
J/ApJS/181/62 : Survey of young solar analogs (Metchev+, 2009)
J/ApJ/693/1084 : Ten new and updated multiplanet systems (Wright+, 2009)
J/A+A/493/645 : Gl 176 radial velocities (Forveille+, 2009)
J/ApJS/168/297 : Stellar parameters of nearby cool stars (Takeda+, 2007)
J/ApJ/646/523 : Exoplanet systems with stellar companions (Raghavan+, 2006)
J/ApJ/646/505 : Catalog of nearby exoplanets (Butler+, 2006)
J/ApJS/159/141 : Spectroscopic properties of cool stars. I. (Valenti+, 2005)
J/A+A/430/165 : Radial velocities for 6691 K and M giants (Famaey+, 2005)
J/A+A/415/391 : The CORALIE survey for extrasolar planets. XII (Mayor+, 2004)
J/A+A/410/1039 : Northern extra-solar planets ELODIE survey I (Perrier+, 2003)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1 A1 --- n_ID [n] n: systems with new planets
(with RV measurements in table 4)
3- 11 A9 --- ID System identifier
13 A1 --- f_ID [c] c: Systems with 3σ trends and above
15- 17 I3 --- Nobs [12/219] Number of observations
19- 29 A11 "Y/M/D" Date1 Start date of observation
31- 41 A11 "Y/M/D" Date2 End date of observation
43- 46 I4 d Dur [1833/6788] Duration
48- 55 F8.4 m/s/yr Trend [-8.8/470] Trend
57- 61 F5.3 m/s/yr e_Trend [0/6] Negative uncertainty on Trend
63- 67 F5.3 m/s/yr E_Trend [0/6] Positive uncertainty on Trend
68 A1 --- f_Trend [ab] Flag on Trend (1)
70- 75 F6.3 m/s Jitter [-7.2/33] Jitter
77- 82 F6.4 m/s e_Jitter [0.003/3] Negative uncertainty on Jitter
84- 90 F7.4 m/s E_Jitter [0.003/15] Positive uncertainty on Jitter
92- 95 A4 --- Ref Orbital solution reference code
(see refs.dat file)
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Note (1): Flag as follows:
a = Because this system has a new outer planet whose period is just covered
by the RV baseline, we fix the trend to zero.
b = Because the RV accelerations in systems HD 50499, HD 68988, HD 72659,
HD 75898, HD 92788, and HD 158038 have some curvature, we fit them with a
two-planet solution. Since the partially resolved orbit and linear trend
are degenerate, we fix the slope to zero in these fits. During these fits,
we also fix the poorly constrained eccentricity of the outer planet to
zero. One caveat is that we assume that the residual RV signals are due
to a single body, even though they could be the sum of multiple bodies.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- ID System identifier
10- 16 F7.1 d JD Julian Date of the observation; JD-2440000
18- 23 F6.1 m/s RVel [-726/534] Radial velocity
25- 29 F5.3 m/s e_RVel [0.7/6.6] The 1σ uncertainty in RVel
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- Ref Reference code
6- 26 A21 --- Auth First author's name
28- 46 A19 --- BibCode Bibcode
48- 66 A19 --- Comm Comment (VizieR catalog's reference)
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 25-Jul-2016