J/ApJ/821/74 27yr of RV observations of HD 219134 (Johnson+, 2016)
A 12-year activity cycle for the nearby planet host star HD 219134.
Johnson M.C., Endl M., Cochran W.D., Meschiari S., Robertson P.,
MacQueen P.J., Brugamyer E.J., Caldwell C., Hatzes A.P., Ramirez I.,
Wittenmyer R.A.
<Astrophys. J., 821, 74-74 (2016)>
=2016ApJ...821...74J 2016ApJ...821...74J (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Radial velocities ; Stars, nearby
Keywords: planetary systems; stars: activity; stars: HD 219134;
stars: rotation; techniques: radial velocities;
techniques: spectroscopic
Abstract:
The nearby (6.5pc) star HD219134 was recently shown by Motalebi+
(2015, J/A+A/584/A72) and Vogt+ (2015ApJ...814...12V 2015ApJ...814...12V) to host several
planets, the innermost of which is transiting. We present 27yr of
radial velocity (RV) observations of this star from the McDonald
Observatory Planet Search program, and 19yr of stellar activity data.
We detect a long-period activity cycle measured in the CaII SHK index,
with a period of 4230±100d (11.7yr), very similar to the 11yr solar
activity cycle. Although the period of the Saturn-mass planet
HD219134h is close to half that of the activity cycle, we argue that
it is not an artifact due to stellar activity. We also find a
significant periodicity in the SHK data due to stellar rotation with a
period of 22.8d. This is identical to the period of planet f
identified by Vogt+ (2015ApJ...814...12V 2015ApJ...814...12V), suggesting that this RV
signal might be caused by rotational modulation of stellar activity
rather than a planet. Analysis of our RVs allows us to detect the
long-period planet HD219134h and the transiting super-Earth HD219134b.
Finally, we use our long time baseline to constrain the presence of
longer period planets in the system, excluding to 1σ objects
with Msini>0.36MJ at 12yr (corresponding to the orbital period of
Jupiter) and Msini>0.72MJ at a period of 16.4yr (assuming a circular
orbit for an outer companion).
Description:
We observed HD 219134 with the coude spectrograph on the 2.7m Harlan
J. Smith Telescope (HJST) at McDonald Observatory. We obtained 295
spectra of HD 219134 between 1988 July 26 UT and 2015 October 16 UT,
using three different spectrograph formats.
We also observed HD 219134 with the HIRES spectrograph on the Keck I
telescope. We obtained 72 spectra between 1996 October 6 and 2000
December 3 UT, and 288 more between 2005 December 9 and 2012 January
11 UT, for a total of 360 spectra.
Objects:
---------------------------------------------------------
RA (ICRS) DE Designation(s)
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23 13 16.98 +57 10 06.1 HD 219134 = TYC 4006-1866-1
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 44 295 HJST radial velocities and S-index data
table2.dat 43 360 Keck/HIRES radial velocities and S-index data
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See also:
III/185 : Search for Jupiter-Mass Companions (Walker+, 1995)
J/ApJS/224/12 : Kepler planetary candidates. VII. 48-month (Coughlin+, 2016)
J/ApJ/818/34 : Radial velocity monitoring of 5 FGK stars (Endl+, 2016)
J/ApJ/817/104 : Keck/HIRES radial velocity obs. of HD32963 (Rowan+, 2016)
J/A+A/585/A134 : HD1461, HD40307, and HD204313 radial velocities (Diaz+, 2016)
J/A+A/584/A72 : A rocky planet at 6.5pc from the Sun (Motalebi+ 2015)
J/ApJ/784/45 : Kepler's multiple planet candidates. III. (Rowe+, 2014)
J/A+A/552/A78 : Solar like stars radial velocities (Zechmeister+, 2013)
J/A+A/552/A27 : Stellar activity and kinematics of FGK stars (Murgas+, 2013)
J/ApJ/764/3 : Hα indices in M low-mass stars (Robertson+, 2013)
J/ApJ/725/875 : Chromospheric activity for CPS stars (Isaacson+, 2010)
J/A+A/521/A12 : Radial velocities of nearby late-type stars (Maldonado+, 2010)
J/A+A/520/A79 : FGK stars chromospheric activity (Martinez-Arnaiz+, 2010)
J/A+A/514/A97 : High-resolution sp. of Late-type stars (Lopez-Santiago+ 2010)
J/ApJ/687/1264 : Age estimation for solar-type dwarfs (Mamajek+, 2008)
J/ApJS/168/297 : Stellar parameters of nearby cool stars (Takeda+, 2007)
J/ApJS/159/141 : Spectroscopic properties of cool stars. I. (Valenti+, 2005)
J/ApJS/141/503 : Radial Velocities for 889 late-type stars (Nidever+, 2002)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- Phase Phase of observational program (1)
5- 7 I3 --- Seq Running sequence number
9- 21 F13.5 d BJD Barycentric Julian Date
23- 27 F5.1 m/s dRV [-58/45] Differential radial velocity (G1)
29- 32 F4.1 m/s e_dRV [3/11]? Uncertainty in dRV (2)
34- 38 F5.3 --- SHK [0.16/0.5]? The SHK index
40- 44 F5.3 --- e_SHK [0.01/0.05]? Uncertainty in SHK
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Note (1): During Phase I of our program (1988 July 26 to 1995 July 20), we
obtained 30 spectra using the telluric O2 band at 6300Å as a
velocity reference.
Phase II (1990 October 14 to 1997 November 16), during which we
obtained 34 spectra, used a standard I2 absorption cell as the
velocity standard. We used spectrograph configurations with a
resolving power of R∼210000 for Phase I and II; only a single spectral
order was observed.
Finally, Phase III (1998 July 16 to present, 231 spectra) continues to
use the I2 cell but uses the Robert G. Tull Spectrograph's TS23
configuration (R=60000 and coverage from 3750 to 10200Å).
See Section 2.1.
Note that although both Phase I and II data were obtained between
1990 and 1995, we list these data in separate portions of the table
rather than interspersing them.
Note (2): The internal uncertainties that we calculated for the Phase I and II
data are not reliable and so are not quoted. The standard deviation
of the measurements are 23m/s and 21m/s for the Phase I and II
data, respectively.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- CCD CCD used in the observation (1)
5- 7 I3 --- Seq Running sequence number
9- 21 F13.5 d BJD Barycentric Julian Date
23- 27 F5.1 m/s dRV [-14/31]? Differential radial velocity (G1)
29- 31 F3.1 m/s e_dRV [3/7]? Uncertainty in dRV
33- 37 F5.3 --- SHK [0.13/0.35]? The SHK index
39- 43 F5.3 --- e_SHK [0.004/0.03]? Uncertainty in SHK
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Note (1): We obtained 72 spectra between 1996 October 6 and 2000 December 3 UT,
and 288 more between 2005 December 9 and 2012 January 11 UT,
for a total of 360 spectra.
The major difference between these data sets is that the earlier
observations used an 2048x2048 Tektronics CCD ("Old", 72 rows),
whereas the newer data set used a 3x1 mosaic of 2048x4096 CCDs
("New"; 288 rows). See section 2.2 for further explanations.
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Global notes:
Note (G1): The velocities have been shifted such that the mean velocity of
each dataset is 0.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 25-Jul-2016