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J/AJ/153/208   LCES HIRES/Keck radial velocity Exoplanet Survey  (Butler+, 2017)

The LCES HIRES/Keck precision radial velocity Exoplanet Survey. Butler R.P., Vogt S.S., Laughlin G., Burt J.A., Rivera E.J., Tuomi M., Teske J., Arriagada P., Diaz M., Holden B., Keiser S. <Astron. J., 153, 208-208 (2017)> =2017AJ....153..208B (SIMBAD/NED BibCode)
ADC_Keywords: Planets ; Stars, nearby ; Stars, dwarfs ; Radial velocities ; Keywords: planetary systems Abstract: We describe a 20 year survey carried out by the Lick-Carnegie Exoplanet Survey Team (LCES), using precision radial velocities from HIRES on the Keck I telescope to find and characterize extrasolar planetary systems orbiting nearby F, G, K, and M dwarf stars. We provide here 60949 precision radial velocities for 1624 stars contained in that survey. We tabulate a list of 357 significant periodic signals that are of constant period and phase, and not coincident in period and/or phase with stellar activity indices. These signals are thus strongly suggestive of barycentric reflex motion of the star induced by one or more candidate exoplanets in Keplerian motion about the host star. Of these signals, 225 have already been published as planet claims, 60 are classified as significant unpublished planet candidates that await photometric follow-up to rule out activity-related causes, and 54 are also unpublished, but are classified as "significant" signals that require confirmation by additional data before rising to classification as planet candidates. Of particular interest is our detection of a candidate planet with Msin(i)=3.8M, and P=9.9 days orbiting Lalande 21185, the fourth-closest main-sequence star to the Sun. For each of our exoplanetary candidate signals, we provide the period and semi-amplitude of the Keplerian orbital fit, and a likelihood ratio estimate of its statistical significance. We also tabulate 18 Keplerian-like signals that we classify as likely arising from stellar activity. Description: We present 60949 precision radial velocities of 1624 stars obtained over the past 20 years from the Lick-Carnegie Exoplanet Survey Team (LCES) survey with the HIgh-Resolution Echelle Spectrometer (HIRES) spectrometer on the Keck I telescope. We tabulate a list of 357 significant periodic signals that are of constant period and phase, and not coincident in period and/or phase with stellar activity indices. For this survey, the HIRES spectrometer was configured to operate at a nominal spectral resolving power of R∼60000 and wavelength range of 3700-8000Å. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file targets.dat 14 1680 Stars observed table1.dat 74 62913 Radial velocities and chromospheric activity indices of all program stars table2.dat 73 357 *Signals in the Keck data sets table3.dat 84 1010 Maximum likelihood parameter estimates and standard errors for the "nuisance" parameters
Note on table2.dat: With likelihood ratio ΔlnLj=lnL(j=k)-lnL(j=k-1) between models with k and k-1 signals for which the ratio exceeds a value corresponding to a 0.1% False Alarm Probability (FAP) threshold of a three-parameter model (amplitude K, period P, and phase Φ).
See also: J/A+A/566/A66 : Correlation of logR'HK with logIHa (Gomes da Silva+, 2014) J/A+A/551/A79 : RV periodic variations in τ Ceti (Tuomi+, 2013) J/ApJ/646/505 : Catalog of nearby exoplanets (Butler+, 2006) J/ApJ/634/625 : Radial velocities and photometry of GJ 876 (Rivera+, 2005) Byte-by-byte Description of file: targets.dat
Bytes Format Units Label Explanations
1- 14 A14 --- Name Target identifier
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 14 A14 --- Name Target identifier 16- 28 F13.5 d BJD Barycentric Julian Date 30- 38 F9.2 m/s RV [-39874.3/42363.6] Radial velocity 40- 45 F6.2 m/s e_RV [0.01/252.9] 1σ uncertainty in RV 47- 53 F7.4 --- S [-5.5/68.9] Chromosperic activity index S-index (1) 55- 62 F8.5 --- H [-1/0.11]? Chromosperic activity index H-index (2) 64- 69 I6 --- Count [67/616935] Median photons per pixel 71- 74 I4 s Exp [-1/2551] Exposure time
Note (1): Obtained from measurement of the emission reversal at the cores of the Fraunhofer H and K lines of Ca II at 3968Å and 3934Å respectively. Note (2): A measure of the chromospheric emission component at the Hα Balmer line of hydrogen at 6563Å (Gomes da Silva et al. 2011A&A...534A..30G). Note that H-index values H≥0.062 are to be considered with caution (see Section 4 in the paper).
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 4 I4 --- Num [4/1672] Target number 6- 15 A10 --- Name Target identifier 17 I1 --- Ns [1/4] Number of signals (nsignals) 19- 24 F6.2 [-] LR [16.5/673.3] Likelihood ratio (ΔlnLk) 26- 35 F10.5 d Per [1/6264.7] Period 37- 45 F9.5 d e_Per [0/573.77] Uncertainty in Per 47- 52 F6.2 m/s K [1.25/840.71] Radial velocity amplitude 54- 59 F6.2 m/s e_K [0.17/165.1] Uncertainty in K 61- 69 A9 --- Signal Interpretation (either Activity, Candidate, Published, or SRC=Signal Requiring Confirmation) (1) 71- 73 A3 --- Note Additional note (1-7) (2)
Note (1): The signals are classified as follows: Published = Signal that have already been published as planet claim; Candidate = Significant unpublished planet candidate that await photometric follow-up to rule out activity-related cause; SRC = Signal Requiring Confirmation by additional data before rising to classification as planet candidate; Activity = Keplerian-like signal that we classify as likely arising from stellar activity. Note (2): Additional notes are defined as follows: 1 = Signal coincides with a photometric rotation period based on ASAS V-band photometry; 2 = Corresponding signal in the S-index data at a very nearby period likely indicative of the rotation period of the star; 3 = Signal not constrained from above in the parameter space as the analyses were limited to 1 day<P<Tobs; 4 = Coincides with the stellar magnetic cycle apparent in the S-index but strong enough as a signal to be interpreted as a candidate planet; 5 = Likely artifact signal caused by orbital evolution of the system; 6 = Daily alias of the known transiting planet orbiting the star with an orbital period of 0.73 days (Winn et al. 2011ApJ...737L..18W); 7 = The strongest S-index counterpart in our sample indicates this signal is likely caused by activity unless one argues that S-index variability cannot have counterparts in radial velocities. Signal reported as a planet candidate.
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 4 I4 --- Num [3/1673] Target number 6- 19 A14 --- Name Target identifier 21- 28 F8.3 m/s/yr dV/dt [-900.31/622.51] Linear acceleration γ 30- 36 F7.3 m/s/yr e_dV/dt [0.035/332.111] Standard error in dV/dt 38- 42 F5.2 m/s sigmaJ [0.32/98.7] Excess white noise or "jitter" (σJ) 44- 48 F5.2 m/s e_sigmaJ [0.07/20.31] Standard error in sigmaJ 50- 58 F9.3 m/s cS [-4866.9/8437.7] Coefficient quantifying linear dependence of the radial velocities on the S-index (cS) 60- 67 F8.3 m/s e_cS [0.18/4622.1] Standard error in cS 69- 75 F7.3 [-] LRS [7.883/159.22]?=0 Likelihood ratio statistic ΔlnLS (1) 77- 84 F8.3 d Per [2.065/6308.8]?=0 Period of the signal in the S-index time-series (PS)
Note (1): ΔlnLS=lnLS(k=1)-lnLS(k=0) represents the likelihood ratio statistic of model with a signal (k=1) in the S-index with respect to a model without a signal (k=0). Only signals exceeding a ratio of 7.82 corresponding to 5% False Alarm Probability (FAP) are shown.
History: From electronic version of the journal
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 07-Aug-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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