J/ApJ/861/149 Kepler Follow-up Observation Program. II. Spectro. (Furlan+, 2018)
The Kepler Follow-up Observation Program.
II. Stellar parameters from medium- and high-resolution spectroscopy.
Furlan E., Ciardi D.R., Cochran W.D., Everett M.E., Latham D.W., Marcy G.W.,
Buchhave L.A., Endl M., Isaacson H., Petigura E.A., Gautier T.N., Huber D.,
Bieryla A., Borucki W.J., Brugamyer E., Caldwell C., Cochran A.,
Howard A.W., Howell S.B., Johnson M.C., MacQueen P.J., Quinn S.N.,
Robertson P., Mathur S., Batalha N.M.
<Astrophys. J., 861, 149 (2018)>
=2018ApJ...861..149F 2018ApJ...861..149F
ADC_Keywords: Abundances, [Fe/H]; Stars, double and multiple; Spectra, optical;
Planets
Keywords: planets and satellites: fundamental parameters;
stars: fundamental parameters; surveys; techniques: spectroscopic
Abstract:
We present results from spectroscopic follow-up observations of stars
identified in the Kepler field and carried out by teams of the Kepler
Follow-up Observation Program. Two samples of stars were observed over
6yr (2009-2015): 614 standard stars (divided into "platinum" and
"gold" categories) selected based on their asteroseismic detections
and 2667 host stars of Kepler Objects of Interest (KOIs), most of them
planet candidates. Four data analysis pipelines were used to derive
stellar parameters for the observed stars. We compare the Teff,
log(g), and [Fe/H] values derived for the same stars by different
pipelines; from the average of the standard deviations of the
differences in these parameter values, we derive error floors of
∼100K, 0.2dex, and 0.1dex for Teff, log(g), and [Fe/H], respectively.
Noticeable disagreements are seen mostly at the largest and smallest
parameter values (e.g., in the giant star regime). Most of the log(g)
values derived from spectra for the platinum stars agree on average
within 0.025dex (but with a spread of 0.1-0.2dex) with the
asteroseismic log(g) values. Compared to the Kepler Input Catalog
(KIC), the spectroscopically derived stellar parameters agree within
the uncertainties of the KIC but are more precise and thus an
important contribution toward deriving more reliable planetary radii.
Description:
Four main facilities were used to carry out the Kepler Follow-up
Observation Program (KFOP) spectroscopic follow-up observations: the
Tillinghast 1.5m telescope with the Tillinghast Reflector Echelle
Spectrograph (TRES), the McDonald 2.7m telescope with the Tull Coude
Spectrograph, the Kitt Peak National Observatory (KPNO) Mayall 4m
telescope with the facility Richey-Chretien long-slit spectrograph (RC
Spec), and the Keck I 10m telescope with the High Resolution Echelle
Spectrometer (HIRES). In addition, a few stars were also observed at
the 2.6m Nordic Optical Telescope (NOT) with the FIber-fed Echelle
Spectrograph (FIES).
The first KFOP observations started in 2009 June and continued through
the following observing seasons up to 2015 October. A few more spectra
were obtained at the Tillinghast 1.5m telescope up to 2016 September,
but they are not included in this work. All spectra cover the optical
wavelength region, and most of them have high resolving power
(R∼45000-65000). Only the spectra obtained with RC Spec at the KPNO 4m
telescope have a medium resolving power of R∼3000.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 86 2667 Summary of KOI host stars with spectroscopic
observations
table3.dat 63 8085 Summary of KFOP spectroscopic observations of
Kepler stars (standard stars, KOI host stars)
table4.dat 130 100 *Stellar parameters of the Platinum standard stars
table6.dat 42 436 *Stellar parameters of the Gold standard stars
derived from Tillinghast spectra with SPC
table7.dat 131 1766 *Stellar parameters of KOI host stars
table9.dat 47 2302 Combined stellar parameters of the Platinum
standard stars, Gold standard stars, and
KOI host stars
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Note on table4.dat, table6.dat, table7.dat:
The SPC code was developed for TRES spectra
(Buchhave+ 2012, J/other/Nat/486.375).
The Kea code was developed for spectra obtained with the Tull Coude
spectrograph at the 2.7m telescope at McDonald Observatory (Endl &
Cochran 2016PASP..128i4502E 2016PASP..128i4502E).
The SpecMatch code was developed for Keck/HIRES spectra
(Petigura 2015PhDT........82P 2015PhDT........82P).
The Newspec code is used primarily on spectra from RC Spec on Kitt
Peak's 4m telescope (Everett+ 2013, J/ApJ/771/107).
See section 4.
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See also:
VI/120 : High-resolution synthetic stellar library (Coelho+, 2005)
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
J/ApJS/190/1 : A survey of stellar families (Raghavan+, 2010)
J/ApJ/728/117 : Kepler planetary candidates. I. (Borucki+, 2011)
J/ApJ/736/19 : Kepler planetary candidates. II. (Borucki+, 2011)
J/AJ/142/112 : KIC photometric calibration (Brown+, 2011)
J/AJ/141/45 : Speckle observations of HIP stars (Horch+, 2011)
J/AJ/142/160 : Kepler Mission. II. EBs in DR2 (Slawson+, 2011)
J/other/Nat/486.375 : Stellar parameters of KOI stars (Buchhave+, 2012)
J/ApJS/199/30 : Eff. temperature scale for KIC stars (Pinsonneault+, 2012)
J/ApJ/757/161 : Spectroscopy of 56 exoplanet host stars (Torres+, 2012)
J/ApJS/204/24 : Kepler planetary candidates. III. (Batalha+, 2013)
J/ApJ/771/107 : Spectroscopy of faint KOI stars (Everett+, 2013)
J/ApJ/767/127 : Asteroseismic solutions for 77 Kepler stars (Huber+, 2013)
J/A+A/558/A106 : Chemical abundances for 83 transit hosts (Mortier+, 2013)
J/ApJS/208/9 : Intrinsic colors & temperatures of PMS stars (Pecaut+, 2013)
J/ApJ/770/69 : Kepler planet candidates radii (Petigura+, 2013)
J/ApJS/210/19 : Kepler planetary candidates. IV. 22 months (Burke+, 2014)
J/ApJS/210/1 : Asteroseismic study of solar-type stars (Chaplin+, 2014)
J/AJ/147/119 : Cat. of sources in Kepler field of view (Coughlin+, 2014)
J/ApJS/211/2 : Revised properties of Q1-16 Kepler targets (Huber+, 2014)
J/ApJS/210/20 : Small Kepler planets radial velocities (Marcy+, 2014)
J/ApJS/215/19 : APOKASC catalog of Kepler red giants (Pinsonneault+, 2014)
J/ApJ/784/45 : Kepler's multiple planet candidates. III. (Rowe+, 2014)
J/ApJ/808/187 : Metallicities of KIC stars without planets (Buchhave+, 2015)
J/ApJS/220/19 : LAMOST obs. in the Kepler field. I. (De Cat+, 2015)
J/ApJS/217/31 : Kepler planetary cand. VI. 4yr Q1-Q16 (Mullally+, 2015)
J/ApJS/217/16 : Kepler planetary candidates. V. 3yr Q1-Q12 (Rowe+, 2015)
J/ApJS/217/18 : Potential transit signals in Kepler Q1-Q17 (Seader+, 2015)
J/ApJS/224/12 : Kepler planetary candidates. VII. 48-month (Coughlin+, 2016)
J/ApJ/827/50 : Kepler faint red giants (Mathur+, 2016)
J/ApJ/822/86 : False positive prob. for Q1-Q17 DR24 KOIs (Morton+, 2016)
J/A+A/587/A64 : Physical properties of giant exoplanets (Santerne+, 2016)
J/MNRAS/463/1297 : Asteroseismology of misclassified red giants (Yu+, 2016)
J/AJ/153/71 : Kepler follow-up obs. program. I. Imaging (Furlan+, 2017)
J/AJ/154/108 : California-Kepler Survey (CKS). II. (Johnson+, 2017)
J/ApJS/229/30 : Revised properties of Q1-17 Kepler targets (Mathur+, 2017)
J/AJ/154/107 : California-Kepler Survey. I. 1305 stars (Petigura+, 2017)
J/ApJS/235/38 : Kepler planetary cand. VIII. DR25 rel. (Thompson+, 2018)
http://exoplanetarchive.ipac.caltech.edu/ : NASA exoplanet archive
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- KOI [1/7619] Kepler Object of Interest designation
6- 13 I8 --- KIC [757450/12885212] Kepler Input Catalog identifier
15 I1 --- CP [0/6] Number of confirmed planets
17 I1 --- PC [0/4] Number of planet candidates
19 I1 --- FP [0/5] Number of false positives
21- 28 F8.1 Rgeo Rp [0.1/200346] Radius, smallest planet in system (1)
30- 36 F7.2 --- KOI-Rp [1.01/7619.01] KOI identifier of smallest planet
in system
38- 42 I5 K Teq [25/14225] Equilibrium temperature of coolest
planet in system (1)
44- 50 F7.2 --- KOI-Teq [1.01/7619.01] KOI identifier of coolest planet
in system
52- 56 F5.2 mag Kpmag [6.9/17.2] Host star Kepler apparent magnitude
58- 62 F5.2 mag Vmag [7.5/17.6] Host star V band apparent magnitude
64- 68 F5.2 mag Ksmag [4.7/14.7] Host star 2MASS Ks band apparent
magnitude
70- 86 A17 --- Tel Observatories where data were obtained (G1)
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Note (1): Note that if a system contains both planets and false positives, only
the planets are used to determine the smallest planet radius and
lowest equilibrium temperature.
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Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- KOI [0/7619] Kepler Object of Interest designation (G2)
6- 13 I8 --- KIC [757450/12885212] Kepler Input Catalog identifier
15- 15 I1 --- Group [0/2] Group number (G3)
17- 20 A4 --- Tel Telescope used (G1)
22- 27 A6 --- Inst Instrument used
29- 33 I5 --- R [60/67000] Resolving power
35- 42 A8 nm Range Spectrograph wavelength coverage
44- 48 F5.1 --- SNR [2/266.3]?=0 Signal-to-Noise Ratio of the spectrum
at lambda
50- 52 I3 nm lambda [440/565]?=0 Wavelength at which SNR was measured
54- 63 A10 "Y/M/D" Date Observation date
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Byte-by-byte Description of file: table[47].dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- KOI [1/7619]? KOI designation
6- 13 I8 --- KIC [1026957/12885212] KIC identifier
15- 18 I4 K Teff1 [4800/6754]? SPC Effective temperature
20- 22 I3 K e_Teff1 [49/128]? SPC uncertainty in Teff
24- 27 F4.2 [cm/s2] log(g)1 [3.2/4.8]? SPC log surface gravity
29- 32 F4.2 [cm/s2] e_log(g)1 [0.1/0.3]? SPC uncertainty in log(g)
34- 38 F5.2 [Sun] [Fe/H]1 [-1/0.5]? SPC Metallicity
40- 43 F4.2 [Sun] e_[Fe/H]1 [0.08/0.2]? SPC uncertainty in [Fe/H]
45- 48 I4 K Teff2 [3737/8875]? Kea Effective temperature
50- 52 I3 K e_Teff2 [25/530]? Kea uncertainty in Teff
54- 57 F4.2 [cm/s2] log(g)2 [1/5]? Kea log surface gravity
59- 62 F4.2 [cm/s2] e_log(g)2 [0.04/0.9]? Kea uncertainty in log(g)
64- 68 F5.2 [Sun] [Fe/H]2 [-1/0.5]? Kea Metallicity
70- 73 F4.2 [Sun] e_[Fe/H]2 [0.02/0.4]? Kea uncertainty in [Fe/H]
75- 78 I4 K Teff3 [0/6562]? SpecMatch Effective temperature
80- 81 I2 K e_Teff3 [60/64]? SpecMatch uncertainty in Teff
83- 86 F4.2 [cm/s2] log(g)3 [2.2/4.8]? SpecMatch log surface gravity
88- 91 F4.2 [cm/s2] e_log(g)3 [0.07/0.1]? SpecMatch uncertainty in log(g)
93- 97 F5.2 [Sun] [Fe/H]3 [-0.7/0.5]? SpecMatch Metallicity
99-102 F4.2 [Sun] e_[Fe/H]3 [0.04/0.1]? SpecMatch uncertainty in [Fe/H]
104-107 I4 K Teff4 [4570/6682]? Newspec Effective temperature
109-110 I2 K e_Teff4 [75]? Newspec uncertainty in Teff
112-115 F4.2 [cm/s2] log(g)4 [4/4.7]? Newspec log surface gravity
117-120 F4.2 [cm/s2] e_log(g)4 [0.15]? Newspec uncertainty in log(g)
122-126 F5.2 [Sun] [Fe/H]4 [-0.3/0.3]? Newspec Metallicity
128-131 F4.2 [Sun] e_[Fe/H]4 [0.1]? Newspec uncertainty in [Fe/H]
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 I8 --- KIC [1430163/12735580] KIC identifier
10- 13 I4 --- KOI [1/5665]? KOI designation
15- 18 I4 K Teff [4699/6662] Effective temperature
20- 21 I2 K e_Teff [49/61] Uncertainty in Teff
23- 26 F4.2 [cm/s2] log(g) [2.3/4.8] log surface gravity
28- 31 F4.2 [cm/s2] e_log(g) [0.1/0.2] Uncertainty in log(g)
33- 37 F5.2 [Sun] [Fe/H] [-0.8/0.5] Metallicity
39- 42 F4.2 [Sun] e_[Fe/H] [0.08] Uncertainty in [Fe/H]
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Byte-by-byte Description of file: table9.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- KOI [0/7619] KOI designation (G2)
6- 13 I8 --- KIC [1026957/12885212] KIC identifier (1)
15- 15 I1 --- Group [0/2]? Group number (G3)
17- 20 I4 K Teff [0/8875] Combined effective temperature (2)
22- 24 I3 K e_Teff [100/530] Uncertainty in Teff
26- 29 F4.2 [cm/s2] log(g) [1/5] Combined log surface gravity (2)
31- 34 F4.2 [cm/s2] e_log(g) [0.2/0.9] Uncertainty in log(g)
36- 40 F5.2 [Sun] [Fe/H] [-1/0.5] Combined metallicity (2)
42- 45 F4.2 [Sun] e_[Fe/H] [0.1/0.4] Uncertainty in [Fe/H]
47 I1 --- Num [1/4] Number of combined measurements
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Note (1): The table lists the parameters for the platinum stars (ordered by
KIC), then those for the gold stars (also ordered by KIC), and
finally those of the KOI host stars (ordered by KOI number).
Note (2): Combined value when more than one measurement was available -
see text for details.
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Global notes:
Note (G1): Observatory as follows:
KP-4 = Kitt Peak 4m;
Keck = Keck I 10m;
McD = McDonald 2.7m;
NOT = Nordic Optical Telescope 2.6m;
Til = Tillinghast 1.5m.
Note (G2): A 0 indicates that the star is in the Kepler field, but was not
identified as a KOI.
Note (G3): Group as follows:
1 = platinum standard stars: Teff values range from ∼4800 to 6700K,
log(g) from 3.3 to 4.6, and [Fe/H] from -1.1 (DR24) or -1.75 (DR25)
to +0.4 --best asteroseismic detections;
2 = gold standard stars: parameter ranges are similar; just a few stars
have Teff<4900 or Teff>6700K --detections of solar-like oscillations;
0 = KOI host star.
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History:
From electronic version of the journal
References:
Furlan et al. Paper I. 2017AJ....153...71F 2017AJ....153...71F Cat. J/AJ/153/71
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 15-Jul-2019