J/ApJ/783/123 Surface gravity for 220 Kepler stars (Campante+, 2014)
Limits on surface gravities of Kepler planet-candidate host stars from
non-detection of solar-like oscillations.
Campante T.L., Chaplin W.J., Lund M.N., Huber D., Hekker S., Garcia R.A.,
Corsaro E., Handberg R., Miglio A., Arentoft T., Basu S., Bedding T.R.,
Christensen-Dalsgaard J., Davies G.R., Elsworth Y.P., Gilliland R.L.,
Karoff C., Kawaler S.D., Kjeldsen H., Lundkvist M., Metcalfe T.S.,
Silva Aguirre V., Stello D.
<Astrophys. J., 783, 123 (2014)>
=2014ApJ...783..123C 2014ApJ...783..123C (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Effective temperatures
Keywords: methods: statistical - planetary systems - stars: late-type -
stars: oscillations - techniques: photometric
Abstract:
We present a novel method for estimating lower-limit surface gravities
(logg) of Kepler targets whose data do not allow the detection of
solar-like oscillations. The method is tested using an ensemble of
solar-type stars observed in the context of the Kepler Asteroseismic
Science Consortium. We then proceed to estimate lower-limit log g for
a cohort of Kepler solar-type planet-candidate host stars with no
detected oscillations. Limits on fundamental stellar properties, as
provided by this work, are likely to be useful in the characterization
of the corresponding candidate planetary systems. Furthermore, an
important byproduct of the current work is the confirmation that
amplitudes of solar-like oscillations are suppressed in stars with
increased levels of surface magnetic activity.
Description:
We propose lower-limit surface gravity estimates for Kepler solar-type
planet-candidate host stars with no detected oscillations, as given in
Table4.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4.dat 74 220 Proposed lower-limit logg estimates for
solar-type KOIs with no detected oscillations
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
J/ApJ/767/127 : Asteroseismic solutions for 77 Kepler stars (Huber+, 2013)
J/ApJS/204/24 : Kepler planetary candidates. III. (Batalha+, 2013)
J/ApJS/199/30 : KIC stars effective temperature scale (Pinsonneault+, 2012)
J/ApJ/753/90 : Stellar parameters of Kepler stars (Mann+, 2012)
J/MNRAS/419/L34 : logg determination in late-type stars (Morel+, 2012)
J/ApJ/736/19 : Kepler planetary candidates. II. (Borucki+, 2011)
J/ApJ/728/117 : Kepler planetary candidates. I. (Borucki+, 2011)
Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- KOI [4/5814]? Kepler Object of Interest number (1)
6- 13 I8 --- KIC [1871056/12403119] Kepler Input Catalog number
15- 20 F6.3 mag Kpmag [9.8/14.74] Kepler-band magnitude mKep
22- 25 I4 K Teff [5036/7062] Effective temperature from
Pinsonneault et al. 2012 (cat. J/ApJS/199/30)
27- 29 I3 K e_Teff [57/273] Error in Teff
31- 34 I4 ppm zeta [24/1286] Proxy of the level of stellar
activity (ζact) (2)
36- 38 I3 ppm e_zeta [11/590] Error in zeta
40- 43 F4.2 [cm/s2] logg [3.4/4.5] Log of marginal detection surface
gravity (log gmd) (3)
45- 48 F4.2 [cm/s2] E_logg [0.04/0.33] Positive uncertainty in logg
50- 53 F4.2 [cm/s2] Elogg [0.01/0.33] Positive uncertainty in logg (4)
55- 58 F4.2 [cm/s2] e_logg [0.04/0.37] Negative uncertainty in logg
60- 63 F4.2 [cm/s2] elogg [0.01/0.37] Negative uncertainty in logg (4)
65- 69 F5.2 [cm/s2] Dlogg [-0.5/1.2]? Individual differential surface
gravity (Δlogg) (5)
71- 74 F4.2 [cm/s2] e_Dlogg [0.04/0.31]? Error in Dlogg
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Note (1): The top eight entries had no assigned KOI identifier at the time of
writing.
Note (2): The magnetic activity proxy was taken as the median of the quarterly
proxy estimates, with an associated uncertainty (ζerror) given by
the Median Absolute Deviation (MAD) of those same quarterly estimates times
the constant scale factor k. See Appendix B for further details.
Note (3): We may convert the marginal detection vmax,md into an equivalent
marginal detection surface gravity, gmd. See Section 2.2 for more
details.
Note (4): Uncertainties are produced by Equation (2):
g∼g☉(vmax/vmax,☉)(Teff/Teff,☉)1/2,
with g☉=27402cm/s2, vmax,☉=3150µHz and Teff,☉=5777K;
and do not take into account the adopted figure of 0.04cm/s2 for the
accuracy.
Note (5): In order to evaluate the performance of our method, we computed
Δlogg, i.e., the difference between the logg from Batalha et al.
2013 (cat. J/ApJS/204/24) and the proposed loggmd. Please refer to
Section 3.2 for further details.
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History:
From electronic version of the journal
(End) Sylvain Guehenneux [CDS] 03-Jun-2016