J/MNRAS/457/2877 Kepler M dwarf stars revised properties (Gaidos+, 2016)
They are small worlds after all: revised properties of Kepler M dwarf stars
and their planets.
Gaidos E., Mann A.W., Kraus A.L., Ireland M.
<Mon. Not. R. Astron. Soc., 457, 2877-2899 (2016)>
=2016MNRAS.457.2877G 2016MNRAS.457.2877G (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Effective temperatures ;
Stars, masses ; Stars, diameters ; Stars, distances
Keywords: stars: abundances - stars: fundamental parameters - stars: late-type -
stars: low-mass - planetary systems - stars: statistics
Abstract:
We classified the reddest (r-J>2.2) stars observed by the NASA Kepler
mission into main-sequence dwarf or evolved giant stars and determined
the properties of 4216 M dwarfs based on a comparison of available
photometry with that of nearby calibrator stars, as well as available
proper motions and spectra. We revised the properties of candidate
transiting planets using the stellar parameters, high-resolution
imaging to identify companion stars, and, in the case of binaries,
fitting light curves to identify the likely planet host. In 49 of 54
systems, we validated the primary as the host star. We inferred the
intrinsic distribution of M dwarf planets using the method of
iterative Monte Carlo simulation. We compared several models of planet
orbital geometry and clustering and found that one where planets are
exponentially distributed and almost precisely coplanar best describes
the distribution of multiplanet systems. We determined that Kepler M
dwarfs host an average of 2.2±0.3 planets with radii of
1-4R⊕ and orbital periods of 1.5-180d. The radius
distribution peaks at ∼1.2R⊕ and is essentially zero at
4R⊕, although we identify three giant planet candidates other
than the previously confirmed Kepler-45b. There is suggestive but not
significant evidence that the radius distribution varies with orbital
period. The distribution with logarithmic orbital period is flat
except for a decline for orbits less than a few days. 12 candidate
planets, including two Jupiter-size objects, experience an irradiance
below the threshold level for a runaway greenhouse on an Earth-like
planet and are thus in a 'habitable zone'.
Description:
We have classified the reddest (M-type) stars observed by the Kepler
prime mission into dwarfs and giants and estimated the properties of
the dwarfs using empirical, model-independent relations with
photometric colours derived from a set of nearby calibrator stars with
established parallaxes (and sometimes angular radii). We also
investigated the multiplicity of 54 of the 73 M dwarfs hosting
candidate planets using AO imaging, and estimated the properties of
candidate stellar companions based on the contrast ratio in the
near-infrared K band, assuming they are at the same distance as the
primary. We combined the revised properties of the stars with fits of
the Kepler light curve transits to re-estimate the properties of the
planets.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 79 4216 Kepler M dwarfs
table2.dat 45 63 Candidate stellar companions of KOIs
table3.dat 115 75 Light curve fit parameters
table4.dat 50 107 Kepler M dwarf candidate planets
--------------------------------------------------------------------------------
See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 I8 --- KIC KIC number
10- 14 F5.3 --- Pdwarf Probability of dwarf
16- 19 I4 K Teff Effective temperature
21- 23 I3 K e_Teff rms uncertainty on Teff
25- 28 A4 --- n_Teff [PHOT/SPEC] Origin of Teff
(photometric or spectroscopic)
30- 34 F5.2 [-] [Fe/H] Metallicity
36- 39 F4.2 [-] e_[Fe/H] rms uncertainty on [Fe/H]
41- 44 A4 --- n_[Fe/H] [PHOT/SPEC] Origin of [Fe/H]
(photometric or spectroscopic)
46- 49 F4.2 Rsun R* Stellar radius
51- 54 F4.2 Rsun e_R* rms uncertainty on R*
56- 59 F4.2 Msun M* Stellar mass
61- 64 F4.2 Msun e_M* rms uncertainty on M*
66- 69 F4.2 mag K'MAG Absolute K' magnitude
71- 74 F4.2 mag e_K'MAG rms uncertainty on K'MAG
76- 79 I4 pc Dist Distance
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 I8 --- KIC KIC number
10- 13 I4 --- KOI KOI star number
15- 19 F5.2 --- DK' K'-band contrast ratio
21- 25 F5.3 arcsec theta Angular separation between the primary and
putative companion
27- 29 I3 deg PA Position angle
31- 34 I4 K Teff ?=0 Effective temperature
36- 38 I3 K e_Teff ?=0 rms uncertainty on Teff
40- 45 F6.4 --- pBACK False-positive (FP) probability that if the
planet candidate were around the fainter
companion/background star it would be larger
than Jupiter and thus probably not a planet
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- KOI KOI planet number (NNNN.NN)
11- 18 I8 --- KIC KIC number
19 A1 --- m_KIC [ABC] Multiplicity index on KIC (1)
23- 28 F6.4 --- Rp/R* Planet-to-star radius ratio
32- 37 F6.4 --- E_Rp/R* Error on Rp/R* (upper value)
41- 46 F6.4 --- e_Rp/R* Error on Rp/R* (lower value)
50- 55 F6.4 --- b Impact parameter
59- 64 F6.4 --- E_b Error on b (upper value)
68- 73 F6.4 --- e_b Error on b (lower value)
77- 82 F6.4 d tau Transit duration
86- 91 F6.4 d E_tau Error on tau (upper value)
95-100 F6.4 d e_tau Error on tau (lower value)
102-109 F8.4 d Per Period
112-115 F4.2 --- Prob ?=- Probability (1)
--------------------------------------------------------------------------------
Note (1): For candidate multistar systems, the probability of the planet
orbiting the given star (ABC) is based on a comparison of stellar densities
derived from transits versus photometry or spectroscopy.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- KOI KOI planet number (NNN.NN)
9- 16 I8 --- KIC KIC number
18- 24 F7.3 d Per Period
26- 30 F5.2 Rgeo Rp Planet radius
32- 35 F4.2 Rgeo e_Rp rms uncertainty on Rp
38- 43 F6.2 Earth Sp Planet irradiance
46- 50 F5.2 Earth e_Sp rms uncertainty on Sp
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 06-Nov-2018