J/ApJ/844/102 KIC star parallaxes from asteroseismology vs Gaia (Huber+, 2017)
Asteroseismology and Gaia: testing scaling relations using 2200 Kepler stars
with TGAS parallaxes.
Huber D., Zinn J., Bojsen-Hansen M., Pinsonneault M., Sahlholdt C.,
Serenelli A., Aguirre V.S., Stassun K., Stello D., Tayar J., Bastien F.,
Bedding T.R., Buchhave L.A., Chaplin W.J., Davies G.R., Garcia R.A.,
Latham D.W., Mathur S., Mosser B., Sharma S.
<Astrophys. J., 844, 102 (2017)>
=2017ApJ...844..102H 2017ApJ...844..102H
ADC_Keywords: Asteroseismology ; Parallaxes, trigonometric ; Photometry, SDSS ;
Photometry, infrared ; Abundances, [Fe/H] ; Stars, diameters
Keywords: parallaxes; stars: distances; stars: fundamental parameters;
stars: late-type; stars: oscillations; techniques: photometric
Abstract:
We present a comparison of parallaxes and radii from asteroseismology
and Gaia DR1 (TGAS) for 2200 Kepler stars spanning from the main
sequence to the red-giant branch. We show that previously identified
offsets between TGAS parallaxes and distances derived from
asteroseismology and eclipsing binaries have likely been overestimated
for parallaxes ≲5-10mas (∼90%-98% of the TGAS sample). The observed
differences in our sample can furthermore be partially compensated by
adopting a hotter Teff scale (such as the infrared flux method)
instead of spectroscopic temperatures for dwarfs and subgiants.
Residual systematic differences are at the ∼2% level in parallax
across three orders of magnitude. We use TGAS parallaxes to
empirically demonstrate that asteroseismic radii are accurate to ∼5%
or better for stars between ∼0.8-8R☉. We find no significant
offset for main- sequence (≲1.5R☉) and low-luminosity RGB stars
(∼3-8R☉), but seismic radii appear to be systematically
underestimated by ∼5% for subgiants (∼1.5-3R☉). We find no
systematic errors as a function of metallicity between [Fe/H]~-0.8 to
+0.4dex, and show tentative evidence that corrections to the scaling
relation for the large frequency separation (Δν) improve the
agreement with TGAS for RGB stars. Finally, we demonstrate that beyond
∼3kpc asteroseismology will provide more precise distances than
end-of-mission Gaia data, highlighting the synergy and complementary
nature of Gaia and asteroseismology for studying galactic stellar
populations.
Description:
Our sample consists of dwarfs, subgiants, and red giants from the
APOGEE-Kepler Asteroseismic Science Consortium (APOKASC,
Pinsonneault+ J/ApJS/215/19), supplemented with seismic detections
using Kepler short-cadence data from Chaplin+ (2014MNRAS.445..946C 2014MNRAS.445..946C)
and Huber+ (2013, J/ApJ/767/127).
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 185 2236 Observational data
table2.dat 302 2236 Derived fundamental properties, distances and
extinctions
--------------------------------------------------------------------------------
See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
I/337 : Gaia DR1 (Gaia Collaboration, 2016)
J/A+A/506/465 : Solar-like oscillations in red giants (Hekker+, 2009)
J/A+A/523/A48 : Gaia photometry (Jordi+, 2010)
J/AJ/142/112 : KIC photometric calibration (Brown+, 2011)
J/A+A/530/A138 : Geneva-Copenhagen survey re-analysis (Casagrande+, 2011)
J/A+A/525/A131 : Solar-like oscillations in Kepler red giants (Hekker+, 2011)
J/ApJ/746/101 : Diameters and temperatures of AFG stars (Boyajian+, 2012)
J/ApJ/757/112 : Stellar diameters. II. K and M-stars (Boyajian+, 2012)
J/other/Nat/486.375 : Stellar parameters of KOI stars (Buchhave+, 2012)
J/ApJS/199/30 : Effective temperatures for KIC stars (Pinsonneault+, 2012)
J/ApJ/757/161 : Spectroscopy of 56 exoplanet host stars (Torres+, 2012)
J/ApJ/767/127 : Asteroseismic solutions for 77 Kepler stars (Huber+, 2013)
J/ApJ/765/L41 : Asteroseismic classification of KIC objects (Stello+, 2013)
J/ApJ/787/110 : Stromgren survey of seismic KIC stars (Casagrande+, 2014)
J/ApJS/215/19 : APOKASC catalog of Kepler red giants (Pinsonneault+, 2014)
J/MNRAS/445/2758 : KIC giants Bayesian dist. & extinctions (Rodrigues+ 2014)
J/ApJ/808/187 : Metallicities of KIC stars without planets (Buchhave+, 2015)
J/MNRAS/454/2863 : Teff against colours calibrations (Huang+, 2015)
J/MNRAS/452/2127 : Parameters of Kepler stars (Silva Aguirre+, 2015)
J/ApJ/832/121 : 4yr RV survey of red giant in eclipsing bin. (Gaulme+, 2016)
J/ApJ/832/L18 : Gaia's DR1 parallaxes vs previous measurements (Jao+, 2016)
J/ApJ/827/50 : Kepler faint red giants (Mathur+, 2016)
J/AJ/152/180 : Bolometric fluxes of EB* in Tycho-2 (Stassun+, 2016)
J/ApJ/831/L6 : Eclipsing binary parallaxes with Gaia data (Stassun+, 2016)
J/A+A/588/A87 : Seismic global parameters of 6111 KIC (Vrard+, 2016)
J/AJ/152/6 : Kepler stars param. with LAMOST & seismic data (Wang+, 2016)
J/A+A/597/A30 : Seismology & spectro. of CoRoGEE red giants (Anders+, 2017)
J/ApJS/229/30 : Revised properties of Q1-17 Kepler targets (Mathur+, 2017)
J/ApJ/838/107 : Distances to RRab stars from WISE and Gaia (Sesar+, 2017)
J/ApJ/835/173 : Kepler asteroseismic LEGACY data. II. (Silva Aguirre+, 2017)
J/ApJ/835/83 : K2 GAP data release. I. Campaign 1 (Stello+, 2017)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 I8 --- KIC [1160789/12735580] Kepler Input Catalog ID
10- 17 F8.3 uHz numax [2/4190] Frequency of maximum oscillation power
19- 25 F7.3 uHz e_numax [0.03/704] Uncertainty in numax (1)
27- 33 F7.3 uHz dnu [0.4/173.3] Large frequency separation (1)
35- 39 F5.3 uHz e_dnu [0.008/8.6] Uncertainty in dnu (1)
41- 48 F8.5 mas plx [-1.5/47] TGAS parallax
50- 56 F7.5 mas e_plx [0.2/1] Uncertainty in plx
58- 63 F6.3 mag BTmag [6.7/15]?=-99 Tycho BT band photometry
65- 69 F5.3 mag e_BTmag [0.01/0.8]?=-99 Uncertainty in BTmag
71- 76 F6.3 mag VTmag [5.9/13]?=-99 Tycho VT band photometry
78- 82 F5.3 mag e_VTmag [0.009/0.3]?=-99 Uncertainty in VTmag
84- 90 F7.3 mag gmag [7.5/13.7]?=-99 SDSS KIC g band magnitude (2)
92- 98 F7.3 mag e_gmag [0.02]?=-99 Uncertainty in gmag
100-106 F7.3 mag rmag [7.2/12.9]?=-99 SDSS KIC r band magnitude (2)
108-114 F7.3 mag e_rmag [0.02]?=-99 Uncertainty in rmag
116-122 F7.3 mag imag [7/12.7]?=-99 SDSS KIC i band magnitude (2)
124-130 F7.3 mag e_imag [0.02]?=-99 Uncertainty in imag
132-138 F7.3 mag zmag [7/12.5]?=-99 SDSS KIC z band magnitude
140-146 F7.3 mag e_zmag [0.02]?=-99 Uncertainty in zmag
148-153 F6.3 mag Jmag [5/11.5]?=-99 2MASS J band magnitude
155-159 F5.3 mag e_Jmag [0/0.3]?=-99 Uncertainty in Jmag
161-166 F6.3 mag Hmag [4.7/11.1]?=-99 2MASS H band magnitude
168-172 F5.3 mag e_Hmag [0/0.2]?=-99 Uncertainty in Hmag
174-179 F6.3 mag Ksmag [4.4/11.1]?=-99 2MASS Ks band magnitude
181-185 F5.3 mag e_Ksmag [0/0.07]?=-99 Uncertainty in Ksmag
--------------------------------------------------------------------------------
Note (1): numax and dnu were calculated using the SYD pipeline,
Huber+ (2009CoAst.160...74H 2009CoAst.160...74H), and taken from version 3.6.5 of the
APOKASC catalog (Pinsonneault+, in prep) for giants and from a
reanalysis of the Chaplin+ (2014, J/ApJS/210/1) sample for dwarfs and
subgiants (Serenelli+, in prep). Note that for our analysis we added a
1% and 0.5% uncertainty in numax and dnu in quadrature to the formal
uncertainties listed here to account for differences between
asteroseismic analysis methods.
Note (2): gri denotes KIC photometry converted into the SDSS scale using the
transformations by Pinsonneault+ (2012, J/ApJS/199/30).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 I8 --- KIC [1160789/12735580] Kepler Input Catalog ID
10- 13 I4 K Teff [3942/6875] Effective temperature (1)
15- 17 I3 K e_Teff [44/110] Uncertainty in Teff (1)
19- 23 F5.3 [cm/s] logg [1.1/4.6] Log of surface gravity (2)
25- 29 F5.3 [cm/s] e_logg [0.003/0.2] Uncertainty in logg (2)
31- 36 F6.3 [Sun] feh [-2.3/0.5] Metallicity, [Fe/H] (1)
38- 42 F5.3 [Sun] e_feh [0.06/0.2] Uncertainty in feh (1)
44- 49 F6.3 Rsun r-dir [0.7/55.3] Stellar radius, direct method
51- 56 F6.3 Rsun E_r-dir [0.01/20.4] Upper uncertainty in r-dir
58- 63 F6.3 Rsun e_r-dir [0.01/20.4] Lower uncertainty in r-dir
65- 68 I4 pc d-dir [20/5019] Distance, direct method
70- 73 I4 pc E_d-dir [1/1665] Upper uncertainty in d-dir
75- 78 I4 pc e_d-dir [1/1665] Lower uncertainty in d-dir
80- 84 F5.3 mag av-dir [0/1.3] Extinction, direct method
86- 91 F6.3 Rsun r-dir-cor [0.7/54.4] Stellar radius,
dnu corrected direct method
93- 98 F6.3 Rsun E_r-dir-cor [0.01/19.6] Upper uncertainty in r-dir-cor
100-105 F6.3 Rsun e_r-dir-cor [0.01/19.6] Lower uncertainty in r-dir-cor
107-110 I4 pc d-dir-cor [21/4754] Distance,
dnu corrected direct method
112-115 I4 pc E_d-dir-cor [1/1478] Upper uncertainty in d-dir-cor
117-120 I4 pc e_d-dir-cor [1/1478] Lower uncertainty in d-dir-cor
122-126 F5.3 mag av-dir-cor [0/1.3] Extinction,
dnu corrected direct method
128-134 F7.3 Rsun r-grid [0.7/62]?=-99 stellar radius, grid modeling
136-142 F7.3 Rsun E_r-grid [0/11]?=-99 Upper uncertainty in r-grid
144-150 F7.3 Rsun e_r-grid [0/12]?=-99 Lower uncertainty in r-grid
152-155 I4 pc d-grid [20/5244]?=-99 distance, grid modeling
157-159 I3 pc E_d-grid [0/570]?=-99 Upper uncertainty in d-grid
161-163 I3 pc e_d-grid [0/894]?=-99 Lower uncertainty in d-grid
165-171 F7.3 mag av-grid [-0.3/0.9]?=-99 extinction, grid modeling
173-179 F7.3 mag E_av-grid [0/0.4]?=-99 Upper uncertainty in av-grid
181-187 F7.3 mag e_av-grid [0/0.3]?=-99 Lower uncertainty in av-grid
189-195 F7.3 Rsun r-grid-cor [0.7/63]?=-99 stellar radius,
dnu corrected grid modeling
197-203 F7.3 Rsun E_r-grid-cor [0/11]?=-99 Upper uncertainty in r-grid-cor
205-211 F7.3 Rsun e_r-grid-cor [0/12]?=-99 Lower uncertainty in r-grid-cor
213-216 I4 pc d-grid-cor [20/5161]?=-99 distance,
dnu corrected grid modeling
218-220 I3 pc E_d-grid-cor [0/624]?=-99 Upper uncertainty in d-grid-cor
222-224 I3 pc e_d-grid-cor [0/879]?=-99 Lower uncertainty in d-grid-cor
226-232 F7.3 mag av-grid-cor [-0.3/0.9]?=-99 extinction,
dnu corrected grid modeling
234-240 F7.3 mag E_av-grid-cor [0/0.4]?=-99 Upper uncertainty
in av-grid-cor
242-248 F7.3 mag e_av-grid-cor [0/0.4]?=-99 Lower uncertainty
in av-grid-cor
250-256 F7.3 Rsun r-gaia [0.5/120]?=-99 stellar radius,
Gaia parallax based
258-264 F7.3 Rsun E_r-gaia [0.02/114]?=-99 Upper uncertainty in r-gaia
266-272 F7.3 Rsun e_r-gaia [0.02/65]?=-99 Lower uncertainty in r-gaia
274-277 I4 pc d-gaia [21/9616]?=-99 distance,
Gaia parallax based
279-282 I4 pc E_d-gaia [0/5818]?=-99 Upper uncertainty in d-gaia
284-287 I4 pc e_d-gaia [0/5098]?=-99 Lower uncertainty in d-gaia
289-295 F7.3 mag av-gaia [-0.01/4.2]?=-99 extinction,
Gaia parallax based
297-298 I2 --- Ev [-1/1]? Evolutionary state (3)
300-302 A3 --- Src Source flag (4)
--------------------------------------------------------------------------------
Note (1): Teff and feh were taken from APOGEE DR13 (SDSS Collaboration
2016arXiv160802013S 2016arXiv160802013S) for giants (src flag = 'apo') and
from Buchave & Latham (2015, J/ApJ/808/187) for dwarfs and subgiants
(src flag = 'spc'). See section 2 for details.
Note (2): logg was calculated from teff and numax given in Table 1.
Note (3): Evolutionary state classifications taken from
Stello+ (2013, J/ApJ/765/L41) and Vrard+ (2016, J/A+A/588/A87)
as follows:
0 = non He-core burning stars;
1 = He-core burning stars;
-1 = stars with unknown evolutionary state..
Note (4): Source flag as follows:
apo = APOGEE DR13, (SDSS Collaboration et al. 2016arXiv160802013S 2016arXiv160802013S)
spc = Stellar Parameter Classification pipeline,
Buchave & Latham (2015, J/ApJ/808/187).
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 05-Mar-2018