J/ApJ/694/1085 Radii of exoplanet host stars (van Belle+, 2009)
Directly determined linear radii and effective temperatures of exoplanet
host stars.
van Belle G.T., von Braun K.
<Astrophys. J., 694, 1085-1098 (2009)>
=2009ApJ...694.1085V 2009ApJ...694.1085V
ADC_Keywords: Stars, double and multiple ; Stars, diameters ; Planets
Effective temperatures ; Extinction ; Interferometry
Keywords: infrared: stars - stars: fundamental parameters -
techniques: interferometric
Abstract:
We present interferometric angular sizes for 12 stars with known
planetary companions, for comparison with 28 additional main-sequence
stars not known to host planets. For all objects we estimate
bolometric fluxes and reddenings through spectral-energy distribution
(SED) fits, and in conjunction with the angular sizes, measurements of
effective temperature. The angular sizes of these stars are
sufficiently small that the fundamental resolution limits of our
primary instrument, the Palomar Testbed Interferometer, are
investigated at the sub-milliarcsecond level and empirically
established based upon known performance limits. We demonstrate that
the effective temperature scale as a function of dereddened (V-K)0
color is statistically identical for stars with and without planets.
Additionally, in an Appendix we provide SED fits for the 166 stars
with known planets which have sufficient photometry available in the
literature for such fits; this derived "XO-Rad" database includes
homogeneous estimates of bolometric flux, reddening, and angular size.
Description:
The Palomar Testbed Interferometer (PTI) is an 85-110m H- and K band
1.6um and 2.2um interferometer located at Palomar Observatory in San
Diego County, California, in nightly operation since 1997. The data
from PTI considered herein cover the range from the beginning of 1998
until the beginning of 2008. In addition to the target stars discussed
herein, appropriate calibration sources were observed as well and can
be found in van Belle et al. (2008, Cat. J/ApJS/176/276).
Additional angular diameters of extrasolar planet hosting stars (EHSs)
were obtained with the Georgia State University CHARA (Center for High
Angular Resolution Astronomy) Array with an intent of detecting
possible face-on binarity masquerading as planetary companionship
(Baines et al. 2008ApJ...682..577B 2008ApJ...682..577B). The CHARA Array is an
optical/near-infrared interferometer similar to PTI, but with longer
baselines (up to 330m), allowing for resolution of smaller objects.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 83 75 New calibration sources used in this
investigation, as discussed in Section 4.2
table2.dat 114 44 Observed and derived supporting parameters for
luminosity class V stars
table3.dat 80 165 The XO-Rad database: estimates from SED Fitting
table6.dat 63 44 Estimates for luminosity class V stars, as
discussed in section 5
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See also:
J/ApJ/680/728 : Diameters of exoplanet host stars (Baines+, 2008)
J/ApJS/176/276 : PTI calibrator catalog (van Belle+, 2008)
http://exoplanet.eu/ : The extrasolar planets encyclopaedia home page
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- --- [HD]
3- 8 I6 --- HD HD number
10- 11 I2 h RAh Hour of right ascension (J2000)
13- 14 I2 min RAm Minute of right ascension (J2000)
16- 21 F6.3 s RAs Second of right ascension (J2000)
23 A1 --- DE- Declination sign (J2000)
24- 25 I2 deg DEd Degree of declination (J2000)
27- 28 I2 arcmin DEm Arcminute of declination (J2000)
30- 33 F4.1 arcsec DEs Arcsecond of declination (J2000)
35- 37 I3 --- Np Number of photometric data points available
for the bolometric flux fitting
39- 48 A10 --- SpType Simbad MK spectral type
50- 54 A5 --- SpTM Spectral template chosen from Pickles (1998,
Cat. J/PASP/110/863) for the fitting
56- 60 F5.3 mag Av Extinction
62- 66 F5.3 mag e_Av Av uncertainty
68- 71 F4.2 --- chi2 χ2ν: the reduced chi-squared value
of the fit
73- 77 F5.3 mas theta Estimated angular size from the fit
79- 83 F5.3 mas e_theta theta uncertainty
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- Sample Sample origin (1)
7- 8 A2 --- --- [HD]
9- 14 I6 --- HD HD number
16- 18 I3 --- NV2 ? Number of visibility points N(V2) (2)
20- 24 F5.3 mas thetUD Uniform Disk (UD) angular size (2)
26- 30 F5.3 mas e_thetUD thetUD uncertainty
32- 35 F4.2 --- chi2 ? Reduced chi-squared value of the fit
37- 41 F5.3 --- V2 ? Calibration of the target star visibility
(V2) (2)
43- 47 F5.3 --- thetR Ratio thetLD/thetUD (2)
49- 53 F5.3 mas thetLD Limb Darkened (LD) angular size (2)
55- 59 F5.3 mas e_thetLD thetLD uncertainty
61- 65 F5.3 mag Av Extinction
67- 71 F5.3 mag e_Av Av uncertainty
73- 79 F7.2 10-11W/m2 Fbol Estimated planetary host star bolometric flux
81- 85 F5.2 10-11W/m2 e_Fbol Fbol uncertainty
87- 94 A8 --- SpType MK spectral type (3)
96- 99 F4.2 mag Vmag V-band magnitude from literature
101-104 F4.2 mag e_Vmag Vmag uncertainty
106-109 F4.2 mag Kmag PTI/CHARA K-band (2.2um) magnitude
111-114 F4.2 mag e_Kmag Kmag uncertainty
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Note (1): Sample as follows:
CS = Control sample: stars not known to host planets
PTI = EHSA sample: known planet hosting stars (observed with PTI, Palomar)
CHARA = EHSA sample: known planet hosting stars (obsreved with CHARA)
Note (2): See section 4.1 for further details.
Note (3): SED fits are accomplished using photometry available in the
literature as the input values, with template spectra from the Pickles
(1998, Cat. J/PASP/110/863) library appropriate for the spectral types
indicated for the stars. Spectral types used in the SED fitting for
all EHS stars are those values found in the Exoplanet Encyclopedia,
which is in turn based upon the respective source discovery papers
cataloged therein. The control sample stars had their spectral types
established from those values found in Hipparcos catalog (Perryman et
al. 1997, Cat. I/239). See section 3 for further details.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 I6 --- HD HD number
8- 12 A5 --- SpTM Spectral template chosen from Pickles (1998,
Cat. J/PASP/110/863) for the fitting
14- 18 I5 K Teff Template effective temperature
20- 23 I4 K e_Teff Teff uncertainty
25- 28 F4.2 --- chi2 Reduced chi-squared value of the fit
30- 32 I3 --- Np Number of photometric data points (1)
34- 40 F7.2 10-11W/m2 Fbol Estimated planetary host star bolometric flux
42- 46 F5.2 10-11W/m2 e_Fbol Fbol uncertainty (in 10-8erg/cm2/s)
48- 51 F4.2 mag Av Estimated reddening
53- 56 F4.2 mag e_Av Av uncertainty
58- 62 F5.3 mas theta Estimated angular diameter
64- 68 F5.3 mas e_theta theta uncertainty
70- 74 F5.2 Rsun Rad Estimated linear radius
76- 80 F5.2 Rsun e_Rad Rad uncertainty
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Note (1): available in the literature used for the spectral template
fitting described in Section 3.
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- Sample Sample origin (1)
7- 8 A2 --- --- [HD]
9- 14 I6 --- HD HD number
16- 21 F6.3 mag (V-K)0 Dereddened V-K color index
23- 27 F5.3 mag e_(V-K)0 (V-K)0 uncertainty
29- 33 I5 K Teff Effective temperature
35- 37 I3 K e_Teff Teff uncertainty
39- 44 F6.3 pc d Heliocentric distance
46- 50 F5.3 pc e_d d uncertainty
52- 57 F6.3 Rsun Rad Linear radius
59- 63 F5.3 Rsun e_Rad Rad uncertainty
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Note (1): Sample as follows:
CS = Control sample: stars not known to host planets
PTI = EHSA sample: known planet hosting stars (PTI)
CHARA = EHSA sample: known planet hosting stars (CHARA)
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 31-Mar-2011