Access to Astronomical Catalogues

← Click to display the menu
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
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). 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:
FileName Lrecl Records Explanations
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
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
Bytes Format Units Label Explanations
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
Byte-by-byte Description of file: table2.dat
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(V^2^) (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
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.
Byte-by-byte Description of file: table3.dat
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
Note (1): available in the literature used for the spectral template fitting described in Section 3.
Byte-by-byte Description of file: table6.dat
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
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)
History: From electronic version of the journal
(End) Emmanuelle Perret [CDS] 31-Mar-2011
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

catalogue service

© UDS/CNRS

Contact