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J/AJ/152/180 Bolometric fluxes of eclipsing binaries in Tycho-2 (Stassun+, 2016)

Eclipsing binaries as benchmarks for trigonometric parallaxes in the Gaia era. Stassun K.G., Torres G. <Astron. J., 152, 180-180 (2016)> =2016AJ....152..180S (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, eclipsing ; Effective temperatures ; Reddening ; Abundances, [Fe/H] ; Extinction ; Parallaxes, trigonometric ; Energy distributions ; Stars, distances Keywords: binaries: eclipsing - catalogs - methods: observational - parallaxes - stars: distances Abstract: We present fits to the broadband photometric spectral energy distributions (SEDs) of 158 eclipsing binaries (EBs) in the Tycho-2 catalog. These EBs were selected because they have highly precise stellar radii, effective temperatures, and in many cases metallicities previously determined in the literature, and thus have bolometric luminosities that are typically good to ≲10%. In most cases the available broadband photometry spans a wavelength range 0.4-10µm, and in many cases spans 0.15-22µm. The resulting SED fits, which have only extinction as a free parameter, provide a virtually model-independent measure of the bolometric flux at Earth. The SED fits are satisfactory for 156 of the EBs, for which we achieve typical precisions in the bolometric flux of ≃3%. Combined with the accurately known bolometric luminosity, the result for each EB is a predicted parallax that is typically precise to ≲5%. These predicted parallaxes-with typical uncertainties of 200µas-are 4-5 times more precise than those determined by Hipparcos for 99 of the EBs in our sample, with which we find excellent agreement. There is no evidence among this sample for significant systematics in the Hipparcos parallaxes of the sort that notoriously afflicted the Pleiades measurement. The EBs are distributed over the entire sky, span more than 10mag in brightness, reach distances of more than 5kpc, and in many cases our predicted parallaxes should also be more precise than those expected from the Gaia first data release. The EBs studied here can thus serve as empirical, independent benchmarks for these upcoming fundamental parallax measurements. Description: We present fits to the broadband photometric Spectral Energy Distributions (SEDs) of 158 eclipsing binaries in the Tycho-2 catalog. The complete list of 158 eclipsing binaries is given in Table1, sorted by Tycho number. The results of the SED fitting procedure are summarized in Table2. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 134 158 Stellar properties of our sample of eclipsing binaries table2.dat 128 158 Results refs.dat 69 73 References
See also: I/337 : Gaia DR1 (Gaia Collaboration, 2016) II/336 : AAVSO Photometric All Sky Survey (APASS) DR9 (Henden+, 2016) II/328 : AllWISE Data Release (Cutri+ 2013) II/312 : GALEX-DR5 (GR5) sources from AIS and MIS (Bianchi+ 2011) I/311 : Hipparcos, the New Reduction (van Leeuwen, 2007) II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003) I/259 : The Tycho-2 Catalogue (Hog+ 2000) I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) J/A+A/580/A23 : Stroemgren-Crawford uvbyβ photometry (Paunzen, 2015) J/AJ/150/154 : Photometry and spectroscopy of V501 Mon (Torres+, 2015) J/AJ/147/36 : Photometry and spectroscopy of AQ Ser (Torres+, 2014) J/ApJ/780/59 : Araucaria project: eclipsing binaries in SMC (Graczyk+, 2014) J/A+A/526/A29 : ASAS low-mass EBs light curves (Helminiak+, 2011) J/AJ/138/1622 : Absolute properties of LV Her (Torres+, 2009) J/AJ/137/507 : Light and velocity curves of VZ Cep (Torres+, 2009) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 26 A26 --- Name System name (G1) 28- 31 I4 --- TYC1 TYC1 of Tycho name 32 A1 --- --- [-] 33- 36 I4 --- TYC2 TYC2 of Tycho name 37 A1 --- --- [-] 38 I1 --- TYC3 TYC3 of Tycho name 40- 45 I6 --- HIP [817/114484]? Hipparcos identifier 47- 53 F7.4 Rsun Rad1 [0.4323/52.12] Radius of primary 55- 60 F6.4 Rsun e_Rad1 [0.002/1.38] Uncertainty in Rad1 62- 68 F7.4 Rsun Rad2 [0.3916/67.63] Radius of secondary 70- 75 F6.4 Rsun e_Rad2 [0.001/1.4] Uncertainty in Rad2 77- 81 I5 K Teff1 [3160/38000] Effective temperature of primary 83- 86 I4 K e_Teff1 [45/2500] Uncertainty in Teff1 88- 92 I5 K Teff2 [3125/34100] Effective temperature of secondary 94- 97 I4 K e_Teff2 [50/2500] Uncertainty in Teff2 99-103 F5.3 mag E(B-V) [0/0.85]? Reddening 105-109 F5.3 mag e_E(B-V) [0.001/0.08]? Uncertainty in E(B-V) 111-117 A7 [Sun] [Fe/H] ? Metallicity of the binary (1) 119-122 F4.2 [Sun] e_[Fe/H] [0.01/0.21]? Uncertainty in [Fe/H] 124-128 A5 --- f_[Fe/H] Metallic-line star flag (Am/Am, Am/-, -/Am) (2) 130-134 A5 --- Ref Literature reference; in refs.dat file
Note (1): Am systems having components with individually measured [Fe/H]: YZ Cas (+0.54±0.11, Am)+(+0.01±0.11, normal); V501 Mon (+0.33±0.08, Am)+(+0.01±0.06, normal); SW CMa (+0.49±0.15, Am)+(+0.61±0.15, Am); HW CMa (+0.28±0.10, Am)+(+0.33±0.10, Am). All uncertainties correspond to 1σ errors. Note (2): Metallicity flags are defined as follows: Am/Am = Both components are metallic-line stars; Am/- = Only the primary is known to have that anomaly.
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 26 A26 --- Name System name (G1) 28- 31 I4 --- TYC1 TYC1 of Tycho name 32 A1 --- --- [-] 33- 36 I4 --- TYC2 TYC2 of Tycho name 37 A1 --- --- [-] 38 I1 --- TYC3 TYC3 of Tycho name 40- 44 F5.2 mag Vmag [1.9/12.43] V band magnitude 46- 50 F5.2 --- chi2 [0.25/85.13] SED fit reduced χν2 value 52 A1 --- fit [*X] Fit flag(s) (* or X) (3) 54- 62 E9.3 mW/m2 Fbol Integrated bolometric flux Fbol (in erg/s/cm2) 64- 70 E7.1 mW/m2 E_Fbol Upper uncertainty on Fbol 72- 78 E7.1 mW/m2 e_Fbol Lower uncertainty on Fbol 80- 83 F4.2 mag AV [0/2.29] Extinction AV 85- 88 F4.2 mag E_AV [0/0.19] Upper uncertainty on AV 90- 93 F4.2 mag e_AV [0/0.31] Lower uncertainty on AV 95-100 F6.1 pc Dist [14.2/5231.2] Predicted distance (4) 102-106 F5.1 pc E_Dist [0.9/769.2] Upper uncertainty on Dist 108-112 F5.1 pc e_Dist [0.9/712.1] Lower uncertainty on Dist 114-118 F5.2 mas plx [0.19/70.58] Predicted parallax 120-123 F4.2 mas E_plx [0.02/8.49] Upper uncertainty on plx 125-128 F4.2 mas e_plx [0.02/7.38] Lower uncertainty on plx
Note (3): SED Fit flags are defined as follows: * = Systems with Teff>15000∼K and a large fraction of their flux extrapolated from a blackbody distribution on the blue side; X = Considered to have poor SED fits. Note (4): With Fbol and Lbol in hand for each eclipsing binary, we can calculate the predicted distance to each eclipsing binary according to Equation (1): Dist=(Lbol/4πFbol)1/2.
Byte-by-byte Description of file: refs.dat
Bytes Format Units Label Explanations
1- 2 I2 --- Ref Reference identifier 4- 22 A19 --- BibCode Bibliographic Code 24- 44 A21 --- Aut Author's name 46- 69 A24 --- Cat VizieR catalog
Global Notes: Note (G1): TX Cnc is an over-contact system (W UMa).
History: From electronic version of the journal
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 06-Mar-2017
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

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