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 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:
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FileName Lrecl Records Explanations
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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
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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
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Bytes Format Units Label Explanations
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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
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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.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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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
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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.
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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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
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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