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J/A+A/434/89    Parameters of LMC detached eclipsing binaries (Michalska+, 2005)

Detached binaries in the Large Magellanic Cloud. A selection of binaries suitable for distance determination. Michalska G., Pigulski A. <Astron. Astrophys. 434, 89 (2005)> =2005A&A...434...89M
ADC_Keywords: Magellanic Clouds ; Binaries, eclipsing ; Effective temperatures ; Stars, diameters Keywords: stars: binaries: eclipsing - Magellanic Clouds - stars: fundamental parameters Abstract: As a result of a careful selection of eclipsing binaries in the Large Magellanic Cloud using the OGLE-II photometric database, we present a list of 98 systems that are suitable targets for spectroscopic observations that would lead to the accurate determination of the distance to the LMC. For these systems we derive preliminary parameters combining the OGLE-II data with the photometry of MACHO and EROS surveys. In the selected sample, 58 stars have eccentric orbits. Among these stars we found fourteen systems showing apsidal motion. The data do not cover the whole apsidal motion cycle, but follow-up observations will allow detailed studies of these interesting objects. Description: Parameters of 98 detached eclipsing binaries in the Large Magellanic Cloud selected as the best for the purpose of distance determination. The first 17 columns refer to the results of the fitting by means of the Wilson-Devinney program, the remaining 16, to the Monte Carlo (M-C) simulations. The errors given for the M-C simulations correspond to the 10% increase of the weighted sum of the squares of residuals (SSR) with respect to the minimum value. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 95 98 List of 98 selected DEBs in the Large Magellanic Cloud table3.dat 181 98 Parameters of the selected systems from Wilson-Devinney fit and Monte Carlo simulations
See also: J/AJ/114/326 : MACHO Variables V. (Alcock+ 1997) J/AcA/53/1 : OGLE eclipsing binaries in LMC (Wyrzykowski+, 2003) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 2 I2 --- Seq Sequential number 3 A1 --- n_Seq [*] Note for good target (1) 5- 14 A10 --- LMCSC OGLE LMC SC field 16- 17 I2 h RAh Right ascension (J2000) (2) 18- 19 I2 min RAm Right ascension (J2000) (2) 20- 24 F5.2 s RAs Right ascension (J2000) (2) 25 A1 --- DE- Declination sign (J2000) (2) 26- 27 I2 deg DEd Declination (J2000) (2) 28- 29 I2 arcmin DEm Declination (J2000) (2) 30- 33 F4.1 arcsec DEs Declination (J2000) (2) 35- 46 A12 --- MACHO MACHO designation 48- 51 I4 --- EROS ? EROS number 52- 60 F9.6 d Porb ? Orbital period 62- 67 F6.3 mag Vmag Johnson V magnitude from OGLE-II (3) 69- 74 F6.3 mag V-I Johnson V-I colour index from OGLE-II (3) 76- 95 A20 --- Rem Remarks (4)
Note (1): * for system that is indicated as good target for distance determination by Wyrzykowski, 2003, Cat. J/AcA/53/1 Note (2): OGLE name, HHMMSSss+DDMMSSs Note (3): The photometry is given for the out-of-eclipse phase at maximum light Note (4): Remarks are: E = system with non-zero eccentricity AM = system with detectable apsidal motion
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 2 I2 --- Seq Sequential number 4- 8 I5 K T1 Effective temperature of star 1 (1) 10- 14 I5 K T2 Effective temperature of star 2 (2) 16- 18 I3 K e_T2 rms error of T2 20- 23 F4.1 deg incl Inclination (2) 25- 27 F3.1 deg e_incl rms error of incl 29- 33 F5.3 --- Sumr Sum of relative radii of star 1 and 2 (2) 35- 39 F5.3 --- e_Sumr rms error of Sumr 41- 44 F4.2 --- Fe1 The parameter Fe for primary eclipse (2)(3) 46- 49 F4.2 --- e_Fe1 rms error of Fe1 51- 54 F4.2 --- Fe2 ? The parameter Fe for secondary eclipse (2)(3) 56- 59 F4.2 --- e_Fe2 ? rms error of Fe2 61- 65 F5.3 --- ecc Eccentricity (2)(4) 67- 71 F5.3 --- e_ecc ? rms error of ecc (5) 73- 77 F5.1 deg omega ? Longitude of periastron (2)(5) 79- 82 F4.1 deg e_omega ? rms error of omega (5) 84- 86 I3 km/s K12 Calculated half-range of radial velocity changes 89- 93 I5 K MC-T2 ? Effective temperature of star 2, from the M-C simulations (6)(8) 96- 99 I4 K E_MC-T2 ? Positive error of MC-T2 (7)(8) 102-105 I4 K e_MC-T2 ? Negative error of MC-T2 (8)(7) 107-110 F4.1 deg MCincl ? Inclination, from the M-C simulations (8)(6) 112-116 F5.1 deg E_MCincl ? Positive error of MC_i (7)(8) 119-122 F4.1 deg e_MCincl ? Negative error of MC_i (7)(8) 124-128 F5.3 --- MCSumr ? Sum of relative radii of star 1 and 2, from the M-C simulations (6)(8) 131-135 F5.3 --- E_MCSumr ? Positive error of MC_Sumr (7)(8) 138-142 F5.3 --- e_MCSumr ? Negative error of MC_Sumr (7)(8) 144-147 F4.2 --- MCFe1 ? The parameter Fe for primary eclipse, from the M-C simulations (3)(6)(8) 150-153 F4.2 --- E_MCFe1 ? Positive error of MC_Fe1 (7)(8) 156-159 F4.2 --- e_MCFe1 ? Negative error of MC_Fe1 (7)(8) 161-164 F4.2 --- MCFe2 ? The parameter Fe for secondary eclipse, from the M-C simulations (3)(6)(8) 167-170 F4.2 --- E_MCFe2 ? Positive error of MC_Fe2 (7)(8) 173-176 F4.2 --- e_MCFe2 ? Negative error of MC_Fe2 (7)(8) 178-179 A2 --- Obs Code for observations used in the M-C simulations (8)(9)
Note (1): Assumed. Sect. 5.1 and Fig. 3 of the paper explains how T1 was derived. Note (2): From the fit by means of Wilson-Devinney program. Note (3): The parameter Fe was defined by Wyithe & Wilson (2001ApJ...559..260W) and equals to Fe=(r1+r2-cos(incl))/(2*r2), where r1 and r2 are relative radii of star 1 and 2, respectively. The radii are measured with respect to the distance between components at the epoch of mid-time of the eclipse. This means that for a circular orbit, Fe is the same for both eclipses, while for an eccentric one, two different values have to be given, for primary and secondary eclipse. In case of a circular orbit the entries in table for secondary eclipse remain empty. Note (4): Assumed to be 0 for circular orbits. Note (5): Field left empty for circular orbits. Note (6): This is the value of the parameter in the parameter space explored by means of the Monte-Carlo simulations for which the smallest sum of squares of the residuals is yielded. Note (7): Errors in M-C simulations are not symmetric, so that both positive and negative deviations are provided. They correspond to such a change of the parameter that yields a 10% increase of the sum of squares of residuals with respect to the minimum value. Note (8): Field left empty for a star with apsidal motion detected. Note (9): The following bands were used for the M-C simulations: O = OGLE-II I band MB = MACHO blue band MR = MACHO red band
Acknowledgements: Gabriela Michalska, michalska(at)astro.uni.wroc.pl
(End) Patricia Vannier [CDS] 25-Jan-2005
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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