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J/ApJ/628/411  Identification and analysis of eclipsing binaries  (Devor+, 2005)

Solutions for 10,000 eclipsing binaries in the bulge fields of OGLE II using DEBiL. Devor J. <Astrophys. J., 628, 411-425 (2005)> =2005ApJ...628..411D
ADC_Keywords: Binaries, eclipsing ; Surveys Keywords: binaries: eclipsing - Galaxy: bulge - stars: statistics - surveys Abstract: We have developed a fully automated pipeline for systematically identifying and analyzing eclipsing binaries within large data sets of light curves. The pipeline is made up of multiple tiers that subject the light curves to increasing levels of scrutiny. After each tier, light curves that did not conform to a given criteria were filtered out of the pipeline, reducing the load on the following, more computationally intensive tiers. As a central component of the pipeline, we created the fully automated Detached Eclipsing Binary Light curve fitter (DEBiL), which rapidly fits large numbers of light curves to a simple model. Using the results of DEBiL, light curves of interest can be flagged for follow-up analysis. As a test case, we analyzed the 218,699 light curves within the bulge fields of the OGLE II survey and produced 10,862 model fits. We point out a small number of extreme examples, as well as unexpected structure found in several of the population distributions. We expect this approach to become increasingly important as light-curve data sets continue growing in both size and number. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table4.dat 450 10862 Parameters from the DEBiL dataset of eclipsing binary systems in the galactic bulge
See also: ftp://sirius.astrouw.edu.pl/ogle/ogle2/ : OGLE II Home Page http://ogledb.astrouw.edu.pl/~ogle/photdb/index.html : OGLE Photometric database. Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 2 I2 --- Field OGLE II bulge field number (BUL_SC number) 4- 7 I4 --- LCNum Light curve number (unique to field; it is not the OGLE star ID) 9- 18 F10.6 d Per Period 20- 27 F8.6 --- Ecc Orbital eccentricity 29- 37 F9.6 --- e_Ecc Absolute uncertainty in Ecc 39- 46 F8.6 --- Rad1 Radius of large star in units of semimajor axis 48- 55 F8.6 --- e_Rad1 Absolute uncertainty in LRad 57- 64 F8.6 --- Rad2 Radius of small star in units of semimajor axis 66- 73 F8.6 --- e_Rad2 Absolute uncertainty in SRad 75- 83 F9.6 mag Imag1 I-band magnitude of large star 85- 93 F9.6 mag e_Imag1 Absolute uncertainty in ImagL 95-106 F12.6 mag Imag2 ?=-1000.000000 I-band magnitude of small star (1) 108-119 F12.6 mag e_Imag2 ?=-1000.000000 Absolute uncertainty in ImagS (1) 121-128 F8.6 --- sini Sine of inclination 130-137 F8.6 --- e_sini Absolute uncertainty in sini 139-146 F8.6 --- T0 ?=-1000.000000 Phased epoch of periastron (2) 148-159 F12.6 d e_T0 ?=-1000.000000 Absolute uncertainty in EpPeri (1) 161-170 F10.6 deg omega ?=-1000.000000 Argument of periastron 172-184 F13.6 deg e_omega ?=-1000.000000 Absolute uncertainty in Arg (1) 186-188 I3 --- Np Number of used data points (not including outliers) 190 I1 --- Nout Number of outliers 192-199 F8.6 --- chi2 Reduced chi squared of the best-fit model 201-210 F10.6 --- chi2avr Reduced chi squared of the average value 212-220 F9.6 --- chi22nd Chi2 of a second order spline (3) 222-231 F10.6 --- chi2sin Reduced chi squared of the sinusoidal best-fit 233-240 F8.6 --- FitSco Fitness score (4) 242-250 F9.6 --- Sig2nd Significance of the secondary dip depth (5) 252-260 F9.6 --- SigHei Significance of the hump height at midpoint between dips (5) 262-270 F9.6 --- SigDif Significance of the hump difference between the two humps (5) 272-280 F9.6 --- Wave Waviness (6) 282-290 F9.6 --- SctSco Scatter score (7) 292-302 F11.6 g/cm3 MeanDen Mean density (8) 304-317 F14.6 g/cm3 MaxDen Maximum density (9) 319-330 F12.6 mag Imag1c ?=-1000.000000 Extinction corrected I-band magnitude of large star magnitude (10) 332-343 F12.6 mag Imag2c ?=-1000.000000 Extinction corrected I-band magnitude of small star magnitude (10) 345-356 F12.6 mag ImagTc ?=-1000.000000 Extinction corrected total binary I-band magnitude (10) 358-366 F9.3 mag ImagUc ?=-1000.000 Udalski's catalog extinction corrected I-band magnitude (10) 368-376 F9.3 mag (V-I)Uc ?=-1000.000 Udalski's catalog extinction corrected (V-I) color (10) 378-386 F9.3 mag Imag ?=-1000.000 Uncorrected I-band magnitude (10) 388-396 F9.3 mag V-I ?=-1000.000 Uncorrected (V-I) color (10) 398-406 F9.3 mag e_Vmag ?=-1000.000 Absolute uncertainty in V-band magnitude (10) 408-416 F9.3 mag e_Imag ?=-1000.000 Absolute uncertainty in I-band magnitude (10) 418-419 I2 h RAh ? Hour of Right Ascension (J2000) 421-422 I2 min RAm ? Minute of Right Ascension (J2000) 424-428 F5.2 s RAs ? Second of Right Ascension (J2000) 430 A1 --- DE- Sign of the Declination (J2000) 431-432 I2 deg DEd ? Degree of Declination (J2000) 434-435 I2 arcmin DEm ? Arcminute of Declination (J2000) 437-440 F4.1 arcsec DEs ? Arcsecond of Declination (J2000) 442-450 F9.6 --- InvProb Inverse of the probability of observing the eclipsing light curve (11)
Note (1): -1000 indicates non-converged parameter. Note (2): Heliocentric Julian date, minus 2450000.0, phased by the period. Note (3): Parabolic fit within a sliding window. Note (4): Position of chi2 between chi2avr and chi22nd; see paper appendix Note (5): In sigma. Note (6): Waviness - special case of the scatter score. Here, we consider only data points in the light curve's plateau (i.e., the region in the phased curve between the eclipsing dips, where both stars are fully exposed). The waviness score is the scatter score of these data points around their median. Note (7): Scatter score is defined as <ΔXi-1ΔXi>/<ΔXi2> Note (8): Mean density: (M1+M2)/((4π/3)(R13+R23) Note (9): Maximum density: (M1+M2)/(4π/3)R23 Note (10): -1000 indicates missing data. Note (11): We unraveled the geometric selection effects by weighting each eclipsing light curve by the inverse of the probability of observing it as eclipsing. For example, if with a random orientation there is a 1% chance of a given binary system's being seen as eclipsing, we will give it a weight of 100 (see Section 5.1 of paper).
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Marianne Brouty [CDS] 06-Dec-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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