First dynamical p-factor determination

Relevant publication:

Physical parameters and the projection factor of the classical Cepheid in the binary system OGLE-LMC-CEP-0227

B. Pilecki, D. Graczyk, G. Pietrzyński, W. Gieren, I. Thompson, W. Freedman, V. Scowcroft, B. Madore, A. Udalski, I. Soszyński, P. Konorski, R. Smolec, N. Nardetto, G. Bono, P. Prada Moroni, J. Storm, A. Gallenne

2013, MNRAS, 436, 953 (← click to see the publication at ADS/arXiv)

A novel method of analysis of double-lined eclipsing binaries containing a radially pulsating star is presented. The combined pulsating-eclipsing light curve is built up from a purely eclipsing light curve grid created using an existing modeling tool. For every pulsation phase the instantaneous radius and surface brightness are taken into account, being calculated from the disentangled radial velocity curve of the pulsating star and from its out-of-eclipse pulsational light curve and the light ratio of the components, respectively. The best model is found using the Markov Chain Monte Carlo method.


Spitzer 3.6 μm model shown for one of primary eclipses.


I-band model of selected eclipses.

The method is applied to the eclipsing binary Cepheid OGLE-LMC-CEP-0227 (Ppuls=3.80 d, Porb=309 d). We analyze a set of new spectroscopic and photometric observations for this binary, simultaneously fitting OGLE V-band, I-band and Spitzer 3.6 μm photometry. We derive a set of fundamental parameters of the system significantly improving the precision comparing to the previous results obtained by our group. The Cepheid mass and radius are M₁=4.165 ± 0.032 M☉ and R₁=34.92 ± 0.34 R☉, respectively.


Physical properties of CEP-0227. The spectral type, radius, gravity (log g), temperature, luminosity (log L) and the observed magnitudes are mean values over the pulsation period. The orbital period is a rest frame value.

For the first time a direct, geometrical and distance-independent determination of the Cepheid projection factor is presented. The value p=1.21 ± 0.03_(stat) ± 0.04_(sys) is consistent with theoretical expectations for a short period Cepheid and interferometric measurements for δ Cep. We also find a very high value of the optical limb darkening coefficients for the Cepheid component, in strong disagreement with theoretical predictions for static atmospheres at a given surface temperature and gravity.


System configuration close to the secondary mid-eclipse. The Cepheid is passing in front of the red giant companion. Star edge line width represents 1-σ formal error in the determination of the radii. The Cepheid radius is a mean value over time and dotted lines represent its minimum and maximum radii. Changes in the radial amplitude of the star that correspond to the p-factor error approximately equal the radius error. The distance between the stars at this phase is about 355 Rsun.

System configuration close to the secondary mid-eclipse. The Cepheid is passing in front of the red giant companion. Star edge line width represents 1-σ formal error in the determination of the radii. The Cepheid radius is a mean value over time and dotted lines represent its minimum and maximum radii. Changes in the radial amplitude of the star that correspond to the p-factor error approximately equal the radius error. The distance between the stars at this phase is about 355 Rsun.