First dynamical pfactor determination
Physical parameters and the projection factor of the classical Cepheid in the binary system OGLELMCCEP0227
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
A novel method of analysis of doublelined eclipsing binaries containing a radially pulsating star is presented. The combined pulsatingeclipsing 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 outofeclipse 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.


Iband model of selected eclipses.

The method is applied to the eclipsing binary Cepheid OGLELMCCEP0227 (Ppuls=3.80 d, Porb=309 d). We analyze a set of new spectroscopic and photometric observations for this binary, simultaneously fitting OGLE Vband, Iband 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 M_{1}=4.165 ± 0.032 M☉ and R_{1}=34.92 ± 0.34 R☉, respectively.

Physical properties of CEP0227. 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 distanceindependent 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 mideclipse. The Cepheid is passing in front of the red giant companion. Star edge line width represents 1σ 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 pfactor error approximately equal the radius error. The distance between the stars at this phase is about 355 Rsun.
