excess obtained with the natural neighbor method. To complement our research on reddening, we used also the Python package named “mwdust”[^4] that uses several existing extinction maps in the Milky Way [@2016ApJ...818..130B]. Using this package, we obtain extinction at a given direction and distance. For the distance 3.02 kpc we have obtained extinction in $V$- and $I$-band A$_V$ = 2.288 mag and A$_I$ = 1.256 mag, what gives E($V-I$) = 1.033 mag roughly confirming the earlier calculation.

The corrected color in primary eclipse obtained with the Recio-Blanco model , viz. $(V-I)_{0}$= 1.47 mag, corresponds to a K2-type star with $\rm T_{c}$ = 4400K [@Drilling2000] (Fig.12). In the following we will assume that this is the effective temperature of the donor star. The relative stability of the primary eclipse might support this conjecture.

  -------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------- --
  ![color-magnitude diagram for stars surrounding OGLE-BLG-ECL-157529. The reddening vector, extinction value and magnitudes of the red clump are from @2013ApJ...769...88N. More details can be found in Section 3.1.[]{data-label="D1"}](blg535_02_91705_cmd.pdf "fig:"){width="0.90\linewidth"}   
  -------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------- --

\[1\][![Temperature versus color for dwarfs (black dots) and giants (red dots) from @Drilling2000 and the best 3$^{th}$ order polynomial fit. 95% confidence and prediction bands are shown by dashed and dashed-light areas, respectively. The position 