the inner galactic region is well known [@Han:2006nx]. We choose $B_0=30\, \mu {\rm G}$ as our fiducial value although smaller and larger values also lead to consistent fits to the haze spectrum and its variation with latitude. Since there is no observational guidance on the specific structure of magnetic field within a couple of kpc from the galactic center, we adopt an exponential form, $f_C(R) = \exp(-R/R_C)$ and set $R_C=1$ kpc. We note that this form for $f_C(R)$ achieves the aim of smoothly transitioning from a spherical magnetic field profile in the inner galactic region to the cylindrical B field profile that are commonly used to fit Haslam data, cosmic ray data and diffuse galactic gamma-ray background [@Strong:1998fr]. Our adopted magnetic field towards the center of the galaxy is consistent with the average magnetic field deduced on scales of order a kpc about the galactic center from observations of non-thermal radio filaments [@LaRosa:2005ai].

We also note that the 408 MHz Haslam maps do not directly constrain the inner galactic magnetic field strengths or structure since the synchrotron signal depends on $n_e B_\perp^{1.8}$ [@Broadbent:1990], where $n_e$ is the number density of electrons contributing to the 408 MHz signal and $B_\perp$ is 