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We present images of C110$\alpha$ and H110$\alpha$ radio recombination line(RRL) emission at 4.8 GHz and images of H166$\alpha$, C166$\alpha$ andX166$\alpha$ RRL emission at 1.4 GHz, observed toward the starforming regionNGC 2024. The 1.4 GHz image with angular resolution $\sim$ 70\arcsec\ isobtained using VLA data. The 4.8 GHz image with angular resolution $\sim$17\arcsec\ is obtained by combining VLA and GBT data. The similarity of the LSRvelocity (10.3 \kms\) of the C110$\alpha$ line to that of lines observed frommolecular material located at the far side of the \HII\ region suggests thatthe photo dissociation region (PDR) responsible for C110$\alpha$ line emissionis at the far side. The LSR velocity of C166$\alpha$ is 8.8 \kms. This velocityis comparable with the velocity of molecular absorption lines observed from theforeground gas, suggesting that the PDR is at the near side of the \HII\region. Non-LTE models for carbon line forming regions are presented. Typicalproperties of the foreground PDR are $T_{PDR} \sim 100$ K, $n_e^{PDR} \sim 5$\cmthree, $n_H \sim 1.7 \times 10^4$ \cmthree, path length $l \sim 0.06$ pc andthose of the far side PDR are $T_{PDR} \sim$ 200 K, $n_e^{PDR} \sim$ 50\cmthree, $n_H \sim 1.7 \times 10^5$ \cmthree, $l \sim$ 0.03 pc. Our modelingindicates that the far side PDR is located within the \HII\ region. We estimatemagnetic field strength in the foreground PDR to be 60 $\mu$G and that in thefar side PDR to be 220 $\mu$G. Our field estimates compare well with the valuesobtained from OH Zeeman observations toward NGC 2024.

VLA and GBT Observations of Orion B (NGC 2024, W12) : Photo-dissociation Region Properties and Magnetic field