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VLA and GBT Observations of Orion B (NGC 2024, W12) : Photo-dissociation Region Properties and Magnetic field
Astrophysics of Galaxies · Submitted 1 Aug 2014
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We estimate magnetic field strength in the foreground PDR to be 60 $\mu$G and that in the far side PDR to be 220 $\mu$G.
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The abstract, sentence by sentence
We present images of C110$\alpha$ and H110$\alpha$ radio recombination line (RRL) emission at 4.8 GHz and images of H166$\alpha$, C166$\alpha$ and X166$\alpha$ RRL emission at 1.4 GHz, observed toward the starforming region NGC 2024. The 1.4 GHz image with angular resolution $\sim$ 70\arcsec\ is obtained 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 LSR velocity (10.3 \kms\) of the C110$\alpha$ line to that of lines observed from molecular material located at the far side of the \HII\ region suggests that the photo dissociation region (PDR) responsible for C110$\alpha$ line emission is at the far side. The LSR velocity of C166$\alpha$ is 8.8 \kms. This velocity is comparable with the velocity of molecular absorption lines observed from the foreground gas, suggesting that the PDR is at the near side of the \HII\ region. Non-LTE models for carbon line forming regions are presented. Typical properties 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 and those 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 modeling indicates that the far side PDR is located within the \HII\ region. We estimate magnetic field strength in the foreground PDR to be 60 $\mu$G and that in the far side PDR to be 220 $\mu$G. Our field estimates compare well with the values obtained from OH Zeeman observations toward NGC 2024.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We present images of C110$\alpha$ and H110$\alpha$ radio recombination line (RRL) emission at 4.8 GHz and images of H166$\alpha$, C166$\alpha$ and X166$\alpha$ RRL emission at 1.4 GHz, observed toward the starforming region NGC 2024. | contribution 0.86 | 0.95 | 0.03 | asserted 0.99 |
| s1 | The 1.4 GHz image with angular resolution $\sim$ 70\arcsec\ is obtained using VLA data. | method 1.00 | 0.88 | 0.02 | asserted 1.00 |
| s2 | The 4.8 GHz image with angular resolution $\sim$ 17\arcsec\ is obtained by combining VLA and GBT data. | method 1.00 | 0.92 | 0.03 | asserted 1.00 |
| s3 | The similarity of the LSR velocity (10.3 \kms\) of the C110$\alpha$ line to that of lines observed from molecular material located at the far side of the \HII\ region suggests that the photo dissociation region (PDR) responsible for C110$\alpha$ line emission is at the far side. | interpretation 0.96 | 0.86 | 0.14 | hedged possibility 0.99 |
| s4 | The LSR velocity of C166$\alpha$ is 8.8 \kms. | result 1.00 | 0.91 | 0.03 | asserted 1.00 |
| s5 | This velocity is comparable with the velocity of molecular absorption lines observed from the foreground gas, suggesting that the PDR is at the near side of the \HII\ region. | interpretation 0.97 | 0.74 | 0.12 | hedged possibility 0.87 |
| s6 | Non-LTE models for carbon line forming regions are presented. | method 0.91 | 0.88 | 0.02 | asserted 0.97 |
| s7 | Typical properties 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 and those 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. | result 1.00 | 0.83 | 0.09 | asserted 0.97 |
| s8 | Our modeling indicates that the far side PDR is located within the \HII\ region. | result 0.51 | 0.94 | 0.18 | hedged possibility 0.70 |
| s9 | We estimate magnetic field strength in the foreground PDR to be 60 $\mu$G and that in the far side PDR to be 220 $\mu$G. | result 1.00 | 0.96 | 0.20 | asserted 1.00 |
| s10 | Our field estimates compare well with the values obtained from OH Zeeman observations toward NGC 2024. | interpretation 0.50 | 0.45 | 0.09 | asserted 0.82 |
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The paper
Original abstract
We present images of C110$\alpha$ and H110$\alpha$ radio recombination line (RRL) emission at 4.8 GHz and images of H166$\alpha$, C166$\alpha$ and X166$\alpha$ RRL emission at 1.4 GHz, observed toward the starforming region NGC 2024. The 1.4 GHz image with angular resolution $\sim$ 70\arcsec\ is obtained 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 LSR velocity (10.3 \kms\) of the C110$\alpha$ line to that of lines observed from molecular material located at the far side of the \HII\ region suggests that the photo dissociation region (PDR) responsible for C110$\alpha$ line emission is at the far side. The LSR velocity of C166$\alpha$ is 8.8 \kms. This velocity is comparable with the velocity of molecular absorption lines observed from the foreground gas, suggesting that the PDR is at the near side of the \HII\ region. Non-LTE models for carbon line forming regions are presented. Typical properties 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 and those 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 modeling indicates that the far side PDR is located within the \HII\ region. We estimate magnetic field strength in the foreground PDR to be 60 $\mu$G and that in the far side PDR to be 220 $\mu$G. Our field estimates compare well with the values obtained from OH Zeeman observations toward NGC 2024.
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