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High resolution studies of the C-BAND and L-BAND radio continuum of the periodic methanol maser source G 9.62 + 0.20E and surrounding sources

High resolution observations of the C-band and L-band radio continuum of the hyper-compact H ii region $\rm G 9.62$ + $\rm 0.20 E$ conducted with the e-MERLIN interferometric array are presented. A flux density of $\rm 2.25 \pm 0.20$  $\rm mJy$ and an angular size of $\rm 127 \pm 22$  $\rm mas$ were...

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Bibliographic Details
Published in:Monthly notices of the Royal Astronomical Society 2024-12
Main Authors: Woode, B, Hoare, M G, Kuditcher, A, Goedhart, S
Format: Article
Language:English
Online Access:Get full text
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Summary:High resolution observations of the C-band and L-band radio continuum of the hyper-compact H ii region $\rm G 9.62$ + $\rm 0.20 E$ conducted with the e-MERLIN interferometric array are presented. A flux density of $\rm 2.25 \pm 0.20$  $\rm mJy$ and an angular size of $\rm 127 \pm 22$  $\rm mas$ were measured for the C-band continuum. At L-band, an upper limit of $\rm 162$  $\rm \mu Jy$ on the integrated flux density was calculated at the continuum’s position. The surrounding sources C and D were detected at levels consistent with previous detections. The results for source E requires a steeper spectrum at L-band than previous observations extrapolated from higher frequencies. This can be explained with a truncated inverse square law density distribution model. We obtain a C-band peak brightness temperature of about $\rm {4000\, \rm {K}}$, which assuming an electron temperature of $\rm {10^{4}}$  $\rm {K}$ translates to an optical depth of $\rm {0.5}$, indicating the continuum is optically thin at C-band going thick at L-band. These results therefore place firm constraints on H ii region models in source E. The periodic variability of methanol masers, as seen in $\rm G 9.62$ + $\rm 0.20 E$, has been explained with the pulsating star, accretion disk, and colliding wind binary models. Some models predict a hypercompact H ii region can provide pumping for methanol masers. In the colliding wind binary model context maser variability is attributed to seed photon modulation. Hence, future H ii models matching our observations could test predictions of these models in terms of the variability profiles of the $\rm {1.6 \, \rm {GHz}}$  $\rm {OH}$ and $\rm {6.7 \, \rm {GHz} }$ methanol masers.
ISSN:0035-8711
1365-2966
DOI:10.1093/mnras/stae2814