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• W3100849372 abstract "Previous radio recombination line (RRL) observations of dust clumps identified in the APEX Telescope Large Area Survey of the Galaxy (ATLASGAL) have led to the detection of a large number of RRLs in the 3mm range. Here, we aim to study their excitation with shorter wavelength (sub)millimeter radio recombination line (submm-RRL) observations. We made observations of submm-RRLs with low principal quantum numbers ($n$ $leq$ 30) using the APEX 12 m telescope, toward 104 HII regions associated with massive dust clumps from ATLASGAL. The observations covered the H25$alpha$, H28$alpha$, and H35$beta$ transitions. Toward a small subsample the H26$alpha$, H27$alpha$, H29$alpha$, and H30$alpha$ lines were observed to avoid contamination by molecular lines at adjacent frequencies. We have detected submm-RRLs (signal-to-noise $geq$ 3 $sigma$) from compact HII regions embedded within 93 clumps. The submm-RRLs are approximately a factor of two brighter than the mm-RRLs and consistent with optically thin emission in local thermodynamic equilibrium (LTE). The average ratio (0.31) of the measured H35$beta$/H28$alpha$ fluxes is close to the LTE value of 0.28. No indication of RRL maser emission has been found. The Lyman photon flux, bolometric, and submm-RRL luminosities toward the submm-RRL detected sources present significant correlations. The trends of dust temperature and the ratio of bolometric luminosity to clump mass, $L_{rm bol}/M_{rm clump}$, indicate that the HII regions are related to the most massive and luminous clumps. By estimating the production rate of ionizing photons, $Q$, from the submm-RRL flux, we find that the $Q$(H28$alpha$) measurements provide estimates of the Lyman continuum photon flux consistent with those determined from 5 GHz radio continuum emission." @default.
• W3100849372 created "2020-11-23" @default.
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• W3100849372 date "2018-08-01" @default.
• W3100849372 modified "2023-10-17" @default.
• W3100849372 title "New detections of (sub)millimeter hydrogen radio recombination lines towards high-mass star-forming clumps" @default.
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• W3100849372 doi "https://doi.org/10.1051/0004-6361/201732330" @default.
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