Please use this identifier to cite or link to this item: http://hdl.handle.net/10995/103266
Title: The PDR structure and kinematics around the compact H ii regions S235 A and S235 C with [C ii], [13C ii], [O i], and HCO+line profiles
Authors: Kirsanova, M. S.
Ossenkopf-Okada, V.
Anderson, L. D.
Boley, P. A.
Bieging, J. H.
Pavlyuchenkov, Y. N.
Luisi, M.
Schneider, N.
Andersen, M.
Samal, M. R.
Sobolev, A. M.
Buchbender, C.
Aladro, R.
Okada, Y.
Issue Date: 2020
Publisher: Oxford University Press
Citation: The PDR structure and kinematics around the compact H ii regions S235 A and S235 C with [C ii], [13C ii], [O i], and HCO+line profiles / M. S. Kirsanova, V. Ossenkopf-Okada, L. D. Anderson, et al. — DOI 10.1093/mnras/staa2142 // Monthly Notices of the Royal Astronomical Society. — 2020. — Vol. 497. — Iss. 3. — P. 2651-2669.
Abstract: The aim of this work is to study structure and gas kinematics in the photodissociation regions (PDRs) around the compact H ii regions S235 A and S235 C. We observe the [C ii], [13C ii], and [O i] line emission, using SOFIA/upGREAT, and complement them by data of HCO+ and CO. We use the [13C ii] line to measure the optical depth of the [C ii] emission, and find that the [C ii] line profiles are influenced by self-absorption, while the [13C ii] line remains unaffected by these effects. Hence, for dense PDRs, [13C ii] emission is a better tracer of gas kinematics. The optical depth of the [C ii] line is up to 10 in S235 A. We find an expanding motion of the [C ii]-emitting layer of the PDRs into the front molecular layer in both regions. Comparison of the gas and dust columns shows that gas components visible neither in the [C ii] nor in low-J CO lines may contribute to the total column across S235 A. We test whether the observed properties of the PDRs match the predictions of spherical models of expanding H ii region + PDR + molecular cloud. Integrated intensities of the [13C ii], [C ii], and [O i] lines are well represented by the model, but the models do not reproduce the double-peaked [C ii] line profiles due to an insufficient column density of C+. The model predicts that the [O i] line could be a more reliable tracer of gas kinematics, but the foreground self-absorbing material does not allow using it in the considered regions. © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.
Keywords: H II REGIONS
INFRARED: ISM
ISM: KINEMATICS AND DYNAMICS
LINE: PROFILES
PHOTODISSOCIATION REGION (PDR)
RADIATIVE TRANSFER
URI: http://hdl.handle.net/10995/103266
Access: info:eu-repo/semantics/openAccess
SCOPUS ID: 85097001494
PURE ID: 14173786
ISSN: 358711
DOI: 10.1093/mnras/staa2142
Appears in Collections:Научные публикации, проиндексированные в SCOPUS и WoS CC

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