Volume 561, January 2014
|Number of page(s)||6|
|Section||Interstellar and circumstellar matter|
|Published online||03 January 2014|
Kinematics of the ionized-to-neutral interfaces in Monoceros R2⋆
1 Los Alamos National Laboratory, PO Box 1663, Los Alamos ( NM ) 87545, USA
2 Observatorio Astronómico Nacional, Apdo. 112, 28803 Alcalá de Henares ( Madrid), Spain
3 Centro de Astrobiología, (INTA-CSIC), Ctra. M-108, km. 4, 28850 Torrejón de Ardoz, Spain
4 LERMA, Observatoire de Paris, 61 Av. de l’Observatoire, 75014 Paris, France
5 I. Physikalisches Institut der Universität zu Köln, Zülpicher Straße 77, 50937 Köln, Germany
6 Université de Toulouse, UPS, IRAP, 9 Avenue du colonel Roche, 31062 Toulouse Cedex 4, France
7 CNRS, UMR 5187, 31028 Toulouse, France
8 Instituto de Radio Astronomía Milimétrica (IRAM), Avenida Divina Pastora 7, Local 20, 18012 Granada, Spain
9 Osservatorio Astrofisico di Arcetri, INAF, Largo E. Fermi 5, 50125 Firenze, Italy
10 Institut de Radioastronomie Millimétrique, 300 Rue de la Piscine, 38406 Saint Martin d’Héres, France
Received: 9 September 2013
Accepted: 31 October 2013
Context. Monoceros R2 (Mon R2), at a distance of 830 pc, is the only ultra-compact H ii region (UC H ii) where its associated photon-dominated region (PDR) can be resolved with the Herschel Space Observatory.
Aims. Our aim is to investigate observationally the kinematical patterns in the interface regions (i.e., the transition from atomic to molecular gas) associated with Mon R2.
Methods. We used the HIFI instrument on board Herschel to observe the line profiles of the reactive ions CH+, OH+, and H2O+ toward different positions in Mon R2. We derive the column density of these molecules and compare them with gas-phase chemistry models.
Results. The reactive ion CH+ is detected both in emission (at central and red-shifted velocities) and in absorption (at blue-shifted velocities). The OH+ ion is detected in absorption at both blue- and red-shifted velocities, with similar column densities; H2O+ is not detected at any of the positions, down to a rms of 40 mK toward the molecular peak. At this position, we find that the OH+ absorption originates in a mainly atomic medium, and therefore is associated with the most exposed layers of the PDR. These results are consistent with the predictions from photo-chemical models. The line profiles are consistent with the atomic gas being entrained in the ionized gas flow along the walls of the cavity of the H ii region. Based on this evidence, we are able to propose a new geometrical model for this region.
Conclusions. The kinematical patterns of the OH+ and CH+ absorption indicate the existence of a layer of mainly atomic gas for which we have derived, for the first time, some physical parameters and its dynamics.
Key words: ISM: abundances / ISM: molecules / ISM: individual objects: Monoceros R2 / photon-dominated region (PDR) / HII regions
© ESO, 2014
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