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Gas and dust in the star-forming region rho Oph A II. The gas in the PDR and in the dense cores
Stockholm University, Faculty of Science, Department of Astronomy.
Number of Authors: 22017 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 608, article id A133Article in journal (Refereed) Published
Abstract [en]

Context. The evolution of interstellar clouds of gas and dust establishes the prerequisites for star formation. The pathway to the formation of stars can be studied in regions that have formed stars, but which at the same time also display the earliest phases of stellar evolution, i.e. pre-collapse/collapsing cores (Class-1), protostars (Class 0), and young stellar objects (Class I, II, III).

Aims. We investigate to what degree local physical and chemical conditions are related to the evolutionary status of various objects in star-forming media.

Methods. rho OphA displays the entire sequence of low-mass star formation in a small volume of space. Using spectrophotometric line maps of H-2, H2O, NH3, N2H+, O-2, OI, CO, and CS, we examine the distribution of the atomic and molecular gas in this dense molecular core. The physical parameters of these species are derived, as are their relative abundances in rho Oph A. Using radiative transfer models, we examine the infall status of the cold dense cores from their resolved line profiles of the ground state lines of H2O and NH3, where for the latter no contamination from the VLA 1623 outflow is observed and line overlap of the hyperfine components is explicitly taken into account.

Results. The stratified structure of this photon dominated region (PDR), seen edge-on, is clearly displayed. Polycyclic aromatic hydrocarbons (PAHs) and OI are seen throughout the region around the exciting star S 1. At the interface to the molecular core 0.05 pc away, atomic hydrogen is rapidly converted into H-2, whereas OI protrudes further into the molecular core. This provides oxygen atoms for the gas-phase formation of O-2 in the core SM1, where X(O-2) similar to 5 x 10(-8). There, the ratio of the O-2 to H2O abundance [X(H2O) similar to 5 x 10(-9)] is significantly higher than unity. Away from the core, O-2 experiences a dramatic decrease due to increasing H2O formation. Outside the molecular core rho Oph A, on the far side as seen from S 1, the intense radiation from the 0.5 pc distant early B-type star HD147889 destroys the molecules.

Conclusions. Towards the dark core SM1, the observed abundance ratio X(O-2)/X(H2O) > 1, which suggests that this object is extremely young, which would explain why O-2 is such an elusive molecule outside the solar system.

Place, publisher, year, edition, pages
2017. Vol. 608, article id A133
Keywords [en]
ISM: individual objects: rho Oph A, ISM: molecules, ISM: abundances, photon-dominated region (PDR), stars: formation, ISM: general
National Category
Physical Sciences
Identifiers
URN: urn:nbn:se:su:diva-150959DOI: 10.1051/0004-6361/201731466ISI: 000418459900004OAI: oai:DiVA.org:su-150959DiVA, id: diva2:1173553
Available from: 2018-01-12 Created: 2018-01-12 Last updated: 2018-01-12Bibliographically approved

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