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Issue A&A
Volume 430, Number 2, February I 2005
Page(s) 549 - 560
Section Interstellar and circumstellar matter
DOI http://dx.doi.org/10.1051/0004-6361:20040437



A&A 430, 549-560 (2005)
DOI: 10.1051/0004-6361:20040437

The interstellar C $\mathsf{^{18}}$O/C $\mathsf{^{17}}$O ratio in the solar neighbourhood: The $\rho$ Ophiuchus cloud

J. G. A. Wouterloot1, 2, J. Brand3 and C. Henkel4

1  Joint Astronomy Centre, 660 N. A'ohoku Place, University Park, 96720 Hilo, Hawaii, USA
    e-mail: j.wouterloot@jach.hawaii.edu
2  Radioastronomisches Institut, Univ. Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
3  Istituto di Radioastronomia, CNR, via Gobetti 101, 40129 Bologna, Italy
4  Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany

(Received 13 March 2004 / Accepted 15 September 2004)

Abstract
Observations of up to ten carbon monoxide (CO and isotopomers) transitions are presented to study the interstellar C 18O/C 17O ratio towards 21 positions in the nearby ( $d\sim140$ pc) low-mass star forming cloud $\rho$ Oph. A map of the C 18O J=1-0 distribution of parts of the cloud is also shown. An average 12C 18O/ 12C 17O isotopomeric ratio of $4.11 \pm 0.14$, reflecting the 18O/ 17O isotope ratio, is derived from Large Velocity Gradient (LVG) calculations. From LTE column densities we derive a ratio of $4.17\pm0.26$. These calculations also show that the kinetic temperature decreases from about 30 K in the cloud envelope to about 10 K in the cloud cores. This decrease is accompanied by an increase of the average molecular hydrogen density from 10 4 cm -3 to $\ga$10 5 cm -3. Towards some lines of sight C 18O optical depths reach values of order unity.


Key words: ISM: abundances -- ISM: clouds -- ISM: molecules -- Galaxy: abundances -- radio lines: ISM -- ISM: individual objects: rho Oph

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