O18O and C18O observations of rho Oph A
  Observations of the (N_J=1_1-1_0) ground state transition of O_2 with the
Odin satellite resulted in a about 5 sigma detection toward the dense core rho
Oph A. At the frequency of the line, 119 GHz, the Odin telescope has a beam
width of 10', larger than the size of the dense core, so that the precise
nature of the emitting source and its exact location and extent are unknown.
The current investigation is intended to remedy this. Telluric absorption makes
ground based O_2 observations essentially impossible and observations had to be
done from space. mm-wave telescopes on space platforms were necessarily small,
which resulted in large, several arcminutes wide, beam patterns. Although the
Earth's atmosphere is entirely opaque to low-lying O_2 transitions, it allows
ground based observations of the much rarer O18O in favourable conditions and
at much higher angular resolution with larger telescopes. In addition, rho Oph
A exhibits both multiple radial velocity systems and considerable velocity
gradients. Extensive mapping of the region in the proxy C18O (J=3-2) line can
be expected to help identify the O_2 source on the basis of its line shape and
Doppler velocity. Line opacities were determined from observations of optically
thin 13C18O (J=3-2) at selected positions. During several observing periods,
two C18O intensity maxima in rho Oph A were searched for in the 16O18O
(2_1-0_1) line at 234 GHz with the 12m APEX telescope. Our observations
resulted in an upper limit on the integrated O18O intensity of < 0.01 K km/s (3
sigma) into the 26.5" beam. We conclude that the source of observed O_2
emission is most likely confined to the central regions of the rho Oph A cloud.
In this limited area, implied O_2 abundances could thus be higher than
previously reported, by up to two orders of magnitude.
