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Please Note: the e-mail address(es) and any external links in this paper were correct when it was written in 1995, but may no longer be valid.
Albert
Nummelin
e-mail:
albert@bele.oso.chalmers.se
Onsala Space Observatory, S-439 92 Onsala, SWEDEN
and 
abundances indicate
shock chemistry in the M core, which could contain an outflow.
The Sgr B2 molecular cloud, located approximately 100 pc from the Galactic
Centre and with a mass of 
, is one of the most extreme
cases among star formation sites (Lis & Goldsmith (1991)). This region contains many
tracers of recent massive star formation: 
resolved ultra-compact HII regions, numerous 
- and OH-masers, large far infrared
luminosity, all of which indicate active formation of O-type stars
(Gordon et al. (1993)). Another prominent characteristic of the Sgr B2 cloud is its
extremely rich chemistry.
The two strongest sources of millimetre and submillimetre emission, each with a
total luminosity of 
30 
that of Orion A, are denoted Sgr
B2(N) (``North'') and Sgr B2(M) (``Middle'') respectively and are currently
being surveyed in the 215-265 GHz region using the SEST in order to learn
about the physical and chemical conditions in this very active star forming
region. Both of these positions correspond to compact clusters of HII
regions and contain very dense and warm gas.
A third position, denoted Sgr B2(NW) (``North-West''), towards a quiescent part of the cloud, is also being surveyed in order to compare physics and chemistry before and after processing in protostellar cores.
Sgr B2 has previously been surveyed at wavelengths around 3 mm (Cummins et al. (1986),Turner (1989),Turner (1991)) and 0.8 mm (Sutton et al. (1991)).
Figure 1: Two sample spectra towards Sgr B2(M) and Sgr B2(N). Because of the
width and density of the spectral lines towards N, a ``line forest'' can easily
be mistaken for a baseline offset.
The observational part of the survey has recently been completed but analysis
has only just begun. Of the 3 observed positions Sgr B2(N) has the strongest
line emission in most molecular species with a few exceptions. The linewidths
are very high (
) and the number of lines per GHz
is also very high (
). With such broad lines and high line
density blending and confusion is a very severe problem in the analysis.
Sgr B2(M) is the stronger of the 3 sources in a few species, the most important
of which are SO and 
. The abundances of some Sulphur species are
predicted to be increased in regions where the gas is shocked (Pineau des Forêts et al. (1993)),
which suggests that M might contain outflows. Otherwise, M has more moderate
linewidths, 
, and fewer lines per GHz
(
) than does N, which makes the data from this source easier to
reduce and analyze. A preliminary line identification contains some 600
identified and unidentified lines towards M.