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Observations are presented of emission lines from organic molecules atfrequencies 32 - 50 GHz in the vicinity of Chamaeleon MMS1. Thischemically-rich dense cloud core habours an extremely young, verylow-luminosity protostellar object and is a candidate first hydrostatic core.Column densities are derived and emission maps are presented for speciesincluding polyynes, cyanopolyynes, sulphuretted carbon-chains and methanol. Thepolyyne emission peak lies about 5000 AU from the protostar, whereas methanolpeaks about 15,000 AU away. Averaged over the telescope beam, the molecularhydrogen number density is calculated to be 10^6 cm^-3 and the gas kinetictemperature is in the range 5 - 7 K. The abundances of long carbon chains arevery large, and are indicative of a non-equilibrium carbon chemistry; C6H andHC7N column densities are 5.9 (+2.9 -1.3) \times 10^11 cm^-2 and 3.3 (+8.0-1.5) \times 10^12 cm^-2, respectively, which are similar to the values foundin the most carbon-chain-rich protostars and prestellar cores known, and areunusually large for star-forming gas. Column density upper limits were obtainedfor the carbon-chain anions C4H- and C6H-, with anion-to-neutral ratios[C4H-]/[C4H] < 0.02% and [C6H-]/[C6H] < 10%, consistent with previousobservations in interstellar clouds and low-mass protostars. Deuterated HC3Nand c-C3H2 were detected. The [DC3N]/[HC3N] ratio of approximately 4% isconsistent with the value typically found in cold interstellar gas.

Organic chemistry of low-mass star-forming cores I: 7 mm spectroscopy of Chamaeleon MMS1