[en] The detection of CO (J = 1-0) emission in the dwarf elliptical galaxy NGC 185 is reported. The presence of massive molecular clouds in this early-type galaxy supports the idea of recent or ongoing stellar formation indicated by the population of blue stars in the center. The CO was detected in two positions in the galaxy, the center, and a prominent dustcloud. The emission profile has two peaks, roughly centered around the systemic velocity. It is found that NGC 185 is overluminous in blue light for its CO luminosity compared with Sc galaxies. This might indicate a higher star-formation efficiency for NGC 185 than for the late-type galaxies

[en] Mapping of the CO(1-0) emission from the spiral galaxy was made with the Onsala 20 m antenna. The observations show that the emission is considerably enhanced in spiral arms which appear to originate as intense ridges of emission about 1 kpc from the nucleus. One of the main objectives for the 1986 observations was to study the variations of the tangential velocity component of molecular gas across a spiral arm. The radial velocity was found to have a velocity shift similar to that predicted by the density wave theory. The present (1986) observations of the inner southern spiral arm of M51 show that the tangential velocity component also behaves in a way which conforms with the density wave model. The molecular arms were compared with the H alpha ionized gas arms of Tully (1974) and it was found that the ionized gas appears to have its maximum intensity slightly outside the molecular arm

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[en] Researchers present maps of the CO-12(1=0) line and the 100 micron and 50 micron far-infrared emission of Centaurus A, as well as measurements of the CO-12(2-1), CO-13(1-0), and the C-18O(1-0) lines at selected positions. The observations were taken with the Swedish-ESO Submillimeter Telescope (SEST) and the CPC instrument on board the Infrared Astronomy Satellite (IRAS). The millimeter data show that the bulk molecular material is closely associated with the dust lane and contained in a disk of about 180 seconds diameter and a total molecular mass of about 2 x 10 to the 8th power solar mass. The total molecular mass of the disk and bulge is of the order of 3 x 10 to the 8th power solar mass. The molecular gas in the nucleus is warm with a kinetic temperature of the order of 15 K and a number density of 10 to the 3rd power to 3 x 10 to the 4th power cm(-3). Absorption features in the CO-12 and CO-13 lines against the nuclear continuum emission indicate that the properties of giant molecular clouds are comparable to those of the Galaxy. The far-infrared data show that to a good approximation the dust temperature is constant across the dust lane at a value of about 42 K. The ratio between the far-infrared luminosity and the total molecular mass is 18 solar luminosity/solar mass and close to the mean value obtained for isolated galaxies. A comparison of the CO-12(1-0) and the far-infrared data indicates that a considerable amount of the far-infrared emission is not intimately associated with massive star formation

[en] The distributions of H¹²CN, H¹³CN, and H¹²CO⁺ have been mapped with 20'' spacing. HC¹⁵N and H¹³CO⁺ were observed toward the map center. The physical properties of the Orion A extended ridge and of the much smaller HCN plateau cloud (angular extension considerably less than that of the 43'' beam) have been estimated on the basis of Gaussian decompositions of the various spectra, combined with cloud modeling

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[en] Emission from SO towards a number of HII regions and molecular clouds with embedded energy sources has been reported by several authors. The authors provide additional spectra and information on observing procedures, and discuss the rest frequencies for the SO and ³⁴SO 1₀→0₁ transitions. (Auth.)

[en] Some 25 previously unreported intestellar lines have been detected in the 3--4 mm spectrum of Orion A and are attributed to methyl formate (HCOOCH₃). A rotational temperature T> or approx. =50 K and a beam-averaged column density Nroughly-equal2(10)¹⁴ cm^-2 are estimated. A new limit on the abundance of formic acid suggests that [HCOOCH₃]/[HCOOH]> or approx. =3. Methyl formate transitions at 76.702 and 76.711 GHz, at 85.927 GHz and at 86.224 GHz clearly correspond to previously reported spectral lines attributed to CH₄, NH₂D, and (CH₃)₂O, respectively. These results suggest that the detections of methane and deuterated ammonia in Orion A should be regarded as tentative only, with important implications for interstellar chemistry and deuterium abundances

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