Molecular abundances in the Magellanic Clouds .2. Deuterated species in the LMC

The first definite discoveries of extragalactic deuterium are reported. DCO+ has been detected in three and DCN has been measured in one star-forming region of the Large Magellanic Cloud (LMC). While the HCO+/DCO+ abundance ratios are found to be 19 +/- 3, 24 +/- 4, and 67 +/- 18 for N113, N44BC and N159HW, respectively, a HCN/DCN abundance ratio of 23 +/- 5 is obtained for N113. These results are consistent with a gas temperature of about 20 K and a D/H ratio of about 1.5 x 10(-5), consistent with that observed in the Galaxy. If the cloud temperature is closer to 30 K, then a D/H ratio is required to be up to an order of magnitude larger. Because this ratio provides a lower limit to the primordial D/H ratio, it indicates that the baryon mass density alone is unable to close the universe.

DENSE GAS IN NEARBY GALAXIES .9. A SURVEY FOR HNC

Ten detections and five tentative detections of hydrogen isocyanide (HNC) J=1-0 emission are reported from a survey including sixteen galaxies. Full maps are presented for the nuclear regions of NGC 253 and IC 342, partial maps for Maffei 2, M 82, and M 83. Toward IC 342, the HNC and HCO+ distributions differ from those observed in 12CO, 13CO, HCN, CS, and NH3. This is likely a consequence of the density structure. Relative HNC abundances are with 10(-10)-10(-9) much smaller than those measured in nearby dark clouds and appear to be slightly smaller than those in regions of massive star formation of the Galactic disk. This is consistent with the presence of dense warm gas or a frequent occurrence of shocks in the nuclear regions of the galaxies observed. As in prominent Galactic star forming regions, 3 mm HNC line emission tends to be weaker than the corresponding emission from HCN and HCO+. Toward Arp 220, however, the 3 mm HNC/HCN line intensity ratio is > 1. HNC/HCO+, HNC/CO, and HNC to 20 cm radio continuum luminosity ratios are also particularly large. A possible interpretation is the presence of cool quiescent gas outside the central region which contains the starburst. In the other ultraluminous galaxy observed, NGC 6240, X(HNC) 10 smaller than in Arp 220, demonstrating that the molecular composition in ultraluminous galaxies is far from being uniform.

A NEW CHEMICAL-MODEL OF THE CIRCUMSTELLAR ENVELOPE SURROUNDING IRC+10216

A new chemical model of the circumstellar envelope surrounding the carbon-rich star IRC+10216 has been developed. This model incorporates a variety of newly measured rapid neutral-neutral reactions between carbon atoms and hydrocarbons and between the radical CN and a variety of stable neutral molecules. In addition, other neutral-neutral reactions in the above two classes or involving atoms such as N or radicals such as C(2n)H have been included with large rate coefficients although they have not yet been studied in the laboratory. Unlike the interstellar case, where the inclusion of these neutral-neutral reactions destroys molecular complexity, our model results for IRC+10216 show that sufficient abundances of large hydrocarbon radicals and cyanpolyynes can be produced to explain observations. We also discuss the formation of H2CN and NH2CN, two potentially observable molecules in IRC+10216.

DENSE GAS IN NEARBY GALAXIES .6. A LARGE C-12/C-13 RATIO IN A NUCLEAR STARBURST ENVIRONMENT

Toward the starburst nucleus of NGC 253, C-12/C-13 line intensity ratios from six carbon bearing molecules (CO, CN, CS, HCN, HCO+, and HNC) are used to confine the possible range of carbon and oxygen isotope ratios. A detailed analysis yields C-12/C-13 approximately 40 and O-16/O-18 approximately 200. Also reported are first detections of (CS)-C-13 and of the 0(0) - 1(-1) E line of methanol (CH3OH) in an extragalactic source.

PROTONATED HCN IN MOLECULAR CLOUDS

Observations of protonated HCN (HCNH+) in a selection of galactic molecular clouds are reported. This species plays a key role in understanding the chemistry of the important high density tracer HCN. HCNH+ has been detected in the nearby cold dust cloud TMC-1 with an ratio relative to HCN of [HCNH+]/[HCN] between 0.015 and 0.26 (preferred value 0.03) and tentatively in DR21(OH) with a ratio of approximately 0.01. This is about 100 times higher than the ratio of protonated carbon monoxide to CO [HCO+]/[CO], but comparable to the [HCS+]/[CS] ratio. Possible explanations of these high abundance ratios are discussed in the light of model calculations.

PHOSPHORUS CHEMISTRY IN DENSE INTERSTELLAR CLOUDS

I have used recent laboratory studies on the reactions of the phosphorus hydride ions, PH(n)+ (n = 0-4) to construct a new model of phosphorus chemistry in interstellar clouds. I find that the non-detection of PN in cold, dark clouds in consistent with the chemical models only if the depletion of phosphorus in large, approximately 10(4) in TMC-1. Although the laboratory studies indicate that organo-phosphorus chains C(n)P can be formed, this large depletion precludes the detection of any phosphorus-bearing moleclues in cold clouds. However, in warm clouds associated with star formation, the depletion of phosphorus may be reduced. In this case one can reproduce the PN abundance toward Orion KL with a depletion factor of about 300. Interestingly, if the organo-phosphorus species are not destroyed by O atoms, I predict fractional abundances in Ori KL of between 10(-11) and 10(-10) for C(n)P (n = 2-4) and HCCP.