Astronomy and Astrophysics – Astronomy
Scientific paper
May 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aas...182.3908b&link_type=abstract
American Astronomical Society, 182nd AAS Meeting, #39.08; Bulletin of the American Astronomical Society, Vol. 25, p.858
Astronomy and Astrophysics
Astronomy
Scientific paper
Using the Owens Valley millimeter array, we have observed several ultraluminous infrared galaxies in CO(1--0) at resolutions as small as 3\arcsec . We have also observed and detected one galaxy, NGC 3690, in HCN(1--0). The galaxies in our sample all have infrared luminosities in excess of 10(11.5) L\sun . These observations are part of an ongoing project to determine the amount and distribution of the large masses (10(10) --10(11) M\sun ) of molecular gas that exist in ultraluminous galaxies. Previous interferometric CO observations have revealed that the molecular gas of ultraluminous galaxies is largely confined to within a couple kiloparsecs or less of the nucleus, so that at a resolution of 6\arcsec , less than or equal to the resolution of almost all previous observations, the molecular gas is unresolved or poorly-resolved. The observations reported here significantly increase the sample of ultraluminous galaxies that have been observed in CO at a resolution of 3\arcsec. Interferometric HCN observations of ultraluminous galaxies have been very rare as of this date. Our HCN detection of NGC 3690, along with a previous Owens Valley CO map from Sargent and Scoville (1991), allows a detailed comparison of the HCN and CO emission in this relatively nearby system (42 Mpc), allowing a comparison of the amount and distribution of molecular gas in dense, potential star-forming cores (n(H_2) ~ 10(5) cm(-3) ) versus more diffuse molecular clouds (n(H_2) ~ 10(2) --10(3) cm(-3) ).
Bryant Peter M.
Scoville Nicholas Z.
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