Multi-Line Observations of Molecular Gas in the Central Region of the Low Star-Formation Efficiency ``Starburst'' Galaxy NGC 4527

Details Multi-Line Observations of Molecular Gas in the Central Region of the Low Star-Formation Efficiency ``Starburst'' Galaxy NGC 4527 Multi-Line Observations of Molecular Gas in the Central Region of the Low Star-Formation Efficiency ``Starburst'' Galaxy NGC 4527

Feb 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003pasj...55...87s&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.55, No.1, pp.87-101

Astronomy and Astrophysics

Astronomy

6

Galaxies: Individual (Ngc 4527), Galaxies: Ism, Galaxies: Starburst, Ism: Molecules

Scientific paper

We performed high-resolution CO(J = 2 -- 1), CO(J = 1 -- 0), HCN(J = 1 -- 0), HCO+(J = 1 --0), and 3mm continuum observations of the low star formation efficiency (SFE) ``starburst'' galaxy NGC 4527 with the Nobeyama Millimeter Array. From CO( J = 1 -- 0) observations, we found two offset ridges with non-circular motion and a central gas concentration. The distribution and kinematics of NGC 4527 are very similar to those of barred spiral galaxies. The distribution of CO(J = 2 -- 1) emission resembles the features of the concentrated component of CO(J = 1 -- 0). HCN(J = 1--0 ) and HCO+(J = 1--0 ) emissions concentrated toward the center have also been detected. The total mass of molecular gas detected in the central r < 30" is 2.5 × 109 M&sun;. The HCN(J = 1--0 )/CO (J = 1--0 ) integrated intensity ratio of 0.075 ± 0.008 in the central r <˜ 3" -- 4" region of NGC 4527 could suggest that the fraction of dense molecular gas to the total molecular gas is small compared with those of prototypical starburst galaxies, such as NGC 253. This suggests that the small dense gas fraction is responsible for the low SFE in the center of NGC 4527, though this interpretation could depend on aperture sizes of the observations. The ratio of the dynamical mass to molecular gas mass is 13% within the central region (r < 500 pc). This suggests that molecular gas within the r < 500 pc region could be in a state of gravitational instability. The low SFE, the small dense gas fraction, and the large amount of gravitationally unstable molecular gas can be explained if NGC 4527 is in the very early phase of starburst phenomena or a pre-starburst phase, and the formation of dense molecular gas will begin and the SFE will increase within a short time scale.

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