A Multi-ionic Kinematic Investigation of NGC 595, a Giant Extragalactic H II Region in M33

Details A Multi-ionic Kinematic Investigation of NGC 595, a Giant Extragalactic H II Region in M33 A Multi-ionic Kinematic Investigation of NGC 595, a Giant Extragalactic H II Region in M33

Aug 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009apj...700.1847l&link_type=abstract

The Astrophysical Journal, Volume 700, Issue 2, pp. 1847-1877 (2009).

Astronomy and Astrophysics

Astronomy

5

Ism: Bubbles, Ism: Individual: Ngc 595, Ism: Kinematics And Dynamics, Stars: Winds, Outflows, Techniques: Interferometric

Scientific paper

Spectro-interferometric observations of the Hα, [O III], and [S II] optical emission lines are combined with radio observations of the 21 cm line in order to obtain a reliable kinematic image of NGC 595, the second largest giant extragalactic H II region in M33. The Hα and [O III] observations reveal that the nebula is exposed to two distinct kinematical regimes. While symmetric, broad velocity profiles dominate a sizeable fraction of the ionized extent, evidence for line splitting is detected in a small region near the most massive stars of the star cluster. A quantitative investigation proposes that two expanding wind-blown bubbles could be held responsible for the observed line splitting. The kinematics of the ionized material presenting one-component velocity profiles likely indicates that Champagne flows are present at the periphery of the molecular component leading to accelerated ionized material in the ambient interstellar medium. In areas not dominated by the photoionization of the molecular clouds, the H+ and S+ material shows a kinematical behavior roughly in agreement with the atomic gas. Mean nonthermal line widths show relatively large, supersonic values especially in [O III]. Models of structure functions indicate that the Hα and [O III] components could be exposed to different turbulent motions which could explain the broadening excess observed for the latter ion. On the full ionized extent of the nebula, the S+ material shows narrower line widths than the two other ions. Combined with the absence of line splitting, these peculiar characteristics indicate that the [S II] component is likely located at the periphery of the nebula and probably does not coexist with Hα and [O III]. The shape of the [S II] structure function is in agreement with a relatively low number of large-scale velocity gradients which partially explains the narrower profiles observed. The mean electron density in the nebula is estimated at 162 ± 106(1σ) cm-3, in agreement with previous studies of similar extragalactic H II regions. We provide the first bidimensional electron density map ever presented for a giant extragalactic nebula.

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