Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006rmxac..26r.187b&link_type=abstract
XI IAU Regional Latin American Meeting of Astronomy (Eds. L. Infante & M. Rubio) Revista Mexicana de Astronomía y Astrofísica (S
Astronomy and Astrophysics
Astronomy
Scientific paper
The origin of the supersonic velocity dispersion of the ionized gas in giant HII regions (GHIIRs) and HII galaxies (HIIGs) is one of the complex topics in the study of theses objects. We observed with Gemini telescope, using GMOS-N/IFU, the central region of II Zw 40 (D ˜ 12 Mpc), a powerful HIIG. The aim is to understand the physical mechanisms which dominate the gas kinematics and the general dynamics, extending the spatially resolved study of the near star forming regions to HIIGs. We build from six frames over the brightest region of the galaxy, the H α monochromatic, radial velocity and velocity dispersion maps. The radial velocity map shows a turbulent field, very similar with those found in Local Group's GHIIRs. From the velocity dispersion map we identified clumps well defined with high σ (up to 65 km s^{-1}), which are associated with a very weak H α emission. Despite of the presence of the high dispersion regions, probably due to fast expanding shells and hot plasma interactions, these regions are poorly represented kinematically in the integrated optical nebular lines. A quantitative way to present these map results is through the σ vs. intensity plot, where some kinematics features of GHIIRs are identified. This method is used to show that the central starburst in II Zw 40, a single super star cluster (SSC), is one of the most powerful known, leading the gas to a smooth turbulent velocity dispersion of ˜ 33 km s^{-1}.
Bordalo Vinicius
Plana Henri
Telles Eduardo
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