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Title:
Galactic Wind in the Nearby Starburst Galaxy NGC 253 Observed with the Kyoto3DII Fabry-Perot Mode
Authors:
Matsubayashi, K.; Sugai, H.; Hattori, T.; Kawai, A.; Ozaki, S.; Kosugi, G.; Ishigaki, T.; Shimono, A.
Affiliation:
AA(Department of Astronomy, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan ), AB(Department of Astronomy, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan ), AC(Subaru Telescope, National Astronomical Observatory of Japan, 650 North A'ohoku Place, Hilo, HI 96720, USA ), AD(Department of Astronomy, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan ), AE(Okayama Astrophysical Observatory, National Astronomical Observatory of Japan, Kamogata, Okayama 719-0232, Japan ), AF(National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan ), AG(Asahikawa National College of Technology, Asahikawa, Hokkaido 071-8142, Japan), AH(Department of Astronomy, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan )
Publication:
The Astrophysical Journal, Volume 701, Issue 2, pp. 1636-1643 (2009). (ApJ Homepage)
Publication Date:
08/2009
Origin:
IOP
ApJ Keywords:
galaxies: individual: NGC 253, galaxies: starburst, ISM: abundances, ISM: jets and outflows
DOI:
10.1088/0004-637X/701/2/1636
Bibliographic Code:
2009ApJ...701.1636M

Abstract

We have observed the central region of the nearby starburst galaxy NGC 253 with the Kyoto Tridimensional Spectrograph II Fabry-Perot mode in order to investigate the properties of its galactic wind. Since this galaxy has a large inclination, it is easy to observe its galactic wind. We produced the Hα, [N II]λ6583, and [S II]λλ6716,6731 images, as well as their line-ratio maps. The [N II]/Hα ratio in the galactic-wind region is larger than those in H II regions in the galactic disk. The [N II]/Hα ratio in the southeastern filament, a part of the galactic wind, is the largest and reaches about 1.5. These large [N II]/Hα ratios are explained by shock ionization/excitation. Using the [S II]/Hα ratio map, we spatially separate the galactic-wind region from the starburst region. The kinetic energy of the galactic wind can be sufficiently supplied by supernovae in a starburst region in the galactic center. The shape of the galactic wind and the line-ratio maps are nonaxisymmetric about the galactic minor axis, which is also seen in M82. In the [N II]λ6583/[S II]λλ6716,6731 map, the positions with large ratios coincide with the positions of star clusters found in the Hubble Space Telescope observation. This means that intense star formation causes strong nitrogen enrichment in these regions. Our unique data of the line-ratio maps including [S II] lines have demonstrated their effectiveness for clearly distinguishing between shocked-gas regions and starburst regions, determining the extent of galactic wind and its mass and kinetic energy, and discovering regions with enhanced nitrogen abundance.
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