Hostname: page-component-cd9895bd7-jn8rn Total loading time: 0 Render date: 2024-12-26T04:47:42.262Z Has data issue: false hasContentIssue false
  • English
  • Français

Tridimensional Observations of Nearby Active Galaxies Using OAO Spectronebulagraph

Published online by Cambridge University Press:  12 April 2016

M. Yoshida ,
Y. Shimizu ,
H. Koyano ,
G. Kosugi ,
K. Aoki ,
H. Ohtani ,
T. Sasaki  and
M. Sasaki
M. Yoshida
Affiliation:
Okayama Astrophysical Observatory, Kamogata-cho, Asakuchi-gun, Okayama 719-02, Japan
Y. Shimizu
Affiliation:
Okayama Astrophysical Observatory, Kamogata-cho, Asakuchi-gun, Okayama 719-02, Japan
H. Koyano
Affiliation:
Okayama Astrophysical Observatory, Kamogata-cho, Asakuchi-gun, Okayama 719-02, Japan
G. Kosugi
Affiliation:
Department of Astronomy, Kyoto University, Kyoto 606-01, Japan
K. Aoki
Affiliation:
Department of Astronomy, Kyoto University, Kyoto 606-01, Japan
H. Ohtani
Affiliation:
Department of Astronomy, Kyoto University, Kyoto 606-01, Japan
T. Sasaki
Affiliation:
National Astronomical Observatory, Mitaka, Tokyo 181, Japan
M. Sasaki
Affiliation:
Shimonoseki City University, Daigaku-cho, Shimonoseki, Yamaguchi 751, Japan

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We developed a slit-scanning type 3D-spectroscopic system named as Spectronebulagraph (hereafter SNG; Kosugi et al. 1994) at Okayama Astrophysical Observatory. A detailed description about SNG is presented by Ohtani et al. elsewhere in this colloquium. We present here the results of the 3D-spectroscopy of four nearby active galaxies by using SNG.

This nearby (at distance of 5.4 Mpc) Magellanic irregular galaxy has many H II regions in its main body suggesting violent star-formation activity. We performed tridimensional observations of NGC 4449 using SNG in order to obtain detailed kinematic structure and then to investigate the star-formation mechanism of NGC 4449. Hα intensity map, Hα velocity field are shown in figure 1. As is obvious in lower panel of figure 1, no global rotational motion was detected. Most impressive feature of the velocity field is kpc-scale mosaic structure of low velocity and high velocity components. Also, many filamentary components were newly found in 3D-datacube of the SNG observation.

Type
3. Integral Field Spectrographs and Spectrometers
Information
International Astronomical Union Colloquium , Volume 149: Tridimensional Optical Spectroscopic Methods in Astrophysics , 1995 , pp. 207 - 208
Copyright
Copyright © Astronomical Society of the Pacific 1995