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Title:
Study of M82 Using Spectra from the Infrared Space Observatory
Authors:
Sohn, Jungjoo; Ann, H. B.; Pak, Soojong; Lee, H. M.
Affiliation:
AA(Department of Earth Science, Pusan National University, Pusan, Korea; Astronomy Program, SEES, Seoul National University, Seoul, Korea; Infrared Astrophysics Group, Institute of Space and Astronautical Science, Japan) AB(Department of Earth Science, Pusan National University, Pusan, Korea) AC(Astronomy Program, SEES, Seoul National University, Seoul, Korea) AD(Astronomy Program, SEES, Seoul National University, Seoul, Korea; Infrared Astrophysics Group, Institute of Space and Astronautical Science, Japan)
Journal:
Journal of the Korean Astronomical Society, vol. 34, no. 1, pp. 17-24
Publication Date:
04/2001
Origin:
JKAS
Keywords:
GALAXIES: STARBURST GALAXIES, INDIVIDUAL(M82), METHODS: DATA ANALYSIS
Abstract Copyright:
(c)Korean Astronomical Society
Bibliographic Code:
2001JKAS...34...17S

Abstract

We have studied the central parts of M82, which is a well-known luminous, starburst galaxy, by analyzing archival data from the Infrared Space Observatory(ISO). M82 was observed at 11 positions covering +45" from the center along the major axis. We analyzed 4 emission lines, [Ar III] 8.99 micron, H2 17.034 micron, [Fe II] 25.98 micron, and [Si II] 34.815 micron from SWS02 data. The integrated flux distributions of these lines are quite different. The H2 line shows symmetric twin peaks at ~18" from the center, which is a general characteristic of molecular lines in starburst or barred galaxies. This line appears to be associated with the rotating molecular ring at around ~200 pc just outside the inner spiral arm. The relative depletion of the H2 line at the center may be due to the active star formation activity which dissociates the H2 molecules. The other lines have peaks at the center and the distributions are nearly symmetric. The line profiles are deconvolved assuming that both intrinsic and instrumental profiles are Gaussian. The velocity dispersion outside the core is found to be ~50 km/s. The central velocity dispersion is much higher than 50 km/s, and different lines give different values. The large central velocity dispersion(sigma) is mostly due to the rotation, but there is also evidence for a high sigma for [Ar III] line. We also generated position-velocity maps for these four lines. We found very diverse features from these maps.

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