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  • Print publication year: 2000
  • Online publication date: August 2010

Near-Infrared Imaging and [OI] Spectroscopy of IC443 using 2MASS and ISO

from 3 - Observations and Models
    • By J. Rho, Infrared Processing and Analysis Center, California Institute of Technology, MS 100-22, Pasadena, CA, 91125, USA, S. Van Dyk, Infrared Processing and Analysis Center, California Institute of Technology, MS 100-22, Pasadena, CA, 91125, USA, T. Jarrett, Infrared Processing and Analysis Center, California Institute of Technology, MS 100-22, Pasadena, CA, 91125, USA, R. M. Cutri, Infrared Processing and Analysis Center, California Institute of Technology, MS 100-22, Pasadena, CA, 91125, USA, W. T. Reach, Infrared Processing and Analysis Center, California Institute of Technology, MS 100-22, Pasadena, CA, 91125, USA
  • Edited by F. Combes, Observatoire de Paris, DEMIRM, G. Pineau des Forets, Observatoire de Paris de Meudon, DAEC
  • Publisher: Cambridge University Press
  • DOI: https://doi.org/10.1017/CBO9780511564635.031
  • pp 201-204

Summary

We present near-infrared imaging of IC443, covering entire supernova remnant (50 diameter) from the Two Micron All Sky Survey (2MASS), which images are taken simultaneously in the J (1.25µm), H (1.65µm) and Ks (2.17µm) bands. Emission from IC443 was detected in all 3 bands from most of the optically bright parts of the remnant, revealing a shell-like morphology. These are the first near-infrared images that covers entire remnant. The color and structure are very different between the northeastern and southern parts. Bright J and H band emission from the northeast rim can be explained mostly by [Fe II] and the rest by hydrogen lines of Pβ and Br10. We also report ISO LWS observation of [O I] (63µm) for 11 positions in the northeast. Strong lines were detected and the strongest line is in the northeastern shell, where 2MASS image showed filamentary structure in J and H. In contrast, the southern ridge is dominated by Ks band light with knotty structure, and has weak J and H band emission. The shocked H2 line emission is well known from the sinus ridge produced by an interaction with dense molecular clouds. The large field of view and color of the 2MASS images show that the H2 emission extends to the east and the northeast. This H2 emission suggests that the interaction with the molecular clouds extends to the front side in the northeast.