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Astron. Astrophys. 315, L149-L152 (1996)

ISOPHOT Maps of NGC6946 in the range tex2html_wrap_inline43 60-200 tex2html_wrap_inline45m*

R.J. Tuffs1, D. Lemke2, C. Xu1, J.I. Davies3, C. Gabriel4, I. Heinrichsen1,4, G. Helou5, H. Hippelein2, N.Y. Lu5, and D. Skaley1,6

1 Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, D-69117 Heidelberg, Germany
2 Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany
3 Department of Physics and Astronomy, University of Wales College of Cardiff, UK
4 European Space Agency Satellite Tracking Station, Apartado 50727, E-28080 Madrid, Spain
5 IPAC 100-22, California Institute of Technology, Pasadena, CA 91125, USA
6 Max-Planck-Institut für Radioastronomie, Auf dem Hugel 69, D-53121 Bonn, Germany

Received 31 July 1996 / Accepted 3 September 1996

Abstract. We present maps of NGC6946 at img1.gif 61 and 205 img3.gif as well as scans through the galaxy at these and at 8 intermediate wavelengths. The bulk of the FIR luminosity arises from a diffuse disk component which extends beyond the 25 mag arcsec-2 B isophote to at least the radius corresponding to the sensitivity limit. A FIR emission counterpart to the outlying HI disk is seen at both 61 and 205 img3.gif , for which a dust to HI mass ratio of 0.0046 is inferred from the 205 img3.gif brightness assuming a dust temperature of 15 K. The disk scale length at both img1.gif 61 and 205 img3.gif is similar to that seen in R-band.

Key words: galaxies - star formation - dust

* Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, the Netherlands and the United Kingdom) and with the participation of ISAS and NASA
** affiliated to the Astrophysics Division, Space Science Department, European Space Agency

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