The [FeII]1.644micron emission in M82 and NGC253: Is it a measure of the supernova rate?

Details The [FeII]1.644micron emission in M82 and NGC253: Is it a measure of the supernova rate? The [FeII]1.644micron emission in M82 and NGC253: Is it a measure of the supernova rate?

2002-12-05

arxiv.org/abs/astro-ph/0212142v1

Astronomy and Astrophysics

Astrophysics

Accepted for publication in AJ, 2003. 18 pages, 10 figures. A version of the paper with high-resolution color figures can be f

Scientific paper

10.1086/367790

We present HST/NICMOS [FeII]1.644micron, Pa-alpha (1.87micron) and continuum images of the starburst galaxies M82 and NGC253 at an unprecedented spatial resolution. In both galaxies we detect [FeII] compact sources superimposed on a diffuse background in the disk of the galaxies together with a component above and below the plane of the galaxy. The radio and [FeII] emissions perpendicular to the disk of M82 show a remarkable similarity to each other, suggesting that both emissions originate in shocks from supernova explosions. We find a spatial correspondence between bright compact [FeII] emitting regions and the location of radio supernova remnants (SNR) for approximately 30-50% of radio SNRs in M82 and NGC253. This lack of a one-to-one correspondence, more than being indicative of a different origin for the radio and [FeII] emission in starbursts, suggests two populations of SNRs: an older population(<10^4yr) traced by the [FeII] emission and a younger population (a few hundred years old) traced by the radio SNRs. We therefore conclude that the [FeII] emission in starburst galaxies provides a good estimate of the supernova activity. Using our newly determined [FeII] luminosities (corrected for extinction) of M82 and NGC253, we reevaluate the calibration of the supernova rate in terms of the [FeII] luminosity for starburst galaxies.

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