Erratum: ``A Spectroscopic Study of the Star-forming Properties of the Center of NGC 4194'' (AJ, 131, 282 [2006])

Astronomy and Astrophysics – Astronomy

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The masses in Table 5, columns (2)-(5), are not the total masses. The masses are actually for stars from 1 to 100 Msolar. To include stars from 0.1 to 1 Msolar the reported masses should be multiplied by a factor of ~2 (see Weistrop et al. 2004). For example, the knots in common with Weistrop et al. (2004) have a median mass of 7.2×106 Msolar when this factor of ~2 is taken into account.
The model we called TIMF (upper cutoff of 30 Msolar) is actually a model with an IMF slope of 3.3 and mass range of 1-100 Msolar. See the 2006 February 8 entry in the Knowledge Base section of the Starburst99 Web site for details. One of our original goals was to determine whether or not the knots formed stars >30 Msolar. An IMF with a slope of 3.3 will have fewer O stars than one with a Salpeter slope. The knots best modeled with TIMF probably have fewer high-mass stars than the knot best modeled with SIMF, but we cannot say that they have no stars more massive than 30 Msolar. Our result is still suggestive, but more work is needed.
We thank C. Leitherer for his help in clarifying these points.

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