Abstract
Analysis of high spatial resolution VLA images shows that the free–free emission from NGC 7538 IRS 1 is dominated by a collimated ionized wind. We have re-analyzed high angular resolution VLA archive data from 6 cm to 7 mm, and measured separately the flux density from the compact bipolar core and the extended (15–3'') lobes. We find that the flux density of the core is ∝να, where ν is the frequency and α is ∼0.7. The frequency dependence of the total flux density is slightly steeper with α = 0.8. A massive optically thick hypercompact core with a steep density gradient can explain this frequency dependence, but it cannot explain the extremely broad recombination line velocities observed in this source. Neither can it explain why the core is bipolar rather than spherical, nor the observed decrease of 4% in the flux density in less than 10 yr. An ionized wind modulated by accretion is expected to vary, because the accretion flow from the surrounding cloud will vary over time. BIMA and CARMA continuum observations at 3 mm show that the free–free emission still dominates at 3 mm. HCO+ J = 1 → 0 observations combined with FCRAO single dish data show a clear inverse P Cygni profile toward IRS 1. These observations confirm that IRS 1 is heavily accreting with an accretion rate ∼2 × 10−4 M☉ yr−1.
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