The Extraordinary Outburst in the Massive Protostellar System NGC6334I-MM1: Strong Increase in Mid-Infrared Continuum Emission

Abstract

In recent years, dramatic outbursts have been identified toward massive protostars via infrared and millimeter dust continuum and molecular maser emission. The longest lived outburst ($>6$ yr) persists in NGC6334I-MM1, a deeply-embedded object with no near-IR counterpart. Using FORCAST and HAWC+ on SOFIA, we have obtained the first mid-infrared images of this field since the outburst began. Despite being undetected in pre-outburst ground-based 18 $\mu$m images, MM1 is now the brightest region at all three wavelengths (25, 37, and 53 $\mu$m), exceeding the ultracompact HII region MM3 (NGC6334F). Combining the SOFIA data with ALMA imaging at four wavelengths, we construct a spectral energy distribution of the combination of MM1 and the nearby hot core MM2. The best-fit Robitaille radiative transfer model yields a luminosity of $(4.9\pm 0.8)\times 10^4{L}_{\odot }$. Accounting for an estimated pre-outburst luminosity ratio MM1:MM2 = $2.1\pm 0.4$, the luminosity of MM1 has increased by a factor of $16.3\pm 4.4$. The pre-outburst luminosity implies a protostar of mass 6.7 $M_{\odot }$, which can produce the ionizing photon rate required to power the pre-outburst hypercompact HII region surrounding the likely outbursting protostar MM1B. The total energy and duration of the outburst exceed the S255IR-NIRS3 outburst by a factor of $\gtrsim 3$, suggesting a different scale of event involving expansion of the protostellar photosphere (to $\gtrsim$ 20 $R_{\odot }$), thereby supporting a higher accretion rate ($\gtrsim$0.0023 $M_{\odot }$ yr${}^{-1}$) and reducing the ionizing photon rate. In the grid of hydrodynamic models of Meyer et al. 2021, the combination of outburst luminosity and magnitude (3) places the NGC6334I-MM1 event in the region of moderate total accretion ($\sim$0.1-0.3 $M_{\odot }$) and hence long duration ($\sim$40-130 yr).

arXiv comment11 pages, 3 figures, 2 tables; accepted for publication in The Astrophysical Journal Letters

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