A Galactic survey of radio jets from massive protostars

Abstract

In conjunction with a previous southern-hemisphere work, we present the largest radio survey of jets from massive protostars to date with high-resolution, ($\sim 0.04^{\prime \prime }$) VLA observations towards two subsamples of massive star-forming regions of different evolutionary statuses: 48 infrared-bright, massive YSOs and 8 IRDCs containing 16 luminous (${\mathrm{L}}_{\mathrm{bol}}>10^3{\mathrm{L}}_{\odot }$) cores. For $94\%$ of the MYSO sample we detect thermal radio ($\alpha \ge -0.1$ whereby $S_{\nu }\propto {\nu }^{\alpha }$) sources coincident with the protostar, of which $84\%$ (13 jets and 25 candidates) are jet-like. Radio luminosity is found to scale with ${\mathrm{L}}_{\mathrm{bol}}$ similarly to the low-mass case supporting a common mechanism for jet production across all masses. Associated radio lobes tracing shocks are seen towards $52\%$ of jet-like objects and are preferentially detected towards jets of higher radio and bolometric luminosities, resulting from our sensitivity limitations. We find jet mass loss rate scales with bolometric luminosity as ${\dot{m}}_{\mathrm{jet}}\propto {{\mathrm{L}}_{\mathrm{bol}}}^{0.9\pm 0.2}$, thereby discarding radiative, line-driving mechanisms as the dominant jet-launching process. Calculated momenta show that the majority of jets are mechanically capable of driving the massive, molecular outflow phenomena since $p_{\mathrm{jet}}>p_{\mathrm{outflow}}$. Finally, from their physical extent we show that the radio emission can not originate from small, optically-thick \textsc{Hii} regions. Towards the IRDC cores, we observe increasing incidence rates/radio fluxes with age using the proxy of increasing luminosity-to-mass $\left(\frac{L}{M}\right)$ and decreasing infrared flux ratios $\left(\frac{S_{70\mu \mathrm{m}}}{S_{24\mu \mathrm{m}}}\right)$. Cores with $\frac{L}{M}<40{\mathrm{L}}_{\mathrm{sol}}{{\mathrm{M}}_{\mathrm{sol}}}^{-1}$ are not detected above ($5.8\mathrm{GHz}$) radio luminosities of $\sim 1{\mathrm{mJy}\mathrm{kpc}}^2$.

arXiv commentTo be published in MNRAS. 20 pages main text (4 tables, 14 figures), 90 pages appendices (6 tables, 66 figures)

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