An SMA and HERSCHEL view of the HMSFR G23.01-0.41

Abstract

We present here the results of our recent SMA observations at 1.3 mm toward the high-mass star-forming region (HMSFR) G23.01-0.41, with both the most extended and compact array configurations, providing sub-arcsecond and high sensitivity maps for different molecular lines (e.g., 12CO and isotopomers, SiO, CH3CN, and CH3OH). We also complement this dataset with the spectral energy distribution (SED) between 3.4 μm and 1.1 mm and the continuum images from the Hi-GAL/Herschel survey. The aim of these observations is twofold: 1) to image at high angular and spectral resolution the flattened, hot molecular core (HMC) detected toward G23.01-0.41, which contains strong masers and a radio continuum source; 2) to compare the spatial distribution and velocity field of the gas close to the central YSO with those of the associated molecular outflow. The dust and molecular line emission trace a flattened structure inside a radius of 8000 AU from the center of radio continuum and maser line emission in the region. The equatorial plane of this HMC is strictly perpendicular to the main elongation of the outflow emission onto the plane of the sky, which extends over a ten times larger region (~0.5 pc). The inner velocity field mapped with the CH3CN (12K-11K) lines outlines that molecular gas rotates about the outflow axis and is simultaneously dragged along the outflow direction indicating Hubble-law expansion. The IR SED from the HMC suggests the presence of a single O9.5 ZAMS star with a mass ~19 M⊙, consistent with the mass required for centrifugal equilibrium.