20 research outputs found

    Hot gas and dust in a protostellar cluster near W3(OH

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    We used the IRAM Interferometer to obtain sub-arcsecond resolution observations of the high-mass star-forming region W3(OH) and its surroundings at a frequency of 220 GHz. With the improved angular resolution, we distinguish 3 peaks in the thermal dust continuum emission originating from the hot core region about 6 arcsec (0.06 pc) east of W3(OH). The dust emission peaks are coincident with known radio continuum sources, one of which is of non-thermal nature. The latter source is also at the center of expansion of a powerful bipolar outflow observed in water maser emission. We determine the hot core mass to be 15 solar masses based on the integrated dust continuum emission. Simultaneously many molecular lines are detected allowing the analysis of the temperature structure and the distribution of complex organic molecules in the hot core. From HNCO lines, spanning a wide range of excitation, two 200 K temperature peaks are found coincident with dust continuum emission peaks suggesting embedded heating sources within them.Comment: 12 pages, 3 figure

    Forming an Early O-type Star Through Gas Accretion?

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    We present high angular resolution (\sim 3'') and sensitive 1.3 mm continuum, cyanogen (CN) and vinyl cyanide (C2_2H3_3CN) line observations made with the Submillimeter Array (SMA) toward one of most highly obscured objects of the W51 IRS2 region, W51 North. We find that the CN line exhibits a pronounced inverse P-Cygni profile indicating that the molecular gas is infalling inwards this object with a mass accretion rate between 4 and 7 ×\times 102^{-2} M_\odot yr1^{-1}. The C2_2H3_3CN traces an east-west rotating molecular envelope that surrounds either a single obscured (proto)star with a kinematic mass of 40 M_{\odot} or a small central cluster of B-type stars and that is associated with a compact high velocity bipolar outflow traced by H2_2O masers and SiO molecular emission. We thus confirm that the W51 North region is part of the growing list of young massive star forming regions that have been associated with infalling motions and with large mass accretion rates (\sim 102^{-2} -- 104^{-4}), strengthening the evidence for massive stars forming with very high accretion rates sufficient to quench the formation of an UCHII region.Comment: Accepted by Astronomy and Astrophysics Letter

    A ring/disk/outflow system associated with W51 North: a very massive star in the making

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    Sensitive and high angular resolution (\sim 0.4\arcsec) SO2_2[222,20_{2,20} \to 221,21_{1,21}] and SiO[5\to4] line and 1.3 and 7 mm continuum observations made with the Submillimeter Array (SMA) and the Very Large Array (VLA) towards the young massive cluster W51 IRS2 are presented. We report the presence of a large (of about 3000 AU) and massive (40 M_\odot) dusty circumstellar disk and a hot gas molecular ring around a high-mass protostar or a compact small stellar system associated with W51 North. The simultaneous observations of the silicon monoxide molecule, an outflow gas tracer, further revealed a massive (200 M_\odot) and collimated (14\sim14^\circ) outflow nearly perpendicular to the dusty and molecular structures suggesting thus the presence of a single very massive protostar with a bolometric luminosity of more than 105^5 L_\odot. A molecular hybrid LTE model of a Keplerian and infalling ring with an inner cavity and a central stellar mass of more than 60 M_\odot agrees well with the SO2_2[222,20_{2,20} \to 221,21_{1,21}] line observations. Finally, these results suggest that mechanisms, such as mergers of low- and intermediate- mass stars, might be not necessary for forming very massive stars.Comment: Accepted by The Astrophysical Journa
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