We have detected strong, highly variable 22.3 GHz water maser emission from the deeply embedded L1448C low-mass protostar. The total maser intensity on 1993 July 5 was 210 Jy km s~(-1) (6 x 10~(-7) solar luminosity), which is two orders of magnitude more than that expected from a protostar with a bolometric luminosity of only 9 solar luminosity. The maser kinematics cannot be fitted with a disk model. Moreover, the L1448C maser spots are perfectly aligned with the collimated molecular outflow. Therefore, we have found the first direct evidence for a connection between a water maser outflow and a molecular outflow. The closest maser spots on either side of the source are separated by only 62 AU. Thus, the wind that originates from the protostar or disk must be collimated into a dense (≈10~6 cm~(-3)) jet within 31 AU of the protostar.
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机译：我们已经从深埋的L1448C低质量原恒星中检测到强的，高度可变的22.3 GHz水激子发射。 1993年7月5日的总maser强度为210 Jy km s〜（-1）（6 x 10〜（-7）太阳光度），比原宿星的辐射强度仅2个数量级高。 9太阳光度。 maser运动学无法安装磁盘模型。此外，L1448C maser点与准直的分子流出物完全对齐。因此，我们找到了水激射流出与分子流出之间联系的第一个直接证据。源两侧的最近maser点仅相隔62 AU。因此，源自原恒星或圆盘的风必须在原恒星31 AU之内被准直成密集的（≈10〜6 cm〜（-3））射流。
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