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In the infrared, the heavily reddened LkH$alpha$ 101 is one of the brightest young stars in the sky. Situated just north of the Taurus-Auriga complex in the L1482 dark cloud, it appears to be an early B-type star that has been serendipitously exposed during a rarely observed stage of early evolution, revealing a remarkable spectrum and a directly-imaged circumstellar disk. While detailed studies of this star and its circumstellar environment have become increasingly sophisticated in the 50 years since Herbig (1956) first pointed it out, the true nature of the object still remains a mystery. Recent work has renewed focus on the young cluster of stars surrounding LkH$alpha$ 101, and what it can tell us about the enigmatic source at its center (e.g., massive star formation timescales, clustered formation mechanisms). This latter effort certainly deserves more intensive study. We describe the current knowledge of this region and point out interesting work that could be done in the future.
Observations of outflows associated with pre-main-sequence stars reveal details about morphology, binarity and evolutionary states of young stellar objects. We present molecular line data from the Berkeley-Illinois-Maryland Association array and Five
The LkH$alpha$ 101 cluster takes its name from its more massive member, the LkH$alpha$ 101star, which is an $sim15$ M$_odot$ star whose true nature is still unknown. The distance to the LkH$alpha$ 101 cluster has been controversial for the last few d
Theory predicts that giant planets and low mass stellar companions shape circumstellar disks by opening annular gaps in the gas and dust spatial distribution. For more than a decade it has been debated whether this is the dominant process that leads
Dust trapping accelerates the coagulation of dust particles, and thus it represents an initial step toward the formation of planetesimals. We report $H$-band (1.6 um) linear polarimetric observations and 0.87 mm interferometric continuum observations
In previous studies, it has been shown that the long term time average jet power, $overline{Q}$, is correlated with the spectral index in the extreme ultraviolet (EUV), $alpha_{EUV}$ (defined by $F_{ u} sim u^{-alpha_{EUV}}$ computed between 700AA,