The environment of the nearest Herbig Ae star has been investigated through a program of multi‐wavelength, high contrast and high spatial resolution imagery, FUV through optical integrated light spectroscopy, and FUV spatially resolved spectroscopy. HD 104237 is the primary of a 5 Myr old aggregate of at least 4 PMS stars, 2 of which in addition to HD 104237 have IR excesses indicating the presence of dust disks. HD 104237 is actively accreting, and is driving a bipolar outflow (HH 669) which can be traced 2.65″ from the star and which is viewed at an inclination of18−11+14°. The counterjet can be traced no closer than 0.6″ (79 AU) from the star, providing a firm upper limit to the size of the disk. The absence of spatially extended H2emission, FUV reflection nebulosity, and mid‐IR PAH emission features are all consistent with dust settling and the presence of a geometrically shadowed disk. The combination of proximity, low reddening, and the high density of disks in the HD 104237 association make this group of stars an ideal laboratory for probing the comparative evolution of planetary systems. © 2004 American Institute of Physics