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We present Chandra-HETGS observations of the Herbig Ae star HD 104237 and theassociated young stars comprising lower mass stars, in the 0.15-1.75\msol massrange, in their pre-main sequence phase. The brightest X-ray source in theassociation is the central system harboring the Herbig Ae primary, and a K3companion. Its X-ray variability indicates modulation possibly on time scalesof the rotation period of the Herbig Ae star, and this would imply that theprimary significantly contributes to the overall emission. The spectrum of theHerbig Ae+K3 system shows a soft component significantly more pronounced thanin other K-type young stars. This soft emission is reminiscent of the unusuallysoft spectra observed for the single Herbig Ae stars HD 163296 and AB Aur, andtherefore we tentatively attribute it to the Herbig Ae of the binary system.The HETGS spectrum shows strong emission lines corresponding to a wide range ofplasma temperatures. The He-like triplet of MgXI and NeIX suggest the presenceof plasma at densities of about $10^{12}$ cm$^{-3}$, possibly indicatingaccretion related X-ray production mechanism.  The analysis of the zero-order spectra of the other sources indicates X-rayemission characteristics typical of pre-main sequence stars of similar spectraltype, with the exception of the T Tauri HD104237-D, whose extremely softemission is very similar to the emission of the classical T Tauri star TW Hya,and suggests X-ray production by shocked accreting plasma.

X-ray Emission from Young Stellar Objects in the \epsilon Chamaeleontis Group: the Herbig Ae Star HD 104237 and Associated Low-Mass Stars