  The HH 24-26 star-forming region within the L1630 dark cloud in Orion
contains a remarkable collection of rare Class 0 and Class I protostars,
collimated molecular and ionized jets, and a luminous but spatially unresolved
ASCA X-ray source. To study the X-ray properties of the embedded protostar
population of that region, we have obtained a deep X-ray image with the ACIS-S
camera on board the Chandra X-Ray Observatory. A number of H-alpha
emission-line objects were detected in the areas surrounding HH 24-26, of which
the weak-line T Tauri star SSV 61 was the brightest source, at a steady
luminosity of 10^31.9 erg/s (0.3-10 keV). Two Class I protostars aligned with
optical jets in HH 24, SSV 63E and SSV 63W, were also detected, as was the
continuum radio source SSV 63NE, which is very likely an extreme Class I or
Class 0 object. We observed no X rays from the Class 0 protostars HH 24-MMS and
HH 25-MMS, nor any from regions of the cloud bounded by HH 25 and HH 26, at a
2-sigma upper limit of 10^30.0 erg/s. HH 26-IR, the Class I object thought to
be the origin of the HH 26 flow, was not detected. Near-infrared spectroscopy
obtained at the NASA IRTF reveals 3 micron ice bands in the spectra of SSV 59,
63E, 63W, and HH 26-IR, and 2.3 micron CO overtone absorption bands for SSV 61.
SSV 60, which lies astride one end of the great arc of nebulosity forming HH
25, exhibits a deep infrared ice band and CO absorption, but is not an X-ray
source, and is most likely a distant background giant of late spectral type.
