Characterizing the Youngest Herschel-detected Protostars II. Molecular
  Outflows from the Millimeter and the Far-infrared
  We present CARMA CO (J=1-0) observations and Herschel PACS spectroscopy,
characterizing the outflow properties toward extremely young and deeply
embedded protostars in the Orion molecular clouds. The sample comprises a
subset of the Orion protostars known as the PACS Bright Red Sources (PBRS)
(Stutz et al. 2013). We observed 14 PBRS with CARMA and 8 of these 14 with
Herschel, acquiring full spectral scans from 55 micron to 200 micron. Outflows
are detected in CO (J=1-0) from 8 of 14 PBRS, with two additional tentative
detections; outflows are also detected from the outbursting protostar HOPS 223
(V2775 Ori) and the Class I protostar HOPS 68. The outflows have a range of
morphologies, some are spatially compact, <10000 AU in extent, while others
extend beyond the primary beam. The outflow velocities and morphologies are
consistent with being dominated by intermediate inclination angles (80 deg > i
> 20 deg). This confirms the interpretation of the very red 24 micron to 70
micron colors of the PBRS as a signpost of high envelope densities, with only
one (possibly two) cases of the red colors resulting from edge-on inclinations.
We detect high-J (J_up > 13) CO lines and/or H_2O lines from 5 of 8 PBRS and
only for those with detected CO outflows. The far-infrared CO rotation
temperatures of the detected PBRS are marginally colder (~230 K) than those
observed for most protostars (~300 K), and only one of these 5 PBRS has
detected [OI] 63 micron emission. The high envelope densities could be
obscuring some [OI] emission and cause a ~20 K reduction to the CO rotation
temperatures.
