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The degree to which the properties of protostars are affected by environmentremains an open question. To investigate this, we look at the Orion A and Bmolecular clouds, home to most of the protostars within 500 pc. At ~400 pc,Orion is close enough to distinguish individual protostars across a range ofenvironments in terms of both the stellar and gas projected densities. As partof the Herschel Orion Protostar Survey (HOPS), we used the Photodetector ArrayCamera and Spectrometer (PACS) to map 108 partially overlapping square fieldswith edge lengths of 5 arcmin or 8 arcmin and measure the 70 micron and 160micron flux densities of 338 protostars within them. In this paper we examinehow these flux densities and their ratio depend on evolutionary state andenvironment within the Orion complex. We show that Class 0 protostars occupy aregion of the 70 micron flux density versus 160 micron to 70 micron fluxdensity ratio diagram that is distinct from their more evolved counterparts. Wethen present evidence that the Integral-Shaped Filament (ISF) and Orion Bcontain protostars with more massive envelopes than those in the more sparselypopulated LDN 1641 region. This can be interpreted as evidence for increasingstar formation rates in the ISF and Orion B or as a tendency for more massiveenvelopes to be inherited from denser birth environments. We also providetechnical details about the map-making and photometric procedures used in theHOPS program.

The Herschel Orion Protostar Survey: Far-Infrared Photometry and Colors of Protostars and Their Variations across Orion A and B