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Intermediate mass protostars, the bridge between the very common solar-likeprotostars and the more massive, but rarer, O and B stars, can only be studiedat high physical spatial resolutions in a handful of clouds. In this paper wepresent and analyze the continuum results from an observing campaign at theSubmillimeter Array targeting two well-studied intermediate mass protostars inOrion, NGC 2071 and L1641 S3 MMS 1. The extended SMA (eSMA) probes structure atangular resolutions up to 0.2", revealing protostellar disks on scales of 200AU. Continuum flux measurements on these scales indicate that a significantamount of mass, a few tens of M{\odot}, are present. Envelope, stellar, anddisk masses are derived using both compact, extended and eSMA configurationsand compared against SED-fitting models. We hypothesize that fragmentation intothree components occurred within NGC 2071 at an early time, when the envelopeswere less than 10% of their current masses, e.g. < 0.5 M{\odot}. Nofragmentation occurred for L1641 S3 MMS 1. For NGC 2071 evidence is given thatthe bulk of the envelope material currently around each source was accretedafter the initial fragmentation. In addition, about 30% of the total core massis not yet associated to one of the three sources. A global accretion model isfavored and a potential accretion history of NGC 2071 is presented. It is shownthat the relatively low level of fragmentation in NGC 2071 was stifled comparedto the expected fragmentation from a Jean's argument.

The Small-Scale Physical Structure and Fragmentation Difference of Two Embedded Intermediate Mass Protostars in Orion