English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

The transition between the proto-star, Class I, and the pre-main sequencestar, Class II, phases is still one of the most uncertain, and important,stages in the knowledge of the process of formation of an individual star,because it is the stage that determines the final mass of the star. We observedthe YSO "Holoea", associated with IRAS 05327+3404, which was classified as anobject in transition between the Class I and Class II phases with severalunusual properties, and appears to be surrounded by large amounts ofcircumstellar material. We used the SMA and BIMA telescopes at millimeter andsub-millimeter wavelengths to observe the dust continuum emission and the CO(1-0) and (2-1), HCO+ (1-0) and (3-2), and HCN (1-0) transitions in the regionaround IRAS 05327+3404. We detected two continuum emission peaks at 1.1-mm: SMM1, the sub-mm counterpart of IRAS 05327+3404, and SMM 2, ~6 arcsec to the West.The emissions of the three molecules show marked differences. The CO emissionnear the systemic velocity is filtered out by the telescopes, and CO mostlytraces the high-velocity gas. The HCO+ and HCN emissions are more centrallyconcentrated around the central parts of the region, and show several intensitypeaks coincident with the sub-mm continuum peaks. We identify two mainmolecular outflows: a bipolar outflow in an E-W direction that would be poweredby SMM 1 and another one in a NE direction, which we associate with SMM 2. Wepropose that the SMM sources are probably Class I objects, with SMM 1 in anearlier evolutionary stage.

Millimetric and sub-millimetric observations of IRAS 05327+3404 "Holoea" in M36