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dc.contributor.authorMinier, V.
dc.contributor.authorPeretto, N.
dc.contributor.authorLongmore, S.
dc.contributor.authorBurton, M.
dc.contributor.authorCesaroni, R.
dc.contributor.authorGoddi, C.
dc.contributor.authorPestalozzi, M.
dc.contributor.authorAndre, P.
dc.date.accessioned2008-03-06T17:20:34Z
dc.date.available2008-03-06T17:20:34Z
dc.date.issued2007
dc.identifier.citationMinier , V , Peretto , N , Longmore , S , Burton , M , Cesaroni , R , Goddi , C , Pestalozzi , M & Andre , P 2007 , Anatomy of the S255-S257 complex - triggered high-mass star formation . in In: Proceedings of the International Astronomical Union (Symposium 237) 2 . Cambridge University Press , pp. 160-164 . https://doi.org/10.1017/S1743921307001391
dc.identifier.otherPURE: 147432
dc.identifier.otherPURE UUID: 51cd91d8-9bbc-4532-89e9-fbd797c6c98b
dc.identifier.otherdspace: 2299/1757
dc.identifier.otherScopus: 37049013956
dc.identifier.urihttp://hdl.handle.net/2299/1757
dc.descriptionOriginal paper can be found at: http://journals.cambridge.org/ Copyright International Astronomical Union DOI : 10.1017/S1743921307001391
dc.description.abstractWe present a multi-wavelength (NIR to radio) and multi-scale (1 AU to 10 pc) study of the S255–S257 complex of young high-mass (proto)stars. The complex consists of two evolved HII regions and a molecular gas filament in which new generations of high mass stars form. Four distinct regions are identified within this dusty filament: a young NIR/optical source cluster, a massive protostar binary, a (sub)millimetre continuum and molecular clump in global collapse and a reservoir of cold gas. Interestingly, the massive binary protostellar system is detected through methanol maser and mid-IR emission at the interface between the NIR cluster and the cold gas filament. The collapsing clump is located to the north of the NIR cluster and hosts a young high-mass star associated with an outflow that is observed in mid-IR, methanol maser and radio emission. We interpret this anatomy as the possible result of triggered star formation, starting with the formation of two HII regions, followed by the compression of a molecular gas filament in which a first generation of high-mass stars forms (the NIR cluster), which then triggers the formation of high mass protostars in its near environment (the massive protostellar binary). The global collapse of the northern clump might be due to both the expansion of the HII regions that squashes the filament. In conclusion, we witness the formation of four generations of clusters of high-mass stars in S255–S257.en
dc.language.isoeng
dc.publisherCambridge University Press
dc.relation.ispartofIn: Proceedings of the International Astronomical Union (Symposium 237) 2
dc.rightsOpen
dc.titleAnatomy of the S255-S257 complex - triggered high-mass star formationen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dcterms.dateAccepted2007
rioxxterms.versionofrecordhttps://doi.org/10.1017/S1743921307001391
rioxxterms.typeOther
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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