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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 710034.0, MPI für Astronomie / Publikationen_mpia
Class 0 protostars in the Perseus molecular cloud: A correlation between the youngest protostars and the dense gas distribution
Authors:Sadavoy, S. I.; Di Francesco, J.; André, P.; Pezzuto, S.; Bernard, J. -. P.; Maury, A.; Men'shchikov, A.; Motte, F.; Nguy, nullval; tilde, nullval; ên-Lu'o'ng, Q.; Schneider, N.; Arzoumanian, D.; Benedettini, M.; Bontemps, S.; Elia, D.; Hennemann, M.; Hill, T.; Könyves, V.; Louvet, F.; Peretto, N.; Roy, A.; White, G. J.
Date of Publication (YYYY-MM-DD):2014
Title of Journal:The Astrophysical Journal Letters
Issue / Number:2
Start Page:id. L18 (6 pp)
Audience:Not Specified
Abstract / Description:We use PACS and SPIRE continuum data at 160 mum, 250 mum, 350 mum, and 500 mum from the Herschel Gould Belt Survey to sample seven clumps in Perseus: B1, B1-E, B5, IC 348, L1448, L1455, and NGC 1333. Additionally, we identify and characterize the embedded Class 0 protostars using detections of compact Herschel sources at 70 mum as well as archival Spitzer catalogs and SCUBA 850 mum photometric data. We identify 28 candidate Class 0 protostars, four of which are newly discovered sources not identified with Spitzer. We find that the star formation efficiency of clumps, as traced by Class 0 protostars, correlates strongly with the flatness of their respective column density distributions at high values. This correlation suggests that the fraction of high column density material in a clump reflects only its youngest protostellar population rather than its entire source population. We propose that feedback from either the formation or evolution of protostars changes the local density structure of clumps.
Free Keywords:dust; extinction; ISM: individual objects: Perseus; stars: formation; stars: protostars
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0004-637X %R 10.1088/2041-8205/787/2/L18
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