CLASS 0 PROTOSTARS IN THE PERSEUS MOLECULAR CLOUD: A CORRELATION BETWEEN THE YOUNGEST PROTOSTARS AND THE DENSE GAS DISTRIBUTION

Journal Article · Sun Jun 01 00:00:00 EDT 2014 · Astrophysical Journal Letters

DOI:https://doi.org/10.1088/2041-8205/787/2/L18· OSTI ID:22365832

Sadavoy, S. I.; Di Francesco, J. ^[1]; André, Ph.; Maury, A.; Men'shchikov, A.; Motte, F.; Hennemann, M.; Könyves, V.; Louvet, F.; Roy, A. ^[2]; Pezzuto, S.; Benedettini, M.; Elia, D. ^[3]; Bernard, J. -P. ^[4]; Nguyên-Lu'o'ng, Q. ^[5]; Schneider, N.; Bontemps, S. ^[6]; Arzoumanian, D. ^[7]; Hill, T. ^[8]; others, and

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1. Department of Physics and Astronomy, University of Victoria, P.O. Box 355, STN CSC, Victoria, BC, V8W 3P6 (Canada)
2. Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot, IRFU/Service dAstrophysique, Saclay, F-91191 Gif-sur-Yvette (France)
3. Istituto di Astrofisica e Planetologia Spaziali, Via Fosso del Cavaliere 100, I-00133 Rome (Italy)
4. CNRS, IRAP, 9 Av. Colonel Roche, BP 44346, F-31028 Toulouse Cedex 4 (France)
5. Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON, M5S 3H8 (Canada)
6. Université de Bordeaux, LAB, UMR 5804, F-33270 Floirac (France)
7. IAS, CNRS (UMR 8617), Université Paris-Sud 11, Bâtiment 121, F-91400 Orsay (France)
8. Joint ALMA Observatory, Alonso de Cordova 3107, Vitacura 763-0355, Santiago (Chile)

We use PACS and SPIRE continuum data at 160 μm, 250 μm, 350 μm, and 500 μm 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 μm as well as archival Spitzer catalogs and SCUBA 850 μm 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.

• OSTI ID: 22365832
• Journal Information: Astrophysical Journal Letters, Vol. 787, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 2041-8205
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
CLOUDS
COSMIC DUST
DENSITY
DETECTION
EFFICIENCY
FEEDBACK
PROTOSTARS
STAR CLUSTERS
STAR EVOLUTION
STARS