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The W43-MM1 mini-starburst ridge, a test for star formation efficiency models

Louvet, F. and Motte, F. and Hennebelle, P. and Maury, A. and Bonnell, I. and Bontemps, S. and Gusdorf, A. and Hill, T. and Gueth, F. and Peretto, N. and Duarte-Cabral, A. and Stephan, G. and Schilke, P. and Csengeri, T. and Nguyên Luong, Q. and Lis, D. C. (2014) The W43-MM1 mini-starburst ridge, a test for star formation efficiency models. Astronomy and Astrophysics, 570 . Art. No. A15. ISSN 0004-6361. https://resolver.caltech.edu/CaltechAUTHORS:20141205-115346503

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Abstract

Context. Star formation efficiency (SFE) theories are currently based on statistical distributions of turbulent cloud structures and a simple model of star formation from cores. They remain poorly tested, especially at the highest densities. Aims. We investigate the effects of gas density on the SFE through measurements of the core formation efficiency (CFE). With a total mass of ~2 × 10^4 M_⊙, the W43-MM1 ridge is one of the most convincing candidate precursors of Galactic starburst clusters and thus one of the best places to investigate star formation. Methods. We used high-angular resolution maps obtained at 3 mm and 1 mm within the W43-MM1 ridge with the IRAM Plateau de Bure Interferometer to reveal a cluster of 11 massive dense cores, and, one of the most massive protostellar cores known. A Herschel column density image provided the mass distribution of the cloud gas. We then measured the “instantaneous” CFE and estimated the SFE and the star formation rate (SFR) within subregions of the W43-MM1 ridge. Results. The high SFE found in the ridge (~6% enclosed in ~8 pc^3) confirms its ability to form a starburst cluster. There is, however, a clear lack of dense cores in the eastern part of the ridge, which may be currently assembling. The CFE and the SFE are observed to increase with volume gas density, while the SFR per free fall time steeply decreases with the virial parameter, α_(vir). Statistical models of the SFR may describe the outskirts of the W43-MM1 ridge well, but struggle to reproduce its inner part, which corresponds to measurements at low α_(vir). It may be that ridges do not follow the log-normal density distribution, Larson relations, and stationary conditions forced in the statistical SFR models.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/1404.4843arXivDiscussion Paper
http://www.aanda.org/articles/aa/abs/2014/10/aa23603-14/aa23603-14.htmlPublisherArticle
http://dx.doi.org/10.1051/0004-6361/201423603DOIArticle
ORCID:
AuthorORCID
Lis, D. C.0000-0002-0500-4700
Additional Information:© 2014 ESO. Article published by EDP Sciences. Received 9 February 2014. Accepted 23 May 2014. Published online 07 October 2014. We thank Christoph Federrath for the fruitful discussions we had on SFR. We are grateful to Alexander Men’shchikov for help in customizing Getsources for interferometric images.
Subject Keywords:stars: formation, stars: protostars, stars: massive, ISM: clouds, submillimeter: ISM, submillimeter: stars
Record Number:CaltechAUTHORS:20141205-115346503
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20141205-115346503
Official Citation:The W43-MM1 mini-starburst ridge, a test for star formation efficiency models F. Louvet, F. Motte, P. Hennebelle, A. Maury, I. Bonnell, S. Bontemps, A. Gusdorf, T. Hill, F. Gueth, N. Peretto, A. Duarte-Cabral, G. Stephan, P. Schilke, T. Csengeri, Q. Nguyen Luong and D. C. Lis A&A 570 A15 (2014) DOI: http://dx.doi.org/10.1051/0004-6361/201423603
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:52437
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:05 Dec 2014 22:11
Last Modified:03 Oct 2019 07:42

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