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; D. C. Lis

doi:10.1051/0004-6361/201423603

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, D. C. Lis

^*Corresponding author for this work

School of Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

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 similar to 2 x 10⁴ 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 pc³) 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.

Original language	English
Article number	15
Number of pages	10
Journal	Astronomy & Astrophysics
Volume	570
Early online date	7 Oct 2014
DOIs	https://doi.org/10.1051/0004-6361/201423603
Publication status	Published - Oct 2014

Keywords

stars: formation
stars: protostars
stars: massive
ISM: clouds
submillimeter: ISM
submillimeter: stars
Nearby molecular clouds
Young stellar objects
G30.79 FIR 10
CYGNUS-X
Initial-highlights
Massive protostars
Prestellar cores
Earliest phases
Magnetic-fields
Forming complex

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Bonnell_2014_A&A_TheW43
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Astrophysics at St Andrews:2012 - 2014: Astrophysics at St Andrews: 2012 - 2014
Horne, K. D. (PI)
Science & Technology Facilities Council
1/10/11 → 31/03/12
Project: Standard

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Louvet, F., Motte, F., Hennebelle, P., Maury, A., Bonnell, I., Bontemps, S., Gusdorf, A., Hill, T., Gueth, F., Peretto, N., Duarte-Cabral, A., Stephan, G., Schilke, P., Csengeri, T., Luong, Q. N., & Lis, D. C. (2014). The W43-MM1 mini-starburst ridge, a test for star formation efficiency models. Astronomy & Astrophysics, 570, Article 15. https://doi.org/10.1051/0004-6361/201423603

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

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 similar to 2 x 104 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 pc3) 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, αvir. 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 αvir. It may be that ridges do not follow the log-normal density distribution, Larson relations, and stationary conditions forced in the statistical SFR models.",

keywords = "stars: formation, stars: protostars, stars: massive, ISM: clouds, submillimeter: ISM, submillimeter: stars, Nearby molecular clouds, Young stellar objects, G30.79 FIR 10, CYGNUS-X, Initial-highlights, Massive protostars, Prestellar cores, Earliest phases, Magnetic-fields, Forming complex",

author = "F. Louvet and F. Motte and P. Hennebelle and A. Maury and I. Bonnell and S. Bontemps and A. Gusdorf and T. Hill and F. Gueth and N. Peretto and A. Duarte-Cabral and G. Stephan and P. Schilke and T. Csengeri and Luong, {Q. Nguyen} and Lis, {D. C.}",

year = "2014",

month = oct,

doi = "10.1051/0004-6361/201423603",

language = "English",

volume = "570",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = "EDP SCIENCES S A",

}

TY - JOUR

T1 - The W43-MM1 mini-starburst ridge, a test for star formation efficiency models

AU - Louvet, F.

AU - Motte, F.

AU - Hennebelle, P.

AU - Maury, A.

AU - Bonnell, I.

AU - Bontemps, S.

AU - Gusdorf, A.

AU - Hill, T.

AU - Gueth, F.

AU - Peretto, N.

AU - Duarte-Cabral, A.

AU - Stephan, G.

AU - Schilke, P.

AU - Csengeri, T.

AU - Luong, Q. Nguyen

AU - Lis, D. C.

PY - 2014/10

Y1 - 2014/10

N2 - 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 similar to 2 x 104 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 pc3) 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, αvir. 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 αvir. It may be that ridges do not follow the log-normal density distribution, Larson relations, and stationary conditions forced in the statistical SFR models.

AB - 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 similar to 2 x 104 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 pc3) 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, αvir. 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 αvir. It may be that ridges do not follow the log-normal density distribution, Larson relations, and stationary conditions forced in the statistical SFR models.

KW - stars: formation

KW - stars: protostars

KW - stars: massive

KW - ISM: clouds

KW - submillimeter: ISM

KW - submillimeter: stars

KW - Nearby molecular clouds

KW - Young stellar objects

KW - G30.79 FIR 10

KW - CYGNUS-X

KW - Initial-highlights

KW - Massive protostars

KW - Prestellar cores

KW - Earliest phases

KW - Magnetic-fields

KW - Forming complex

U2 - 10.1051/0004-6361/201423603

DO - 10.1051/0004-6361/201423603

M3 - Article

SN - 0004-6361

VL - 570

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

M1 - 15

ER -

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

Abstract

Keywords

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Astrophysics at St Andrews:2012 - 2014: Astrophysics at St Andrews: 2012 - 2014

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