Understanding the star formation efficiency in dense gas: Initial results from the CAFFEINE survey with ArTeMiS

被引：5

作者：

Mattern, M. ^{[1
]}

Andre, Ph. ^{[1
]}

Zavagno, A. ^{[2
,3
]}

Russeil, D. ^{[2
]}

Roussel, H. ^{[4
]}

Peretto, N. ^{[5
]}

Schuller, F. ^{[6
]}

Shimajiri, Y. ^{[7
]}

Di Francesco, J. ^{[8
,9
]}

Arzoumanian, D. ^{[10
]}

Reveret, V. ^{[1
]}

De Breuck, C. ^{[11
]}

机构：

[1] Univ Paris Cite, Univ Paris Saclay, CNRS, CEA,AIM,Lab Astrophys AIM, F-91191 Gif Sur Yvette, France

[2] Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France

[3] Inst Univ France, Paris, France

[4] Sorbonne Univ, CNRS, UMR 7095, IAP, F-75014 Paris, France

[5] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, Wales

[6] Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany

[7] Kyushu Kyoritsu Univ, 1-8 Jiyugaoka,Yahatanishi Ku, Kitakyushu, Fukuoka 8078585, Japan

[8] Natl Res Council Canada, Herzberg Astron & Astrophys Res Ctr, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada

[9] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada

[10] Natl Astron Observ Japan, Osawa 2-21-1, Mitaka, Tokyo 1818588, Japan

[11] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany

来源：

ASTRONOMY & ASTROPHYSICS | 2024年 / 688卷

关键词：

stars: formation; ISM: clouds; ISM: structure; submillimeter: ISM; YOUNG STELLAR OBJECTS; MOLECULAR CLOUDS; MASS FUNCTION; HI-GAL; FORMATION RATES; MILKY-WAY; PRESTELLAR CORES; ATOMIC-GAS; HERSCHEL; EVOLUTION;

D O I：

10.1051/0004-6361/202449908

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Despite recent progress, the question of what regulates the star formation efficiency (SFE) in galaxies remains one of the most debated problems in astrophysics. According to the dominant picture, star formation (SF) is regulated by turbulence and feedback, and the SFE is similar to 1-2% or less per local free-fall time on all scales from Galactic clouds to high-redshift galaxies. In an alternate scenario, the star formation rate (SFR) in galactic disks is linearly proportional to the mass of dense gas above some critical density threshold similar to 10(4) cm(-3). Aims. We aim to discriminate between these two pictures thanks to high-resolution submillimeter and mid-infrared imaging observations, which trace both dense gas and young stellar objects (YSOs) for a comprehensive sample of 49 nearby massive SF complexes out to a distance of d similar to 3 kpc in the Galactic disk. Methods. We used data from CAFFEINE, a complete 350/450 mu m survey with APEX/ArTeMiS of the densest portions of all southern molecular clouds at d less than or similar to 3 kpc, in combination with Herschel data to produce column density maps at a factor of similar to 4 higher resolution (8 '') than standard Herschel column density maps (36 ''). Our maps are free of any saturation effect around luminous high-mass pro-tostellar objects and resolve the structure of dense gas and the typical similar to 0.1 pc width of molecular filaments out to 3 kpc, which is the most important asset of the present study and is impossible to achieve with Herschel data alone. Coupled with SFR estimates derived from Spitzer mid-infrared observations of the YSO content of the same clouds, this allowed us to study the dependence of the SFE on density in the CAFFEINE clouds. We also combine our findings with existing SF efficiency measurements in nearby clouds to extend our analysis down to lower column densities. Results. Our results suggest that the SFE does not increase with density above the critical threshold and support a scenario in which the SFE in dense gas is approximately constant (independent of free-fall time). However, the SF efficiency measurements traced by Class I YSOs in nearby clouds are more inconclusive, since they are consistent with both the presence of a density threshold and a dependence on density above the threshold. Overall, we suggest that the SF efficiency in dense gas is primarily governed by the physics of filament fragmentation into protostellar cores.

引用

页数：21

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