Star Formation Rates of Massive Molecular Clouds in the Central Molecular Zone

被引：38

作者：

Lu, Xing ^{[1
]}

Zhang, Qizhou ^{[2
]}

Kauffmann, Jens ^{[3
]}

Pillai, Thushara ^{[4
]}

Ginsburg, Adam ^{[5
]}

Mills, Elisabeth A. C. ^{[6
]}

Kruijssen, J. M. Diederik ^{[7
]}

Longmore, Steven N. ^{[8
]}

Battersby, Cara ^{[9
]}

Liu, Hauyu Baobab ^{[10
]}

Gu, Qiusheng ^{[11
]}

机构：

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

[2] Harvard & Smithsonian, Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA

[3] MIT, Haystack Observ, 99 Millstone Rd, Westford, MA 01886 USA

[4] Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA

[5] Natl Radio Astron Observ, 1003 Lopezville Rd, Socorro, NM 87801 USA

[6] Brandeis Univ, Dept Phys, 415 South St, Waltham, MA 02453 USA

[7] Heidelberg Univ, Astron Rechen Inst, Zentrum Astron, Monchhofstr 12-14, D-69120 Heidelberg, Germany

[8] Liverpool John Moores Univ, Astrophys Res Inst, 146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England

[9] Univ Connecticut, Dept Phys, 2152 Hillside Rd, Storrs, CT 06269 USA

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

[11] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China

来源：

ASTROPHYSICAL JOURNAL | 2019年 / 872卷 / 02期

基金：

欧洲研究理事会; 美国国家航空航天局;

关键词：

Galaxy: center; ISM: clouds; stars: formation; WATER MASER SURVEY; GALACTIC-CENTER; METHANOL MASERS; DYNAMICAL MODEL; SAGITTARIUS-D; OH/IR STARS; MILKY-WAY; GAS; DUST; H2O;

D O I：

10.3847/1538-4357/ab017d

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We investigate star formation at very early evolutionary phases in five massive clouds in the inner 500 pc of the Galaxy, the Central Molecular Zone (CMZ). Using interferometer observations of H2O masers and ultra-compact H II regions, we find evidence of ongoing star formation embedded in cores of 0.2. pc scales and greater than or similar to 10(5) cm(-3) densities. Among the five clouds, SgrC possesses a high (9%) fraction of gas mass in gravitationally bound and/or protostellar cores, and follows the dense (greater than or similar to 10(4) cm(-3)) gas star formation relation that is extrapolated from nearby clouds. The other four clouds have less than 1% of their cloud masses in gravitationally bound and/or protostellar cores, and star formation rates 10 times lower than predicted by the dense gas star formation relation. At the spatial scale of these cores, the star formation efficiency is comparable to that in Galactic disk sources. We suggest that the overall inactive star formation in these CMZ clouds could be because there is much less gas confined in gravitationally bound cores, which may be a result of the strong turbulence in this region and/or the very early evolutionary stage of the clouds when collapse has only recently started.

引用

页数：34

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