The physical conditions in IRDC clumps from Herschel/HIFI observations of H2O

被引：9
|
作者：
Shipman, R. F. [1 ,2 ]
van der Tak, F. F. S. [1 ,2 ]
Wyrowski, F. [3 ]
Herpin, F. [4 ,5 ]
Frieswijk, W. [6 ]
机构：
[1] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands
[2] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands
[3] Max Planck Inst Radioastron, D-53010 Bonn, Germany
[4] Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France
[5] CNRS, UMR 5804, LAB, F-33270 Floirac, France
[6] ASTRON Netherlands Inst Radio Astron, NL-7991 PD Dwingeloo, Netherlands
来源：
ASTRONOMY & ASTROPHYSICS | 2014年 / 570卷
关键词：
stars: formation; stars: massive; ISM: clouds; evolution; INFRARED-DARK CLOUD; STAR-FORMING REGIONS; HIGH-MASS PROTOSTARS; HIERARCHICAL FRAGMENTATION; WATER-ABSORPTION; MOLECULAR LINE; KEY PROGRAM; HIFI; G28.34+0.06; G11.11-0.12;
D O I：
10.1051/0004-6361/201423912
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
Context. The earliest phases of high-mass star formation are poorly understood. Aims. Our goal is to determine the physical conditions and kinematic structure of massive starforming cloud clumps. Methods. We analyse H2O 557 GHz line profiles observed with HIFI toward four positions in two infrared-dark cloud clumps. By comparison with ground-based (CO)-O-17, N2H+, CH3OH, and NH3 line observations, we constrain the volume density and kinetic temperature of the gas and estimate the column density and abundance of H2O and N2H+. Results. The observed water lines are complex with emission and absorption components. The absorption is redshifted and consistent with a cold envelope, while the emission is interpreted as resulting from proto-stellar outflows. The gas density in the clumps is similar to 10(7) cm(-3). The o-H2O outflow column density is 0.3-3.0 x 10(14) cm(2). The o-H2O absorption column density is between 1.5 x 10(14) and 2.6 x 10(15) cm(2) with cold o-H2O abundances between 1.5 x 10(-9) and 3.1 x 10(-8). Conclusions. All clumps have high gas densities (similar to 10(7) cm(3)) and display infalling gas. Three of the four clumps have outflows. The clumps form an evolutionary sequence as probed by H2O N2H+, NH3, and CH3OH. We find that G28-MM is the most evolved, followed by G11-MM and then G28-NH3. The least evolved clump is G11-NH3 which shows no signposts of starformation; G11-NH3 is a high-mass pre-stellar core.
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页数：14
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