Herschel view of the Taurus B211/3 filament and striations: evidence of filamentary growth?

被引：439

作者：

Palmeirim, P. ^{[1
]}

Andre, Ph. ^{[1
]}

Kirk, J. ^{[2
]}

Ward-Thompson, D. ^{[3
]}

Arzoumanian, D. ^{[1
]}

Koenyves, V. ^{[1
,4
]}

Didelon, P. ^{[1
]}

Schneider, N. ^{[1
,5
]}

Benedettini, M. ^{[6
]}

Bontemps, S. ^{[5
]}

Di Francesco, J. ^{[7
,8
]}

Elia, D. ^{[6
]}

Griffin, M. ^{[2
]}

Hennemann, M. ^{[1
]}

Hill, T. ^{[1
]}

Martin, P. G. ^{[9
]}

Men'shchikov, A. ^{[1
]}

Molinari, S. ^{[6
]}

Motte, F. ^{[1
]}

Luong, Q. Nguyen ^{[9
]}

Nutter, D. ^{[2
]}

Peretto, N. ^{[1
]}

Pezzuto, S. ^{[6
]}

Roy, A. ^{[9
]}

Rygl, K. L. J. ^{[6
]}

Spinoglio, L. ^{[6
]}

White, G. L. ^{[10
,11
]}

机构：

[1] CEA DSM CNRS Univ Paris Diderot, CEA Saclay, IRFU Serv Astrophys, Lab AIM, F-91191 Gif Sur Yvette, France

[2] Cardiff Univ, Sch Phys & Astron, Cardiff CF29 3AA, S Glam, Wales

[3] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England

[4] Univ Paris 11, CNRS, UMR 8617, Inst Astrophys Spatiale, F-91405 Orsay, France

[5] Univ Bordeaux, CNRS INSU, UMR 5804, Lab Astrophys Bordeaux, F-33271 Floirac, France

[6] INAF IAPS, I-00133 Rome, Italy

[7] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada

[8] Univ Victoria, Dept Phys & Astron, STN CSC, Victoria, BC V8W 3P6, Canada

[9] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada

[10] STFC Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England

[11] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England

来源：

ASTRONOMY & ASTROPHYSICS | 2013年 / 550卷

关键词：

stars: formation; ISM: individual objects: B211; ISM: clouds; ISM: structure; evolution; submillimeter: ISM; MOLECULAR CLOUD; STAR-FORMATION; DENSE CORES; PROTOSTARS; ORIGIN; AQUILA;

D O I：

10.1051/0004-6361/201220500

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present first results from the Herschel Gould Belt survey for the B211/L1495 region in the Taurus molecular cloud. Thanks to their high sensitivity and dynamic range, the Herschel images reveal the structure of the dense, star-forming filament B211 with unprecedented detail, along with the presence of striations perpendicular to the filament and generally oriented along the magnetic field direction as traced by optical polarization vectors. Based on the column density and dust temperature maps derived from the Herschel data, we find that the radial density profile of the B211 filament approaches power-law behavior, rho proportional to r(-2.0 +/- 0.4), at large radii and that the temperature profile exhibits a marked drop at small radii. The observed density and temperature profiles of the B211 filament are in good agreement with a theoretical model of a cylindrical filament undergoing gravitational contraction with a polytropic equation of state: P proportional to rho(gamma) and T proportional to rho(gamma-1), with gamma = 0.97 +/- 0.01 < 1 (i.e., not strictly isothermal). The morphology of the column density map, where some of the perpendicular striations are apparently connected to the B211 filament, further suggests that the material may be accreting along the striations onto the main filament. The typical velocities expected for the infalling material in this picture are similar to 0.5-1 km s(-1), which are consistent with the existing kinematical constraints from previous CO observations.

引用

页数：9

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