Palmeirim, P., André, Ph., Kirk, J., Ward-Thompson, Derek, Arzoumanian, D., Könyves, V., Didelon, P., Schneider, N., Benedettini, M., Bontemps, S., Di Francesco, J., Elia, D., Griffin, M., Hennemann, M., Hill, T., Martin, P. G., Men’shchikov, A., Molinari, S., Motte, F., Nguyen Luong, Q., Nutter, D., Peretto, N., Pezzuto, S., Roy, A., Rygl, K. L. J., Spinoglio, L. and White, G. L. (2013) Herschel view of the Taurus B211/3 filament and striations: evidence of filamentary growth? Astronomy & Astrophysics, 550 . A38. ISSN 0004-6361
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Official URL: http://dx.doi.org/10.1051/0004-6361/201220500
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.
|Uncontrolled Keywords (separate with ;):||stars: formation; ISM: individual objects: B211; ISM: clouds; ISM: structure; evolution; submillimeter: ISM; MOLECULAR CLOUD; STAR-FORMATION; DENSE CORES; PROTOSTARS; COMPLEX; ORIGIN; AQUILA|
|Subjects:||Physical sciences > Astronomy|
|Schools:||Faculty of Science and Technology > School of Physical Sciences and Computing > Jeremiah Horrocks Institute|
|Deposited By:||Helen Cooper|
|Deposited On:||29 Jul 2014 15:10|
|Last Modified:||09 Aug 2016 15:20|
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