Volume 566, June 2014
|Number of page(s)||19|
|Section||Interstellar and circumstellar matter|
|Published online||09 June 2014|
Herschel-Planck dust optical-depth and column-density maps
I. Method description and results for Orion
University of MilanDepartment of Physics, via Celoria 16, 20133
2 Centro de Astrobiología, INTA-CSIC, PO Box 78, 28691 Villanueva de la Cañada, Madrid, Spain
3 University of Vienna, Türkenschanzstrasse 17, 1180 Vienna, Austria
4 Harvard-Smithsonian Center for Astrophysics, Mail Stop 72, 60 Garden Street, Cambridge, MA 02138, U.S.A.
Accepted: 25 March 2014
We present high-resolution, high dynamic range column-density and color-temperature maps of the Orion complex using a combination of Planck dust-emission maps, Herschel dust-emission maps, and 2MASS NIR dust-extinction maps. The column-density maps combine the robustness of the 2MASS NIR extinction maps with the resolution and coverage of the Herschel and Planck dust-emission maps and constitute the highest dynamic range column-density maps ever constructed for the entire Orion complex, covering 0.01 mag < AK < 30 mag, or 2 × 1020 cm-2 < N < 2 × 1023 cm-2. We determined the ratio of the 2.2 μm extinction coefficient to the 850μm opacity and found that the values obtained for both Orion A and B are significantly lower than the predictions of standard dust models, but agree with newer models that incorporate icy silicate-graphite conglomerates for the grain population. We show that the cloud projected probability distribution function, over a large range of column densities, can be well fitted by a simple power law. Moreover, we considered the local Schmidt-law for star formation, and confirm earlier results, showing that the protostar surface density Σ∗ follows a simple law Σ∗ ∝ Σgasβ, with β ~ 2.
Key words: ISM: clouds / dust, extinction / ISM: structure / ISM: individual objects: Orion molecular cloud
© ESO, 2014
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