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 dustemission 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 < 5 × 1023 cm-2. We determined the ratio of the 2:2 μm extinction coefficient to the 850 μm 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*∝ Σβgas, with β 2. © ESO, 2014.
Herschel-Planck dust optical-depth and column-density maps : I. Method description and results for Orion / M. Lombardi, H. Bouy, J. Alves, C.J. Lada. - In: ASTRONOMY & ASTROPHYSICS. - ISSN 0004-6361. - 566:(2014). [10.1051/0004-6361/201323293]
Herschel-Planck dust optical-depth and column-density maps : I. Method description and results for Orion
M. LombardiPrimo
;
2014
Abstract
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 dustemission 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 < 5 × 1023 cm-2. We determined the ratio of the 2:2 μm extinction coefficient to the 850 μm 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*∝ Σβgas, with β 2. © ESO, 2014.File | Dimensione | Formato | |
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