Volume 572, December 2014
|Number of page(s)||30|
|Section||Interstellar and circumstellar matter|
|Published online||20 November 2014|
Dust properties inside molecular clouds from coreshine modeling and observations ⋆
1 LERMA & UMR8112 du CNRS, Observatoire de Paris, 61, Av. de l’Observatoire, 75014 Paris, France
2 Department of Physics, PO Box 64, University of Helsinki 00014, Finland
3 Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, USA
4 GEPI Observatoire de Paris, CNRS, Université Paris Diderot, Place Jules Janssen, 92190 Meudon, France
5 Laboratoire d’Astrophysique Instrumentation Modelisation (AIM) Paris-Saclay, CEA Saclay, 91191 Gif-sur-Yvette, France
6 Université Grenoble Alpes, IPAG, 38000 Grenoble, France
7 CNRS, IPAG, 38000 Grenoble, France
8 Université de Toulouse, UPS-OMP, IRAP, 31028 Toulouse Cedex 4, France
9 CNRS, IRAP, 9 Av. colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France
10 Space Telescope Science Institute, Baltimore, MD, 21218, USA
11 Finnish Centre for astronomy with ESO, University of Turku, Väisäläntie 20, 21500 Piikkiö, Finland
Received: 28 April 2014
Accepted: 16 July 2014
Context. Using observations to deduce dust properties, grain-size distribution, and physical conditions in molecular clouds is a highly degenerate problem.
Aims. The coreshine phenomenon, a scattering process at 3.6 and 4.5 μm that dominates absorption, has revealed its ability to explore the densest parts of clouds. We use this effect to constrain the dust parameters. The goal is to investigate to what extent grain growth (at constant dust mass) inside molecular clouds is able to explain the coreshine observations. We aim to find dust models that can explain a sample of Spitzer coreshine data. We also examine the consistency with near-infrared data we obtained for a few clouds.
Methods. We selected four regions with a very high occurrence of coreshine cases: Taurus-Perseus, Cepheus, Chameleon, and L183/L134. We built a grid of dust models and investigated the key parameters to reproduce the general trend of surface brightnesses and intensity ratios of both coreshine and near-infrared observations with the help of a 3D Monte Carlo radiative transfer code. The grid parameters allowed us to investigate the effect of coagulation upon spherical grains up to 5 μm in size derived from the DustEm diffuse interstellar medium grains. Fluffiness (porosity or fractal degree), ices, and a handful of classical grain-size distributions were also tested. We used the near- and mostly mid-infrared intensity ratios as strong discriminants between dust models.
Results. The determination of the background-field intensity at each wavelength is a key issue. In particular, an especially strong background field explains why we do not see coreshine in the Galactic plane at 3.6 and 4.5 μm. For starless cores, where detected, the observed 4.5 μm/3.6 μm coreshine intensity ratio is always lower than ~0.5, which is also what we find in the models for the Taurus-Perseus and L183 directions. Embedded sources can lead to higher fluxes (up to four times higher than the strongest starless core fluxes) and higher coreshine ratios (from 0.5 to 1.1 in our selected sample). Normal interstellar radiation-field conditions are sufficient to find suitable grain models at all wavelengths for starless cores. The standard interstellar grains are not able to reproduce observations and, because of the multiwavelength approach, only a few grain types meet the criteria set by the data. Porosity does not affect the flux ratios, while the fractal dimension helps to explain coreshine ratios, but does not seem able to reproduce near-infrared observations without a mix of other grain types.
Conclusions. Combined near- and mid-infrared wavelengths confirm the potential of revealing the nature and size distribution of dust grains. Careful assessment of the environmental parameters (interstellar and background fields, embedded or nearby reddened sources) is required to validate this new diagnostic.
Key words: ISM: clouds / dust, extinction / infrared: ISM / radiative transfer
Table 1 and appendices are available in electronic form at http://www.aanda.org
© ESO, 2014
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