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The meaning of WISE colours - I. the Galaxy and its satellites
| Indexado |
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| DOI | 10.1093/MNRAS/STU1087 | ||||
| Año | 2014 | ||||
| Tipo | artículo de investigación |
Citas Totales
Autores Afiliación Chile
Instituciones Chile
% Participación
Internacional
Autores
Afiliación Extranjera
Instituciones
Extranjeras
Abstract
Through matches with the Sloan Digital Sky Survey (SDSS) catalogue we identify the location of various families of astronomical objects in WISE colour space. We identify reliable indicators that separate Galactic/local from extragalactic sources and concentrate here on the objects in our Galaxy and its closest satellites. We develop colour and magnitude criteria that are based only on WISE data to select asymptotic giant branch (AGB) stars with circumstellar dust shells, and separate them into O-rich and C-rich classes. With these criteria we produce an all-sky map for the count ratio of the two populations. The map reveals differences between the Galactic disc, the Magellanic Clouds and the Sgr Dwarf Spheroidal galaxy, as well as a radial gradient in the Large Magellanic Cloud (LMC) disc. We find that the C:O number ratio for dusty AGB stars increases with distance from the LMC centre about twice as fast as measured for near-IR selected samples of early AGB stars. Detailed radiative transfer models show that WISE colours are well explained by the emission of centrally heated dusty shells where the dust has standard properties of interstellar medium (ISM) grains. The segregation of different classes of objects in WISE colour space arises from differences in properties of the dust shells: those around young stellar objects have uniform density distributions while in evolved stars they have steep radial profiles.
| Ord. | Autor | Género | Institución - País |
|---|---|---|---|
| 1 | Nikutta, R. | Hombre |
Universidad Nacional Andrés Bello - Chile
UNIV KENTUCKY - Estados Unidos University of Kentucky - Estados Unidos |
| 2 | Hunt-Walker, Nicholas | Hombre |
UNIV WASHINGTON - Estados Unidos
University of Washington, Seattle - Estados Unidos University of Washington - Estados Unidos |
| 3 | Nenkova, M. | Mujer |
Seneca Coll - Canadá
Seneca College of Applied Arts & Technology - Canadá |
| 4 | Ivezic, Zeljko | Hombre |
UNIV WASHINGTON - Estados Unidos
University of Washington, Seattle - Estados Unidos University of Washington - Estados Unidos |
| 5 | Elitzur, Moshe | Hombre |
UNIV KENTUCKY - Estados Unidos
University of Kentucky - Estados Unidos |
| Fuente |
|---|
| FONDECYT |
| National Science Foundation |
| NSF |
| NASA |
| National Aeronautics and Space Administration |
| Alfred P. Sloan Foundation |
| U.S. Department of Energy Office of Science |
| Hungarian Academy of Sciences |
| JPL/Caltech |
| ALMA-CONICYT Fund |
| Participating Institutions |
| ORAU |
| Directorate for Mathematical and Physical Sciences |
| Agradecimiento |
|---|
| We are grateful to Maria-Rosa Cioni for illuminating discussions and for making her data available to us. We reproduced fig. 12 from Wright et al. (2010) as part of our Fig. 2 by permission of the AAS and the authors. We thank Chao-Wei Tsai for providing us a high-quality version. We thank both referees for their helpful suggestions which improved the paper. We express our gratitude to Xavier Koenig for reminding us of the disk/shell dichotomy of YSO models (see Section 4.3), and to James Davenport for his insightful post-submission comments on the variability information in the WISE database. We are also thankful to Patricia Arevalo and Ron Wilhelm for helpful discussions. RN acknowledges support by the ALMA-CONICYT fund, project No. 31110001, and by FONDECYT grant No. 3140436.. ZI thanks the Hungarian Academy of Sciences for its support through the Distinguished Guest Professor grant No. E-1109/6/2012.. ZI and NHW acknowledge support by NSF grant AST-1008784 to the University of Washington. ME acknowledges NASA support and the award of an NPP Senior Fellowship from ORAU, which supported a sabbatical leave at JPL/Caltech where much of this work was completed. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/.SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, NewMexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. This research has made use of the NED which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Some of the results in this paper have been derived using the HEALPIX/HEALPY package (Gorski et al. 2005). |
