Properties of M31

被引：0
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作者：
Montalto, M. [1 ,2 ]
Seitz, S. [1 ,2 ]
Riffeser, A. [1 ]
Hopp, U. [1 ,2 ]
Lee, C.-H. [1 ]
Schönrich, R. [1 ]
机构：
[1] University Observatory Munich, Scheinerstrasse 1, 81679 Munich, Germany
[2] Max-Planck Institute for Extraterrestrial Physics, Giessenbachstrasse, 85748 Garching, Germany
来源：
Astronomy and Astrophysics | 2009年 / 507卷 / 01期
关键词：
Aims.Observations acquired by the Spitzer Space Telescope and improvements to theoretical modeling of dust emission properties are used to discuss the distribution of dust and its characteristics in the closest neighbor spiral galaxy M31. These data are then used with GALEX FUV; NUV; and SDSS images to study the age dependence of the dust heating process. Methods. Spitzer IRAC/MIPS maps of M31 were matched together and compared to dust emission models allowing us to constrain the dust mass; the intensity of the mean radiation field; the abundance of polycyclic aromatic hydrocarbon (PAH) particles. The total infrared emission (TIR) was analyzed as a function of UV and optical colors and compared to predictions of models that consider age-dependent dust heating. Results.We demonstrate that cold-dust component emission dominates the infrared spectral energy distribution of M31. The mean intensity of the radiation field heating the dust is low (typically U 4000 A and that dust in M31 appears mainly heated by populations a few Gyr old even across the star-forming ring.We also found that the attenuation varies radially peaking close to 10 kpc and decreases more rapidly with radius in the inner regions of M31 than in the outer regions in agreement with previous studies. We finally derived the attenuation map of M31 at 6 /px resolution (∼100 pc/px along the plane of M31). Conclusions. © 2009 ESO;
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页码：283 / 300
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