MOU Shuang-qian, MIAO Jing-ren, MAO Ye-wei
Journal of Guangzhou University(Natural Science Edition).
2025, 24(3):
20-30.
In this study, by analyzing the imaging data for the nearby spiral galaxy M81 (NGC 3031) obtained with the Spitzer Space Telescope at 3.6 μm and 4.5 μm, morphological parameters at the two bands and color index for the bulge and the disk of the galaxy are obtained, based on which, spatial distributions of the surface brightness and the color index for the galaxy and its substructures are deeply investigated. The software GALFIT is used to decompose the galaxy with two Sérsic components. By separating the bulge and the disk from the galaxy, images of the color index (3.6~4.5 μm) for the two substructures are created. In the results, the Sérsic index of M81 at 3.6 μm and 4.5 μm band is 4.27 and 5.13, respectively, confirming it as a classical bulge. The Sérsic index n ≈ 1.1 of the disk complies with the feature of an exponential disk. The effective radius of the bulge in the 3.6 μm band (72.24 arcsec) is smaller than in the 4.5 μm band (87.03 arcsec), and hence more compact in morphology, which may be related to the difference in sensitivity to stellar population properties at different bands. Analysis of the color index shows that the color difference between the bulge and the disk is not obvious (the color index is -0.08), but the overall color index for the galaxy (about -0.09) is bluer than those for the bulge and the disk. In the radial profiles, the color index of the disk decreases gradually with the radius, with the gradient about 0.33 mag/arcsec2, suggesting a decrease in stellar population age from the center to the edge. The color index for the bulge slightly decreases within a small radial range (< 70 arcsec), with the gradient about 0.13 mag/arcsec2, suggesting older central stars than those at outer areas. The overall color index for the galaxy shows a flat trend extending to large radii, suggesting similar ages for outer stars. In the center, the color index for the disk is larger than that for the bulge, which may be caused by different processes in the formation and evolution of different substructures. In the next work, we will conduct the multi-band decomposition of the galaxy, and construct spatially resolved spectral energy distributions for its substructure, respectively.