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From Near-infrared to Millimeter: An Investigation of the Dust Content in the NGC1512/1510 Pair

We combine new ASTE/AzTEC 1.1 mm maps of the galaxy pair NGC1512/1510 with archival Spitzer IRAC and MIPS images covering the wavelength range 3.6–160 μm from the SINGS project. The availability of the 1.1 mm map enables us to measure the long–wavelength tail of the dust emission in each galaxy, and in sub–galactic regions in NGC1512, and to derive accurate dust masses. The two galaxies form a high–metallicity, large spiral (NGC1512)/low– metallicity compact dwarf (NGC1510) pair, which we use to compare similarities and contrast differences. From the models of Draine et al. (2007), the total dust masses are 1.5×10 M⊙ and ∼6.4×10 5 M⊙ for NGC1512 and NGC1510, respectively. The derived dust/H i ratio is within expectations of low–metallicity galaxies for NGC1510, but it is much lower, by at least a factor of 5, than expected for NGC1512. In contrast, regions within NGC1512, specififically the central region and the arms, do not show such unusually low dust/H i values, suggesting the possibility that a fraction of the H i included in the determination of the dust/H i ratio of NGC1512 is not associated with the star forming disk. Using two–temperature modified–blackbody fits to the far–infrared/mm data of the two galaxies and the sub–regions of NGC1512, we derive dust masses associated with the warm and cool dust temperature components. As generally expected, the warm dust temperature of the low–metallicity, low–mass NGC1510 (Tw∼36 K) is substantially higher than the corresponding warm temperature of the high–metallicity spiral NGC1512 (Tw∼24 K). However, in both galaxies the data require that a substantial fraction (>93%) of the total dust mass is in a cool, ∼14–16 K, dust component, similarly to what determined for a few other nearby galaxies. In the sub–galactic regions of NGC1512, the warm dust component represents a much larger fraction of the total dust content, in agreement