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We combine new ASTE/AzTEC 1.1 mm maps of the galaxy pair NGC 1512/1510 witharchival Spitzer IRAC and MIPS images covering the wavelength range 3.6--160 umfrom the SINGS project to derive accurate dust masses in each galaxy, and insub--galactic regions in NGC 1512. The two galaxies form a pair consisting of alarge, high--metallicity spiral (NGC 1512) and a low metallicity, blue compactdwarf (NGC 1510). The derived total dust masses are (2.4+/-0.6) 10^7 Msun and(1.7+/-3.6) 10^5 Msun for NGC 1512 and NGC 1510, respectively. The derivedratio of dust mass to H I gas mass for the galaxy pair (0.0034) is much lowerthan expected, while regions within NGC 1512, specifically the central regionand the arms, do not show such unusually low ratios; furthermore, thedust--to--gas ratio is within expectations for NGC 1510. These results suggestthat a fraction of the H I included in the determination of the M_d/M_HI ratioof the NGC 1512/1510 pair is not associated with the star forming disks/regionsof either galaxy. We also perform simple two--temperature (warm + cold)modified--blackbody fits to the far--infrared/mm data. The warm dusttemperature of the low--metallicity NGC 1510 (~36 K) is substantially higherthan that of the high--metallicity NGC 1512 (~24 K). In both galaxies, asubstantial fraction (>93%) of the total dust mass is in a cool dust component,with temperatures 14--16 K for NGC 1512 and 15--24 K for NGC 1510. In contrast,the warm dust in the arms and central regions of NGC 1512 represents a muchlarger fraction of the total dust content, in agreement with the fact that allthree regions have higher specific star formation rates than the average in thegalaxy.

An Investigation of the Dust Content in the Galaxy pair NGC 1512/1510 from Near-Infrared to Millimeter Wavelengths