Three-dimensional Structure and Dust Extinction in the Small Magellanic Cloud
Petia Yanchulova Merica-Jones, Karin M. Sandstrom, L. Clifton Johnson, Andrew E. Dolphin, Julianne J. Dalcanton, Karl Gordon, Julia Roman-Duval, Daniel R. Weisz, Benjamin F. Williams
Abstract
Abstract We examine the three-dimensional structure and dust extinction properties in a ∼200 pc × 100 pc region in the southwest bar of the Small Magellanic Cloud (SMC). We model a deep Hubble Space Telescope optical color–magnitude diagram (CMD) of red clump and red giant branch stars in order to infer the dust extinction and galactic structure. We model the distance distribution of the stellar component with a Gaussian and find a centroid distance of 65.2 kpc (distance modulus μ = 19.07 mag) with an FWHM ≈ 11.3 kpc. This large extent along the line of sight reproduces results from previous studies using variable stars and red clump stars. Additionally, we find an offset between the stellar and dust distributions, with the dust on the near side relative to the stars by 3.22 kpc, resulting in a 73% reddened fraction of stars. Modeling the dust layer with a log-normal A V distribution indicates a mean extinction 〈 A V 〉 = 0.41 ± 0.09 mag. We also calculate A V / N H = 3.2–4.2 × 10 −23 mag cm 2 H −1 , which is significantly lower than the Milky Way value but is comparable to previous SMC dust-to-gas ratio measurements. Our results yield the first joint dust extinction and 3D geometry properties in a key region in the SMC. This study demonstrates that CMD modeling can be a powerful tool to simultaneously constrain dust extinction and geometry properties in nearby galaxies.