Reddening maps of the Magellanic Clouds using spectral energy distribution fitting of red giants

TL;DR

This study creates detailed reddening maps of the Magellanic Clouds using spectral energy distribution fitting of red giants, highlighting the impact of stellar atmosphere models on reddening estimates.

Contribution

It introduces a method combining optical and near-infrared photometry to map reddening and assesses how different stellar atmosphere models affect the results.

Findings

Mean reddening: E(B-V)=0.076 mag for LMC, 0.058 mag for SMC.

Differences up to 0.03 mag in reddening due to atmospheric models.

Higher and structured reddening in LMC, especially around 30 Doradus.

Abstract

Robust reddening maps of the Large and Small Magellanic Clouds (LMC/SMC) are crucial for a wide range of astrophysical studies, including the calibration of the cosmic distance ladder, investigations of stellar populations in low-metallicity environments, and the characterization of interstellar dust properties. We aim to construct reddening maps of the Magellanic Clouds using spectral energy distribution (SED) fitting, and to investigate the impact of different stellar atmosphere models on the resulting maps. We combined optical ($ugriz$) photometry from the SMASH survey with near-infrared ($YJK_{\rm s}$) photometry from the VMC survey for red giant branch (RGB) stars. Observed SEDs were matched to synthetic photometry derived from three atmosphere model grids. Our maps cover 34.5 deg$^2$ of the LMC and 24.5 deg$^2$ of the SMC at 4 arcmin resolution. We find mean reddening values of $E(B-V)=0.076 \pm 0.022$ mag for the LMC and $0.058 \pm 0.024$ mag for the SMC. We found that employing different atmospheric models results in differences up to 0.03 mag in the mean reddening. Canonical $R_V$ values for the Magellanic Clouds (3.41 for LMC and 2.74 for SMC, Gordon et al. 2003) provide results consistent with previous studies. We confirm higher and more structured reddening in the LMC compared to the SMC, with 30 Doradus standing out as the dominant high-reddening region. Our results show that the absolute reddening scale depends on the choice of stellar atmosphere models, while the relative spatial structure of the reddening maps remains stable.