Mid-infrared extinction toward the Galactic center

Abstract

We determine the mid-infrared (MIR, $\sim$5~μm--22~μm) extinction towards the Galactic center using MIRI/MRS integral field unit (IFU) observations of the central $3^{\prime \prime }\times 3^{\prime \prime }$ region (near 5~μm) to $7^{\prime \prime }\times 7^{\prime \prime }$ region (near 22~μm). To measure the MIR extinction, we employ two approaches: modeling the intrinsic-to-observed dust thermal spectrum and assessing the differential extinction between hydrogen recombination lines. Expanding on prior work, we directly model the dust-opacity distribution along the line of sight, and we make available a Python code that provides a flexible tool for deriving intrinsic dust emission spectra. We confirm the spatial variability of extinction across the field, demonstrating that dusty sources--such as IRS~29N--exhibit higher local extinction. Furthermore, we verify the absence of PAH emission features in the Galactic center MIR spectra. Using the two complementary methods, we derive a refined ``best guess'' MIR extinction law for Sgr A* and the surrounding Galactic-center region. By applying the extinction law to a MIR flare measurement discussed in a companion paper Michail et al. 2025, we estimate a residual relative extinction uncertainty for the short MIRI/MRS grating on the order of $0.2\mathrm{mag}$ {from $\sim$5 to $\sim$18~μm\ and $\sim$0.3~mag from $\sim$18 to $\sim$22~μm}, consistent with our uncertainty estimate.

Accepted for publications in ApJ, Sgr A* SED companion paper posted to arXiv today (Michail et al.) and extinction correction results are used in IMBH constraint paper (Roychowdhury et al., 2025, PASP) also posted to arXiv today

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