Milky Way Mid-Infrared Spitzer Spectroscopic Extinction Curves: Continuum and Silicate Features
AffiliationSteward Observatory, University of Arizona
MetadataShow full item record
PublisherIOP Publishing Ltd
CitationGordon, K. D., Misselt, K. A., Bouwman, J., Clayton, G. C., Decleir, M., Hines, D. C., Pendleton, Y., Rieke, G., Smith, J. D. T., & Whittet, D. C. B. (2021). Milky Way Mid-Infrared Spitzer Spectroscopic Extinction Curves: Continuum and Silicate Features. Astrophysical Journal, 916(1).
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AbstractWe measured the mid-infrared (MIR) extinction using Spitzer photometry and spectroscopy (3.6-37 μm) for a sample of Milky Way sight lines (mostly) having measured ultraviolet extinction curves. We used the pair method to determine the MIR extinction that we then fit with a power law for the continuum and modified Drude profiles for the silicate features. We derived 16 extinction curves having a range of A(V) (1.8-5.5) and R(V) values (2.4-4.3). Our sample includes two dense sight lines that have 3 μm ice feature detections and weak 2175 Å bumps. The average A(λ)/A(V) diffuse sight-line extinction curve we calculate is lower than most previous literature measurements. This agrees better with literature diffuse dust grain models, though it is somewhat higher. The 10 μm silicate feature does not correlate with the 2175 Å bump, for the first time providing direct observational confirmation that these two features arise from different grain populations. The strength of the 10 μm silicate feature varies by ∼2.5 and is not correlated with A(V) or R(V). It is well fit by a modified Drude profile with strong correlations seen between the central wavelength, width, and asymmetry. We do not detect other features with limits in A(λ)/A(V) units of 0.0026 (5-10 μm), 0.004 (10-20 μm), and 0.008 (20-40 μm). We find that the standard prescription of estimating R(V) from C E(K s - V)/E(B - V) has C = -1.14 and a scatter of ∼7%. Using the IRAC 5.6 μm band instead of K s gives C = -1.03 and the least scatter of ∼3%. © 2021. The American Astronomical Society. All rights reserved..
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