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Constraints on the OH-to-H Abundance Ratio in Infrared-bright Galaxies Derived from the Strength of the OH 35 μm Absorption Feature

  • Authors: Myra Stone, Sylvain Veilleux, Eduardo González-Alfonso, Henrik Spoon, and Eckhard Sturm

2018 The Astrophysical Journal 853 132.

  • Provider: AAS Journals

Caption: Figure 4.

Examples of OH 35 line profile fits for each of the 12 different continuum-subtracted spectra in IRAS F17208-0014. Line colors and styles are the same as that for Figure 3. “p1, p2, p3” indicate first-, second-, and third-order polynomial fits to the continuum, respectively. “v1” refers to the “lower-limit” pivot points in Figure 1. “v2” refers to the “upper-limit” pivot points, and “v3” to the best-fit-by-eye pivot points. “k1, k2, k3” are the orders of the spline fitted to the continuum. For example, “v2k3” is the third-order spline fit to the continuum using the upper-limit pivot points. The gray dotted vertical lines mark the rest wavelengths of the OH 35 doublet (34.60 and 34.63 μm) at systemic velocity.

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