tokens: (red crosses for the flux, yellow shadows for the flux error) is also plotted. We first subtract the stellar light in the SED by assuming a Rayleigh–Jeans tail scaled by the WISE W1 band data point and then fit the data points at 8–1000 μ m with the modified blackbody + MIR power-law model (namely, CMC fits; green lines). The final model SED is shown as dark gray lines. The T , α , and β parameters derived from the CMC fits are indicated in the top right corner of each panel. In a similar fashion as Rémy-Ruyer et al. ( 2013 ), a single modified blackbody is also fit to the Herschel data points for comparison (light gray line). Table 7 Low-metallicity Galaxies Used to Derive the Templates Note. Column (1): the galaxy name. Column (2): the metallicity 12 + log(O/H). Column (3): the dust temperature derived from the CMC fit (see text). Column (4): the FIR emission index. Column (5): the MIR power-law index. Column (6): the existence of the MIR Spitzer spectrum: good —the galaxy has a full range 5–35 μ m MIR spectrum; limited —the galaxy has an MIR spectrum with limited coverage; poor —IC 10 is quite extended, as judged from its MIPS 24 μ m image, making the Spitzer spectrum a poor reflection of the overall MIR continuum. Figure 10 shows the full IR SEDs (after adding the Spitzer spectra) for the 19 DGS galaxies. The MIR continua derived from the photometry fitting and those directly obtained from the MIR spectra are consistent. The MIR regions of these low-metallicity objects present substantial forbidden-line emissions and weak or no polycyclic aromatic hydrocarbon emission (e.g., Wu et al. 2006 , 2007 ), which contribute little to the continuum. For the final model SEDs of the 19 DGS galaxies, we discard the MIR portion of the fit SED continua based on WISE and Herschel photometry and replace it with scaled Spitzer spectra. Figure 10. Full IR SEDs of the 19 DGS galaxies that have Spitzer /IRS low-resolution spectra with high enough S/N, sequenced by their metallicity with the lowest at the bottom. The Spitzer spectra are scaled to match the continuum SEDs. A.3. Features of Low-metallicity Galaxy Templates Figure 11 compares the 19 low-metallicity templates with the normal SF galaxy templates in Rieke et al. ( 2009 ). The SEDs of these dwarf galaxies show a lot of variation. Compared with the solar-metallicity galaxies, the low-metallicity IR SEDs derived in this work tend to have the following features: 1. Higher FIR dust temperature. For the low-metallicity galaxies, the typical dust temperature is T dust = 34 ± 7.7. Our value is similar to the result by Rémy-Ruyer et al. ( 2013 ) ( T dust ∼ 32 K). Compared with the Herschel KINGFISH sample ( T dust ∼ 23 K; Rémy-Ruyer et al. 2013 ), which contains more metal-rich environments, the dust in these low-metallicity systems is generally warmer. 2. Steeply rising MIR continua. For low-metallicity galaxies in this work, the MIR continua slope α = 3.8 ± 0.8, which is much larger than typical
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