tokens: is seen between q 24 and for the entire sample, with a correlation coefficiency of 0.33. The second panel of Figure 5 shows that metal-poor galaxies have on average warmer color than metal-rich ones, but no apparent correlation between q 24 and . Actually, the two galaxies with the highest around 0.4 show almost the largest and smallest q 24 , respectively. The above result confirms a previous finding of no relation between and f (60 μ m)/ f (100 μ m) (Wu et al. 2008 ). The last panel of Figure 5 illustrates some weak dependence of on the far-IR color , with a correlation coefficiency of 0.26. Figure 5. vs. the IR color of , , and . The red points denote metal-poor galaxies and black points are for metal-rich galaxies. The two horizontal dashed lines indicate the average values of metal-poor and metal-rich galaxies, respectively. Figure 6 investigates the dependence of on the three IR colors mentioned above. A weak correlation is seen between and , with a correlation coefficiency of −0.34. Overall, the metal-poor and metal-rich galaxies share the same range in , as already mentioned above. At the same , q 70 is smaller for metal-poor galaxies compared to metal-rich galaxies. The two metal-poor galaxies with the highest show low q 70 , but not as extremely as expected, if there is a relation. The dependence of q 70 on is very weak, with a correlation coefficiency of −0.05. At the same color, metal-poor galaxies on average occupy lower regimes compared to metal-rich ones. Among two metal-poor galaxies with the highest , only one shows a lower q 70 than the remaining galaxies. The last panel shows no strong relation between and the far-IR color , with a correlation coefficiency of about −0.2. Figure 6. Same as Figure 5 but for . Figure 7 shows as a function of the three IR colors mentioned above. The first panel indicates a weak dependence of q 100 on , with a correlation coefficiency of −0.42. At the same color, metal-poor galaxies show somewhat lower than metal-rich galaxies. SBS 0335-052E, which has the highest , does not show the lowest q 100 . In the second panel, a stronger trend is present for the with, with a correlation coefficiency of −0.53. The two galaxies with the highest have the lowest q 100 among the whole sample. In the last panel, the dependence of q 100 on is weak, with a correlation coefficiency of −0.33. Figure 7. Same as Figure 5 but for . as a function of IR color is shown in Figure 8 . An inverse relation of with is present, with a correlation coefficiency of −0.63. The relation between and is also apparent, with a correlation coefficiency of −0.43. The relationship between and is the strongest one, with a correlation coefficiency of −0.71, indicating that the low of metal-poor galaxies is associated with their high . Figure 8. Same as Figure 5 but for . In summary, for the whole sample, including both metal-rich and metal-poor galaxies, only shows good relationships with the three IR colors. Previous studies of
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