E(B – V), N(H I), AND N(H2)

摘要

We consider the structure of the N(H I)-E(B – V) relationship when H I is measured in the 21 cm radio line and E(B – V) is defined by far-IR dust-derived measures. We derive reddening-dependent corrections to N(H I) based on interferometric absorption measurements over the past 30?yr that follow a single power-law relationship ?E(B – V)1.074 at 0.02 E(B – V) 3?mag. Corrections to 21?cm line-derived H I column densities are too small to have had any effect on the ratio N(H I)/E(B – V) = 8.3 × 1021 cm–2?mag–1 we derived at 0.015 E(B – V) 0.075?mag and |b| ≥ 20°; they are also too small to explain the break in the slope of the N(H I)-E(B – V) relation at E(B – V) 0.1?mag that we demonstrated around the Galaxy at |b|≥20°. The latter must therefore be attributed to the onset of H2?formation and we show that models of H2 formation in a low-density diffuse molecular gas can readily explain the inflected N (H I) – E(B – V) relationship. Below |b| = 20° N(H I)/E(B – V) measured at 0.015 E(B – V) 0.075?mag increases steadily down to |b| = 8° where sightlines with small E(B – V) no longer occur. By contrast, the ratio N(H I)/E(B – V) measured over all E(B – V) declines to N(H I)/E(B – V) = 5-6 × 1021 cm–2?mag–1 at |b| 30°, perhaps providing an explanation of the difference between our results and the gas/reddening ratios measured previously using stellar spectra.