We present a detailed study of an estimator of the H I column density, based on a combination of H I 21 cm absorption and H I 21cm emission spectroscopy. This `isothermal’ estimate is given by NHI, ISO = 1.823 × 1018 ∫ [tautot × TB / [ 1 – e-tautot]dV, where tautot is the total H I 21cm optical depth along the sightline and TB is the measured brightness temperature. We have used a Monte Carlo simulation to quantify the accuracy of the isothermal estimate by comparing the derived NHI, ISO with the true H I column density NHI. The simulation was carried out for a wide range of sightlines, including gas in different temperature phases and random locations along the path. We find that the results are statistically insensitive to the assumed gas temperature distribution and the positions of different phases along the line of sight. The median value of the ratio of the true H I column density to the isothermal estimate, NHI/NHI, ISO, is within a factor of 2 of unity while the 68.2 per cent confidence intervals are within a factor of ≈3 of unity, out to high H I column densities, <=5 × 1023 cm-2 per 1 km s-1 channel, and high total optical depths, <=1000. The isothermal estimator thus provides a significantly better measure of the H I column density than other methods, within a factor of a few of the true value even at the highest columns, and should allow us to directly probe the existence of high H I column density gas in the Milky Way.

Chengalur, Jayaram N.; Kanekar, Nissim; Roy, Nirupam

2013, Monthly Notices of the Royal Astronomical Society, 432, 3074-3079

http://adsabs.harvard.edu/abs/2013MNRAS.432.3074C