Column-density estimation from the equivalent widths of absorption doublets
- 1Department of Particle Physics and Astrophysics, Weizmann Institute of Science , Rehovot 76100 ,
Abstract
Na small ID absorption is widely used to estimate the dust extinction towards Galactic and extragalactic sources, but the inferred column densities are unreliable once the lines saturate. We present an analytical framework for estimating column densities from the equivalent widths (EWs) of absorption-line doublets. The method requires only that the two doublet members be measured separately – the velocity structure need not be resolved – so a resolving power λ /Δ λ ≳ 103 suffices for Na small ID, two orders of magnitude below velocity-resolved methods. For the Gaussian curve of growth, the classical inversion reduces to a universal saturation correction depending only on the doublet ratio, R= EW2/ EW1: At fixed R, the inferred column density is linear in the measured EW. The formulation yields the exact Gaussian inversion, Nκ ̃, which provides the Doppler parameter; a closed-form second-order approximation; and a strict lower bound, Nmin, valid for an arbitrary velocity structure. We recommend reporting Nmin: an optimal, assumption-free lower bound, within a few per cent of Nκ ̃ for R≳ 1.4 and at most a factor 3.5 below it at R=1.1. The ratio Nκ ̃/N2nd provides a per-object saturation diagnostic. We validate the framework against published profile-fitting Na small ID column densities towards Galactic sightlines and Type Ia supernovae, using only the integrated EWs. An explicit closed-form formula converts the two EWs into an extinction estimate through the observed log N(Na small I)–AV relation. A public implementation with full uncertainty propagation accompanies the paper.
Versions
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BibTeX
@article{badash2026columndensity,
title = {{Column-density estimation from the equivalent widths of absorption doublets}},
author = {Avshalom Badash and Doron Kushnir},
journal = {Monthly Notices of the Royal Astronomical Society},
year = {2026},
month = oct,
doi = {10.1093/mnras/stag1921},
url = {https://academic.oup.com/mnras/article/doi/10.1093/mnras/stag1921/8898885},
note = {CC BY 4.0},
}
RIS
TY - JOUR
TI - Column-density estimation from the equivalent widths of absorption doublets
AU - Avshalom Badash
AU - Doron Kushnir
PY - 2026
DA - 2026/10/09
JO - Monthly Notices of the Royal Astronomical Society
DO - 10.1093/mnras/stag1921
UR - https://academic.oup.com/mnras/article/doi/10.1093/mnras/stag1921/8898885
AB - Na small ID absorption is widely used to estimate the dust extinction towards Galactic and extragalactic sources, but the inferred column densities are unreliable once the lines saturate. We present an analytical framework for estimating column densities from the equivalent widths (EWs) of absorption-line doublets. The method requires only that the two doublet members be measured separately – the velocity structure need not be resolved – so a resolving power λ /Δ λ ≳ 10^3 suffices for Na small ID, two orders of magnitude below velocity-resolved methods. For the Gaussian curve of growth, the classical inversion reduces to a universal saturation correction depending only on the doublet ratio, R= EW_2/ EW_1: At fixed R, the inferred column density is linear in the measured EW. The formulation yields the exact Gaussian inversion, N_κ ̃, which provides the Doppler parameter; a closed-form second-order approximation; and a strict lower bound, N_min, valid for an arbitrary velocity structure. We recommend reporting N_min: an optimal, assumption-free lower bound, within a few per cent of N_κ ̃ for R≳ 1.4 and at most a factor 3.5 below it at R=1.1. The ratio N_κ ̃/N_2nd provides a per-object saturation diagnostic. We validate the framework against published profile-fitting Na small ID column densities towards Galactic sightlines and Type Ia supernovae, using only the integrated EWs. An explicit closed-form formula converts the two EWs into an extinction estimate through the observed log N(Na small I)–A_V relation. A public implementation with full uncertainty propagation accompanies the paper.
SN - 0035-8711
SN - 1365-2966
ER -