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Extinction Effects in Spiral Galaxy Rotation Curves

Carlos Valotto·Riccardo Giovanelli
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Abstract

Observations show that the slope of the inner part of the H$α$/[NII] rotation curves of disk galaxies is depressed by extinction: at fixed luminosity, the observed slope is in fact seen to depend on the disk inclination to the line of sight. Using a simple extinction model, we are able to reproduce well the observed trends. The model assumes an exponential distribution, both in the radial and $z$ directions, identical for star--forming regions and dust. Fits to the data are optimized by varying the scale height and scale length of absorbers, as well as the disk's central optical depth $τ_\circ$, as seen face--on. The observations indicate that disk central opacity increases with total luminosity. Model fits for the most luminous galaxies (brighter than $M-5\log h=-21.4$ in the I band) yield $τ_\circ \simeq 3.5^{+4.0}_{-2.0}$, near $λ=0.66$ $μ$m. The large uncertainty on the inferred value of $τ_\circ$ is due to the poorly known characteristics of the distribution of absorbers in the disk, as well as to the likelihood of strong departures from an exponential radial distribution near the galaxy centers.

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Carlos Valotto, Riccardo Giovanelli. 2004-03-23. Extinction Effects in Spiral Galaxy Rotation Curves. https://doi.org/10.1086/421359

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