The 23.01 release of Cloudy. (arXiv:2311.10163v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Gunasekera_C/0/1/0/all/0/1">Chamani M. Gunasekera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hoof_P/0/1/0/all/0/1">Peter A. M. van Hoof</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chatzikos_M/0/1/0/all/0/1">Marios Chatzikos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferland_G/0/1/0/all/0/1">Gary J. Ferland</a>
We announce the C23.01 update of Cloudy. This corrects a simple coding error,
present since $sim$ 1990, in one routine that required a conversion from the
line-center to the mean normalization of the Ly$alpha$ optical depth. This
affects the destruction of H I Ly$alpha$ by background opacities. Its largest
effect is upon the Ly$alpha$ intensity in high-ionization dusty clouds, where
the predicted intensity is now up to three times stronger. Other properties
that depend on Ly$alpha$ destruction, such as grain infrared emission, change
in response.
We announce the C23.01 update of Cloudy. This corrects a simple coding error,
present since $sim$ 1990, in one routine that required a conversion from the
line-center to the mean normalization of the Ly$alpha$ optical depth. This
affects the destruction of H I Ly$alpha$ by background opacities. Its largest
effect is upon the Ly$alpha$ intensity in high-ionization dusty clouds, where
the predicted intensity is now up to three times stronger. Other properties
that depend on Ly$alpha$ destruction, such as grain infrared emission, change
in response.
http://arxiv.org/icons/sfx.gif
