UCL Astrophysics Group
- Contact Us
- Astrophysics Seminars
- Departmental Events
- Research Topics
- Undergraduate Studies
- PhD Admissions
- University of London Observatory
- Astrophysics Wiki Pages
- Vacancies page
- Group Support and Policies
- Galactic Star Formation and the ISM
- Astrochemistry and the Birth of Massive Stars
- The Dust Grain Ice Formation Inverse Problem
SMMOL (Spherical Multi-level MOLecular line radiative transfer) is a molecular line radiative transfer code that uses Accelerated Lambda Iteration (Scharmer and Carlsson 1985; Rybick and Hummer 1991, Harper 1994) to solve the coupled level population and line transfer problem in spherical geometry. The code uses a discretised grid and a ray tracing methodology. The code is designed for high optical depth regimes and can cope with maser emission as long as the spatial-velocity sampling is fine enough.
It uses the Leiden Molecular Database interface and it uses the method of Schoenberg (1988) to convolve the emergent flux with a telescope response function.
The code (source and examples) is available on request from Jeremy Yates (jyates AT star.ucl.ac.uk).
ISO LWS Fabry-Perot ortho-water line profiles (dashed lines) compared with theoretical line profiles calculated with SMMOL using UCL_CHEM input parameters. From Lerate et al. (MNRAS, 406, 2445, 2010).
Page last modified on 21 sep 10 12:01 by Michael Barlow