LIME - a flexible, non-LTE line excitation and radiation transfer method for millimeter and far-infrared wavelengths

By Christian N. Brinch, M. Hogerheijde. 2010

218 citations recorded by the source corpus.

We present a new code for solving the molecular and atomic excitation and radiation transfer problem in a molecular gas and predicting emergent spectra. This code works in arbitrary three dimensional geometry using unstructured Delaunay latices for the transport of photons. Various physical models can be used as input, ranging from analytical descriptions over tabulated models to SPH simulations. To generate the Delaunay grid we sample the input model randomly, but weigh the sample probability with the molecular density and other parameters, and thereby we obtain an average grid point separation that scales with the local opacity. Our code does photon very efficiently so that the slow convergence of opaque models becomes traceable. When convergence between the level populations, the radiation field, and the point separation has been obtained, the grid is ray-traced to produced images that can readily be compared to observations. Because of the high dynamic range in scales that can be resolved using this type of grid, our code is particularly well suited for modeling of ALMA data. Our code can furthermore deal with overlapping lines of multiple molecular and atomic species.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/d6fa0f3a9514bf301796a916871260e12b379710

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Atomic and Molecular Physics, and Optics

In Spectroscopy

Citations in the corpus

THE TW Hya DISK AT 870 μm: COMPARISON OF CO AND DUST RADIAL STRUCTURES (2011, methodology): “We then feed that information into the radiative transfer modeling code LIME (Brinch & Hogerheijde 2010) to solve the non-LTE molecular excitation conditions of the model and generate a synthetic high-resolution model cube for the CO J=3−2 transition.”
A Three-dimensional View of Turbulence: Constraints on Turbulent Motions in the HD 163296 Protoplanetary Disk Using DCO+ (2017, methodology): “A similar effect can be seen in Figure 13 of Simon et al. (2015), where they employ a density and temperature structure similar to that used here, but fed through the LIME radiative transfer code (Brinch & Hogerheijde 2010).”
Measuring turbulence in TW Hydrae with ALMA: methods and limitations (2016, methodology): “The model was run through the LIME radiative transfer code (Brinch & Hogerheijde 2010) for a range of inclinations, i = {0◦, 5◦ , 6◦ , 7◦ , 8◦ , 9◦}, assuming no turbulent broadening.”
Turbulence in the TW Hya Disk (2018, methodology): “Synthetic CO data are generated based on the temperature, density, and abundance distribution from Kama et al. (2016), and fed through LIME (Brinch & Hogerheijde 2010) to generate model images of CO(2-1).”
A Kinematical Detection of Two Embedded Jupiter-mass Planets in HD 163296 (2018, methodology): “Facilities: ALMA Software: emcee (Foreman-Mackey, et al. 2013), celerite(Foreman-Mackeyetal.2017),CASA(McMullin, et al. 2007), LIME (Brinch & Hogerheijde 2010), FARGO-3D (Beńıtez-Llambay & Masset 2016), scipy (Jones et al. 2001) REFERENCES ALMA Partnership, Brogan, C. L., Pérez, L. M., et…”
A SPATIALLY RESOLVED VERTICAL TEMPERATURE GRADIENT IN THE HD 163296 DISK (2013, methodology): “…calculate the CO level populations using the non-local thermodynamic equilibrium (non-LTE) molecular excitation and radiative transfer package LIME (Brinch & Hogerheijde 2010) and molecular data from (A color version of this figure is available in the online journal.) the LAMDA database (Schöier…”
The warm gas atmosphere of the HD 100546 disk seen by Herschel - Evidence of a gas-rich, carbon-poor atmosphere? (2012, background): “(A.10), (A.12), and (A.13) form a coupled problem, which is computationally very demanding to solve (see for example Hogerheijde & van der Tak 2000; Brinch & Hogerheijde 2010).”