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

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.

[1]  T. Gombosi,et al.  SIMULATIONS OF WINDS OF WEAK-LINED T TAURI STARS. II. THE EFFECTS OF A TILTED MAGNETOSPHERE AND PLANETARY INTERACTIONS , 2010, 1007.3874.

[2]  B. Shustov,et al.  A method for molecular-line radiative-transfer computations and its application to a two-dimensional model for the starless core L1544 , 2004 .

[3]  V. Icke,et al.  Transport on adaptive random lattices. , 2006, Physical review. E, Statistical, nonlinear, and soft matter physics.

[4]  L. Auer,et al.  Short characteristic integration of radiative transfer problems: Formal solution in two-dimensional slabs , 1988 .

[5]  K. Zagorovsky,et al.  GAS EMISSION FROM DEBRIS DISKS AROUND A AND F STARS , 2010, 1007.3343.

[6]  N. Evans,et al.  Evidence for Protostellar Collapse in B335 , 1992 .

[7]  A. H. Barrett,et al.  Radio Observations of OH in the Interstellar Medium , 1963, Nature.

[8]  I. Kamp,et al.  Hot and cool water in Herbig Ae protoplanetary disks A challenge for Herschel , 2009, 0906.0448.

[9]  David P. Dobkin,et al.  The quickhull algorithm for convex hulls , 1996, TOMS.

[10]  T. Henning,et al.  Chemistry in Disks. IV. Benchmarking gas-grain chemical models with surface reactions , 2010, 1007.2302.

[11]  S. P. Lloyd,et al.  Least squares quantization in PCM , 1982, IEEE Trans. Inf. Theory.

[12]  V. Springel E pur si muove: Galilean-invariant cosmological hydrodynamical simulations on a moving mesh , 2009, 0901.4107.

[13]  G. Herzberg,et al.  Note on CH^{+} in Interstellar Space and in the Laboratory. , 1941 .

[14]  K. Menten,et al.  TRIGONOMETRIC PARALLAX OF W51 MAIN/SOUTH , 2010, 1006.4218.

[15]  R. Indebetouw,et al.  Interpreting Spectral Energy Distributions from Young Stellar Objects. I. A Grid of 200,000 YSO Model SEDs , 2006, astro-ph/0608234.

[16]  E. Young,et al.  Spectroscopic Evidence for Infall around an Extraordinary IRAS Source in Ophiuchus , 1986 .

[17]  C. Dominik,et al.  UvA-DARE ( Digital Academic Repository ) Flaring vs . self-shadowed disks : The SEDs of Herbig Ae / Be stars , 2004 .

[18]  M. Juvela,et al.  Numerical methods for non-LTE line radiative transfer: Performance and convergence characteristics , 2002, astro-ph/0208503.

[19]  C. Dullemond,et al.  Chemistry and line emission from evolving Herbig Ae disks , 2006, astro-ph/0611223.

[20]  F. Shu Self-similar collapse of isothermal spheres and star formation. , 1977 .

[21]  P. Goldreich,et al.  Spectral Energy Distributions of T Tauri Stars with Passive Circumstellar Disks , 1997, astro-ph/9706042.