The DIRTY Model. I. Monte Carlo Radiative Transfer through Dust

By K. Gordon, K. Misselt, A. Witt, G. Clayton. 2000

141 citations recorded by the source corpus.

We present the DIRTY (DustI Radiative Transfer, Yeah!) radiative transfer model in this paper and a companion paper. This model computes the polarized radiative transfer of photons from arbitrary distributions of stars through arbitrary distributions of dust using Monte Carlo techniques. The dust re-emission is done self-consistently with the dust absorption and scattering and includes all three important emission paths: equilibrium thermal emission, nonequilibrium thermal emission, and the aromatic features emission. The algorithm used for the radiative transfer allows for the efficient computation of the appearance of a model system as seen from any viewing direction. We present a simple method for computing an upper limit on the output quantity uncertainties for Monte Carlo radiative transfer models that use the weighted photon approach.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/f5837478b9808a73daa55197ef4f4b1b9da2afbb

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In Astronomy and Astrophysics

1. C. Conroy
2. L. Hernquist
3. P. Hopkins
4. R. Dav'e
5. P. V. van Dokkum
6. A. Shapley
7. Naveen A. Reddy
8. C. Steidel

Citations in the corpus

• THE CHARACTERISTIC STAR FORMATION HISTORIES OF GALAXIES AT REDSHIFTS z ∼ 2–7 (2012, background): “…in order to derive self-consistently the reddening of starlight based upon direct dust indicators (e.g., such as the midor far-infrared dust continuum), thus accounting for the total energy budget when fitting for the stellar populations (Gordon et al. 2001; Misselt et al. 2001; Noll et al. 2009).”
• A TWO-PARAMETER MODEL FOR THE INFRARED/SUBMILLIMETER/RADIO SPECTRAL ENERGY DISTRIBUTIONS OF GALAXIES AND ACTIVE GALACTIC NUCLEI (2014, background): “…spectrum, their various parameters can yield insight into the physical characteristics of the system (e.g., Silva et al. 1998; Popescu et al. 2000; Gordon et al. 2001; 1Department of Physics & Astronomy, University of Wyoming, Laramie, WY 82071, USA; ddale@uwyo.edu 2Infrared Processing and…”
• Lyman α radiative transfer in a multiphase medium (2005, methodology): “There have been many studies of the radiative transfer of UV continuum photons in a clumpy, dusty ISM, using a variety of techniques (e.g. Witt & Gordon 1996; Vársoi & Dwek 1999; Gordon et al 2001), but none with extensions to resonance line photons.”
• EFFICIENT THREE-DIMENSIONAL NLTE DUST RADIATIVE TRANSFER WITH SKIRT (2011, methodology): “Our overall approach is comparable to the DIRTY (Gordon et al. 2001; Misselt et al. 2001) and TRADING (Bianchi 2008) radiative transfer codes and we refer the interested reader to these papers 3 for more details.”
• A simple model to interpret the ultraviolet, optical and infrared emission from galaxies (2008, background): “…from stars and dust in galaxies has been to solve the radiative transfer equation for idealised (bulge + disc) spatial distributions of stars and dust (e.g. Rowan-Robinson 1980; Efstathiou & Rowan-Robinson 1990; Gordon et al. 2001; Misselt et al. 2001; Popescu et al. 2000; Misiriotis et al. 2001).”
• Star Formation in the Milky Way and Nearby Galaxies (2012, background): “The accuracy of these pre- scriptions rests heavily on the presumed (but uncertain) intrinsic colors, the shape of the dust extinction curve, and the complicated effects of geometry and scattering when averaging over a large physical region (e.g., Gordon et al. 2001).”
• Fitting the integrated spectral energy distributions of galaxies (2010, methodology): “Existing Monte-Carlo codes that have been applied to galaxies include SUNRISE (Jonsson 2006; Jonsson et al. 2010), DIRTY (Gordon et al. 2001; Misselt et al. 2001), TRADING (Bianchi et al. 1996, 2000; Bianchi 2008), SKIRT (Baes et al. 2003), and RADISHE (Chakrabarti and Whitney 2009).”
• CIGALE: a python Code Investigating GALaxy Emission (2018, background): “So far this constraint has largely confined radiative transfer models to theoretical studies (e.g. Gordon et al. 2001; Tuffs et al. 2004; Trayford et al. 2017) and to only a handful of in-depth observational case studies, generally on edge-on galaxies (e.g. Xilouris et al. 1999; Popescu et al.…”
• High-resolution panchromatic spectral models of galaxies including photoionization and dust (2009, methodology): “There are many Monte Carlo radiation transfer codes in use (Gordon et al. 2001; Jonsson 2006; Chakrabarti & Whitney 2009; Li et al. 2007; Bianchi 2008, to name a few that are applied to galaxies) but the basic idea is the same: to solve the radiation transfer problem the way nature does, by simply…”
• Dust formation in early galaxies (2003, methodology): “Much fuller methodS for considering escape and absorption of radiation in a clumpy dusty environment are given by Városi & Dwek (1999) and Gordon et al (2001), but for an order-of-magnitude estimate here we just consider the optical depths through a cloud of fixed mass, divided in various ways.”
• The extragalactic background light and the gamma-ray opacity of the universe (2012, methodology): “The SED of a galaxy can be determined with radiative transfer models, such as GRASIL (Silva et al., 1998), DIRTY (Gordon et al., 2001), or DUSTY (Nenkova et al., 2000).”
• Deriving Physical Properties from Broadband Photometry with Prospector: Description of the Model and a Demonstration of its Accuracy Using 129 Galaxies in the Local Universe (2016, methodology): “A relationship between the dust attenuation optical depth and the shape of the attenuation curve in galaxies has been predicted both analytically (Bruzual et al. 1988) and numerically, with radiative transfer codes (Witt et al. 1992; Witt & Gordon 2000; Gordon et al. 2001; Chevallard et al. 2013).”
• Three-Dimensional Dust Radiative Transfer ∗ (2013, methodology): “Scattering of photons from dust grains naturally produces polarized radiation (see, e.g., Gordon et al. 2001, figure 2).”
• Modelling the spectral energy distribution of galaxies - V. The dust and PAH emission SEDs of disk galaxies (2010, methodology): “…Semionov & Vansevic̆ius 2005a, Semionov & Vansevic̆ius 2006) and Monte-Carlo (MC) techniques (Witt et al. 1992, Bianchi et al. 1996, de Jong 1996, Gordon et al. 2001, Baes & Dejonghe 2002, Baes et al. 2003, Baes et al. 2005, Jonsson 2006, Baes 2008, Bianchi 2008, Chakrabarti & Whitney…”
• Structure of Disk-dominated Galaxies. I. Bulge/Disk Parameters, Simulations, and Secular Evolution (2002, background): “Using far-infrared (FIR) to B-band flux ratios, as well as radiation transfer models for the dust (Gordon et al. 2001), we have tested for the origin of type II signature as being due to extinction.”
• Three-dimensional radiative transfer modeling of AGN dusty tori as a clumpy two-phase medium (2011, unknown): “Similar to most modern Monte Carlo codes (e.g.Gordon et al. 2001; Wolf 2003; Niccolini, Woitke, & Lopez 2003; Bianchi 2008), the SKIRT code contains many deterministic elements which makes the Monte Carlo technique orders of magnitude mor efficient than the naive Monte Carlo recipe.”