16 research outputs found
FitSKIRT: genetic algorithms to automatically fit dusty galaxies with a Monte Carlo radiative transfer code
We present FitSKIRT, a method to efficiently fit radiative transfer models to
UV/optical images of dusty galaxies. These images have the advantage that they
have better spatial resolution compared to FIR/submm data. FitSKIRT uses the
GAlib genetic algorithm library to optimize the output of the SKIRT Monte Carlo
radiative transfer code. Genetic algorithms prove to be a valuable tool in
handling the multi- dimensional search space as well as the noise induced by
the random nature of the Monte Carlo radiative transfer code. FitSKIRT is
tested on artificial images of a simulated edge-on spiral galaxy, where we
gradually increase the number of fitted parameters. We find that we can recover
all model parameters, even if all 11 model parameters are left unconstrained.
Finally, we apply the FitSKIRT code to a V-band image of the edge-on spiral
galaxy NGC4013. This galaxy has been modeled previously by other authors using
different combinations of radiative transfer codes and optimization methods.
Given the different models and techniques and the complexity and degeneracies
in the parameter space, we find reasonable agreement between the different
models. We conclude that the FitSKIRT method allows comparison between
different models and geometries in a quantitative manner and minimizes the need
of human intervention and biasing. The high level of automation makes it an
ideal tool to use on larger sets of observed data.Comment: 14 pages, 10 figures; accepted for publication in Astronomy and
Astrophysic
The distribution of interstellar dust in CALIFA edge-on galaxies via oligochromatic radiative transfer fitting
We investigate the amount and spatial distribution of interstellar dust in
edge-on spiral galaxies, using detailed radiative transfer modeling of a
homogeneous sample of 12 galaxies selected from the CALIFA survey. Our
automated fitting routine, FitSKIRT, was first validated against artificial
data. This is done by simultaneously reproducing the SDSS -, -, - and
-band observations of a toy model in order to combine the information
present in the different bands. We show that this combined, oligochromatic
fitting, has clear advantages over standard monochromatic fitting especially
regarding constraints on the dust properties. We model all galaxies in our
sample using a three-component model, consisting of a double exponential disc
to describe the stellar and dust discs and using a S\'ersic profile to describe
the central bulge. The full model contains 19 free parameters, and we are able
to constrain all these parameters to a satisfactory level of accuracy without
human intervention or strong boundary conditions. Apart from two galaxies, the
entire sample can be accurately reproduced by our model. We find that the dust
disc is about 75% more extended but only half as high as the stellar disc. The
average face-on optical depth in the V-band is and the spread of
within our sample is quite substantial, which indicates that some spiral
galaxies are relatively opaque even when seen face-on.Comment: 18 pages, 6 figures, 4 tables, Accepted for publication in MNRA
The shape of dark matter haloes - IV. The structure of stellar discs in edge-on galaxies
We present optical and near-infrared archival observations of eight edge-on galaxies. These observations are used to model the stellar content of each galaxy using the FITSKIRT software package. Using FITSKIRT, we can self-consistently model a galaxy in each band simultaneously while treating for dust. This allows us to measure accurately both the scalelength and scaleheight of the stellar disc, plus the shape parameters of the bulge. By combining these data with the previously reported integrated magnitudes of each galaxy, we can infer their true luminosities.We have successfully modelled seven out of the eight galaxies in our sample.We find that stellar discs can be modelled correctly, but we have not been able to model the stellar bulge reliably. Our sample consists for the most part of slowly rotating galaxies and we find that the average dust layer is much thicker than is reported for faster rotating galaxie
Herschel observations of edge-on spirals (Heroes) IV. Dust energy balance problem
We present results of the detailed dust energy balance study for the seven large edge-on galaxies in the HEROES sample using three-dimensional (3D) radiative transfer (RT) modelling. Based on available optical and near-infrared (NIR) observations of the HEROES galaxies, we derive the 3D distribution of stars and dust in these galaxies. For the sake of uniformity, we apply the same technique to retrieve galaxy properties for the entire sample: we use a stellar model consisting of a Sérsic bulge and three double-exponential discs (a superthin disc for a young stellar population and thin and thick discs for old populations). For the dust component, we adopt a double-exponential disc with the new THEMIS dust-grain model. We fit oligochromatic RT models to the optical and NIR images with the fitting algorithm fitskirt and run panchromatic simulations with the skirt code at wavelengths ranging from ultraviolet to submillimeter. We confirm the previously stated dust energy balance problem in galaxies: for the HEROES galaxies, the dust emission derived from our RT calculations underestimates the real observations by a factor 1.5-4 for all galaxies except NGC 973 and NGC 5907 (apparently, the latter galaxy has a more complex geometry than we used). The comparison between our RT simulations and the observations at mid-infrared-submillimetre wavelengths shows that most of our galaxies exhibit complex dust morphologies (possible spiral arms, star-forming regions, more extended dust structure in the radial and vertical directions). We suggest that, in agreement with results from the literature, the large- and small-scale structure is the most probable explanation for the dust energy balance problem
HERschel Observations of Edge-on Spirals (HEROES). IV. Dust energy balance problem
We present results of the detailed dust energy balance study for the seven
large edge-on galaxies in the HEROES sample using 3D radiative transfer (RT)
modelling. Based on available optical and near-infrared observations of the
HEROES galaxies, we derive the 3D distribution of stars and dust in these
galaxies. For the sake of uniformity, we apply the same technique to retrieve
galaxy properties for the entire sample: we use a stellar model consisting of a
S\'ersic bulge and three double-exponential discs (a superthin disc for a young
stellar population and thin and thick discs for old populations). For the dust
component, we adopt a double-exponential disc with the new THEMIS dust-grain
model. We fit oligochromatic radiative transfer (RT) models to the optical and
near-infrared images with the fitting algorithm FitSKIRT and do panchromatic
simulations with the SKIRT code at wavelengths ranging from ultraviolet to
submillimeter. We confirm the previously stated dust energy balance problem in
galaxies: for the HEROES galaxies, the dust emission derived from our RT
calculations underestimates the real observations by a factor 1.5-4 for all
galaxies except NGC 973 and NGC 5907 (apparently, the latter galaxy has a more
complex geometry than we used). The comparison between our RT simulations and
the observations at mid-infrared-submillimeter wavelengths shows that most of
our galaxies exhibit complex dust morphologies (possible spiral arms,
star-forming regions, more extended dust structure in the radial and vertical
directions). We suggest that, in agreement with the results from Saftly et al.
(2015), the large- and small-scale structure is the most probable explanation
for the dust energy balance problem.Comment: 53 pages, 31 figures, Accepted for publication in Astronomy &
Astrophysic
High-resolution, 3D radiative transfer modeling: I. The grand-design spiral galaxy M 51
International audienceContext. Dust reprocesses about half of the stellar radiation in galaxies. The thermal re-emission by dust of absorbed energy is considered to be driven merely by young stars so is often applied to tracing the star formation rate in galaxies. Recent studies have argued that the old stellar population might be responsible for a non-negligible fraction of the radiative dust heating.Aims. In this work, we aim to analyze the contribution of young (≲100 Myr) and old (~10 Gyr) stellar populations to radiative dust heating processes in the nearby grand-design spiral galaxy M 51 using radiative transfer modeling. High-resolution 3D radiative transfer (RT) models are required to describe the complex morphologies of asymmetric spiral arms and clumpy star-forming regions and to model the propagation of light through a dusty medium. Methods. In this paper, we present a new technique developed to model the radiative transfer effects in nearby face-on galaxies. We construct a high-resolution 3D radiative transfer model with the Monte-Carlo code SKIRT to account for the absorption, scattering, and non-local thermal equilibrium (NLTE) emission of dust in M 51. The 3D distribution of stars is derived from the 2D morphology observed in the IRAC 3.6 μm, GALEX FUV, Hα, and MIPS 24 μm wavebands, assuming an exponential vertical distribution with an appropriate scale height. The dust geometry is constrained through the far-ultraviolet (FUV) attenuation, which is derived from the observed total-infrared-to-far-ultraviolet luminosity ratio. The stellar luminosity, star formation rate, and dust mass have been scaled to reproduce the observed stellar spectral energy distribution (SED), FUV attenuation, and infrared SED.Results. The dust emission derived from RT calculations is consistent with far-infrared and submillimeter observations of M 51, implying that the absorbed stellar energy is balanced by the thermal re-emission of dust. The young stars provide 63% of the energy for heating the dust responsible for the total infrared emission (8−1000 μm), while 37% of the dust emission is governed through heating by the evolved stellar population. In individual wavebands, the contribution from young stars to the dust heating dominates at all infrared wavebands but gradually decreases towards longer infrared and submillimeter wavebands for which the old stellar population becomes a non-negligible source of heating. Upon extrapolation of the results for M 51, we present prescriptions for estimating the contribution of young stars to the global dust heating based on a tight correlation between the dust heating fraction and specific star formation rate
Three-dimensional continuum radiative transfer simulations of dusty systems
3D continuum radiative transfer is one of the remaining grand challenge problems in computational astrophysics. Yet it is key to understanding the three-dimensional structure of astronomical objects for which we can observe only two-dimensional projections on the plane of the sky. We present SKIRT, a Monte Carlo code designed to treat 3D continuum radiative transfer problems in dusty systems. It has been used to study the effects of dust absorption, scattering and emission on the observed properties of galaxies, circumstellar discs and AGNs. The code can handle arbitrary geometries and different dust mixtures, even at large optical depths and/or including very small grains. We present a number of recent computational techniques that have been instrumental in making the code fast and reliable, even for complex geometries. We also show some recent 3D simulations to highlight the possibilities of modern radiative transfer codes