14 research outputs found
On the probability distribution function of the mass surface density of molecular clouds. II
The probability distribution function (PDF) of the mass surface density of
molecular clouds provides essential information about the structure of
molecular cloud gas and condensed structures out of which stars may form. In
general, the PDF shows two basic components: a broad distribution around the
maximum with resemblance to a log-normal function, and a tail at high mass
surface densities attributed to turbulence and self-gravity. In a previous
paper, the PDF of condensed structures has been analyzed and an analytical
formula presented based on a truncated radial density profile, with central density and inner radius
, widely used in astrophysics as a generalization of physical density
profiles. In this paper, the results are applied to analyze the PDF of
self-gravitating, isothermal, pressurized, spherical (Bonnor-Ebert spheres) and
cylindrical condensed structures with emphasis on the dependence of the PDF on
the external pressure and on the overpressure ,
where is the central pressure. Apart from individual clouds, we also
consider ensembles of spheres or cylinders, where effects caused by a variation
of pressure ratio, a distribution of condensed cores within a turbulent gas,
and (in case of cylinders) a distribution of inclination angles on the mean PDF
are analyzed. The probability distribution of pressure ratios is
assumed to be given by , where , ,
, and are fixed parameters.Comment: 24 pages, 14 figure
The Spectral Energy Distribution of Self-gravitating Interstellar Clouds. I. Spheres
We derive the spectral energy distribution (SED) of dusty, isothermal, self-gravitating, stable and spherical clouds externally heated by the ambient interstellar radiation field (ISRF). For a given radiation field and dust properties, the radiative transfer problem is determined by the pressure of the surrounding medium and by the cloud mass expressed as a fraction of the maximum stable cloud mass above which the clouds become gravitationally unstable. To solve the radiative transfer problem, a ray-tracing code is used to accurately derive the light distribution inside the cloud. This code considers both anisotropic scattering on dust grains and multiple scattering events. The dust properties inside the clouds are assumed to be the same as in the diffuse interstellar medium in our Galaxy. We analyze the effect of the pressure, the critical mass fraction, and the ISRF on the SED and present brightness profiles in the visible, the IR/FIR, and the submillimeter/millimeter regime with the focus on the scattered emission and the thermal emission from PAH molecules and dust grains
The Spectral Energy Distribution of Self-gravitating Interstellar Clouds I. Spheres
We derive the spectral energy distribution (SED) of dusty, isothermal, self
gravitating, stable and spherical clouds externally heated by the ambient
interstellar radiation field. For a given radiation field and dust properties,
the radiative transfer problem is determined by the pressure of the surrounding
medium and the cloud mass expressed as a fraction of the maximum stable cloud
mass above which the clouds become gravitational unstable.
To solve the radiative transfer problem a ray-tracing code is used to
accurately derive the light distribution inside the cloud. This code considers
both non isotropic scattering on dust grains and multiple scattering events.
The dust properties inside the clouds are assumed to be the same as in the
diffuse interstellar medium in our galaxy. We analyse the effect of the
pressure, the critical mass fraction, and the ISRF on the SED and present
brightness profiles in the visible, the IR/FIR and the submm/mm regime with the
focus on the scattered emission and the thermal emission from PAH-molecules and
dust grains.Comment: accepted for publication in ApJS, May 2008, v176n1 issu
Modelling the Pan-Spectral Energy Distribution of Starburst Galaxies: IV The Controlling Parameters of the Starburst SED
We combine the the stellar spectral synthesis code Starburst99, the nebular
modelling code MAPPINGSIII, and a 1-D dynamical evolution model of HII regions
around massive clusters of young stars to generate improved models of the
spectral energy distribution (SED) of starburst galaxies. We introduce a
compactness parameter, C, which characterizes the specific intensity of the
radiation field at ionization fronts in HII regions, and which controls the
shape of the far-IR dust re-emission, often referred to loosely as the dust
``temperature''. We also investigate the effect of metallicity on the overall
SED and in particular, on the strength of the PAH features. We provide
templates for the mean emission produced by the young compact HII regions, the
older (10 - 100 Myr) stars and for the wavelength-dependent attenuation
produced by a foreground screen of the dust used in our model. We demonstrate
that these components may be combined to produce a excellent fit to the
observed SEDs of star formation dominated galaxies which are often used as
templates (Arp 220 and NGC 6240). This fit extends from the Lyman Limit to
wavelengths of about one mm. The methods presented in both this paper and in
the previous papers of this series allow the extraction of the physical
parameters of the starburst region (star formation rates, star formation rate
history, mean cluster mass, metallicity, dust attenuation and pressure) from
the analysis of the pan-spectral SED.Comment: 35 pages, 21 figures, accepted for publication in ApJS full-res
available at http://www.strw.leidenuniv.nl/~brent/publications/SEDIV.pd
Intracluster Dust and Far Infrared Emission
We make predictions for the diffuse far-infrared (FIR) emission from dust in the intracluster medium (ICM) of the Virgo cluster. The dust injection rate from known sources in the cluster is unlikely to give rise to a detectable diffuse FIR IC emission. However, the outer regions of dynamically young clusters have a further potential source of IC grains since they are still accreting freshly infalling spiral galaxies which are presumably contained in an accreting intergalactic medium (IGM). We show that cosmics ray driven winds from the infalling spirals can inject grains into a subvirial IGM that is external to the observed X-ray-emitting ICM. Predictions for the Virgo cluster are generalised to other clusters, and the possibility of detection of dynamically young clusters at cosmological distances is discussed. Although dominated by discrete source emission from galactic disks, it is possible that diffuse sub-mm dust emission from the ICM could be detected in experiments similar to those designed to map the sub-mm excess due to the Sunyaev-Zeldovich effect in distant clusters. We further discuss the implications of our proposed scenario for the optical extinction in clusters, as well as for the properties and dust content of the IGM. Further implications for environmental effects on the chemical evolution of spiral galaxies are also considered
On the probability distribution function of the mass surface density of molecular clouds. II.
Determining the fraction of dust heating from young and old stellar populations with 3D dust radiative transfer
Abstract. A major difficulty hampering the accuracy of UV/optical star formation rate tracers is the effect of interstellar dust, absorbing and scattering light produced by both young and old stellar populations (SPs). Although empirically calibrated corrections or energy balance SED fitting are often used for fast de-reddening of galaxy stellar emission, eventually only radiative transfer calculations can provide self-consistent predictions of galaxy model spectra, taking into account important factors such as galaxy inclination, different morphological components, nonlocal heating of the dust and scattered radiation. In addition, dust radiative transfer can be used to determine the fraction of monochromatic dust emission powered by either young or old
SPs. This calculation needs to take into account the different response of the dust grains to the UV and optical radiation field, depending on the grain size and composition. We determined the dust heating fractions, on both global and local scales, for a high-resolution galaxy model by using our 3D ray-tracing dust radiative transfer code “DART-Ray”. We show the results obtained using this method and discuss the consequences for star formation rate indicators