Modeling the Pan-Spectral Energy Distribution of Starburst Galaxies. IV. The Controlling Parameters of the Starburst SED

By B. Groves, M. Dopita, R. Sutherland, Lisa J. Kewley, J. Fischera, C. Leitherer, B. Brandl, W. V. van Breugel. 2007

190 citations recorded by the source corpus.

We combine the stellar spectral synthesis code Starburst99, the nebular modeling code MAPPINGS III and a one-dimensional dynamical evolution model of H II 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 H II regions and which controls the shape of the far-infrared (IR) dust reemission, 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 polycyclic aromatic hydrocarbon (PAH) features. We provide templates for the mean emission produced by the young compact H II 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 1 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.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/dd06483c3bb403389acbd5b882043f61d41b1989

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

Citations in the corpus

A Compendium of Far-Infrared Line and Continuum Emission for 227 Galaxies Observed by the Infrared Space Observatory (2008, background): “…1991; Spinoglio & Malkan 1992; Rubin et al. 1994; Kaufman et al. 1999; Abel et al. 2005; Le Petit et al. 2006; Meijerink, Spaans, Israel 2007; Groves et al. 2008), these fine structure transitions can be used to derive gas temperatures, densities, and the intensity of the radiation fields in…”
The CO-H2 Conversion Factor in Disc Galaxies and Mergers (2011, methodology): “These birthclouds contain HIIregions and photodissociation regions (PDRs) whose SEDs are calculated utilising 1D MAPPINGSIII photoionisation models (Groves et al. 2004, 2008; Jonsson et al. 2010).”
The formation of high-redshift submillimetre galaxies (2009, background): “For young stellar clusters, which are still located in their nascent birth clouds of molecular gas, the input spectrum includes the effects of the H II regions and photodissociation regions (PDRs) surrounding the clusters (Groves et al. 2008).”
A physical model for z∼ 2 dust-obscured galaxies (2009, methodology): “5 of Groves et al. 2008).”
The eagle simulations of galaxy formation: Public release of halo and galaxy catalogues (2015, methodology): “, 2003; Camps and Baes, 2015), with galaxev (Bruzual and Charlot, 2003) and mappings iii (Groves et al., 2008) spectra to represent star particles and young Hii regions respectively, as described by Trayford et al.”
Dusty Star Forming Galaxies at High Redshift (2014, background): “The UV absorption and subsequent long-wavelength re-emission from the cold PDRs surrounding young stellar clusters formed in the galaxy merger is captured in sunrise via the inclusion of mappings photoionization calculations (Groves et al., 2008).”
A TWO-PARAMETER MODEL FOR THE INFRARED/SUBMILLIMETER/RADIO SPECTRAL ENERGY DISTRIBUTIONS OF GALAXIES AND ACTIVE GALACTIC NUCLEI (2014, background): “…Science Center, California Institute of Technology, Pasadena, CA 91125, USA 5School of Astronomy and Space Science, Nanjing University, Nanjing, 210093, China 2 Siebenmorgen & Krügel 2007; Draine & Li 2007; da Cunha et al. 2008; Galliano et al. 2008; Groves et al. 2008; Hermelo et al. 2013).”
Submillimetre galaxies in a hierarchical universe: number counts, redshift distribution, and implications for the IMF (2012, methodology): “The (sub)mm fluxes are similar if the LMC or SMC dust models are used. at H averford C ollege L ibrary on Septem ber 30, 2014 http://m nras.oxfordjournals.org/ D ow nloaded from Once the star and BH particles are assigned SEDs and the dust density field is specified, SUNRISE performs the radiative t”
ON SIZES, KINEMATICS, M/L GRADIENTS, AND LIGHT PROFILES OF MASSIVE COMPACT GALAXIES AT z ∼ 2 (2010, methodology): “In addition, SUNRISE uses a sub-grid model to account for the attenuation by birthclouds (HII and photodissociation regions) that surround young star clusters, computed using the photoionization code MAPPINGS (Groves et al. 2008).”
Fitting the integrated spectral energy distributions of galaxies (2010, methodology): “However to determine the emission from other elements, or to take account of both gas and dust absorption, full radiative transfer is needed using photoionization codes such as CLOUDY (Ferland et al. 1998) or Mappings III (Groves et al. 2008).”
Modeling the Panchromatic Spectral Energy Distributions of Galaxies (2013, methodology): “…starlight (or simply the radiation field) to predict IR emission (Desert, Boulanger & Puget 1990; Silva et al. 1998; Devriendt, Guiderdoni & Sadat 1999; Popescu et al. 2000; Dale et al. 2001; Piovan, Tantalo & Chiosi 2006; Jonsson 2006; Draine & Li 2007; Groves et al. 2008; Popescu et al. 2011).”
Modelling the spectral energy distribution of galaxies - V. The dust and PAH emission SEDs of disk galaxies (2010, methodology): “The solid line is the adopted model for the PDR dust, PAH emission from Groves et al. (2008), having compactness parameterlog(C) = 6.5, metallicity 1.0, and PDR column densitylog(N) = 22.0.”
High-resolution panchromatic spectral models of galaxies including photoionization and dust (2009, methodology): “…closely the details of the local environment, such as metallicity, radiation field (including hard spectrum AGN), clumpy versus diffuse ISM, etc., with the details of the dust, such as the PAH fraction (as done within Groves et al. 2008), or dust size distribution (i.e. Milky Way versus LMC).”
THE EMISSION BY DUST AND STARS OF NEARBY GALAXIES IN THE HERSCHEL KINGFISH SURVEY (2011, background): “This appears to be consistent with Groves et al. (2008), who found in their SEDmodels that the IR peak shifts to longer wavelengths and becomes broader with increasing metallicity, due to the increasing dust column and the increasing mechanical luminosity of starburst regions.”
The effect of photoionization on the cooling rates of enriched, astrophysical plasmas (2008, result): “In Figure 1 we compare our CIE results (i.e., cloudy version 07.02) with those of Gnat & Sternberg (2007) (who used cloudy version 06.02), Sutherland & Dopita (1993) (who used mappings) and also with mappings iii (version r; Groves et al. 2008).”