Simultaneously modelling far-infrared dust emission and its relation to CO emission in star-forming galaxies. Issue 1 (21st April 2016)

• Record Type: Journal Article
• Authors: Shetty, Rahul; Roman-Duval, Julia; Hony, Sacha; Cormier, Diane; Klessen, Ralf S.; Konstandin, Lukas K.; Loredo, Thomas; Pellegrini, Eric W.; Ruppert, David
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 460:Issue 1(2016)
• Page Start: 67
• Page End: 81
• Publication Date: 2016-04-21
• Subjects: methods: statistical -- stars: formation -- galaxies: ISM -- Magellanic Clouds -- galaxies: star formation; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stw930
• Languages: English
• ISSNs: 0035-8711

Abstract

Abstract: We present a method to simultaneously model the dust far-infrared (FIR) spectral energy distribution (SED) and the total infrared – carbon monoxide (CO) integrated intensity ( S IR – I CO ) relationship. The modelling employs a hierarchical Bayesian (HB) technique to estimate the dust surface density, temperature ( T eff ), and spectral index at each pixel from the observed FIR maps. Additionally, given the corresponding CO map, the method simultaneously estimates the slope and intercept between the FIR and CO intensities, which are global properties of the observed source. The model accounts for correlated and uncorrelated uncertainties, such as those present in Herschel observations. Using synthetic data sets, we demonstrate the accuracy of the HB method, and contrast the results with common non-hierarchical fitting methods. As an initial application, we model the dust and gas on 100 pc scales in the Magellanic Clouds from Herschel FIR and NANTEN CO observations. The slopes of the log S IR –log I CO relationship are similar in both galaxies, falling in the range 1.1–1.7. However, in the Small Magellanic Cloud the intercept is nearly three times higher, which can be explained by its lower metallicity than the Large Magellanic Cloud (LMC), resulting in a larger S IR per unit I CO . The HB modelling evidences an increase in T eff in regions with the highest I CO in the LMC. This may be due to enhanced dust heating in the densest molecular regions from young stars. Such simultaneous dust and gas modelling may reveal variations in the properties of the interstellar medium and its association with other galactic characteristics, such as star formation rates and/or metallicities.