[Si II], [Fe II], [C II], and H2 Emission from Massive Star-forming Regions

By M. Kaufman, M. Wolfire, D. Hollenbach. 2006

231 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/3c181e48e7e57edf5a8a9ee73af226f6607a32f2

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Citations in the corpus

Diagnostics of irradiated dense gas in galaxy nuclei. II. A grid of XDR and PDR models (2006, background): “Wolfire et al. (1990) were the first to show [CII]/[SiII] contour plots for PDRs. Recently, Kaufman et al. (2006) showed updated plots for [SiII] and [FeII] for PDR gas.”
An Overview of the Dwarf Galaxy Survey (2013, background): “These important cooling lines are diagnostics to probe the FUV flux, the gas density (n) and temperature (T), and the filling factor of the ionized gas and photodissociation regions (e.g., Wolfire et al. 1990; Kaufman et al. 2006).”
A Herschel/PACS Far-infrared Line Emission Survey of Local Luminous Infrared Galaxies (2017, methodology): “The PDRT is based on the models developed by Kaufman et al. (1999, 2006), which calculate the temperature structure and line emission from a PDR, based on the formalism for a one-dimensional semi-infinite slab (Tielens & Hollenbach 1985).”
OBSERVATIONS OF Arp 220 USING HERSCHEL-SPIRE: AN UNPRECEDENTED VIEW OF THE MOLECULAR GAS IN AN EXTREME STAR FORMATION ENVIRONMENT (2011, background): “We explore a PDR model grid (Kaufman et al. 2006; Wolfire et al. 2010) with predic- tions for CO line fluxes from J = 1-0 to J = 30-29, generated over a large range in density ( 101 − 107 cm−3) and incident FUV flux, Log G0 (-0.5 – 6.5), where G0 is the FUV flux in units of the local interstellar…”
The applicability of far-infrared fine-structure lines as star formation rate tracers over wide ranges of metallicities and galaxy types (2014, background): “Indeed, PDR models have shown that this ratio increases toward higher gas density and radiation field strength (Kaufman et al. 2006).”
WATER, O2, AND ICE IN MOLECULAR CLOUDS (2008, methodology): “The numerical code we have developed to model the chemical and thermal structure of an opaque cloud externally illuminated by FUV flux is based on our previous models of PDRs, which are described in Tielens & Hollenbach (1985), Hollenbach et al. (1991), and Kaufman et al. (1999, 2006).”
The Herschel Dwarf Galaxy Survey - I. Properties of the low-metallicity ISM from PACS spectroscopy (2015, background): “We note that there is no study on large samples of galaxies that self-consistently models the H ii region and the PDR, besides the work on IR luminous galaxies by Abel et al. (2009) and Graciá-Carpio et al. (2011) and on individual objects in Kaufman et al. (2006).”
THE DARK MOLECULAR GAS (2010, methodology): “The distribution of temperature, density, and abundances within the H I, H2, and CO layers are calculated using the PDR code of Kaufman et al. (2006).”
Warm Molecular Hydrogen in the Spitzer SINGS Galaxy Sample (2007, background): “The H2 line ratios, compared with the PDRmodel of Kaufman et al. (2006), do not indicate lower gas densities, on average, in galaxies with OPRhigh T < 3 than in galaxies with OPRhigh T ¼ 3.”