THE 2013 RELEASE OF CLOUDY

By G. Ferland, R. Porter, P. V. Hoof, R. Williams, N. Abel, M. Lykins, G. Shaw, W. Henney, P. C. S. U. O. Kentucky, U. Georgia and 9 more. 2013

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This is a summary of the 2013 release of the plasma simulation code Cloudy. Cloudy models the ionization, chemical, and thermal state of material that may be exposed to an external radiation field or other source of heating, and predicts observables such as emission and absorption spectra. It works in terms of elementary processes, so is not limited to any particular temperature or density regime. This paper summarizes advances made since the last major review in 1998. Much of the recent development has emphasized dusty molecular environments, improvements to the ionization/chemistry solvers, and how atomic and molecular data are used. We present two types of simulations to demonstrate the capability of the code. We consider a molecular cloud irradiated by an X-ray source such as an active nucleus and show how treating EUV recombination lines and the full SED affects the observed spectrum. A second example illustrates the very wide range of particle and radiation density that can be considered.

Subfields: Atmospheric Science, Atomic and Molecular Physics, and Optics, Mechanics of Materials

View Paper: https://www.semanticscholar.org/paper/e8bb92e8712c1ffc0c68ae109da441aee62feea9

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Citations in the corpus

H$_2$ formation on interstellar dust grains: the viewpoints of theory, experiments, models and observations (2017, methodology): “…and grains. urrent major examples include the Meudon PDR code ( Le Bour- ot et al., 2012; Le Petit et al., 2006 ), the KOSMA- τ code ( Röllig t al., 2013; Störzer et al., 1996 ), CLOUDY ( Ferland et al., 2013 ), and he PDR codes of Kaufman et al. (2006) , 1999 ) or of Meijerink and paans (2005) .”
A BUDGET AND ACCOUNTING OF METALS AT z ∼ 0: RESULTS FROM THE COS-HALOS SURVEY (2013, result): “00, last described by Ferland et al. 2013) models that are consistent with the column densities of the H I and metal ions determined from the observed UV spectra.”
CIGALE: a python Code Investigating GALaxy Emission (2018, methodology): “To model the nebular emission in CIGALE we have adopted nebular templates based on Inoue (2011), which have been generated using CLOUDY 13.01 (Ferland et al. 1998, 2013).”
A new determination of the primordial He abundance using the He i λ10830 Å emission line: cosmological implications (2014, methodology): “Izotov et al. (2013) have also checked the validity of the above overall procedure for determining the He abundance by using photoionisation CLOUDY models (Ferland et al. 1998, 2013).”
Spectroscopic detections of C iii] λ1909 Å at z ≃ 6–7: a new probe of early star-forming galaxies and cosmic reionization (2014, methodology): “We use the latest version of the Bruzual & Charlot (2003) stellar population synthesis model with the standard photoionisation code CLOUDY (Ferland et al. 2013) to describe both the stellar and gaseous emission (Gutkin et al., in preparation, who follow the prescription of Charlot & Longhetti 2001).”
Modelling and interpreting spectral energy distributions of galaxies with BEAGLE (2016, methodology): “These models combine the stellar population synthesis code described in Section 2.1 above with the latest version of the photoionization code CLOUDY (version 13.3, last described by Ferland et al. 2013).”
A bright year for tidal disruptions (2015, unknown): “18 of Ferland et al. 2013). by the ionization parameter, which for the TDE ejecta is given by ξ = 4πFH nej = πcmpEH nejVn ≈ πmpRnLacc nejVn(1 − A) ≈ { 1.5 × 103 erg cm s−1 β1/2η−1 f 3/2in,−2 M 1/3 •,6 m −7/30 ?”
Lyα and C iii] emission in z = 7–9 Galaxies: accelerated reionization around luminous star-forming systems? (2016, methodology): “The version of BEAGLE used here relies on the models of Gutkin et al. (in preparation), who follow the prescription of Charlot & Longhetti (2001) to describe the emission from stars and the interstellar gas, based on a combination of the latest version of the Bruzual & Charlot (2003) stellar populat”
Photometric redshifts for the SDSS Data Release 12 (2016, background): “…– is a difficulty because of the number of extra parameters needed to model the interstellar medium, but additional theoretical assumptions (Stasińska 1984; Fioc & Rocca-Volmerange 1997; Ferland et al. 2013) or empirical line estimation (Győry et al. 2011; Beck et al. 2016) can still be used.”
J1154+2443: a low-redshift compact star-forming galaxy with a 46 per cent leakage of Lyman continuum photons (2017, methodology): “Comparing the extinction-corrected Lyα/Hβ flux ratio of 31.3 (Table 6) and the case B flux ratio of 31.9 obtained with the cloudy code (Ferland et al. 1998, 2013) for an electron temperature Te = 18300K and an electron number density Ne = 1000 cm−3, we find that the Lyα escape fraction is fesc(Lyα)…”
Deriving model-based Te-consistent chemical abundances in ionized gaseous nebulae (2014, methodology): “Besides, a large grid of cloudy (Ferland et al. 2013) photoionisation models was computed and their relative optical emission lines, O/H, N/O, and log U were collected.”
De re metallica: the cosmic chemical evolution of galaxies (2018, methodology): “Generally, the classical approach is to use detailed photoionization codes, such as CLOUDY (Ferland et al., 2013) or Mappings (Binette, 1985; Sutherland & Dopita, 1993; Dopita et al., 2013) to generate a grid of models out of which a number of line ratios are extracted and proposed as diagnostics…”
The Herschel Dwarf Galaxy Survey - I. Properties of the low-metallicity ISM from PACS spectroscopy (2015, methodology): “We model the H ii region and PDR simultaneously with the spectral synthesis code Cloudy v.13.03 (Ferland et al. 2013).”
Big Three Dragons: A z = 7.15 Lyman-break galaxy detected in [O iii] 88 μm, [C ii] 158 μm, and dust continuum with ALMA (2018, methodology): “Harikane et al. (2018) have interpreted the trend with photoionization models of CLOUDY (Ferland et al. 2013) implemented in spectral energy distribution (SED) models of BEAGLE (Chevallard & Charlot 2016).”
Spectroscopic detection of C iv λ1548 in a galaxy at z = 7.045: implications for the ionizing spectra of reionization-era galaxies (2015, methodology): “We use the models of Feltre et al. 2015 in prep., which represent the narrow line emission region (NLR) of the AGN and have been realized with the photoionization code CLOUDY (latest version C13.”
Ultraviolet emission lines in young low-mass galaxies at z ≃ 2: physical properties and implications for studies at z > 7 (2014, background): “…Longhetti (2001), they neglect the contribution by stars older than 10Myr to nebular emission and use the latest version of the standard photoionization code CLOUDY (Ferland et al. 2013) to compute the emission-line spectrum generated by younger stars, assuming that galaxies are ionization bounded.”
The Circumgalactic Medium (2017, methodology): “Radiative transfer models like Cloudy (Ferland et al. 2013) are used to build PIE models (e.g. Bergeron & Stasińska 1986; Prochaska et al. 2004; Lehnert et al. 2013; Werk et al. 2014; Turner et al. 2015), which are parametrized by density nH , or equivalently the ionization parameter logU ≡ Φ/nHc,…”
Fluctuating feedback-regulated escape fraction of ionizing radiation in low-mass, high-redshift galaxies (2017, methodology): “We include an extra cooling term for metals, using tabulated rates computed with Cloudy (last described in Ferland et al. 2013) above 104 K.”