The MAPPINGS III Library of Fast Radiative Shock Models

By M. Allen, B. Groves, M. Dopita, R. Sutherland, Lisa J. Kewley. 2008

533 citations recorded by the source corpus.

We present a new library of fully radiative shock models calculated with the MAPPINGS III shock and photoionization code. The library consists of grids of models with shock velocities in the range vs = 100–1000 km s−1 and magnetic parameters B/n1/2 of 10−4 to 10 μG cm3/2 for five different atomic abundance sets and for a preshock density of 1.0 cm−3. In addition, solar abundance model grids have been calculated for densities of 0.01, 0.1, 10, 100, and 1000 cm−3 with the same range in vs and B/n1/2. Each model includes components of both the radiative shock and its photoionized precursor, ionized by the extreme ultraviolet (EUV) and soft X-ray radiation generated in the radiative gas. We present the details of the ionization structure, the column densities, and the luminosities of the shock and its precursor. Emission-line ratio predictions are separately given for the shock and its precursor as well as for the composite shock+precursor structure to facilitate comparison with observations in cases in which the shock and its precursor are not resolved. Emission-line ratio grids for shock and shock+precursor are presented on standard line ratio diagnostic diagrams, and we compare these grids to observations of radio galaxies and a sample of AGNs and star-forming galaxies from the Sloan Digital Sky Survey. This library is available online, along with a suite of tools to enable the analysis of the shocks and the easy creation of emission line ratio diagnostic diagrams. These models represent a significant increase in parameter space coverage over previously available models and, therefore, provide a unique tool in the diagnosis of emission by shocks.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/5cd08bbfb2dc1afccd4ffce4ef3515015282ab08

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

1. P. Hopkins
2. L. Hernquist
3. M. Cappellari
4. C. Conroy
5. P. V. van Dokkum
6. R. Dav'e
7. R. Somerville
8. T. Naab

In Nuclear and High Energy Physics

1. A. Benson
2. T. Naab
3. Lisa J. Kewley
4. R. Yan
5. Joss Bland-Hawthorn
6. M. McQuinn
7. T. Heckman
8. M. Dopita

Citations in the corpus

• H$_2$ formation on interstellar dust grains: the viewpoints of theory, experiments, models and observations (2017, background): “Fast shocks, ranging over 100 − 10 0 0 km s −1 , heat the gas to high temperatures ( T ≈ 10 6 − 10 8 K), and produce EUV and X-ray photons that photo-ionize the tenuous medium ( Allen et al., 2008 ).”
• GAS-PHASE OXYGEN GRADIENTS IN STRONGLY INTERACTING GALAXIES. I. EARLY-STAGE INTERACTIONS (2010, background): “In fact, the north half of UGC 12914 has a significant number of regions with multiple velocity components and shocklike line ratios (Allen et al. 2008; Rich et al. 2010).”
• THE COS-HALOS SURVEY: ORIGINS OF THE HIGHLY IONIZED CIRCUMGALACTIC MEDIUM OF STAR-FORMING GALAXIES (2016, methodology): “Here we use the results of Allen et al. (2008) who produce tables that are valid for solar metallicity, shock speeds that range from 100 − 1000 km s−1 and pressure exerted by the transverse magnetic field (Bn− 1 2 ) ranging from 10−4 µG cm−3/2 - 10 µG cm−3/2.”
• The SAMI Galaxy Survey: shocks and outflows in a normal star-forming galaxy (2014, methodology): “The density indicators [S II] λλ6716,31 come from the post-shock recombination regions where the gas densities are expected to be higher than the pre-shock densities (e.g., figure 12 in Allen et al. 2008).”
• A characteristic oxygen abundance gradient in galaxy disks unveiled with CALIFA (2013, background): “On the other hand it does not guarantee the exclusion of other sources of non stellar ionization that can populate this area, such as shocks (e.g., Allen et al. 2008; Levesque et al. 2010), postAGB stars (e.g., Kehrig et al. 2012), and dusty AGNs (e.g., Groves et al. 2004).”
• Nuclear activity versus star formation: emission-line diagnostics at ultraviolet and optical wavelengths (2015, methodology): “…emission from H ii regions and AGN often rely on the predictions of standard photoionization codes, such as MAPPINGS (Sutherland & Dopita 1993; Allen et al. 2008; Dopita et al. 2013) and CLOUDY (Ferland 1993; Ferland et al. 1998, 2013), which have both undergone regular updates over the past…”
• A Herschel/PACS Far-infrared Line Emission Survey of Local Luminous Infrared Galaxies (2017, background): “…which is based on the Starburst99 stellar evolution synthesis mod- els (Leitherer et al. 1999) and the shock and photoionization mappings iii code (Allen et al. 2008), to explore the properties of the dense ionized gas surrounding newly formed stars as a function of the main physical parameters…”
• SDSS-IV MaNGA : the impact of diffuse ionized gas on emission-line ratios, interpretation of diagnostic diagrams and gas metallicity measurements (2016, background): “[O i]/Hα is also an excellent tracer of shocks (Dopita et al. 2000; Kewley et al. 2002; Allen et al. 2008).”
• Relativistic jet feedback in high-redshift galaxies – I. Dynamics (2016, unknown): “Dopita 1993; Allen et al. 2008).”
• Galaxy formation theory (2010, methodology): “These functions were calculated using the MappingsIII code of Allen et al. (2008) with a photoionizing background computed self-consistently from the galaxy formation model ofBenson et al. (2002a) and an assumed metallicity of Z = 0.3Z⊙.”
• The Circumgalactic Medium (2017, background): “…heat across the bound- 14 Tumlinson, Peeples, & Werk ary (Gnat, Sternberg & McKee 2010; Armillotta et al. 2016), and (4) ionized gas behind radiative shocks, perhaps produced by strong galactic winds (Dopita & Sutherland 1996; Heckman et al. 2002; Allen et al. 2008; Gnat & Sternberg 2009).”
• SDSS IV MaNGA – spatially resolved diagnostic diagrams: a proof that many galaxies are LIERs (2016, background): “It is well known that the BPT diagram does not represent a good test for shock ionisation, as shock models cover larger areas of both the LIER and SF sequences (Allen et al. 2008; Rich et al. 2010, 2011; Ho et al. 2014; Alatalo et al. 2016).”
• EVIDENCE FOR WIDE-SPREAD ACTIVE GALACTIC NUCLEUS-DRIVEN OUTFLOWS IN THE MOST MASSIVE z ∼ 1–2 STAR-FORMING GALAXIES (2014, background): “…derived from the (A color version of this figure is available in the online journal.) data of our sample and compares them with various recent excitation/ionization models (Kewley et al. 2001, 2006, 2013; Allen et al. 2008; Rich et al. 2010, 2011; Sharp & BlandHawthorn 2010; Newman et al. 2014).”