How do supernova remnants cool? -- I. Morphology, optical emission lines, and shocks

Abstract

Supernovae (SNe) inject $\sim 10^{51}$ erg in the interstellar medium, thereby shocking and heating the gas. A substantial fraction of this energy is later lost via radiative cooling. We present a post-processing module for the FLASH code to calculate the cooling radiation from shock-heated gas using collisional excitation data from MAPPINGS V. When applying this tool to a simulated SN remnant (SNR), we find that most energy is emitted in the EUV. However, optical emission lines ($[$O III$]$, $[$N II$]$, $[$S II$]$, H$\alpha$, H$\beta$) are usually best observable. Our shock detection scheme shows that [S II] and [N II] emissions arise from the thin shell surrounding the SNR, while [O III], H$\alpha$, and H$\beta$ originate from the volume-filling hot gas inside the SNR bubble. We find that the optical emission lines are affected by the SNR's complex structure and its projection onto the plane of the sky because the escaping line luminosity can be reduced by 10 -- 80\% due to absorption along the line-of-sight. Additionally, the subtraction of contaminating background radiation is required for the correct classification of an SNR on the oxygen or sulphur BPT diagrams. The electron temperature and density obtained from our synthetic observations match well with the simulation but are very sensitive to the assumed metallicity.

arXiv comment18 pages, 13 figures, accepted for publication in MNRAS

References in corpus (82)

• SciPy 1.0--Fundamental Algorithms for Scientific Computing in Python
• Array Programming with NumPy
• The Sloan Digital Sky Survey: Technical Summary
• The chemical composition of the Sun
• Star Formation in Galaxies Along the Hubble Sequence
• The Host Galaxies of AGN
• Theoretical Modeling of Starburst Galaxies
• Dust Grain Size Distributions and Extinction in the Milky Way, LMC, and SMC
• A Multi-Code Analysis Toolkit for Astrophysical Simulation Data
• Nuclear Activity in Nearby Galaxies
• The MAPPINGS III Library of Fast Radiative Shock Models
• PyNeb: a new tool for analyzing emission lines. I. Code description and validation of results
• Understanding Galaxy Evolution through Emission Lines
• Supernova remnants: the X-ray perspective
• Momentum Injection by Supernovae in the Interstellar Medium
• The SILCC (SImulating the LifeCycle of molecular Clouds) project: I. Chemical evolution of the supernova-driven ISM
• The Definitive Abundance of Interstellar Oxygen
• Semi-empirical analysis of Sloan Digital Sky Survey galaxies III. How to distinguish AGN hosts
• Simulating the formation of molecular clouds. I. Slow formation by gravitational collapse from static initial conditions
• Planetary Nebulae as Standard Candles. XII. Connecting the Population I and Population II Distance Scales
• X-Ray Emission From the Shell-Type SNR G347.3-0.5
• The PHANGS-MUSE survey -- Probing the chemo-dynamical evolution of disc galaxies
• A revised catalogue of 294 Galactic supernova remnants
• The SILCC (SImulating the LifeCycle of molecular Clouds) project - II. Dynamical evolution of the supernova-driven ISM and the launching of outflows
• The energy and momentum input of supernova explosions in structured and ionised molecular clouds
• The SILCC project: III. Regulation of star formation and outflows by stellar winds and supernovae
• Modeling the Warm Ionized Interstellar Medium and Its Impact on Elemental Abundance Studies
• The Abundance of Interstellar Nitrogen
• Modelling CO formation in the turbulent interstellar medium
• Modelling the supernova-driven ISM in different environments
• Effects of Pre-ionisation in Radiative Shocks I: Self-Consistent Models
• SILCC-Zoom: The dynamical and chemical evolution of molecular clouds
• Variable interstellar radiation fields in simulated dwarf galaxies: supernovae versus photoelectric heating
• Mutual influence of supernovae and molecular clouds
• The Generation and Dissipation of Interstellar Turbulence - Results from Large Scale High Resolution Simulations
• SILCC VI -- Multi-phase ISM structure, stellar clustering, and outflows with supernovae, stellar winds, ionising radiation and cosmic rays
• The SILCC project --- IV. Impact of dissociating and ionising radiation on the interstellar medium and Halpha emission as a tracer of the star formation rate
• Theoretical ISM pressure and electron density diagnostics for local and high-redshift galaxies
• Supernova feedback in a local vertically stratified medium: interstellar turbulence and galactic winds
• Ion-by-ion Cooling efficiencies
• Imprints of galaxy evolution on H ii regions Memory of the past uncovered by the CALIFA survey
• Composite Spectra in Merging U/LIRGs Caused by Shocks
• Tree-based solvers for adaptive mesh refinement code FLASH - I: gravity and optical depths
• Abundances and Physical Conditions in the Warm Neutral Medium Towards mu Columbae
• XMM-Newton observations of the Galactic Supernova Remnant CTB 109 (G109.1-1.0)
• Optical IFU Observations of the Brightest Cluster Galaxy NGC 4696: The Case for a Minor Merger and Shock-excited Filaments
• Supernova-blast waves in wind-blown bubbles, turbulent, and power-law ambient media
• Supernova Remnants Interacting with Molecular Clouds: X-ray and Gamma-ray Signatures
• The SILCC project - V. The impact of magnetic fields on the chemistry and the formation of molecular clouds
• Extensive Online Shock Model Database
• 3D MHD modeling of the expanding remnant of SN 1987A. Role of magnetic field and non-thermal radio emission
• Discovery of New Interacting Supernova Remnants in the Inner Galaxy
• SILCC VII -- Gas kinematics and multiphase outflows of the simulated ISM at high gas surface densities
• Circumstellar interaction in supernovae in dense environments - an observational perspective
• Hot phase generation by supernovae: resolution, chemistry and thermal conduction
• Is molecular cloud turbulence driven by external supernova explosions?
• The many faces of LINER-like galaxies: a WISE view
• Galaxy emission line classification using 3D line ratio diagrams
• Constraining Photoionization Models With a Reprojected Optical Diagnostic Diagram
• Multi-dimensional simulations of the expanding supernova remnant of SN 1987A
• Chandra observation of the Galactic supernova remnant CTB 109 (G109.1-1.0)
• A Machine Learning Artificial Neural Network Calibration of the Strong-Line Oxygen Abundance
• Powerful t-SNE technique leading to clear separation of type-2 AGN and HII galaxies in BPT diagrams
• Kinematics of the Galactic SNR G109.1-1.0 (CTB 109)
• Numerical simulations of supernova remnants in turbulent molecular clouds
• Discovery of optical emission from the supernova remnant G 32.8-0.1 (Kes 78)
• SHOCKFIND - An algorithm to identify magnetohydrodynamic shock waves in turbulent clouds
• Multidimensional Data Driven Classification of Emission-line Galaxies
• Multi-wavelength study of the G 82.2+5.3 supernova remnant
• Dynamical Evolution and Radiative Processes of Supernova Remnants
• The supernova remnants G67.7+1.8, G31.5-0.6 and G49.2-0.7
• Non-equilibrium ionisation and radiative transport in an evolving supernova remnant
• Deep optical observations of the supernova remnants G 126.2+1.6, G 59.8+1.2 and G 54.4-0.3
• Deep optical study of the mixed-morphology supernova remnant G 132.7+1.3 (HB3)
• First optical light from the supernova remnant G 17.4-2.3
• The kinematics of the bi-lobal supernova remnant G 65.3+5.7 - Paper II
• Optical Emission Associated with the Galactic Supernova Remnant G179.0+2.6
• Constraining the Age and Distance of the Galactic Supernova Remnant G156.2+5.7 by H-alpha Expansion Measurements
• Optical emission lines in the most massive galaxies: morphology, kinematics and ionisation properties
• A Machine Learning Approach to Integral Field Unit Spectroscopy Observations: II. HII Region LineRatios
• First 3D Morpho-Kinematic model of Supernova Remnants. The case of VRO 42.05.01 (G 166.0+4.3)
• 3D Hydrodynamic Simulations of the Galactic Supernova Remnant CTB 109

Cited by in corpus (5)

• Discovery of $\sim$2200 new supernova remnants in 19 nearby star-forming galaxies with MUSE spectroscopy
• Cloud Formation by Supernova Implosion
• SISSI: Supernovae in a stratified, shearing interstellar medium -- I. The geometry of supernova remnants
• How do supernova remnants cool? II. Machine learning analysis of supernova remnant simulations
• Discovery of young, oxygen-rich supernova remnants in PHANGS-MUSE galaxies