Supernova Remnants as Clues to Their Progenitors

Patnaude, Daniel; Badenes, Carles

doi:10.1007/978-3-319-21846-5_98

Cited by 9 publications

(9 citation statements)

References 62 publications

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“…The shock-heated SN ejecta become luminous in the SNR phase, which can probe the progenitor type and the detailed explosion mechanism. Meanwhile, the shocked circumstellar material (CSM) can help to trace the history of the progenitor evolution up to thousands even millions of years before the explosion (see, e.g., Patnaude & Badenes 2017, for a recent review). However, identification of the progenitor and explosion type for individual SNRs remains a major challenge in SNR studies.…”

Section: Sn Progenitormentioning

confidence: 99%

An XMM-Newton X-Ray View of Supernova Remnant W49B: Revisiting Its Recombining Plasmas and Progenitor Type

Sun

Chen

2020

ApJ

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We present a comprehensive X-ray spectroscopy and imaging study of supernova remnant W49B using archival XMM-Newton observations. The overionization state of the shocked ejecta in W49B is clearly indicated by the radiative recombination continua of Si XIV, S XV, and Fe XXV, combined with the Lyα lines of Ca and Fe. The line flux images of W49B indicate high emission measures of the central bar-like region for almost all the emission lines, while the equivalent width maps reveal a stratified structure for the metal abundance distributions. The global spectrum of W49B is well reproduced by a model containing one collisional ionization equilibrium (CIE) plasma component and two recombining plasma (RP) components. The CIE plasma represents the shocked interstellar medium, which dominates the X-ray emitting volume in W49B with a mass ∼ 450M . The two RP components with a total mass ∼ 4.6M are both dominated by the ejecta material, but characterized by different electron temperatures (∼ 1.60 keV and ∼ 0.64 keV). The recombination ages of the RP components are estimated as ∼ 6000 yr and ∼ 3400 yr, respectively. We then reveal the possibility of a thermal conduction origin for the high-temperature RP in W49B by calculating the conduction timescale. The metal abundance ratios of the ejecta in W49B are roughly consistent with a core-collapse explosion model with a 15M progenitor, except for a rather high Mn/Fe. A Type Ia origin can explain the Mn abundance, while it predicts much higher ejecta masses than observed values for all the metal species considered in our analysis.

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Section: Sn Progenitormentioning

confidence: 99%

An XMM-Newton X-Ray View of Supernova Remnant W49B: Revisiting Its Recombining Plasmas and Progenitor Type

Sun

Chen

2020

ApJ

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“…When the mesa models reach core-collapse, determined to be when Fe core infall exceeds 1000 km s −1 , we save the final model and pass it to the Supernova Explosion Code (snec). As discussed in Patnaude et al (2017), snec (Morozova et al 2015) has been modified to include explosive nucleosynthesis (the so-called approx21 network), and a Helmholtz Equation of State (Timmes & Swesty 2000). The progenitor models are exploded with snec, and evolved to an age of 100 days.…”

Section: Modeling Supernovae With Snecmentioning

confidence: 99%

“…Core-collapse (CC) supernova remnants (SNR) are important drivers of galactic evolution, as well as tracers of massive star populations and their evolution. Broadband observations have yielded a wealth of information about remnants, but coupling observations to theory requires sifting through a great deal of uncertainty in the parameters that dictate evolution (e.g., Patnaude & Badenes 2017). In particular, stellar mass loss rates throughout the life of the progenitor star can have a strong impact on the structure and dynamics of the resulting remnant (Patnaude et al 2015(Patnaude et al , 2017.…”

Section: Introductionmentioning

confidence: 99%

“…In the case of some Type IIP SNe, radio observations indicate quasi-steady mass loss up to nearly the point of core collapse (e.g., SN 2011ja; Chakraborti et al 2016), while optical observations of so-called "supernova impostors" suggest that some progenitors undergo massive, eruptive events only a few years before the onset of core collapse (e.g., SN 2009fk;SN 2009ip;Moriya et al 2011;Margutti et al 2014). Thus, current theories of stellar mass loss focus on wind-driven versus episodic events following the onset of core-carbon burning (Patnaude et al 2017). An important probe of these mass loss mechanisms comes from the forward shock emission of young SNR.…”

Section: Introductionmentioning

confidence: 99%

“…We use the "Modules for Experiments in Stellar Astrophysics" (mesa; Paxton et al 2011Paxton et al , 2013Paxton et al , 2015Paxton et al , 2018Paxton et al , 2019 for the stellar evolution, assuming purely line driven winds with rates from van Loon et al (2005) and de Jager et al (1988). At the onset of core collapse, the progenitor models are coupled to the "Supernova Explosion Code" (snec; Morozova et al 2015) modified to include explosive nucleosynthesis (Patnaude et al 2017). Finally, the output from snec is coupled to our "cosmic-ray hydrodynamics" code (ChN; Ellison et al 2007;Patnaude et al 2009Patnaude et al , 2010Lee et al 2014), to simulate the SNR evolution.…”

Section: Introductionmentioning

confidence: 99%

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A Grid of Core-Collapse Supernova Remnant Models I: The Effect of Wind-Driven Mass-Loss

Jacovich,

Patnaude,

Slane

et al. 2021

Preprint

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Massive stars can shed material via steady, line-driven winds, eruptive outflows, or mass-transfer onto a binary companion. In the case of single stars, the mass is deposited by the stellar wind into the nearby environment. After the massive star explodes, the stellar ejecta interact with this circumstellar material (CSM), often-times resulting in bright X-ray line emission from both the shock-heated CSM and ejecta. The amount of material lost by the progenitor, the mass of ejecta, and its energetics all impact the bulk spectral characteristics of this X-ray emission. Here we present a grid of core-collapse supernova remnant models derived from models for massive stars with zero age main sequence masses of ∼ 10 -30 M evolved from the pre-main sequence stage with wind-driven mass-loss. Evolution is handled by a multi-stage pipeline of software packages. First, we use mesa (Modules for Experiments in Stellar Astrophysics) to evolve the progenitors from pre-main sequence to iron core collapse. We then use the Supernova Explosion Code (snec) to explode the mesa models, and follow them for the first 100 days following core-collapse. Finally, we couple the snec output, along with the CSM generated from mesa mass-loss rates, into the Cosmic-Ray Hydrodynamics code (ChN) to model the remnant phase to 7000 years post core-collapse. At the end of each stage, we compare our outputs with those found in the literature, and we examine any qualitative and quantitative differences in the bulk properties of the remnants and their spectra based on the initial progenitor mass, as well as mass-loss history.

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Discovery of ~2200 new supernova remnants in 19 nearby star-forming galaxies with MUSE spectroscopy

Li,

Kreckel,

Sarbadhicary

et al. 2024

A&A

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Supernova feedback injects energy and turbulence into the interstellar medium (ISM) in galaxies, influences the process of star formation, and is essential to understanding the formation and evolution of galaxies. In this paper we present the largest extragalactic survey of supernova remnant (SNR) candidates in nearby star-forming galaxies using exquisite spectroscopic maps from MUSE. Supernova remnants (SNRs) exhibit distinctive emission-line ratios and kinematic signatures, which are apparent in optical spectroscopy. Using optical integral field spectra from the PHANGS--MUSE project, we identified SNRs in 19 nearby galaxies at sim 100 pc scales. We used five different optical diagnostics: (1) line ratio maps of S ii /Halpha ; (2) line ratio maps of O i /Halpha ; (3) velocity dispersion map of the gas; and (4) and (5) two line ratio diagnostic diagrams from Baldwin, Phillips Terlevich (BPT) diagrams to identify and distinguish SNRs from other nebulae. Given that our SNRs are seen in projection against H ii regions and diffuse ionized gas, in our line ratio maps we used a novel technique to search for objects with S ii /Halpha or O i /Halpha in excess of what is expected at fixed Halpha surface brightness within photoionized gas. In total, we identified 2,233 objects using at least one of our diagnostics, and defined a subsample of 1,166 high-confidence SNRs that were detected with at least two diagnostics. The line ratios of these SNRs agree well with the MAPPINGS shock models and we validate our technique using the well-studied nearby galaxy M83, where all the SNRs we found are also identified in literature catalogs, and we recovered 51<!PCT!> of the known SNRs. The remaining 1,067 objects in our sample were detected with only one diagnostic, and we classified them as SNR candidates. We find that sim 35<!PCT!> of all our objects overlap with the boundaries of H ii regions from literature catalogs, highlighting the importance of using indicators beyond line intensity morphology to select SNRs We find that the O i /Halpha line ratio is responsible for selecting the most objects (1,368; 61<!PCT!>); however, only half are classified as SNRs, demonstrating how the use of multiple diagnostics is key to increasing our sample size and improving our confidence in our SNR classifications.

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Supernova Remnants as Clues to Their Progenitors

Cited by 9 publications

References 62 publications

An XMM-Newton X-Ray View of Supernova Remnant W49B: Revisiting Its Recombining Plasmas and Progenitor Type

An XMM-Newton X-Ray View of Supernova Remnant W49B: Revisiting Its Recombining Plasmas and Progenitor Type

A Grid of Core-Collapse Supernova Remnant Models I: The Effect of Wind-Driven Mass-Loss

Discovery of ~2200 new supernova remnants in 19 nearby star-forming galaxies with MUSE spectroscopy

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