CONSTRAINING EXPLOSION TYPE OF YOUNG SUPERNOVA REMNANTS USING 24 μm EMISSION MORPHOLOGY

Peters, Charee; Lopez, Laura A.; Ramírez-Ruiz, E.; Stassun, Keivan G.; Figueroa‐Feliciano, E.

doi:10.1088/2041-8205/771/2/l38

Cited by 22 publications

(32 citation statements)

References 49 publications

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“…In addition, studies of the X-ray and infrared morphologies of SNRs (Lopez et al 2009;Peters et al 2013) suggest that, as a class, type Ia and CC SNRs have distinct symmetries: type Ia remnants are statistically more spherical and mirror symmetric than the CC SNRs. However, this method cannot give definite results for individual objects: Prominent counterexamples include SNR 1E 0102.2−7219, a textbook CC SNR which is highly symmetric (Flanagan et al 2004), and MCSNR J0547−7025, which is a type Ia SNR (based on its X-ray spectrum Hendrick et al 2003, this work) with "anomalous" ejecta distribution (Lopez et al 2009).…”

Section: The Typing Of Snrs In Generalmentioning

confidence: 99%

The population of X-ray supernova remnants in the Large Magellanic Cloud

Maggi

Haberl

Kavanagh

et al. 2016

A&A

156

205

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Aims. We present a comprehensive X-ray study of the population of supernova remnants (SNRs) in the Large Magellanic Cloud (LMC). Using primarily XMM-Newton observations, we conduct a systematic spectral analysis of LMC SNRs to gain new insight into their evolution and the interplay with their host galaxy. Methods. We combined all the archival XMM-Newton observations of the LMC with those of our Very Large Programme LMC survey. We produced X-ray images and spectra of 51 SNRs, out of a list of 59 objects compiled from the literature and augmented with newly found objects. Using a careful modelling of the background, we consistently analysed all the X-ray spectra and measure temperatures, luminosities, and chemical compositions. The locations of SNRs are compared to the distributions of stars, cold gas, and warm gas in the LMC, and we investigated the connection between the SNRs and their local environment, characterised by various star formation histories. We tentatively typed all LMC SNRs, in order to constrain the ratio of core-collapse to type Ia SN rates in the LMC. We also compared the column densities derived from X-ray spectra to H i maps, thus probing the three-dimensional structure of the LMC. Results. This work provides the first homogeneous catalogue of the X-ray spectral properties of SNRs in the LMC. It offers a complete census of LMC remnants whose X-ray emission exhibits Fe K lines (13% of the sample), or reveals the contribution from hot supernova ejecta (39%), which both give clues to the progenitor types. The abundances of O, Ne, Mg, Si, and Fe in the hot phase of the LMC interstellar medium are found to be between 0.2 and 0.5 times the solar values with a lower abundance ratio [α/Fe] than in the Milky Way. The current ratio of core-collapse to type Ia SN rates in the LMC is constrained to N CC /N Ia = 1.35( +0.11 −0.24 ), which is lower than in local SN surveys and galaxy clusters. Our comparison of the X-ray luminosity functions of SNRs in Local Group galaxies (LMC, SMC, M31, and M33) reveals an intriguing excess of bright objects in the LMC. Finally, we confirm that 30 Doradus and the LMC Bar are offset from the main disc of the LMC to the far and near sides, respectively.

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Section: The Typing Of Snrs In Generalmentioning

confidence: 99%

The population of X-ray supernova remnants in the Large Magellanic Cloud

Maggi

Haberl

Kavanagh

et al. 2016

A&A

156

205

View full text Add to dashboard Cite

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“…The Type Ia SNRs separate naturally from the CC SNRs in both diagrams. Figures are adapted from Lopez et al (2011) and Peters et al (2013). spectra from surrounding light echoes (e.g., Rest et al 2005, Krause et al 2008, Rest et al 2008.…”

Section: Distinguishing Type Ia and Core-collapse Snrsmentioning

confidence: 99%

“…In this paper, we identify and map the overionized plasma in W49B in order to constrain the physical origin of the rapid cooling. For this analysis, we employ the recent 220 ks Chandra X-ray Observatory Advanced CCD Imaging Spectrometer (ACIS) observation of W49B (Lopez et al 2013). Although Chandra is dominated by background above ∼8 keV and thus is not capable of discerning the Fe RRC, we can identify the overionized plasma another way.…”

Section: Influences Of the Environment And The Surrounding Medium On mentioning

confidence: 99%

The Morphologies and Kinematics of Supernova Remnants

Lopez

Fesen

2018

Space Sci Rev

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We review the major advances in understanding the morphologies and kinematics of supernova remnants (SNRs). Simulations of SN explosions have improved dramatically over the last few years, and SNRs can be used to test models through comparison of predictions with SNRs' observed large-scale compositional and morphological properties as well as the three-dimensional kinematics of ejecta material. In particular, Cassiopeia A -the youngest known core-collapse SNR in the Milky Way -offers an up-close view of the complexity of these explosive events that cannot be resolved in distant, extragalactic sources. We summarize the progress in tying SNRs to their progenitors' explosions through imaging and spectroscopic observations, and we discuss exciting future prospects for SNR studies, such as X-ray microcalorimeters.

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“…However, several evolved SNRs have been discovered (in X-rays) in the Magellanic Clouds with an iron-rich, centrally bright emission (Nishiuchi et al 2001;Hendrick et al 2003;van der Heyden et al 2004;Seward et al 2006;Borkowski et al 2006;Bozzetto et al 2013b), naturally leading to their classification as type Ia remnants. In addition, studies of the X-ray and infrared morphologies of SNRs (Lopez et al 2009;Peters et al 2013) suggest that, as a class, type Ia and CC SNRs have distinct symmetries: type Ia remnants are more spherical and mirror symmetric than the CC SNRs. A&A 561, A76 (2014) Finally, clues to the type of remnants are provided by the study of the stellar population around the SNRs.…”

Section: Introductionmentioning

confidence: 99%

Four new X-ray-selected supernova remnants in the Large Magellanic Cloud

Maggi

Haberl

Kavanagh

et al. 2014

A&A

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Aims. We present a detailed multi-wavelength study of four new supernova remnants (SNRs) in the Large Magellanic Cloud (LMC). The objects were identified as SNR candidates in X-ray observations performed during the survey of the LMC with XMM-Newton. Methods. Data obained with XMM-Newton are used to investigate the morphological and spectral features of the remnants in X-rays. We measure the plasma conditions, look for supernova (SN) ejecta emission, and constrain some of the SNR properties (e.g. age and ambient density). We supplement the X-ray data with optical, infrared, and radio-continuum archival observations, which allow us to understand the conditions resulting in the current appearance of the remnants. Based on the spatially-resolved star formation history (SFH) of the LMC together with the X-ray spectra, we attempt to type the supernovae that created the remnants. Results. We confirm all four objects as SNRs, to which we assign the names MCSNR J0508−6830, MCSNR J0511−6759, MCSNR J0514−6840, and MCSNR J0517−6759. In the first two remnants, an X-ray bright plasma is surrounded by very faint [S ii] emission. The emission from the central plasma is dominated by Fe L-shell lines, and the derived iron abundance is greatly in excess of solar. This establishes their type Ia (i.e. thermonuclear) SN origin. They appear to be more evolved versions of other Magellanic Cloud iron-rich SNRs which are centrally-peaked in X-rays. From the two other remnants (MCSNR J0514−6840 and MCSNR J0517−6759), we do not see ejecta emission. At all wavelengths at which they are detected, the local environment plays a key role in their observational appearance. We present evidence that MCSNR J0517−6759 is close to and interacting with a molecular cloud, suggesting a massive progenitor.

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CONSTRAINING EXPLOSION TYPE OF YOUNG SUPERNOVA REMNANTS USING 24 μm EMISSION MORPHOLOGY

Cited by 22 publications

References 49 publications

The population of X-ray supernova remnants in the Large Magellanic Cloud

The population of X-ray supernova remnants in the Large Magellanic Cloud

The Morphologies and Kinematics of Supernova Remnants

Four new X-ray-selected supernova remnants in the Large Magellanic Cloud

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