X‐Ray Emission from Multiphase Shock in the Large Magellanic Cloud Supernova Remnant N49

Park, Sangwook; Burrows, D. N.; Garmire, G. P.; Nousek, J. A.; Hughes, John P.; Williams, R. M.

doi:10.1086/367619

Cited by 49 publications

(90 citation statements)

References 54 publications

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“…Based on a simple Sedov model for the SNR, Hughes et al (1998) concluded that the swept-up mass was the order of 200 M . Park et al (2003) recently conducted a detailed study of its X-ray properties using Chandra, confirming that the SNR is relatively young, on the order of 6000 yrs. They find that although most of the emission is dominated by interstellar material (ISM), the Chandra observations appear to show "explosion fragments" on the SW side of the SNR in X-rays.…”

Section: Introductionmentioning

confidence: 92%

Dust in the bright supernova remnant N49 in the LMC

Otsuka¹,

Loon

Long³

et al. 2010

A&A

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We investigate the dust associated with the supernova remnant (SNR) N49 in the Large Magellanic Cloud (LMC) as observed with the Herschel Space Observatory. N49 is unusually bright because of an interaction with a molecular cloud along its eastern edge. We have used PACS and SPIRE to measure the far IR flux densities of the entire SNR and of a bright region on the eastern edge of the SNR where the SNR shock is encountering the molecular cloud. Using these fluxes supplemented with archival data at shorter wavelengths, we estimate the dust mass associated with N49 to be about 10 M . The bulk of the dust in our simple two-component model has a temperature of 20-30 K, similar to that of nearby molecular clouds. Unfortunately, as a result of the limited angular resolution of Herschel at the wavelengths sampled with SPIRE, the uncertainties are fairly large. Assuming this estimate of the dust mass associated with the SNR is approximately correct, it is probable that most of the dust in the SNR arises from regions where the shock speed is too low to produce significant X-ray emission. The total amount of warm 50-60 K dust is ∼0.1 or 0.4 M , depending on whether the dust is modeled in terms of carbonaceous or silicate grains. This provides a firm lower limit to the amount of shock heated dust in N49.

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Section: Introductionmentioning

confidence: 92%

Dust in the bright supernova remnant N49 in the LMC

Otsuka¹,

Loon

Long³

et al. 2010

A&A

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“…No compelling evidence for overabundant O or Fe is found, but Si-and S-rich ejecta features are detected by Chandra (Park et al 2003a(Park et al , 2012. These can be interpreted as explosive O-burning or incomplete Si-burning deep inside a CC SN explosion; however, the Si/S ejecta mass ratio favour a type Ia origin (Park et al 2003a(Park et al , 2012. The soft gamma-ray repeater SGR…”

Section: Appendix A: the Epic Backgroundmentioning

confidence: 99%

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

Maggi

Haberl

Kavanagh

et al. 2016

A&A

149

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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“…To investigate the spatial distribution of Si and S line emission across the remnant on a finer scale than that of the spectral extraction regions, we produced continuum-subtracted (CS) line images and equivalent-width ( EW ) images (see, e.g., Park et al 2003), shown in Figure 5. Narrowband images used for deriving the CS and EW images were filtered in energy according to Table 4 and binned by 8 00 to provide a sufficient number of counts in the faint SNR regions.…”

Section: Spectral Analysismentioning

confidence: 99%

“…Another example is the only ME SNR in the Large Magellanic Cloud, N49 ( Brogan et al 2004). This remnant also has an irregular shell morphology in both radio and X-rays, with a bright region to the southeast (e.g., Park et al 2003), which can similarly be explained as resulting from expansion in a density gradient produced by the presence of a molecular cloud, as mapped by Banas et al (1997). Thus, if ME and MM SNRs are the same class of the SNRs and there is a single mechanism to explain their appearance and spectral characteristics, the observations of G349.7+ 0.2 would support the projection model.…”

Section: Implications For Mixed-morpholog Gy Snrsmentioning

confidence: 99%

ChandraDetection of Ejecta in the Small‐Diameter Supernova Remnant G349.7+0.2

Lazendić

Slane

Hughes

et al. 2005

ApJ

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We present high-resolution X-ray observations of the small-diameter supernova remnant (SNR) G349.7+0.2 with Chandra. The overall SNR spectrum can be described by two spectral components. The soft component is in ionization equilibrium and has a temperature of %0.8 keV; the hard spectral component has a temperature of %1.4 keV, an ionization timescale of %5 ; 10 11 cm À3 s, and enhanced abundances of Si. The spatially resolved spectral modeling shows that S may also be enhanced, at least in some regions. The enhanced abundances clearly point to the presence of an ejecta component in this remnant. Using the available H i and CO data toward G349.7+0.2 we derive a column density of %7 ; 10 22 cm À2 along the line of sight to the SNR, which is consistent with our X-ray data. The X-ray morphology of G349.7+0.2 is strikingly similar to that at radio wavelengths-an irregular shell with a brighter eastern side-which is consistent with expansion in a medium with a large-scale density gradient. The remnant is known to be interacting with a molecular cloud (from the presence of OH (1720 MHz) masers), but this interaction is probably limited to the central portion of the SNR, as seen in SNR IC 443. We found that H i clouds are present in the SNR region, which supports the notion that G349.7+0.2 belongs to a class of remnants evolving in the intercloud medium (such are IC 443 and W44), which is also responsible for the remnant's morphology. G349.7+0.2 does not have the mixed-morphology found for other maser-emitting SNRs studied to date in X-rays, but its morphology can be explained by a projection model for mixed-morphology SNRs. We have identified a point source close to the center of the SNR with a luminosity of L X (0:5 10:0 keV) $ (0:2 2:3) ; 10 34 d 22 ergs s À1 , which is consistent with that of the compact central objects found in a few other Galactic SNRs.

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X‐Ray Emission from Multiphase Shock in the Large Magellanic Cloud Supernova Remnant N49

Cited by 49 publications

References 54 publications

Dust in the bright supernova remnant N49 in the LMC

Dust in the bright supernova remnant N49 in the LMC

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

ChandraDetection of Ejecta in the Small‐Diameter Supernova Remnant G349.7+0.2

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