Forbidden Iron Lines and Dust Destruction in Supernova Remnant Shocks: The Case of N49 in the Large Magellanic Cloud

Dopita, Michael A.; Seitenzahl, Ivo R.; Sutherland, Ralph S.; Vogt, F.; Winkler, P. F.; Blair, William P.

doi:10.3847/0004-637x/826/2/150

Cited by 29 publications

(59 citation statements)

References 74 publications

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“…For the refractory elements normally trapped in dust grains, our results are generally consistent with the conclusions of (Dopita et al 2016b) and ) that dust has been mostly destroyed in the region emitting the [Fe II] lines, while a smaller fraction has been destroyed in the Fe III and Fe VII zones, consistent with the models of Seab & Shull (1983) and Borkowski & Dwek (1995). However, in Kepler, virtually all dust has been destroyed.…”

Section: Small Magellanic Cloudsupporting

confidence: 90%

Calibrating Interstellar Abundances Using Supernova Remnant Radiative Shocks

Dopita

Seitenzahl

Sutherland

et al. 2019

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Using integral field data we extract the optical spectra of shocked interstellar clouds in Kepler's supernova remnant located in the inner regions of our Galaxy, as well as in the Large Magellanic Cloud (LMC), the Small Magellanic Cloud (SMC), NGC6822 and IC 1613. Using self-consistent shock modelling, we make a new determination of the chemical composition of the interstellar medium (ISM) in N, O, Ne, S, Cl and Ar in these galaxies and obtain accurate estimates of the fraction of refractory grains destroyed in the shock. By comparing our derived abundances with those obtained in recent works using observations of B stars, F supergiant stars and HII regions, we provide a new calibration for abundance scaling in the range 7.9 12 + log O/H 9.1.

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Section: Small Magellanic Cloudsupporting

confidence: 90%

Calibrating Interstellar Abundances Using Supernova Remnant Radiative Shocks

Dopita

Seitenzahl

Sutherland

et al. 2019

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“…Without definitive evidence as to its type (Park et al 2012), N49 might be such an object, since it is interacting with a relatively high density (at least 2-25 cm −3 , Sankrit et al 2004;Dopita et al 2016). Symmetrically, it can not excluded that some CC SNRs are found at the low ionisation end.…”

Section: Evolution Of Fe K Lines In Snrsmentioning

confidence: 99%

Fe K and ejecta emission in SNR G15.9+0.2 withXMM-Newton

Maggi

Acero

2017

A&A

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Aims. We present a study of the Galactic supernova remnant SNR G15.9+0.2 with archival XMM-Newton observations. Methods. EPIC data are used to investigate the morphological and spectral properties of the remnant, searching in particular for supernova ejecta and Fe K line emission. By comparing the SNR's X-ray absorption column density with the atomic and molecular gas distribution along the line of sight, we attempt to constrain the distance to the SNR. Results. Prominent line features reveal the presence of ejecta. Abundance ratios of Mg, Si, S, Ar, and Ca strongly suggest that the progenitor of SNR G15.9+0.2 was a massive star with a main sequence mass likely in the range 20-25 M ⊙ , strengthening the physical association with a candidate central compact object detected with Chandra. Using EPIC's collective power, Fe K line emission from SNR G15.9+0.2 is detected for the first time. We measure the line properties and find evidence for spatial variations. We discuss how the source fits within the sample of SNRs with detected Fe K emission and find that it is the core-collapse SNR with the lowest Fe K centroid energy. We also present some caveats regarding the use of Fe K line centroid energy as a typing tool for SNRs. Only a lower limit of 5 kpc is placed on the distance to SNR G15.9+0.2, constraining its age to t S NR 2 kyr.

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“…This favors the detection of SNRs propagating into dense media. An extreme example is the small (16 pc), bright SNR N49, which is located near a dense cloud in the LMC (e.g., Dopita et al 2016). Many of the small SNRs in M83 are likely to be objects of this sort.…”

Section: What Are the Small-diameter Snrs That We Do See?mentioning

confidence: 99%

“…Although there are 68 SNRs in the spectroscopic sample with diameters less than 21 pc, or 1 , none shows evidence either of broad lines or of interaction with highly enriched ejecta, except the remnant of SN1957D and B12-174a, which, as we have reported in Blair et al (2015), is most likely a the remnant of a SN that exploded within the last 100 years but that was not reported by contemporary observers. Most of the other small-diameter SNRs are most likely ones that have evolved rapidly following their origin as SNe exploding in relatively dense interstellar environments, similar to N49 in the LMC (Dopita et al 2016). …”

Section: None Of the 22 [O Iii]-bright Objects (Selected In Hopes Of mentioning

confidence: 99%

A Spectroscopic Study of the Rich Supernova Remnant Population in M83^∗

Winkler

Blair

Long

2017

ApJ

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We report the results from a spectrophotometric study sampling the 300 candidate supernova remnants (SNRs) in M83 identified through optical imaging with Magellan/IMACS and HST/WFC3. Of the 118 candidates identified based on a high [S II] λλ 6716,6731 to Hα emission ratio, 117 show spectroscopic signatures of shock-heated gas, confirming them as SNRs-the largest uniform set of SNR spectra for any galaxy. Spectra of 22 objects with a high [O III] λ 5007 to Hα emission ratio, selected in an attempt to identify young ejecta-dominated SNRs like Cas A, reveal only one (previously reported) object with the broad ( 1000 km s −1 ) emission lines characteristic of ejecta-dominated SNRs, beyond the known SN1957D remnant. The other 20 [O III]-selected candidates include planetary nebulae, compact H II regions, and one background QSO. Although our spectroscopic sample includes 22 SNRs smaller than 11 pc, none of the other objects shows broad emission lines; instead their spectra stem from relatively slow (∼ 200 km s −1 ) radiative shocks propagating into the metal-rich interstellar medium of M83. With six SNe in the past century, one might expect more of M83's small-diameter SNRs to show evidence of ejecta; this appears not to be the case. We attribute their absence to several factors, including that SNRs expanding into a dense medium evolve quickly to the ISM-dominated phase, and that SNRs expanding into regions already evacuated by earlier SNe are probably very faint.

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Forbidden Iron Lines and Dust Destruction in Supernova Remnant Shocks: The Case of N49 in the Large Magellanic Cloud

Cited by 29 publications

References 74 publications

Calibrating Interstellar Abundances Using Supernova Remnant Radiative Shocks

Calibrating Interstellar Abundances Using Supernova Remnant Radiative Shocks

Fe K and ejecta emission in SNR G15.9+0.2 withXMM-Newton

A Spectroscopic Study of the Rich Supernova Remnant Population in M83^∗

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Forbidden Iron Lines and Dust Destruction in Supernova Remnant Shocks: The Case of N49 in the Large Magellanic Cloud

Cited by 29 publications

References 74 publications

Calibrating Interstellar Abundances Using Supernova Remnant Radiative Shocks

Calibrating Interstellar Abundances Using Supernova Remnant Radiative Shocks

Fe K and ejecta emission in SNR G15.9+0.2 withXMM-Newton

A Spectroscopic Study of the Rich Supernova Remnant Population in M83∗

Contact Info

Product

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A Spectroscopic Study of the Rich Supernova Remnant Population in M83^∗