<i>SPITZER</i>IRS OBSERVATIONS OF THE XA REGION IN THE CYGNUS LOOP SUPERNOVA REMNANT

Sankrit, Ravi; Raymond, J. C.; Bautista, M. A.; Gaetz, T. J.; Williams, Brian J.; Blair, William P.; Borkowski, Kazimierz J.; Long, Knox S.

doi:10.1088/0004-637x/787/1/3

Cited by 16 publications

(17 citation statements)

References 47 publications

(61 reference statements)

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“…In order to check this result, we ran a grid of shock models with pre-shock H density n H = 10.0 cm −3 , with LGC abundances, but otherwise covering the same parameter range as the LMC grid. We found that a very good agreement with the "cusp region" spectroscopy given in Table 2 of Sankrit et al (2014) could be obtained with a model with v s = 200 km s −1 and a magnetic β = 1.0, with all elements depleted by the amount corresponding to = -D log 0.7…”

Section: Comparison With the Cygnus Loop Snrsupporting

confidence: 76%

“…The radiative shock in the cusp region of the Cygnus Loop has not yet had time to become fully radiative (Dopita &Binette 1983 andRaymond et al 1988). Consequently, the final model fit was terminated at a temperature of 7000 K, as recommended by Sankrit et al (2014). This provides a peak electron density in the model of n e = 150 cm −3 , in the middle range of that derived from the [S II] doublet,   n 100 250 e cm −3 , In Table 5, we give the observed and the predicted line intensities of the refractory element C, Si, and Fe lines given by this model.…”

Section: Comparison With the Cygnus Loop Snrmentioning

confidence: 99%

“…Fe estimated by Sankrit et al (2014) tail of the shock is missing. This is precisely the zone in which the N49 results imply the fastest grain destruction rates.…”

Section: Comparison With the Cygnus Loop Snrmentioning

confidence: 99%

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

Dopita

Seitenzahl

Sutherland

et al. 2016

ApJ

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We present the results of a complete integral-field survey of the bright supernova remnant (SNR) N49 in the Large Magellanic Cloud, obtained with the WiFeS instrument mounted on the ANU 2.3 m telescope at Siding Spring Observatory. From theoretical shock modeling with the new MAPPINGS 5.1 code, we have, for the first time, subjected the optical Fe emission line spectrum of an SNR to a detailed abundance and dynamical analysis covering eight separate stages of ionization. This allows us to derive the dust depletion factors as a function of ionization stage. We have shown that there is substantial (30%-90%) destruction of Fe-bearing dust grains in these fast shocks (v s ∼ 250 km s −1 ), and we have confirmed that the dominant dust destruction occurs through the nonthermal sputtering and grain-grain collision mechanisms developed in a number of theoretical works.

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Section: Comparison With the Cygnus Loop Snrsupporting

confidence: 76%

Section: Comparison With the Cygnus Loop Snrmentioning

confidence: 99%

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

Dopita

Seitenzahl

Sutherland

et al. 2016

ApJ

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“…The lines identified are typical of those seen in other supernova remnants (Arendt et al 1999;Oliva et al 1999;Temim et al 2006;Neufeld et al 2007;Smith et al 2009;Andersen et al 2011;Ghavamian et al 2012;Sankrit et al 2014). The accuracy of the measurement of the line strengths is limited by the modest S/N of some lines, and the presence of strong (sometimes dominant) and structured background emission from the ISM in some of the lines.…”

Section: Emission Line (Gas) Evolutionmentioning

confidence: 82%

Infrared Continuum and Line Evolution of the Equatorial Ring Around Sn 1987a

Arendt

Dwek

Bouchet

et al. 2016

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Spitzer observations of SN 1987A have now spanned more than a decade. Since day ∼4000, mid-infrared (mid-IR) emission has been dominated by that from shock-heated dust in the equatorial ring (ER). From 6000 to 8000 days after the explosion, Spitzer observations included broadband photometry at 3.6-24 μm, and low and moderate resolution spectroscopy at 5-35 μm. Here we present later Spitzer observations, through day 10,377, which include only the broadband measurements at 3.6 and 4.5 μm. These data show that the 3.6 and 4.5 μm brightness has clearly begun to fade after day ∼8500, and no longer tracks the X-ray emission as well as it did at earlier epochs. This can be explained by the destruction of the dust in the ER on timescales shorter than the cooling time for the shocked gas. We find that the evolution of the late time IR emission is also similar to the now fading optical emission. We provide the complete record of the IR emission lines, as seen by Spitzer prior to day 8000. The past evolution of the gas as seen by the IR emission lines seems largely consistent with the optical emission, although the IR [Fe II] and [Si II] lines show different, peculiar velocity structures.

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“…We would be grateful for any feedback, query, or comment on the code and its accompanying documentation. PyNeb has already been used in a number of papers (García-Rojas et al 2012, 2014Esteban et al 2013Esteban et al , 2014Kameswara Rao et al 2013;Nicholls et al 2013Nicholls et al , 2014Marino et al 2013;Delgado-Inglada & Rodríguez 2014;Mesa-Delgado et al 2014;Sankrit et al 2014;Ho et al 2014;Pérez-Montero 2014). The scientific community is invited to keep using it for their projects.…”

Section: Concluding Remarks: the Present And Future Of Pynebmentioning

confidence: 99%

PyNeb: a new tool for analyzing emission lines

Luridiana

Morisset

Shaw

2014

A&A

499

409

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Analysis of emission lines in gaseous nebulae yields direct measures of physical conditions and chemical abundances and is the cornerstone of nebular astrophysics. Although the physical problem is conceptually simple, its practical complexity can be overwhelming since the amount of data to be analyzed steadily increases; furthermore, results depend crucially on the input atomic data, whose determination also improves each year. To address these challenges we created PyNeb, an innovative code for analyzing emission lines. PyNeb computes physical conditions and ionic and elemental abundances and produces both theoretical and observational diagnostic plots. It is designed to be portable, modular, and largely customizable in aspects such as the atomic data used, the format of the observational data to be analyzed, and the graphical output. It gives full access to the intermediate quantities of the calculation, making it possible to write scripts tailored to the specific type of analysis one wants to carry out. In the case of collisionally excited lines, PyNeb works by solving the equilibrium equations for an n-level atom; in the case of recombination lines, it works by interpolation in emissivity tables. The code offers a choice of extinction laws and ionization correction factors, which can be complemented by user-provided recipes. It is entirely written in the python programming language and uses standard python libraries. It is fully vectorized, making it apt for analyzing huge amounts of data. The code is stable and has been benchmarked against IRAF/NEBULAR. It is public, fully documented, and has already been satisfactorily used in a number of published papers.

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SPITZERIRS OBSERVATIONS OF THE XA REGION IN THE CYGNUS LOOP SUPERNOVA REMNANT

Cited by 16 publications

References 47 publications

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

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

Infrared Continuum and Line Evolution of the Equatorial Ring Around Sn 1987a

PyNeb: a new tool for analyzing emission lines

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