<i>HUBBLE SPACE TELESCOPE</i>/ADVANCED CAMERA FOR SURVEYS NARROWBAND IMAGING OF THE KEPLER SUPERNOVA REMNANT

Sankrit, Ravi; Blair, William P.; Frattare, L. M.; Rudnick, Lawrence; DeLaney, Tracey; Harrus, I.; Ennis, J.

doi:10.1088/0004-6256/135/2/538

Cited by 17 publications

(18 citation statements)

References 25 publications

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“…The detailed structure of the region was revealed by our first epoch HST images (Sankrit et al 2008) as consisting of arc-shaped Balmer dominated filaments tracing a shock front and trailing radiative knots due to Rayleigh-Taylor like instabilities. The clear correlation between the emitting structures in the X-ray and in Hα may be seen in Figure 11.…”

Section: The Ejecta Knotmentioning

confidence: 88%

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Second Epoch Hubble Space Telescope Observations of Kepler’s Supernova Remnant: The Proper Motions of Balmer Filaments*

Sankrit

Raymond

Blair

et al. 2016

ApJ

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We report on the proper motions of Balmer-dominated filaments in Kepler's supernova remnant using high resolution images obtained with the Hubble Space Telescope at two epochs separated by about 10 years. We use the improved proper motion measurements and revised values of shock velocities to derive a distance to Kepler of 5.1 0.7 0.8 -+ kpc. The main shock around the northern rim of the remnant has a typical speed of 1690 km s −1 and is encountering material with densities of about 8 cm −3 . We find evidence for the variation of shock properties over small spatial scales, including differences in the driving pressures as the shock wraps around a curved cloud surface. We find that the Balmer filaments ahead of the ejecta knot on the northwest boundary of the remnant are becoming fainter and more diffuse. We also find that the Balmer filaments associated with circumstellar material in the interior regions of the remnant are due to shocks with significantly lower velocities and that the brightness variations among these filaments trace the density distribution of the material, which may have a disk-like geometry.

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Section: The Ejecta Knotmentioning

confidence: 88%

“…A thorough discussion of the optical emission from Kepler, including references to past work, may be found in Sankrit et al (2008).…”

Section: Overview Of the Optical Emissionmentioning

confidence: 99%

Second Epoch Hubble Space Telescope Observations of Kepler’s Supernova Remnant: The Proper Motions of Balmer Filaments*

Sankrit

Raymond

Blair

et al. 2016

ApJ

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“…For Kepler’s remnant we used observations in the filters 658, 660 and 502 nm where the emission originates from Hα+[N ii ], [N ii ] and [O iii ], respectively (e.g. Sankrit et al 2008). Bad pixels were masked by hand.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…The Kepler SN event was first seen by Johannes Kepler in 1604 and the remnant has a shell‐like structure ∼3 arcmin in diameter. Estimates of its distance, using H i absorption features, range from 3.9 to 6 kpc (Reynoso & Goss 1999; Sankrit et al 2008). Its classification has been controversial (see the excellent reviews in Blair et al 2007; Reynolds et al 2008; Sankrit et al 2008) with evidence pointing towards both Type Ia – the thermonuclear explosion of a low‐mass accreting star in a binary system – and Type Ib – the core collapse of a massive star.…”

Section: Kepler’s Supernova Remnantmentioning

confidence: 99%

“…Estimates of its distance, using H i absorption features, range from 3.9 to 6 kpc (Reynoso & Goss 1999; Sankrit et al 2008). Its classification has been controversial (see the excellent reviews in Blair et al 2007; Reynolds et al 2008; Sankrit et al 2008) with evidence pointing towards both Type Ia – the thermonuclear explosion of a low‐mass accreting star in a binary system – and Type Ib – the core collapse of a massive star. The deepest X‐ray analysis with Chandra (Reynolds et al 2008), however, suggests that a Type Ia is the most likely classification using both iron abundance constraints and the lack of a neutron star.…”

Section: Kepler’s Supernova Remnantmentioning

confidence: 99%

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Dust in historical Galactic Type Ia supernova remnants with Herschel★

Gomez

Clark

Nozawa

et al. 2012

Monthly Notices of the Royal Astronomical Society

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The origin of interstellar dust in galaxies is poorly understood, particularly the relative contributions from supernovae and the cool stellar winds of low-intermediate-mass stars. Recently, large masses of newly formed dust have been discovered in the ejecta of core-collapse supernovae. Here, we present Herschel Photodetector Array Camera and Spectrometer (PACS) and Spectral and Photometric Imaging Receiver (SPIRE) photometry at 70-500 µm of the historical, young supernova remnants: Kepler and Tycho, both thought to be the remnants of Type Ia explosion events. We detect a warm dust component in Kepler's remnant with T d = 82 +4 −6 K and mass ∼(3.1 +0.8 −0.6 ) × 10 −3 M ; this is spatially coincident with thermal X-ray emission and optical knots and filaments, consistent with the warm dust originating in the circumstellar material swept up by the primary blast wave of the remnant. Similarly for Tycho's remnant, we detect warm dust at 90 +5 −7 K with mass (8.6 +2.3 −1.8 )×10 −3 M . Comparing the spatial distribution of the warm dust with X-rays from the ejecta and swept-up medium, and Hα emission arising from the post-shock edge, we show that the warm dust is swept up interstellar material. We find no evidence of a cool (25-50 K) component of dust with mass ≥0.07 M as observed in core-collapse remnants of massive stars. Neither the warm or cold dust components detected here are spatially coincident with supernova ejecta material. We compare the lack of observed supernova dust with a theoretical model of dust formation in Type Ia remnants which predicts dust masses of 88(17) × 10 −3 M for ejecta expanding into ambient surrounding densities of 1(5) cm −3 . The model predicts that silicon-and carbon-rich dust grains will encounter, at most, the interior edge of the observed dust emission at ∼400 years, confirming that the majority of the warm dust originates from swept-up circumstellar or interstellar grains (for Kepler and Tycho, respectively). The lack of cold dust grains in the ejecta suggests that Type Ia remnants do not produce substantial quantities of iron-rich dust grains and has important consequences for the 'missing' iron mass observed in ejecta. Finally, although, we cannot completely rule out a small mass of freshly formed supernova dust, the Herschel observations confirm that significantly less dust forms in the ejecta of Type Ia supernovae than in the remnants of core-collapse explosions.

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Dust and Molecular Formation in Supernovae

Matsuura¹

2016

Handbook of Supernovae

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HUBBLE SPACE TELESCOPE/ADVANCED CAMERA FOR SURVEYS NARROWBAND IMAGING OF THE KEPLER SUPERNOVA REMNANT

Cited by 17 publications

References 25 publications

Second Epoch Hubble Space Telescope Observations of Kepler’s Supernova Remnant: The Proper Motions of Balmer Filaments*

Second Epoch Hubble Space Telescope Observations of Kepler’s Supernova Remnant: The Proper Motions of Balmer Filaments*

Dust in historical Galactic Type Ia supernova remnants with Herschel★

Dust and Molecular Formation in Supernovae

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