The Destruction of the Circumstellar Ring of Sn 1987a

Fransson, Claes; Larsson, Josefin; Migotto, K.; Pesce, Dominic W.; Challis, P.; Chevalier, Roger A.; Kirshner, R.; Leibundgut, B.; Lundqvist, Peter; McCray, Richard; Spyromilio, J.; Taddia, F.; Jerkstrand, A.; Mattila, S.; Smith, Nathan; Sollerman, J.; Wheeler, J. C.; Crotts, Arlin; Garnavich, P.; Heng, Kevin; Lawrence, Stephen S.; Panagia, N.; Pun, C. S. J.; Sonneborn, G.; Sugerman, Ben

doi:10.1088/2041-8205/806/1/l19

Cited by 74 publications

(125 citation statements)

References 30 publications

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“…The image in the broad F625W filter, shown in Figure 1, is completely dominated by emission from Hα and is thus very useful for comparison with the STIS results. The image has previously been analyzed in Fransson et al (2015), where further details about the observations are provided.…”

Section: Hst/wfc3 Observationmentioning

confidence: 99%

“…The STIS spectrum in Figure 3 has been corrected for scattered light from the ring using the fact that the lines from the ring are narrow (FWHM~-300 km s 1 , e.g., Fransson et al 2015) compared with the lines from the ejecta, which have FWHM~-2500 km s 1 . The narrow lines can thus be removed by subtracting a rescaled ring spectrum from the spectrum extracted from the ejecta region.…”

Section: Ejecta Spectramentioning

confidence: 99%

“…We further note that the left panel of Figure 13 also shows a non-uniform flux evolution of the ring, with the eastern side fading and the western side brightening. The evolution of the ring is discussed in detail in Fransson et al (2015). 2 , which implies a flux increase of~30% in the last 1000 days.…”

Section: Time Evolutionmentioning

confidence: 99%

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Three-Dimensional Distribution of Ejecta in Supernova 1987a at 10,000 Days

Larsson

Fransson

Spyromilio³

et al. 2016

ApJ

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Due to its proximity, SN1987A offers a unique opportunity to directly observe the geometry of a stellar explosion as it unfolds. Here we present spectral and imaging observations of SN1987A obtained ∼10,000 days after the explosion with HST/STIS and VLT/SINFONI at optical and near-infrared wavelengths. These observations allow us to produce the most detailed 3D map of Hα to date, the first 3D maps for 44 Ti. The time evolution of Hα shows that it is predominantly powered by X-rays from the ring, in agreement with previous findings. All lines that have sufficient signal show a similar large-scale 3D structure, with a north-south asymmetry that resembles a broken dipole. This structure correlates with early observations of asymmetries, showing that there is a global asymmetry that extends from the inner core to the outer envelope. On smaller scales, the two brightest lines, Hα and [Si I]+[Fe II] 1.644 μm, show substructures at the level of ∼200-1000 km s -1 and clear differences in their 3D geometries. We discuss these results in the context of explosion models and the properties of dust in the ejecta.

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Section: Hst/wfc3 Observationmentioning

confidence: 99%

Section: Ejecta Spectramentioning

confidence: 99%

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Three-Dimensional Distribution of Ejecta in Supernova 1987a at 10,000 Days

Larsson

Fransson

Spyromilio³

et al. 2016

ApJ

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“…Spitzer observations commenced near day 6100 (Bouchet et al 2006) while the number and brightness of hotspots around the ER were increasing (Gröningsson et al 2008a;Fransson et al 2015). This epoch is also when the soft X-ray light curve turned up (Park et al 2005(Park et al , 2006, indicating that the shock started interacting with dense protrusions from the ER.…”

Section: Introductionmentioning

confidence: 99%

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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“…The dust emission peaks near the notable gap in the optical HST map (Fransson et al 2015). Figure 1 shows the SN 1987A 315 GHz image in comparison to several other wavelength bands.…”

Section: Preliminary Resultsmentioning

confidence: 97%

High-Resolution Observations of Dust in SN 1987A

Cigan¹,

Gomez²,

Matsuura

2017

Proc. IAU

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Abstract. The dust produced by supernovae is an important topic for understanding supernova physics and the chemical evolution of galaxies. Recent ALMA observations of SN 1987A have allowed us to peer into the inner ejecta to the cool dust, with spatial resolution from 0. 3 at ∼300 GHz down to 0. 09 at ∼680 GHz -an improvement over the previous 300 GHz Cycle 0 observations at 0. 69. Comparison of the dust location and morphology with other multiwavelength emission presents an interesting picture of the role dust plays in the ejecta. The mm-FIR SED is compared to radiative models to study the dust composition 30 years after the initial explosion. Fits to the ring emission also probe the drift of the center of the system over time.

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The Destruction of the Circumstellar Ring of Sn 1987a

Cited by 74 publications

References 30 publications

Three-Dimensional Distribution of Ejecta in Supernova 1987a at 10,000 Days

Three-Dimensional Distribution of Ejecta in Supernova 1987a at 10,000 Days

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

High-Resolution Observations of Dust in SN 1987A

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