PROBING FINAL STAGES OF STELLAR EVOLUTION WITH X-RAY OBSERVATIONS OF SN 2013ej

Chakraborti, Sayan; Ray, Alak; Margutti, R.; Pooley, David; Bose, S.; Sutaria, Firoza; Chandra, Poonam; Dwarkadas, Vikram V.; Ryder, S. D.; Maeda, Keiichi

doi:10.3847/0004-637x/817/1/22

Cited by 34 publications

(49 citation statements)

References 44 publications

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“…Dust-scattering Model SN 2013ej exhibits X-ray evidence for an interaction with tenuous CSM (Chakraborti et al 2016), the density of which is consistent with the mass loss of a typical RSG wind. Moreover, as we show in Section 3, CSM interaction persists at late times, implying the presence of a highly extended tenuous CSM envelope.…”

Section: Spectropolarimetric Modelingmentioning

confidence: 79%

“…We suspect that the unusual polarization characteristics of SN 2013ej are the result of CSM interaction, which we already know was occurring during the recombination phase, based on the persistent X-ray emission (Chakraborti et al 2016). We also know that the CSM interaction was geometrically asymmetric based on the multipeaked morphology of broad Hα emission at late times (see Figure 9).…”

Section: Polarization Via Aspherical Csm Interactionmentioning

confidence: 99%

“…Chakraborti et al (2016) reported the results of long-term X-ray monitoring observations between days 13 and 145, confirming persistent interaction with CSM from a preexplosion steady wind with a density and mass-loss rate typical of an RSG ( »´- M M 3 10 6 ), which must have been blowing for at least 400 years. Thermal dust emission is another documented feature of SN 2013ej.…”

Section: Introductionmentioning

confidence: 95%

“…An illustration of this potential scenario is presented in Figure 16. Note that the detection of persistent X-rays by Chakraborti et al (2016) implies CSM interaction outside the photosphere, with the RSG wind; the embedded equatorially enhanced interaction that potentially creates the ellipsoidal photosphere is a separate component. At late times, emission from the reverse shock-excited ejecta will be enhanced along the same equatorial direction, potentially creating the multipeaked Hα morphology we observe at >800 days.…”

Section: Polarization Via Aspherical Csm Interactionmentioning

confidence: 99%

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Asphericity, Interaction, and Dust in the Type Ii-P/Ii-L Supernova 2013ej in Messier 74

Mauerhan

Dyk

Johansson

et al. 2017

ApJ

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SN 2013ej is a well-studied core-collapse supernova (SN) that stemmed from a directly identified red supergiant (RSG) progenitor in galaxy M74. The source exhibits signs of substantial geometric asphericity, X-rays from persistent interaction with circumstellar material (CSM), thermal emission from warm dust, and a light curve that appears intermediate between supernovae of Types II-P and II-L. The proximity of this source motivates a close inspection of these physical characteristics and their potential interconnection. We present multiepoch spectropolarimetry of SN 2013ej during the first 107 days and deep optical spectroscopy and ultraviolet through infrared photometry past ∼800 days. SN 2013ej exhibits the strongest and most persistent continuum and line polarization ever observed for a SN of its class during the recombination phase. Modeling indicates that the data are consistent with an oblate ellipsoidal photosphere, viewed nearly edge-on and probably augmented by optical scattering from circumstellar dust. We suggest that interaction with an equatorial distribution of CSM, perhaps the result of binary evolution, is responsible for generating the photospheric asphericity. Relatedly, our late-time optical imaging and spectroscopy show that asymmetric CSM interaction is ongoing, and the morphology of broad Hα emission from shock-excited ejecta provides additional evidence that the geometry of the interaction region is ellipsoidal. Alternatively, a prolate ellipsoidal geometry from an intrinsically bipolar explosion is also a plausible interpretation of the data but would probably require a ballistic jet of radioactive material capable of penetrating the hydrogen envelope early in the recombination phase. Finally, our latest space-based optical imaging confirms that the late interaction-powered light curve dropped below the stellar progenitor level, confirming the RSG star's association with the explosion.

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Section: Spectropolarimetric Modelingmentioning

confidence: 79%

Section: Polarization Via Aspherical Csm Interactionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 95%

Section: Polarization Via Aspherical Csm Interactionmentioning

confidence: 99%

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Asphericity, Interaction, and Dust in the Type Ii-P/Ii-L Supernova 2013ej in Messier 74

Mauerhan

Dyk

Johansson

et al. 2017

ApJ

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“…Depending on the decline in the light curve, SNeII can be further subclassified as SNIIL for a linear decline and SNIIP for sustained brightness before an eventual decline. However, drawing distinctions between SNIILandIIP is less obvious considering an existing continuum of observed properties (Faran et al 2014;Sanders et al 2015;Chakraborti et al 2016;Gall et al 2015;Pejcha & Prieto 2015).…”

Section: Introductionmentioning

confidence: 99%

LINE IDENTIFICATIONS OF TYPE I SUPERNOVAE: ON THE DETECTION OF Si II FOR THESE HYDROGEN-POOR EVENTS

Parrent

Milisavljević

Söderberg

et al. 2016

ApJ

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Here we revisit line identifications of type I supernovae (SNe I) and highlight trace amounts of unburned hydrogen as an important free parameter for the composition of the progenitor. Most one-dimensional stripped-envelope models of supernovae indicate that observed features near 6000-6400 Å in typeI spectra are due to more than Si IIλ6355. However, while an interpretation of conspicuous Si IIλ6355 can approximate 6150 Å absorption features for all SNe Ia during the first month of free expansion, similar identifications applied to 6250 Å features of SNe Ib and Ic have not been as successful. When the corresponding synthetic spectra are compared with highquality timeseries observations, the computed spectra are frequently too blue in wavelength. Some improvement can be achieved with Fe II lines that contribute redward of 6150 Å; however, the computed spectra either remain too blue or the spectrum only reaches a fair agreement when the rise-time to peak brightness of the model conflicts with observations by a factor of two. This degree of disagreement brings into question the proposed explosion scenario. Similarly, a detection of strong Si IIλ6355 in the spectra of broadlined Ic and super-luminous events of type I/R is less convincing despite numerous model spectra used to show otherwise. Alternatively, we suggest 6000-6400 Å features are possibly influenced by either trace amounts of hydrogen or blueshifted absorption and emission in Hα, the latter being an effect which is frequently observed in the spectra of hydrogen-rich, SNe II.

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Explosive and Radio-Selected Transients: Transient Astronomy with Square Kilometre Array and its Precursors

et al. 2016

Self Cite

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With the high sensitivity and wide-field coverage of the Square Kilometre Array (SKA), large samples of explosive transients are expected to be discovered. Radio wavelengths, especially in commensal survey mode, are particularly well suited for uncovering the complex transient phenomena. This is because observations at radio wavelengths may suffer less obscuration than in other bands (e.g. optical/IR or Xrays) due to dust absorption. At the same time, multiwaveband information often provides critical source classification rapidly than possible with only radio band data. Therefore, multiwaveband observational efforts with wide fields of view will be the key to progress of transients astronomy from the middle 2020s offering unprecedented deep images and high spatial and spectral resolutions. Radio observations of gamma ray bursts (GRBs) with SKA will uncover not only much fainter bursts and verifying claims of sensitivity limited population versus intrinsically dim GRBs, they will also unravel the enigmatic population of orphan afterglows. The supernova rate problem caused by dust extinction in optical bands is expected to be solved in the SKA era. In addition, the debate of single degenerate scenario versus double degenerate scenario will be put to rest for the progenitors of thermonuclear supernovae, since highly sensitive measurements will lead to very accurate mass loss estimation in these supernovae. One also expects to detect gravitationally lensed supernovae in far away Universe in the SKA bands. Radio counterparts of the gravitational waves are likely to become a reality once SKA comes online. In addition, SKA is likely to discover various new kinds of transients.

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PROBING FINAL STAGES OF STELLAR EVOLUTION WITH X-RAY OBSERVATIONS OF SN 2013ej

Cited by 34 publications

References 44 publications

Asphericity, Interaction, and Dust in the Type Ii-P/Ii-L Supernova 2013ej in Messier 74

Asphericity, Interaction, and Dust in the Type Ii-P/Ii-L Supernova 2013ej in Messier 74

LINE IDENTIFICATIONS OF TYPE I SUPERNOVAE: ON THE DETECTION OF Si II FOR THESE HYDROGEN-POOR EVENTS

Explosive and Radio-Selected Transients: Transient Astronomy with Square Kilometre Array and its Precursors

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