Disentangling Dust Components in SN 2010jl: The First 1400 Days

Bevan, A. M.; Krafton, K.; Wesson, R.; Andrews, J. E.; Montiel, E.; Niculescu-Duvaz, M.; Barlow, M. J.; De Looze, I.; Clayton, G. C.

doi:10.48550/arxiv.2004.01503

Cited by 2 publications

(2 citation statements)

References 40 publications

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“…H-poor interacting SNe can be brighter in the NIR than in the optical at 100 days, this was seen most prominently in Type Ibn SN 2006jc (Pastorello et al 2007). This has been attributed to dust formation when accompanied by a rapid decline in the optical light curves or asymmetries in emission lines (see, Pastorello et al 2008b;Bevan et al 2020), or from the heating of pre-existing dust ('infrared echo'; e.g., Tartaglia et al 2020). We observed SN 2018gjx in the H band using IO:I on the LT some 130 days after first detection.…”

Section: Light Curvesmentioning

confidence: 99%

SN 2018gjx reveals that some SNe Ibn are SNe IIb exploding in dense circumstellar material

Prentice,

Maguire,

Boian

et al. 2020

Preprint

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We present the data and analysis of SN 2018gjx, an unusual low-luminosity transient with three distinct spectroscopic phases. Phase I shows a hot blue spectrum with signatures of ionised circumstellar material (CSM), Phase II has the appearance of broad SN features, consistent with those seen in a Type IIb supernova at maximum light, and Phase III is that of a supernova interacting with helium-rich CSM, similar to a Type Ibn supernova. This event provides an apparently rare opportunity to view the inner workings of an interacting supernova. The observed properties can be explained by the explosion of a star in an aspherical CSM. The initial light is emitted from an extended CSM (∼ 4000 R ), which ionises the exterior unshocked material. Some days after, the SN photosphere envelops this region, leading to the appearance of a SN IIb. Over time, the photosphere recedes in velocity space, revealing interaction between the supernova ejecta and the CSM that partially obscures the supernova nebular phase. Modelling of the initial spectrum reveals a surface composition consistent with compact H-deficient Wolf-Rayet and LBV stars. Such configurations may not be unusual, with SNe IIb being known to have signs of interaction so at least some SNe IIb and SNe Ibn may be the same phenomena viewed from different angles or, possibly with differing CSM configurations.

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Section: Light Curvesmentioning

confidence: 99%

SN 2018gjx reveals that some SNe Ibn are SNe IIb exploding in dense circumstellar material

Prentice,

Maguire,

Boian

et al. 2020

Preprint

View full text Add to dashboard Cite

show abstract

“…SN 2010jl is a slowly-declining 1988Z-like object that exhibits a power-law luminosity decline at early times (Stoll et al 2011;Zhang et al 2012;Maeda et al 2013;Fransson et al 2014;Ofek et al 2014c;Jencson et al 2016). Although SN 2010jl was observed intensively over a range of wavelengths (Chandra et al 2012(Chandra et al , 2015Williams & Fox 2015;Bevan et al 2020), the origin of the dust traced by its IR observations is still a matter of debate. The dust might have formed within a cool dense shell located within the wake of the supernova shock wave which is positioned at the interface between the rapidly expanding supernova ejecta and the dense CSM (e.g., Smith et al 2011;Gall et al 2014;Maeda et al 2013).…”

Section: Introductionmentioning

confidence: 99%

The Carnegie Supernova Project II. Observations of SN 2014ab possibly revealing a 2010jl-like SN IIn with pre-existing dust

Moriya,

Stritzinger,

Taddia

et al. 2020

Preprint

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We present optical and near-infrared photometry and spectroscopy of the Type IIn supernova (SN) 2014ab, obtained by the Carnegie Supernova Project II (CSP-II) and initiated immediately after its optical discovery. We also present mid-infrared photometry obtained by the Wide-field Infrared Survey Explorer (WISE) satellite extending from 56 days prior to the optical discovery to over 1600 days. The light curve of SN 2014ab evolves slowly, while the spectra exhibit strong emission features produced from the interaction between rapidly expanding ejecta and dense circumstellar matter. The light curve and spectral properties are very similar to those of SN 2010jl. The estimated mass-loss rate of the progenitor of SN 2014ab is of the order of 0.1 M ⊙ yr −1 under the assumption of spherically symmetric circumstellar matter and steady mass loss. Although the mid-infrared luminosity increases due to emission from dust, which is characterized by a blackbody temperature close to the dust evaporation temperature (∼ 2000 K), no clear signatures of in situ dust formation within the cold dense shell located behind the forward shock are observed in SN 2014ab in early phases. Mid-infrared emission of SN 2014ab may originate from pre-existing dust located within dense circumstellar matter that is heated by the SN shock or shock-driven radiation. Finally, for the benefit of the community, we also present in an Appendix five near-infrared spectra of SN 2010jl obtained between 450 to 1300 days post discovery.

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Disentangling Dust Components in SN 2010jl: The First 1400 Days

Cited by 2 publications

References 40 publications

SN 2018gjx reveals that some SNe Ibn are SNe IIb exploding in dense circumstellar material

SN 2018gjx reveals that some SNe Ibn are SNe IIb exploding in dense circumstellar material

The Carnegie Supernova Project II. Observations of SN 2014ab possibly revealing a 2010jl-like SN IIn with pre-existing dust

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