A Six-year Image-subtraction Light Curve of SN 2010jl

Ofek, E. O.; Zackay, Barak; Gal‐Yam, A.; Sollerman, J.; Fransson, Claes; Fremling, C.; Kulkarni, S. R.; Nugent, P.; Yaron, O.; Kasliwal, M. M.; Masci, Frank J.; Laher, Russ R.

doi:10.1088/1538-3873/ab0a19

Cited by 4 publications

(4 citation statements)

References 70 publications

(96 reference statements)

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“…Also during this period, the visible light curve begins a steeper decline. This drop in the optical could be attributed to a number of causes (see Ofek et al 2019), but its coincidental timing with the sharp rise in the IR and increasing line asymmetries may indicate a link with the onset of dust formation in the CDS or ejecta. The first observations after the gap were on day 374 (JHKs) and day 464 (Spitzer).…”

Section: Discussionmentioning

confidence: 99%

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

Bevan

Krafton

Wesson

et al. 2020

ApJ

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The luminous Type IIn SN 2010jl shows strong signs of interaction between the SN ejecta and dense circumstellar material. Dust may be present in the unshocked ejecta; the cool, dense shell (CDS) between the shocks in the interaction region; or in the circumstellar medium (CSM). We present and model new optical and infrared photometry and spectroscopy of SN 2010jl from 82 to 1367 days since explosion. We evaluate the photometric and spectroscopic evolution using the radiative transfer codes MOCASSIN and DAMOCLES, respectively. We propose an interaction scenario and investigate the resulting dust formation scenarios and dust masses. We find that SN 2010jl has been continuously forming dust based on the evolution of its infrared emission and optical spectra. There is evidence for preexisting dust in the CSM as well as new dust formation in the CDS and/or ejecta. We estimate that 0.005-0.01 M e of predominantly carbon dust grains has formed in SN 2010jl by ∼1400 days post-outburst. Unified Astronomy Thesaurus concepts: Core-collapse supernovae (304); Type II supernovae (1731); Circumstellar dust (236); Dust continuum emission (412); Dust nebulae (413); Astronomical models (86); Radiative transfer (1335); Extinction (505); Circumstellar shells (242); Dust shells (414)

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Section: Discussionmentioning

confidence: 99%

“…In Figure 8, the SEDs are at the same epoch and scaled to the same distance, and there is about four orders of magnitude more dust luminosity from SN 2010jl. Ofek et al (2019) preformed a similar exercise by showing that 1 M e of 56 Ni was not enough to reproduce the light curve.…”

Section: How Is the Dust Heated?mentioning

confidence: 99%

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

Bevan

Krafton

Wesson

et al. 2020

ApJ

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show abstract

“…In Figure 8, the SEDs are at the same epoch and scaled to the same distance and there is about four orders of magnitude more dust luminosity from SN 2010jl. Ofek et al (2019) preformed a similar exercise by showing that 1 M of 56 Ni was not enough to reproduce the light curve.…”

Section: How Is the Dust Heated?mentioning

confidence: 99%

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

Bevan,

Krafton,

Wesson

et al. 2020

Preprint

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The luminous Type IIn SN 2010jl shows strong signs of interaction between the SN ejecta and dense circumstellar material. Dust may be present in the unshocked ejecta, the cool, dense shell between the shocks in the interaction region, or in the circumstellar medium. We present and model new optical and infrared photometry and spectroscopy of SN 2010jl from 82 to 1367 days since explosion. We evaluate the photometric and spectroscopic evolution using the radiative transfer codes mocassin and damocles, respectively. We propose an interaction scenario and investigate the resulting dust formation scenarios and dust masses. We find that SN 2010jl has been continuously forming dust based on the evolution of its infrared emission and optical spectra. There is evidence for pre-existing dust in the circumstellar medium as well as new dust formation in the cool, dense shell and/or ejecta. We estimate that 0.005-0.01 M of predominantly carbon dust grains has formed in SN 2010jl by ∼1400 d post-outburst.

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“…Some of the most extreme exemplars are characterised by long-lasting, slowly evolving light curves. SN 2010jl is an archetypal long-lived type IIn event, reaching an absolute magnitude of ∼ −19.9 mag in the V band and remaining bright for several years (Stoll et al 2011;Ofek et al 2019).…”

Section: Introductionmentioning

confidence: 99%

A long life of excess: The interacting transient SN 2017hcc

Moran

Fraser

Kotak

et al. 2023

A&A

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In this study we present the results of a five-year follow-up campaign of the long-lived type IIn supernova SN 2017hcc, found in a spiral dwarf host of near-solar metallicity. The long rise time (57 ± 2 days, ATLAS o band) and high luminosity (peaking at −20.78 ± 0.01 mag in the ATLAS o band) point towards an interaction of massive ejecta with massive and dense circumstellar material (CSM). The evolution of SN 2017hcc is slow, both spectroscopically and photometrically, reminiscent of the long-lived type IIn, SN 2010jl. An infrared (IR) excess was apparent soon after the peak, and blueshifts were noticeable in the Balmer lines starting from a few hundred days, but appeared to be fading by around +1200 d. We posit that an IR light echo from pre-existing dust dominates at early times, with some possible condensation of new dust grains occurring at epochs >∼+800 d.

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A Six-year Image-subtraction Light Curve of SN 2010jl

Cited by 4 publications

References 70 publications

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

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

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

A long life of excess: The interacting transient SN 2017hcc

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