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

Bevan, Antonia; Krafton, Kelsie; Wesson, R.; Andrews, Jennifer E.; Montiel, Edward; Niculescu-Duvaz, Maria; Barlow, M. J.; Looze, I. De; Clayton, Geoffrey C.

doi:10.3847/1538-4357/ab86a2

Cited by 36 publications

(44 citation statements)

References 50 publications

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“…While SN 2010jl exhibits near-IR and mid-IR rebrightening and a quite long plateau after ∼400 days, it is preceded by an X-ray/Hα peak somewhere between 200 and 300 days. As previously noted (e.g., Fransson et al 2014;Gall et al 2014;Sarangi et al 2018;Bevan et al 2020), an IR excess before ∼400 days may be the consequence of heating of pre-existing dust, while mid-IR flux at a later time may originate either from new dust in the CDS and/or the ejecta or from CSM dust. Sarangi et al (2018) presented a comparative analysis of mid-IR and X-ray LCs, and we complete that comparison here with the addition of an Hα LC (adopted from Fransson et al 2014).…”

Section: A Comprehensive Multiwavelength Overview Of Lcs Of Interacting Snementioning

confidence: 53%

“…In the first few hundreds of days after explosion, when hot (T  1000 K) components of gas and dust tend to dominate the ejecta and/or its environment, the IRAC measurements probe the peak of the dust blackbody emission and provide the best constraints on the physical parameters. Such measurements have been illustrated with several SNe II-P (see, e.g., Sugerman et al 2006;Meikle et al 2007;Kotak et al 2009;Andrews et al 2010Andrews et al , 2011bSzalai et al 2011;Szalai & Vinkó 2013) and several interacting SNe (SN 2005ip-Fox et al 2010Stritzinger et al 2012;SN 2006jd-Stritzinger et al 2012SN 2010jl-Andrews et al 2011aFransson et al 2014;Sarangi et al 2018;Bevan et al 2020;SN 2013L-Andrews et al 2017Taddia et al 2020;SN 2014C-Tinyanont et al 2019bSN 2015da-Tartaglia et al 2020.…”

Section: Mid-ir Color Curves and Dust Temperaturesmentioning

confidence: 98%

“…If we compare these values with the mid-IR LC evolution of the objects (Figures 2 and 3), we can see that the brightest ones (SNe 2007rt, 2010jl, and 2013cj) exhibit a faster decline after ∼1000 days. In the case of SN 2010jl, comprehensive multiwavelength studies and detailed analyses of ongoing dust formation exist (e.g., Andrews et al 2011a;Gall et al 2014;Fransson et al 2014;Sarangi et al 2018;Bevan et al 2020); unfortunately, there are no similar data sets in the cases of SN 2007rt and SN 2013cj. Another group of SNe IIn (SNe 2005ip, 2006jd, and 2013L) seem to be a bit fainter during the first ∼2000 days (note, however, that in the first two cases there are no mid-IR data before ∼950 days and ∼1150 days, respectively), but decline more slowly thereafter.…”

Section: Type Iin Snementioning

confidence: 99%

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Spitzer’s Last Look at Extragalactic Explosions: Long-term Evolution of Interacting Supernovae

Szalai

Fox

Arendt³

et al. 2021

ApJ

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Here we present new, yet final, mid-infrared (mid-IR) data for supernovae (SNe) based on measurements with the Spitzer Space Telescope. Comparing our recent 3.6 and 4.5 μm photometry with previously published mid-IR and further multiwavelength data sets, we were able to draw some conclusions about the origin and heating mechanism of the dust in these SNe or in their environments, as well as about possible connection with circumstellar matter (CSM) originating from pre-explosion mass-loss events in the progenitor stars. We also present new results regarding both certain SN classes and single objects. We highlight the mid-IR homogeneity of SNe Ia-CSM, which may be a hint of their common progenitor type and of their basically uniform circumstellar environments. Regarding single objects, it is worth highlighting the late-time interacting Type Ib SNe 2003gk and 2004dk, for which we present the first-ever mid-IR data, which seem to be consistent with clues of ongoing CSM interaction detected in other wavelength ranges. Our current study suggests that long-term mid-IR follow-up observations play a key role in a better understanding of both pre-and post-explosion processes in SNe and their environments. While Spitzer is not available anymore, the expected unique data from the James Webb Space Telescope, as well as long-term near-IR follow-up observations of dusty SNe, can bring us closer to the hidden details of this topic.Unified Astronomy Thesaurus concepts: Supernovae (1668); Infrared astronomy (786); Infrared telescopes (794); Circumstellar matter (241); Circumstellar dust (236)

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Section: A Comprehensive Multiwavelength Overview Of Lcs Of Interacting Snementioning

confidence: 53%

Section: Mid-ir Color Curves and Dust Temperaturesmentioning

confidence: 98%

Section: Type Iin Snementioning

confidence: 99%

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Spitzer’s Last Look at Extragalactic Explosions: Long-term Evolution of Interacting Supernovae

Szalai

Fox

Arendt³

et al. 2021

ApJ

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“…Smith et al (2016b) find that such long-lived emission from SNe IIn requires mass-loss episodes from the SN progenitor to occur for 1000 yr preceding the explosion. Some SNe IIn also show signs of pre-existing dust in the CSM shell revealed through infrared (IR) observations (e.g., SN 2010jl, Bevan et al 2020;SN 2014ab, Moriya et al 2020SN 2017hcc, Smith & Andrews 2020. Other transients show CSM interaction for a brief period, perhaps indicating a more confined CSM (e.g., SN 2008fq, Taddia et al 2013SN 2018zd, Zhang et al 2020.…”

Section: Introductionmentioning

confidence: 99%

A systematic reclassification of Type IIn supernovae

Ransome

Habergham-Mawson

Darnley

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Type IIn supernovae (SNe IIn) are a relatively infrequently observed subclass of SNe whose photometric and spectroscopic properties are varied. A common thread among SNe IIn are the complex multiple-component hydrogen Balmer lines. Owing to the heterogeneity of SNe IIn, online databases contain some outdated, erroneous, or even contradictory classifications. SN IIn classification is further complicated by SN “impostors” and contamination from underlying H ii regions. We have compiled a catalogue of systematically classified nearby (redshift z < 0.02) SNe IIn using the Open Supernova Catalogue (OSC). We present spectral classifications for 115 objects previously classified as SNe IIn. Our classification is based upon results obtained by fitting multiple Gaussians to the Hα profiles. We compare classifications reported by the OSC and Transient Name Server (TNS) along with the best matched templates from SNID. We find that 28 objects have been misclassified as SNe IIn. TNS and OSC can be unreliable; they disagree on the classifications of 51 of the objects and contain a number of erroneous classifications. Furthermore, OSC and TNS hold misclassifications for 34 and twelve (respectively) of the transients we classify as SNe IIn. In total, we classify 87 SNe IIn. We highlight the importance of ensuring that online databases remain up to date when new or even contemporaneous data become available. Our work shows the great range of spectral properties and features that SNe IIn exhibit, which may be linked to multiple progenitor channels and environment diversity. We set out a classification sche me for SNe IIn based on the Hα profile which is not greatly affected by the inhomogeneity of SNe IIn.

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“…Some researches interpret the IR excess as the evidence of newly-formed dust (Smith et al 2012;Maeda et al 2013;Gall et al 2014), while others suggest a pre-existing and unshocked CSM dust grains (Andrews et al 2011;Fox et al 2013;Fransson et al 2014). Moreover, Bevan et al (2020) and Chugai (2018) propose that SN 2010jl presents both evidence of pre-existing dust in CSM and newly-formed dust in cold dense shell and/or ejecta. Gall et al (2014) derived the extinction curves of SN 2010jl from the attenuation of emission lines, and found rapid (in 40 -240 days) dust formation and inferred the presence of very large (> 1 micron) grains.…”

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confidence: 99%

Dust Models for the Extinction of Type IIn Supernova SN 2010jl

Li,

Gao,

Jiang

et al. 2022

Preprint

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The unusual extinction curves of SN 2010jl provide an excellent opportunity to investigate the properties of dust formed by core-collapse supernovae. By using a series of dust models with different compositions and grain size distributions, we fit the extinction curves of SN 2010jl and find that a silicate-graphite mixture dust model characterized by exponentially cutoff powerlaw size distributions can well reproduce its unusual extinction curves. The best-fit results show that the extinctions derived from the dust models are consistent with the observed values at all epochs. However, the total-to-selective extinction ratio 𝑅 𝑉 is about 2.8 -3.1, which is significantly smaller than the value of 𝑅 𝑉 ≈ 6.4 derived by Gall et al. The best-fit models indicate that the dust grains around SN 2010jl are possibly composed of small-size astronomical silicate grains and micron-size graphite grains. In addition, by fitting the optical to mid-infrared spectral energy distribution, we find that the dust mass around SN 2010jl increases with time, up to 0.005 𝑀 around 1300 days after peak brightness, which is consistent with previous estimates.

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

Cited by 36 publications

References 50 publications

Spitzer’s Last Look at Extragalactic Explosions: Long-term Evolution of Interacting Supernovae

Spitzer’s Last Look at Extragalactic Explosions: Long-term Evolution of Interacting Supernovae

A systematic reclassification of Type IIn supernovae

Dust Models for the Extinction of Type IIn Supernova SN 2010jl

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