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

Szalai, T.; Fox, O.; Arendt, Richard G.; Dwek, Eli; Andrews, Jennifer E.; Clayton, Geoffrey C.; Filippenko, A. V.; Johansson, Joel; Kelly, Patrick L.; Krafton, Kelsie; Marston, A. P.; Mauerhan, Jon C.; Dyk, Schuyler D. Van

doi:10.3847/1538-4357/ac0e2b

Cited by 20 publications

(15 citation statements)

References 118 publications

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“…With this conversion, W 1 − W 2 ∼ 1.2 corresponds to I1 − I2 ∼ 0.9, consistent with those of normal SNe with dust emission detected (Szalai et al 2021). We detected no significant changes in the MIR colors of SN 2017egm and SN 2017gci, and the red colors (W 1 − W 2 ∼ 1) suggest that dust emission is also notable in them.…”

Section: The Declining Groupsupporting

confidence: 88%

“…Similarly, the dust origin in most normal SNe remains unclear as the emitting dust can be either pre-existing or newly formed (e.g., Fox et al 2011;Szalai & Vinko 2013;Tinyanont et al 2016;Szalai et al 2019Szalai et al , 2021. This ambiguity hinders further research on some important topics, such as the mass loss of the SN progenitor for the case of pre-existing dust and the dust formation efficiency for the case of newly formed dust.…”

Section: Introductionmentioning

confidence: 99%

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A Mid-infrared Study of Superluminous Supernovae

Sun,

Xiao,

2022

Preprint

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We present the mid-infrared (MIR) light curves (LC) of 10 superluminous supernovae (SLSNe) at z < 0.12 based on WISE data at 3.4 and 4.6 µm. Three of them, including PS15br, SN 2017ens, and SN 2017err show rebrightening which started at 200-400 days and ended at 600-1000 days, indicating the presence of dust. In four of the left seven SLSNe, dust emission was detected with monochromatic luminosities of 10 7 ∼ 10 8 L at epochs of 100-500 days based on MIR colors W 1 − W 2 ∼ 1. Among the three SLSNe which show rebrightening, we further analysed PS15br and SN 2017ens. We modeled the SEDs at 500-700 days, which gives dust temperatures of 600-1100 K, dust masses of 10 −2 M , and luminosities of 10 8 ∼ 10 9 L . Considering the time delay and the huge amount of energy released, the emitting dust can hardly be pre-existing dust heated whether collisionally by shocks or radiatively by peak SLSN luminosity or shock emission. Instead, it can be newly formed dust additionally heated by the interaction of circumstellar medium, indicated by features in their spectra and slowly declining bolometric LCs. The dust masses appear to be ten times greater than those formed in normal core-collapse supernovae at similar epochs. Combining with the analysis of SN 2018bsz by Chen et al. ( 2022), we suggest that SLSNe have higher dust formation efficiency, although future observations are required to reach a final conclusion.

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Section: The Declining Groupsupporting

confidence: 88%

Section: Introductionmentioning

confidence: 99%

A Mid-infrared Study of Superluminous Supernovae

Sun,

Xiao,

2022

Preprint

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“…Most SNe show signs of interaction within a few years of their evolution with rarer cases showing interaction on timescales of O( 10) years [e.g., [108][109][110][111][112][113][114]. Since the maximum time, t max (corresponding to r max ) depends on the extent of the CSM, YSNe with extended CSM could have t max ∼ O(10) years.…”

Section: Neutrino Productionmentioning

confidence: 99%

High energy particles from young supernovae: gamma-ray and neutrino connections

Sarmah,

Chakraborty,

Tamborra

et al. 2022

Preprint

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Up to about one year after explosion, core-collapse supernovae ("young supernovae," YSNe) are factories of high-energy neutrinos and gamma-rays as the shock accelerated protons efficiently interact with the protons in the dense circumstellar medium. We explore the detection prospects of secondary particles from YSNe of Type IIn, II-P, IIb/II-L, and Ib/c. Type IIn YSNe are found to produce the largest flux of neutrinos and gamma-rays, followed by II-P YSNe. Fermi-LAT and the Cherenkov Telescope Array (IceCube-Gen2) have the potential to detect Type IIn YSNe up to 10 Mpc (4 Mpc), with the remaining YSNe Types being detectable closer to Earth. We also find that YSNe may dominate the diffuse neutrino background, especially between 10 TeV and 10 3 TeV, while they do not constitute a dominant component to the isotropic gamma-ray background observed by Fermi-LAT. At the same time, the IceCube high-energy starting events and Fermi-LAT data already allow us to exclude a large fraction of the model parameter space of YSNe otherwise inferred from multi-wavelength electromagnetic observations of these transients.

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“…At later times (> 100 days), the line profiles are no longer consistent with electron scattering. Profiles are often fit by multiple Gaussians (e.g., Kiewe et al 2012;Szalai et al 2021). Although reasonable fits can be obtained, there is not a clear theory that points to Gaussian line shapes.…”

Section: Introductionmentioning

confidence: 99%

The luminous type IIn supernova SN 2017hcc: Infrared bright, X-ray, and radio faint

Chandra

Chevalier

James

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We present multiwavelength observations of supernova (SN) 2017hcc with the Chandra X-ray telescope and the X-ray telescope onboard Swift (Swift-XRT) in X-ray bands, with the Spitzer and the TripleSpec spectrometer in near-infrared (IR) and mid-IR bands and with the Karl G. Jansky Very Large Array (VLA) for radio bands. The X-ray observations cover a period of 29 to 1310 days, with the first X-ray detection on day 727 with the Chandra. The SN was subsequently detected in the VLA radio bands from day 1000 onwards. While the radio data are sparse, synchrotron-self absorption is clearly ruled out as the radio absorption mechanism. The near- and the mid-IR observations showed that late time IR emission dominates the spectral energy distribution. The early properties of SN 2017hcc are consistent with shock breakout into a dense mass-loss region, with $\dot{M} \sim 0.1$M⊙ yr−1 for a decade. At few 100 days, the mass-loss rate declined to ∼0.02 M⊙ yr−1, as determined from the dominant IR luminosity. In addition, radio data also allowed us to calculate a mass-loss rate at around day 1000, which is two orders of magnitude smaller than the mass-loss rate estimates around the bolometric peak. These values indicate that the SN progenitor underwent an enhanced mass-loss event a decade before the explosion. The high ratio of IR to X-ray luminosity is not expected in simple models and is possible evidence for an asymmetric circumstellar region.

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

Cited by 20 publications

References 118 publications

A Mid-infrared Study of Superluminous Supernovae

A Mid-infrared Study of Superluminous Supernovae

High energy particles from young supernovae: gamma-ray and neutrino connections

The luminous type IIn supernova SN 2017hcc: Infrared bright, X-ray, and radio faint

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