On the nature of Type IIn/Ia–CSM supernovae: optical and near-infrared spectra of SN 2012ca and SN 2013dn

Fox, O.; Silverman, J. M.; Filippenko, A. V.; Mauerhan, Jon C.; Becker, Juliette; Borish, H. Jacob; Cenko, S. Bradley; Clubb, K. I.; Graham, M. L.; Hsiao, E. Y.; Kelly, Patrick L.; Lee, William H.; Marion, G. H.; Milisavljevic, Dan; Parrent, J.; Shivvers, I.; Skrutskie, Michael F.; Smith, Nathan; Wilson, John C.; Zheng, W.

doi:10.1093/mnras/stu2435

Cited by 61 publications

(66 citation statements)

References 83 publications

(95 reference statements)

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“…Silverman et al (2013) reported on the discovery of additional SNe Ia-CSM in archival and Palomar Transient Factory (PTF; Law et al 2009) data, raising the total number to 16 objects. Two more events have been reported since this study (Inserra et al 2014;Fox et al 2015). Curiously, Anderson et al (2012) have shown that the distribution of SN IIn locations with respect to star formation lies between those of SNe Ia and those of SNe from more massive stars.…”

Section: Introductionmentioning

confidence: 57%

Supernova spectra below strong circumstellar interaction

Leloudas

Hsiao

Johansson

et al. 2015

A&A

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We construct spectra of supernovae (SNe) interacting strongly with a circumstellar medium (CSM) by adding SN templates, a blackbody continuum, and an emission-line spectrum. In a Monte Carlo simulation we vary a large number of parameters, such as the SN type, brightness and phase, the strength of the CSM interaction, the extinction, and the signal to noise ratio (S/N) of the observed spectrum. We generate more than 800 spectra, distribute them to ten different human classifiers, and study how the different simulation parameters affect the appearance of the spectra and their classification. The SNe IIn showing some structure over the continuum were characterized as "SNe IInS" to allow for a better quantification. We demonstrate that the flux ratio of the underlying SN to the continuum f V is the single most important parameter determining whether a spectrum can be classified correctly. Other parameters, such as extinction, S/N, and the width and strength of the emission lines, do not play a significant role. Thermonuclear SNe get progressively classified as Ia-CSM, IInS, and IIn as f V decreases. The transition between Ia-CSM and IInS occurs at f V ∼ 0.2−0.3. It is therefore possible to determine that SNe Ia-CSM are found at the (un-extincted) magnitude range −19.5 > M > −21.6, in very good agreement with observations, and that the faintest SN IIn that can hide a SN Ia has M = −20.1. The literature sample of SNe Ia-CSM shows an association with 91T-like SNe Ia. Our experiment does not support that this association can be attributed to a luminosity bias (91T-like being brighter than normal events). We therefore conclude that this association has real physical origins and we propose that 91T-like explosions result from single degenerate progenitors that are responsible for the CSM. Despite the spectroscopic similarities between SNe Ibc and SNe Ia, the number of misclassifications between these types was very small in our simulation and mostly at low S/N. Combined with the SN luminosity function needed to reproduce the observed SN Ia-CSM luminosities, it is unlikely that SNe Ibc constitute an important contaminant within this sample. We show how Type II spectra transition to IIn and how the Hα profiles vary with f V . SNe IIn fainter than M = −17.2 are unable to mask SNe IIP brighter than M = −15. A more advanced simulation, including radiative transfer, shows that our simplified model is a good first order approximation. The spectra obtained are in good agreement with real data.

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Section: Introductionmentioning

confidence: 57%

Supernova spectra below strong circumstellar interaction

Leloudas

Hsiao

Johansson

et al. 2015

A&A

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“…Such an envelope might be created by pre-explosion mass loss or a binary interaction. There is mounting evidence for the existence of such dense stellar environments around other transients such as SN Type IIn (Fransson et al 2014, and references therein), SN Type IIb (Nakar & Piro 2014), SN Type Ibn (e.g., Matheson et al 2000;Pastorello et al 2008;Gorbikov et al 2014), and SN Type Ia-CSM (Silverman et al 2013;Fox et al 2015).…”

Section: Shock Breakout or Central Engine?mentioning

confidence: 99%

Jet or shock breakout? The low-luminosity GRB 060218

Irwin

Chevalier

2016

Mon. Not. R. Astron. Soc.

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We consider a model for the low-luminosity gamma-ray burst GRB 060218 that plausibly accounts for multiwavelength observations to day 20. The model components are: (1) a long-lived (t j ∼ 3000 s) central engine and accompanying low-luminosity (L j ∼ 10 47 erg s −1 ), semirelativistic (γ ∼ 10) jet; (2) a low-mass (∼ 4 × 10 −3 M ) envelope surrounding the progenitor star; and (3) a modest amount of dust (A V ∼ 0.1 mag) in the interstellar environment. Blackbody emission from the transparency radius in a low-power jet outflow can fit the prompt thermal X-ray emission, and the nonthermal X-rays and γ-rays may be produced via Compton scattering of thermal photons from hot leptons in the jet interior or the external shocks. The later mildly relativistic phase of this outflow can produce the radio emission via synchrotron radiation from the forward shock. Meanwhile, interaction of the associated SN 2006aj with a circumstellar envelope extending to ∼ 10 13 cm can explain the early optical emission. The X-ray afterglow can be interpreted as a light echo of the prompt emission from dust at ∼ 30 pc. Our model is a plausible alternative to that of Nakar, who recently proposed shock breakout of a jet smothered by an extended envelope as the source of prompt emission. Both our results and Nakar's suggest that bursts such as GRB 060218 may originate from unusual progenitors with extended circumstellar envelopes, and that a jet is necessary to decouple the prompt emission from the supernova.

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“…Alternatively, the emitting dust could be interstellar in nature and illuminated by the optical flash (i.e., an "IR echo"). We first test the IR echo scenario by using Equation (2) to estimate the predicted temperature of dust at a distance ofc t 2, which is where the hottest dust is located if heated by the optical/UV flash (e.g., Fox et al 2011Fox et al , 2015. At t≈460 days and given an optical/UV outburst luminosity of L≈3×10 6 L e , the predicted dust temperature is 43 K, significantly less than the temperature estimated at day 460 (T d ≈850±73 K).…”

Section: Post-outburst Re-brightening: Evidence Of Progenitor Survivamentioning

confidence: 99%

RISING FROM THE ASHES: MID-INFRARED RE-BRIGHTENING OF THE IMPOSTOR SN 2010da IN NGC 300

Lau

Kasliwal

Bond

et al. 2016

ApJ

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We present multi-epoch mid-infrared (IR) photometry and the optical discovery observations of the "impostor" supernova (SN) 2010da in NGC300 using new and archival Spitzer Space Telescope images and ground-based observatories. The mid-infrared counterpart of SN2010da was detected as Spitzer Infrared Intensive Transient Survey (SPIRITS)14bme in the SPIRITS, an ongoing systematic search for IR transients. Before erupting on 2010 May 24, the SN2010da progenitor exhibited a constant mid-IR flux at 3.6 and only a slight ∼10% decrease at 4.5 μm between 2003 November and 2007 December. A sharp increase in the 3.6 μm flux followed by a rapid decrease measured ∼150 days before and ∼80 days after the initial outburst, respectively, reveal a mid-IR counterpart to the coincident optical and high luminosity X-ray outbursts. At late times, after the outburst (∼2000 days), the 3.6 and 4.5 μm emission increased to over a factor of twotimes the progenitor flux and is currently observed (as of 2016 Feb) to be fading, but still above the progenitor flux. We attribute the re-brightening mid-IR emission to continued dust production and increasing luminosity of the surviving system associated with SN2010da. We analyze the evolution of the dust temperature (T d ∼700-1000 K), mass (M d ∼0.5-3.8×10 −7 M e ), luminosity (L IR ∼1.3-3.5×10 4 L e ), and the equilibrium temperature radius (R eq ∼6.4-12.2 au) in order to resolve the nature of SN2010da. We address the leading interpretation of SN2010da as an eruption from a luminous blue variable high-mass X-ray binary (HMXB) system. We propose that SN2010da is instead a supergiant (sg)B[e]-HMXB based on similar luminosities and dust masses exhibited by two other known sgB[e]-HMXB systems. Additionally, the SN2010da progenitor occupies a similar region on a mid-IR color-magnitude diagram (CMD) with known sgB[e] stars in the Large Magellanic Cloud. The lower limit estimated for the orbital eccentricity of the sgB[e]-HMXB (e>0.82) from X-ray luminosity measurements is high compared to known sgHMXBs and supports the claim that SN2010da may be associated with a newly formed HMXB system.

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On the nature of Type IIn/Ia–CSM supernovae: optical and near-infrared spectra of SN 2012ca and SN 2013dn

Cited by 61 publications

References 83 publications

Supernova spectra below strong circumstellar interaction

Supernova spectra below strong circumstellar interaction

Jet or shock breakout? The low-luminosity GRB 060218

RISING FROM THE ASHES: MID-INFRARED RE-BRIGHTENING OF THE IMPOSTOR SN 2010da IN NGC 300

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