SN2012ca: a stripped envelope core-collapse SN interacting with dense circumstellar medium

Inserra, C.; Smartt, S. J.; Scalzo, R.; Fraser, M.; Pastorello, A.; Childress, M.; Pignata, G.; Jerkstrand, A.; Kotak, R.; Benetti, S.; Valle, M. Della; Gal‐Yam, A.; Mazzali, P. A.; Smith, K.; Sullivan, M.; Valenti, S.; Yaron, O.; Young, D. R.; Reichart, D.

doi:10.1093/mnrasl/slt138

Cited by 28 publications

(53 citation statements)

References 47 publications

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“…Many NIR spectra of various SN types obtained by CSP-II have already been published in single-object papers: the rebrightening of SN 2009ip (Margutti et al 2014), the Type IIb SN 2011hs (Bufano et al 2014), the broad-lined Type Ic SN 2012ap (Milisavljevic et al 2015), the Type Ib SN 2012au (Milisavljevic et al 2013), the Type II SN 2012aw (Dall'Ora et al 2014), the Type IIn SN 2012ca (Fox et al 2015), the Type IIL SN 2013by (Valenti et al 2015), the Type Ib/c SN 2013ge (Drout et al 2016), as well as the SN 2002cxlike SN 2012Z (Stritzinger et al 2015) and SN 2014ck (Tomasella et al 2016). Note that SN 2012ca may be a SN Ia interacting with its surrounding circumstellar medium as noted by several studies (Inserra et al 2014(Inserra et al , 2016Fox et al 2015) An atlas of the NIR spectra of supernovae of various types is plotted in Figure 4. The dominant ion species are labeled.…”

Section: Sample Characteristicsmentioning

confidence: 99%

Carnegie Supernova Project-II: The Near-infrared Spectroscopy Program

Hsiao

Phillips

Marion

et al. 2018

PASP

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Corresponding author: E. Y. Hsiao ehsiao@fsu.edu * This paper includes data gathered with the 6.5-m Magellan telescopes at Las Campanas Observatory, Chile. Hsiao et al.Shifting the focus of Type Ia supernova (SN Ia) cosmology to the near-infrared (NIR) is a promising way to significantly reduce the systematic errors, as the strategy minimizes our reliance on the empirical width-luminosity relation and uncertain dust laws. Observations in the NIR are also crucial for our understanding of the origins and evolution of these events, further improving their cosmological utility. Any future experiments in the rest-frame NIR will require knowledge of the SN Ia NIR spectroscopic diversity, which is currently based on a small sample of observed spectra. Along with the accompanying paper, Phillips et al. (2018), we introduce the Carnegie Supernova Project-II (CSP-II), to follow up nearby SNe Ia in both the optical and the NIR. In particular, this paper focuses on the CSP-II NIR spectroscopy program, describing the survey strategy, instrumental setups, data reduction, sample characteristics, and future analyses on the data set. In collaboration with the Harvard-Smithsonian Center for Astrophysics (CfA) Supernova Group, we obtained 661 NIR spectra of 157 SNe Ia. Within this sample, 451 NIR spectra of 90 SNe Ia have corresponding CSP-II follow-up light curves. Such a sample will allow detailed studies of the NIR spectroscopic properties of SNe Ia, providing a different perspective on the properties of the unburned material, radioactive and stable nickel produced, progenitor magnetic fields, and searches for possible signatures of companion stars.

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Section: Sample Characteristicsmentioning

confidence: 99%

Carnegie Supernova Project-II: The Near-infrared Spectroscopy Program

Hsiao

Phillips

Marion

et al. 2018

PASP

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“…2 would merge before it explodes as a SN Ia, leaving the WD at the center of the CE and essentially forming a single AGB star with an overmassive core. If the core is spun down within its envelope and carbon is ignited at the center of the hybrid CONe core while there still is a massive envelope around it, the resulting supernova would have some very unusual properties (produce a SN I 1/2 in the nomen-clature of Iben & Renzini 1983), with properties between those of a core-collapse (CC) SN and a SN Ia, an example of which may be provided by SN 2012ca (Inserra et al 2014(Inserra et al , 2016. If the envelope is ejected before carbon is ignited in the center, it would lead to the thermonuclear explosion of an apparently single CONe WD.…”

Section: An Example Of a Delayed Dynamical Instabilitymentioning

confidence: 99%

Do SN 2002cx-like and SN Ia-CSM Objects Share the Same Origin?

Meng

Podsiadlowski

2018

ApJ

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SN 2002cx-like and SN Ia-CSM objects show similar early spectra and both belong to a young stellar population, suggesting that they could share the same progenitor origin. Adopting the framework of the common-envelope-wind (CEW) model developed in Meng & Podsiadlowski (2017), we here propose that both subclasses of SNe Ia are caused by the explosion of hybrid carbon-oxygen-neon white dwarfs (CONe WDs) in single-degenerate systems, where SNe Ia-CSM explode in systems with a massive common envelope (CE) of ∼ 1 M ⊙ , while SN 2002cxlike events correspond to those events where most of the CE has been lost in a wind. Using binary-population-synthesis (BPS) calculations, we estimate a number ratio of SNe Ia-CSM to SN 2002cx-like objects between 1 3 and 2 3 , consistent with observational constraints, and an overall contribution from hybrid CONe WDs to the total SN Ia population that also matches the observed number from these peculiar objects. Our model predicts a statistical sequence of CSM density from SN Ia-CSM to SN 2002cx-like events and normal SNe Ia, consistent with existing radio constraints. We also find a new subclass of hybrid SNe which share the properties of Type II and Type Ia SNe, consistent with some observed SNe, which do not have a surviving companion. In some cases these could even produce SNe Ia from apparently single WDs.

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“…There are several arguments against this view including the detailed spectroscopic differences between SNe Ia and SNe Ic, such as the S ii W-shaped feature at ∼5400 Å (seen in SN 2002ic), or the existence of clear cases, such as PTF11kx (Dilday et al 2012). Inserra et al (2014) argued that SN 2012ca was another Ic-CSM event based on the likely detection of blueshifted O, Mg, and C in late-time spectra. However, these line identifications were challenged by Fox et al (2015), who propose that these lines can instead be due to coronal Fe emission, and thus favour a thermonuclear origin for this SN.…”

Section: Normal Eventsmentioning

confidence: 99%

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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SN2012ca: a stripped envelope core-collapse SN interacting with dense circumstellar medium

Cited by 28 publications

References 47 publications

Carnegie Supernova Project-II: The Near-infrared Spectroscopy Program

Carnegie Supernova Project-II: The Near-infrared Spectroscopy Program

Do SN 2002cx-like and SN Ia-CSM Objects Share the Same Origin?

Supernova spectra below strong circumstellar interaction

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