Light curve and spectral evolution of the Type IIb supernova 2011fu

Kumar, Brajesh; Pandey, S. B.; Sahu, D. K.; Vinkó, J.; Москвитин, А. С.; Anupama, G. C.; Bhatt, V. K.; Ordasi, A.; Nagy, Andrea; Соколов, В. В.; Sokolova, T. N.; Komarova, V. N.; Kumar, Brijesh; Bose, S.; Roy, R.; Sagar, Ram

doi:10.1093/mnras/stt162

Cited by 52 publications

(49 citation statements)

References 92 publications

(141 reference statements)

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“…This lightcurve evolution is indicative of a massive progenitor that explodes via core collapse. A similar early-time bump was also detected in the Type Ib SN 1999ex (Stritzinger et al 2002), and in recent years early bumps have been used to constrain the radius of the progenitor star in a number of cases, such as SN 2008D (Chevalier & Fransson 2008;Bersten et al 2013), SN 2011dh (Arcavi et al 2011;Soderberg et al 2012;Bersten et al 2012), SN 2011fu (Kumar et al 2013), SN 2011hs (Bufano et al 2014), SN 2013df (Morales-Garoffolo et al 2014, and SN 2016gkg (Tartaglia et al 2017;Arcavi et al 2017). …”

Section: Introductionmentioning

confidence: 64%

The Carnegie Supernova Project I

Stritzinger

Anderson

Contreras

et al. 2018

A&A

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The first phase of the Carnegie Supernova Project (CSP-I) was a dedicated supernova follow-up program based at the Las Campanas Observatory that collected science data of young, low-redshift supernovae between 2004 and 2009. Presented in this paper is the CSP-I photometric data release of low-redshift stripped-envelope core-collapse supernovae. The data consist of optical (uBgVri) photometry of 34 objects, with a subset of 26 having near-infrared (Y JH) photometry. Twenty objects have optical pre-maximum coverage with a subset of 12 beginning at least five days prior to the epoch of B-band maximum brightness. In the near-infrared, 17 objects have pre-maximum observations with a subset of 14 beginning at least five days prior to the epoch of J-band maximum brightness. Analysis of this photometric data release is presented in companion papers focusing on techniques to estimate host-galaxy extinction and the light-curve and progenitor star properties of the sample. The analysis of an accompanying visual-wavelength spectroscopy sample of ∼150 spectra will be the subject of a future paper.

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Section: Introductionmentioning

confidence: 64%

The Carnegie Supernova Project I

Stritzinger

Anderson

Contreras

et al. 2018

A&A

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“…At the expected positions of He I λ5876, the mean spectra of SNe Ic show a broad feature but no obvious absorption feature at t Vmax ;−10 and 0 days, a weak absorption feature at t Vmax ;10 days, and a strong absorption feature at t Vmax ;20 days. However, this feature, which one might identify as He I λ5876, could be due to other elements such as Na I D, as claimed by many authors (e.g., Branch et al 2002;Elmhamdi et al 2006;Kumar et al 2013;Marion et al 2014) who use spectral synthesis calculations. Most importantly, the mean spectra of SNe Ic show no convincing signs of He I λλ6678 and 7065 either.…”

Section: Are There Weak He I Lines In Spectra Of Sne Ic?mentioning

confidence: 94%

Analyzing the Largest Spectroscopic Data Set of Stripped Supernovae to Improve Their Identifications and Constrain Their Progenitors

Liu

Modjaz

Bianco

et al. 2016

ApJ

125

220

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Using the largest spectroscopic data set of stripped-envelope core-collapse supernovae (stripped SNe), we present a systematic investigation of spectral properties of Type IIb SNe (SNe IIb), Type Ib SNe (SNe Ib), and Type Ic SNe (SNe Ic). Prior studies have been based on individual objects or small samples. Here, we analyze 242 spectra of 14 SNe IIb, 262 spectra of 21 SNe Ib, and 207 spectra of 17 SNe Ic based on the stripped SN data set of Modjaz et al. and other published spectra of individual SNe. Each SN in our sample has a secure spectroscopic ID, a date of V-band maximum light, and most have multiple spectra at different phases. We analyze these spectra as a function of subtype and phase in order to improve the SN identification scheme and constrain the progenitors of different kinds of stripped SNe. By comparing spectra of SNe IIb with those of SNe Ib, we find that the strength of Hα can be used to quantitatively differentiate between these two subtypes at all epochs. Moreover, we find a continuum in observational properties between SNe IIb and Ib. We address the question of hidden He in SNe Ic by comparing our observations with predictions from various models that either include hidden He or in which He has been burnt. Our results favor the He-free progenitor models for SNe Ic. Finally, we construct continuum-divided average spectra as a function of subtype and phase to quantify the spectral diversity of the different types of stripped SNe.

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“…There are now numerous cases of cooling envelope emission observed in various types of core collapse SNe caught soon after explosion: one SN II [25], several SNe IIb [8,35,44,94,95,96], two SNe Ib [92,93,131], and two SNe Ic-bl with GRBs [e.g. 99, 115, though the latter suggest that the emission is from a cooling jet cocoon, not a cooling stellar envelope].…”

Section: Shock Breakout and Cooling Envelope Emissionmentioning

confidence: 99%

New regimes in the observation of core-collapse supernovae

2019

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Core-collapse Supernovae (CCSNe) mark the deaths of stars more massive than about eight times the mass of the sun (M ) and are intrinsically the most common kind of catastrophic cosmic explosions. They can teach us about many important physical processes, such as nucleosynthesis and stellar evolution, and thus, they have been studied extensively for decades. However, many crucial questions remain unanswered, including the most basic ones regarding which kinds of massive stars achieve which kind of explosions and how. Observationally, this question is related to the open puzzles of whether CCSNe can be divided into distinct types or whether they are drawn from a population with a continuous set of properties, and of what progenitor characteristics drive the diversity of observed explosions. Recent developments in wide-field surveys and rapid-response followup facilities are helping us answer these questions by providing two new tools: (1) large statistical samples which enable population studies of the most common SNe, and reveal rare (but extremely informative) events that question our standard understanding of the explosion physics involved, and (2) observations of early SNe emission taken shortly after explosion which carries signatures of the progenitor structure and mass loss history. Future facilities will increase our capabilities and allow us to answer many open questions related to these extremely energetic phenomena of the Universe.We focus this short review on a few open questions which are being tackled by new facilities for quick discovery and rapidresponse followup, as well as for studying CCSNe in large numbers. For a more exhaustive review of the field see recent compilations such as the Handbook of Supernovae [1]. The CCSN Classification LandscapeSN classification has been a challenge since the 1940's [2], but especially recently, as innovative surveys have brought a large increase of new and debated types. Classification schemes are important as physically motivated ones can give crucial insight into the explosion physics and stellar evolution pathways that lead to the different kinds of important explosions.The classical classification scheme [e.g., 3, 4] relies mostly on spectra and has two main types: Type I SNe (SNe I) which do not show hydrogen lines, and Type II SNe (SNe II) which do.In Figure 1 (left panel), we present spectra around peak brightness of the main CCSN classes. Among them, SNe II are perhaps the most heterogeneous class with a large range of observed photometric and spectroscopic properties. Because of this diversity, they can be further divided into several subclasses. The first historical subclassification was based on the light curve shape: SNe showing a linear decline (in magnitudes) in their light curve were named SNe IIL, while SNe showing a quasiconstant luminosity or a plateau for several weeks were called SNe IIP [13]. Later it was discovered that Type IIP and IIL SNe can also be distinguished by a subtle difference in their spectra, with SNe IIP showing deeper absor...

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Light curve and spectral evolution of the Type IIb supernova 2011fu

Cited by 52 publications

References 92 publications

The Carnegie Supernova Project I

The Carnegie Supernova Project I

Analyzing the Largest Spectroscopic Data Set of Stripped Supernovae to Improve Their Identifications and Constrain Their Progenitors

New regimes in the observation of core-collapse supernovae

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