PANCHROMATIC OBSERVATIONS OF SN 2011dh POINT TO A COMPACT PROGENITOR STAR

Söderberg, A. M.; Margutti, R.; Zauderer, B. A.; Krauss, M. I.; Katz, Boaz; Chomiuk, Laura; Dittmann, Jason; Nakar, Ehud; Sakamoto, T.; Kawai, N.; Hurley, K.; Barthelmy, S. D.; Toizumi, T.; Morii, M.; Chevalier, Roger A.; Gurwell, M. A.; Petitpas, G.; Rupen, M. P.; Alexander, K. D.; Levesque, Emily M.; Fransson, Claes; Brunthaler, A.; Bietenholz, M. F.; Чугай, Н. Н.; Grindlay, Jonathan E.; Copete, A.; Connaughton, V.; Briggs, M. S.; Meegan, C.; Kienlin, A. von; Zhang, X.; Rau, A.; Golenetskii, S.; Mazets, E.; Cline, T. L.

doi:10.1088/0004-637x/752/2/78

Cited by 111 publications

(159 citation statements)

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“…Optical and NIR photometry and spectroscopy, mainly from the first 50 days, have been published by A11, M11, Tsvetkov et al (2012, hereafter T12), Vinkó et al (2012, hereafter V12), Marion et al (2013, hereafter M13), Van Dyk et al (2013, hereafter D13) and Sahu et al (2013, hereafter S13). Radio and millimeter observations have been published by Martí-Vidal et al (2011), Krauss et al (2012), Bietenholz et al (2012), Soderberg et al (2012) and Horesh et al (2013) and X-ray observations by Soderberg et al (2012), Sasaki & Ducci (2012) and Campana & Immler (2012). The SN has been monitored in the ultraviolet (UV) using Swift, in the mid-infrared (MIR) using Spitzer and at sub-millimeter wavelengths using Herschel.…”

Section: Supernova 2011dhmentioning

confidence: 99%

“…Using approximate models A11 argued that the SN cooled too fast and Soderberg et al (2012) that the speed of the shock was too high to be consistent with an extended progenitor. However, in B12 we have used detailed hydrodynamical modelling to show that a 3.3-4 M helium core with an attached thin and extended hydrogen envelope well reproduces the early photometric evolution and is also consistent with the temperature inferred from early spectra.…”

Section: Supernova 2011dhmentioning

confidence: 99%

“…The findings in B12 are in good agreement with those in M11 and the issue now seems to be settled by the disappearance of the yellow supergiant. See also Maeda (2012) for a discussion of the assumptions made in Soderberg et al (2012).…”

Section: Supernova 2011dhmentioning

confidence: 99%

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Optical and near-infrared observations of SN 2011dh – The first 100 days

Ergon

Sollerman

Fraser

et al. 2014

A&A

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We present optical and near-infrared (NIR) photometry and spectroscopy of the Type IIb supernova (SN) 2011dh for the first 100 days. We complement our extensive dataset with Swift ultra-violet (UV) and Spitzer mid-infrared (MIR) data to build a UV to MIR bolometric lightcurve using both photometric and spectroscopic data. Hydrodynamical modelling of the SN based on this bolometric lightcurve have been presented in Bersten et al. (2012, ApJ, 757, 31). We find that the absorption minimum for the hydrogen lines is never seen below ∼11 000 km s −1 but approaches this value as the lines get weaker. This suggests that the interface between the helium core and hydrogen rich envelope is located near this velocity in agreement with the Bersten et al. (2012) He4R270 ejecta model. Spectral modelling of the hydrogen lines using this ejecta model supports the conclusion and we find a hydrogen mass of 0.01-0.04 M to be consistent with the observed spectral evolution. We estimate that the photosphere reaches the helium core at 5-7 days whereas the helium lines appear between ∼10 and ∼15 days, close to the photosphere and then move outward in velocity until ∼40 days. This suggests that increasing non-thermal excitation due to decreasing optical depth for the γ-rays is driving the early evolution of these lines. The Spitzer 4.5 µm band shows a significant flux excess, which we attribute to CO fundamental band emission or a thermal dust echo although further work using late time data is needed. The distance and in particular the extinction, where we use spectral modelling to put further constraints, is discussed in some detail as well as the sensitivity of the hydrodynamical modelling to errors in these quantities. We also provide and discuss pre-and post-explosion observations of the SN site which shows a reduction by ∼75 percent in flux at the position of the yellow supergiant coincident with SN 2011dh. The B, V and r band decline rates of 0.0073, 0.0090 and 0.0053 mag day −1 respectively are consistent with the remaining flux being emitted by the SN. Hence we find that the star was indeed the progenitor of SN 2011dh as previously suggested by Maund et al. (2011, ApJ, 739, L37) and which is also consistent with the results from the hydrodynamical modelling.

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Section: Supernova 2011dhmentioning

confidence: 99%

Section: Supernova 2011dhmentioning

confidence: 99%

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Optical and near-infrared observations of SN 2011dh – The first 100 days

Ergon

Sollerman

Fraser

et al. 2014

A&A

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125

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“…Collisions of matter outside the star might also occur and significantly influence the observational features of the resulting transient. Matzner et al (2013) discussed SN 2011dh in the context of oblique shock breakout, and suggested that the resulting asphericity of the highest-velocity ejecta might explain why the early-time luminosity and radio emission indicated a compact progenitor (Arcavi et al 2011;Soderberg et al 2012), even though post-explosion images clearly showed that the SN stemmed from an extended YSG (Van Dyk et al 2013); the reason for the discrepancy lies in the unrealistic assumption of spherical symmetry. Interestingly, oblique shock breakout in SN 2011dh might also explain why the SN exhibited the strongest continuum polarization during the earliest stages, since the photosphere was in the outer envelope of the quasihomologous flow where velocities are highest.…”

Section: Oblique Shock Breakoutmentioning

confidence: 99%

“…Remarkably, a yellow supergiant (YSG) star was found to be spatially coincident with the SN in HST archival images of the galaxy Maund et al 2011;Van Dyk et al 2011). It was unclear whether this star was the actual progenitor of the explosion, a neighbor, or even a surviving companion star to a more compact progenitor as initially hypothesized on the basis of its early-time luminosity (Arcavi et al 2011) and radio emission (Soderberg et al 2012). Eventually, the identification of the YSG as the true progenitor was solidified after the SN had faded, revealing that the YSG star had disappeared (Van Dyk et al 2013).…”

Section: Introductionmentioning

confidence: 98%

Spectropolarimetry of SN 2011dh in M51: geometric insights on a Type IIb supernova progenitor and explosion

Mauerhan

Williams

Leonard

et al. 2015

Monthly Notices of the Royal Astronomical Society

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Abstract We present seven epochs of spectropolarimetry of the Type IIb supernova (SN IIb) 2011dh in M51, spanning 86 d of its evolution. The first epoch was obtained 9 d after the explosion, when the photosphere was still in the depleted hydrogen layer of the stripped-envelope progenitor. Continuum polarization is securely detected at the level of P ≈ 0.5 per cent through day 14 and appears to diminish by day 30, which is different from the prevailing trends suggested by studies of other core-collapse SNe. Time-variable modulations in P and position angle are detected across P-Cygni line features. H α and He i polarization peak after 30 d and exhibit position angles roughly aligned with the earlier continuum, while O i and Ca ii appear to be geometrically distinct. We discuss several possibilities to explain the evolution of the continuum and line polarization, including the potential effects of a tidally deformed progenitor star, aspherical radioactive heating by fast-rising plumes of 56Ni from the core, oblique shock breakout, or scattering by circumstellar material. While these possibilities are plausible and guided by theoretical expectations, they are not unique solutions to the data. The construction of more detailed hydrodynamic and radiative-transfer models that incorporate complex aspherical geometries will be required to further elucidate the nature of the polarized radiation from SN 2011dh and other SNe IIb.

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Observational and Physical Classification of Supernovae

Gal‐Yam¹

2016

Handbook of Supernovae

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This chapter describes the current classification scheme of supernovae (SNe). This scheme has evolved over many decades and now includes numerous SN Types and sub-types. Many of these are universally recognized, while there are controversies regarding the definitions, membership and even the names of some sub-classes; we will try to review here the commonly-used nomenclature, noting the main variants when possible. SN Types are defined according to observational properties; mostly visible-light spectra near maximum light, as well as according to their photometric properties. However, a long-term goal of SN classification is to associate observationally-defined classes with specific physical explosive phenomena. We show here that this aspiration is now finally coming to fruition, and we establish the SN classification scheme upon direct observational evidence connecting SN groups with specific progenitor stars. Observationally, the broad class of Type II SNe contains objects showing strong spectroscopic signatures of hydrogen, while objects lacking such signatures are of Type I, which is further divided to numerous subclasses. Recently a class of super-luminous SNe (SLSNe, typically 10 times more luminous than standard events) has been identified, and it is discussed. We end this chapter by briefly describing a proposed alternative classification scheme that is inspired by the stellar classification system. This system presents our emerging physical understanding of SN explosions, while clearly separating robust observational properties from physical inferences that can be debated. This new system is quantitative, and naturally deals with events distributed along a continuum, rather than being strictly divided into discrete classes. Thus, it may be more suitable to the coming era where SN numbers will quickly expand from a few thousands to millions of events.Comment: Extended final draft of a chapter in the "SN Handbook". Comments most welcom

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PANCHROMATIC OBSERVATIONS OF SN 2011dh POINT TO A COMPACT PROGENITOR STAR

Abstract: We report the discovery and detailed monitoring of X-ray emission associated with the Type IIb SN 2011dh using data from the Swift and Chandra satellites,

Cited by 111 publications

References 53 publications

Optical and near-infrared observations of SN 2011dh – The first 100 days

Optical and near-infrared observations of SN 2011dh – The first 100 days

Spectropolarimetry of SN 2011dh in M51: geometric insights on a Type IIb supernova progenitor and explosion

Observational and Physical Classification of Supernovae

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