SN 2008S: an electron-capture SN from a super-AGB progenitor?

Botticella, M. T.; Pastorello, A.; Smartt, S. J.; Meikle, W. P. S.; Benetti, S.; Kotak, R.; Cappellaro, E.; Crockett, R. M.; Mattila, S.; Sereno, Mauro; Patat, F.; Tsvetkov, D. Yu.; Loon, Jacco Th. van; Abraham, Dulcy M.; Agnoletto, I.; Arbour, R.; Benn, Chris; Rico, G. Di; Elias‐Rosa, N.; Gorshanov, D. L.; Harutyunyan, A.; Hunter, David J.; Lorenzi, V.; Keenan, F. P.; Maguire, K.; Méndez, J.; Mobberley, Martin; Navasardyan, H.; Ries, C.; Stanishev, V.; Taubenberger, S.; Trundle, C.; Turatto, M.; Volkov, I. M.

doi:10.1111/j.1365-2966.2009.15082.x

Cited by 162 publications

(197 citation statements)

References 117 publications

(254 reference statements)

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“…This luminosity is comparable to that of an evolved ∼10 M star and is well below that corresponding to the more massive stars thought to be required for non-supernova eruptions. Subsequent analyses of the progenitor by Botticella et al (2009) and Wesson et al (2010) were consistent with those by Prieto et al (2008).…”

Section: Introductionmentioning

confidence: 54%

“…The photometry was obtained using DAOPHOT and ALLSTAR (Stetson 1987(Stetson , 1992. The optical data were calibrated using 4-24 local standards from Welch et al (2007) for the V and R bands and from Botticella et al (2009) for the U and B bands. The near-IR LBT data were calibrated using 3-6 Two Micron All Sky Survey stars in the field.…”

Section: Observations and Resultsmentioning

confidence: 99%

“…Debates about these possible origins have been raging ever since then, based on both theoretical and observational arguments. They are basically divided into the (some kind of) supernova camp Botticella et al 2009;Pumo et al 2009) and the (some kind of) massive star outburst camp (Berger et al 2009;Smith et al 2009;Bond et al 2009;Kashi et al 2010;Humphreys et al 2011). Berger et al (2009 and Smith et al (2009) favor relatively massive stars similar to the upper bounds found by Gogarten et al (2009).…”

Section: Introductionmentioning

confidence: 99%

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Dust to Dust: Three Years in the Evolution of the Unusual Sn 2008s

Szczygiel

Prieto²,

Kochanek

et al. 2012

ApJ

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We obtained late-time optical and near-IR imaging of SN 2008S with the Large Binocular Telescope, near-IR data with the Hubble Space Telescope, and mid-IR data with the Spitzer Space Telescope. We find that (1) it is again invisible at optical (UBVR) wavelengths to magnitude limits of approximately 25 mag, (2) while detected in the near-IR (H) at approximately 24.8 mag, it is fading rapidly, and (3) it is still brighter than the progenitor at 3.6 and 4.5 μm in the mid-IR with a slow, steady decline. The IR detections in 2010 December are consistent with dust emission at a blackbody temperature of T 640 K and a total luminosity of L 200,000 L , much higher than the L 40,000 L luminosity of the obscured progenitor star. The local environment also shows no evidence for stars significantly more massive than 10 M , consistent with the progenitor being an 8-10 M super asymptotic giant branch star.

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Section: Introductionmentioning

confidence: 54%

Section: Observations and Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Dust to Dust: Three Years in the Evolution of the Unusual Sn 2008s

Szczygiel

Prieto²,

Kochanek

et al. 2012

ApJ

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“…It fully allows for the effects of light-travel time across the dust distribution. Versions of this model have also been used in Meikle et al (2007), Mattila et al (2008), Botticella et al (2009), and Kotak et al (2009). The model assumes a spherically symmetric cloud of grains centered on the SN, with a concentric dust-free cavity at the center.…”

Section: The Warm Component: Early-phase Ir Excess Due To a Cdsmentioning

confidence: 99%

DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004dj

Meikle¹,

Kotak²,

Farrah³

et al. 2011

ApJ

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We present mid-infrared (MIR) spectroscopy of a Type II-plateau supernova, SN 2004dj, obtained with the Spitzer Space Telescope, spanning 106-1393 days after explosion. MIR photometry plus optical/near-IR observations are also reported. An early-time MIR excess is attributed to emission from non-silicate dust formed within a cool dense shell (CDS). Most of the CDS dust condensed between 50 days and 165 days, reaching a mass of 0.3 × 10 −5 M . Throughout the observations, much of the longer wavelength (>10 μm) part of the continuum is explained as an IR echo from interstellar dust. The MIR excess strengthened at later times. We show that this was due to thermal emission from warm, non-silicate dust formed in the ejecta. Using optical/near-IR line profiles and the MIR continua, we show that the dust was distributed as a disk whose radius appeared to be shrinking slowly. The disk radius may correspond to a grain destruction zone caused by a reverse shock which also heated the dust. The dust-disk lay nearly face-on, had high opacities in the optical/near-IR regions, but remained optically thin in the MIR over much of the period studied. Assuming a uniform dust density, the ejecta dust mass by 996 days was (0.5 ± 0.1) × 10 −4 M and exceeded 10 −4 M by 1393 days. For a dust density rising toward the center the limit is higher. Nevertheless, this study suggests that the amount of freshly synthesized dust in the SN 2004dj ejecta is consistent with that found from previous studies and adds further weight to the claim that such events could not have been major contributors to the cosmic dust budget.

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“…At the moment the only certain test to distinguish stellar eruptions from genuine CC SN explosions is to observe the outcome of the transient event: the surviving progenitor star in the case of eruptive event or a compact SN remnant in the case of CC SN explosion (Chevalier 2005). We also need to understand the diversity of these transients that may reflect different eruption or explosion mechanisms (luminous red novae, stellar mergers in low mass systems, erupting OH/IR stars, weak EC SNe from super-AGB stars) (Kulkarni et al 2007;Prieto et al 2008;Botticella et al 2009;Kochanek 2011).…”

Section: What Is the Nature Of Sn Impostors?mentioning

confidence: 99%

Supernovae and Gaia

Altavilla

Botticella²,

Turatto³

2012

Astrophys Space Sci

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Despite decades of dedicated efforts there are still basic questions to answer with regard to Supernova progenitor systems and explosion mechanisms. In particular, in the last years a number of exceptionally bright objects and extremely faint events have demonstrated an unexpected large Supernova variety.The large number of Supernovae candidates at different redshifts provided by the next generation surveys, from ground and space, will allow to reach a better insight of the Supernova events in all their flavours. In particular it will be the possible to assess the systematics of type Ia Supernovae as distance indicator at any redshift.The Gaia astrometric mission is expected to discover a huge number of transient events, including Supernovae, which will be immediately disseminated to the astronomical community by a transients alert system for a suitable follow up.

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SN 2008S: an electron-capture SN from a super-AGB progenitor?

Cited by 162 publications

References 117 publications

Dust to Dust: Three Years in the Evolution of the Unusual Sn 2008s

Dust to Dust: Three Years in the Evolution of the Unusual Sn 2008s

DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004dj

Supernovae and Gaia

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