Type IIP supernova SN 2004et: a multiwavelength study in X-ray, optical and radio

Misra, Kuntal; Pooley, D.; Chandra, Poonam; Bhattacharya, Dipankar; Ray, Alak; Sagar, Ram; Lewin, W. H. G.

doi:10.1111/j.1365-2966.2007.12258.x

Cited by 66 publications

(77 citation statements)

References 36 publications

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“…They found that a star with an A less massive progenitor is expected if we use the wind density recovered for the SN 2004et pre-SN from X-ray observations. These data suggest the mass-loss rate of (2−2.5) × 10 −6 M yr −1 , assuming the wind velocity of 10 km s −1 (Rho et al 2007;Misra et al 2007). Using the RSG life-time of 7 × 10 5 yr for the 25 M main-sequence star (Hirshi et al 2004), we find the mass lost at the RSG phase to be ∼1.6 M with an uncertainty of ∼ ± 1 M .…”

Section: Progenitor Massmentioning

confidence: 96%

High mass of the type IIP supernova 2004et inferred from hydrodynamic modeling

Utrobin

Чугай

2009

A&A

110

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Context. Previous studies of type IIP supernovae have inferred that progenitor masses recovered from hydrodynamic models are higher than 15 M . Aims. To verify the progenitor mass of this supernova category, we attempt a parameter determination of the well-observed luminous type IIP supernova 2004et. Methods. We model the bolometric light curve and the photospheric velocities of SN 2004et by means of hydrodynamic simulations in an extended parameter space. Results. From hydrodynamic simulations and observational data, we infer a presupernova radius of 1500 ± 140 R , an ejecta mass of 24.5 ± 1 M , an explosion energy of (2.3 ± 0.3) × 10 51 erg, and a radioactive 56 Ni mass of 0.068 ± 0.009 M . The estimated progenitor mass on the main sequence is in the range of 25−29 M . In addition, we find clear signatures of the explosion asymmetry in the nebular spectra of SN 2004et. Conclusions. The measured progenitor mass of SN 2004et is significantly higher than the progenitor mass suggested by the preexplosion images. We speculate that the mass inferred from hydrodynamic modeling is overestimated and crucial missing factors are multi-dimensional effects.

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Section: Progenitor Massmentioning

confidence: 96%

High mass of the type IIP supernova 2004et inferred from hydrodynamic modeling

Utrobin

Чугай

2009

A&A

110

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“…Photometric and spectroscopic monitoring programs began in earnest soon thereafter. Results from optical monitoring are summarized by Sahu et al (2006) and Misra et al (2007).…”

Section: Sn 2004etmentioning

confidence: 99%

“…To explore this proposition further, we make use of the MIR photometry (see Table 1) and spectra (Figure 3), together with optical photometry (Sahu et al 2006;Misra et al 2007) and spectra (Sahu et al 2006).…”

Section: Evidence For Dustmentioning

confidence: 99%

DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004et

Kotak

Meikle

Farrah

et al. 2009

ApJ

187

290

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We present mid-infrared (MIR) observations of the Type II-plateau supernova (SN) 2004et, obtained with the Spitzer Space Telescope between 64 and 1406 days past explosion. Late-time optical spectra are also presented. For the period 300-795 days past explosion, we argue that the spectral energy distribution (SED) of SN 2004et comprises (1) a hot component due to emission from optically thick gas, as well as free-bound radiation; (2) a warm component due to newly formed, radioactively heated dust in the ejecta; and (3) a cold component due to an IR echo from the interstellar-medium dust of the host galaxy, NGC 6946. There may also have been a small contribution to the IR SED due to free-free emission from ionized gas in the ejecta. We reveal the first-ever spectroscopic evidence for silicate dust formed in the ejecta of a supernova. This is supported by our detection of a large, but progressively declining, mass of SiO. However, we conclude that the mass of directly detected ejecta dust grew to no more than a few times 10 −4 M . We also provide evidence that the ejecta dust formed in comoving clumps of fixed size. We argue that, after about two years past explosion, the appearance of wide, box-shaped optical line profiles was due to the impact of the ejecta on the progenitor circumstellar medium and that the subsequent formation of a cool, dense shell was responsible for a later rise in the MIR flux. This study demonstrates the rich, multifaceted ways in which a typical core-collapse supernova and its progenitor can produce and/or interact with dust grains. The work presented here adds to the growing number of studies that do not support the contention that SNe are responsible for the large mass of observed dust in high-redshift galaxies.

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“…Spectroscopic observations of SN 1999ga. The spectrum at 39.5 days is the one used to classify SN 1999ga (Salvo et al 1999 (Gezari et al 2009;Miller et al 2009), the type IIL SNe 1979C (Balinskaya et al 1980;de Vaucouleurs et al 1981;Barbon et al 1982b), 1980K (Barbon et al 1982aButa 1982;Tsvetkov 1983), 1990K (Cappellaro et al 1995b), 1994aj (Benetti et al 1998; the transitional type IIP/IIL SN 1992H (Clocchiatti et al 1996); the peculiar SN 1987A (Whitelock et al 1989, and references therein) and the type IIP SNe 2004et (Sahu et al 2006;Misra et al 2007) and 2005cs (Tsvetkov et al 2006;Pastorello et al 2006Pastorello et al , 2009. The explosion epochs of SNe IIL have been estimated to occur roughly 2−3 weeks before their maximum light (Patat et al 1993).…”

Section: Late Spectral Evolutionmentioning

confidence: 99%

SN 1999ga: a low-luminosity linear type II supernova?

Pastorello

Crockett

Martin

et al. 2009

A&A

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Context. Type II-linear supernovae are thought to arise from progenitors that have lost most of their H envelope by the time of the explosion, and they are poorly understood because they are only occasionally discovered. It is possible that they are intrinsically rare, but selection effects due to their rapid luminosity evolution may also play an important role in limiting the number of detections. In this context, the discovery of a subluminous type II-linear event is even more interesting. Aims. We investigate the physical properties and characterise the explosion site of the type II SN 1999ga, which exploded in the nearby spiral galaxy NGC 2442. Methods. Spectroscopic and photometric observations of SN 1999ga allow us to constrain the energetics of the explosion and to estimate the mass of the ejected material, shedding light on the nature of the progenitor star in the final stages of its life. The study of the environment in the vicinity of the explosion site provides information on a possible relation between these unusual supernovae and the properties of the galaxies hosting them. Results. Despite the lack of early-time observations, we provide reasonable evidence that SN 1999ga was probably a type II-linear supernova that ejected a few solar masses of material, with a very small amount of radioactive elements of the order of 0.01 M .

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Type IIP supernova SN 2004et: a multiwavelength study in X-ray, optical and radio

Cited by 66 publications

References 36 publications

High mass of the type IIP supernova 2004et inferred from hydrodynamic modeling

High mass of the type IIP supernova 2004et inferred from hydrodynamic modeling

DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004et

SN 1999ga: a low-luminosity linear type II supernova?

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