Early-Time
                    <i>Spitzer</i>
                    Observations of the Type II Plateau Supernova SN 2004dj

Kotak, R.; Meikle, P.; Dyk, Schuyler D. Van; Höflich, Peter; Mattila, S.

doi:10.1086/432719

Cited by 62 publications

(85 citation statements)

References 20 publications

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“…They show features and evolution very similar to the available MIR spectra of a few SNe, including SN 1987A (Wooden et al 1993;Roche et al 1993 Table 4). presented and discussed by Kotak et al (2005). We include these spectra in the present study for completeness, but the conclusions for them are generally the same as those of Kotak et al (2005).…”

Section: Spectral Features and Evolutionmentioning

confidence: 88%

“…The errors represent the standard deviation of the data from the three different photometry methods. Kotak et al (2005) presented some MIR photometric points observed at ∼100 days after explosion. Their reported flux values are generally consistent with ours, but there are some differences (mainly in channels 4.5 and 24 μm).…”

Section: Mir Photometry With Spitzermentioning

confidence: 99%

“…The earliest observations have been presented by Kotak et al (2005). In the following sections we analyze the Spitzer and Hubble observations that show signs of dust formation (Sects.…”

Section: Introductionmentioning

confidence: 99%

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Dust formation in the ejecta of the type II-P supernova 2004dj

Szalai

Vinkó

Balog

et al. 2011

A&A

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Aims. Core-collapse supernovae (CC SNe), especially type II-Plateau ones, are thought to be important contributors to cosmic dust production. SN 2004dj, one of the closest and brightest SN since 1987A, offered a good opportunity to examine dust-formation processes. To find signs of newly formed dust, we analyze all available mid-infrared (MIR) archival data from the Spitzer space telescope. Methods. We re-reduced and analyzed data from IRAC, MIPS, and IRS instruments obtained between +98 and +1381 days after explosion and generated light curves and spectra for each epoch. Observed spectral energy distributions are fitted with both analytic and numerical models, using the radiative-transfer code MOCASSIN for the latter ones. We also use imaging polarimetric data obtained at +425 days by the Hubble space telescope.Results. We present convincing evidence of dust formation in the ejecta of SN 2004dj from MIR light curves and spectra. Significant MIR excess flux is detected in all bands between 3.6 and 24 μm. In the optical, a ∼0.8% polarization is also detected at a 2-sigma level, which exceeds the interstellar polarization in that direction. Our analysis shows that the freshly-formed dust around SN 2004dj can be modeled assuming a nearly spherical shell that contains amorphous carbon grains, which cool from ∼700 K to ∼400 K between +267 and +1246 days. Persistent excess flux is found above 10 μm, which is explained by a cold (∼115 K) dust component. If this cold dust is of circumstellar origin, it is likely to be condensed in a cool, dense shell between the forward and reverse shocks. Pre-existing circumstellar dust is less likely, but cannot be ruled out. An upper limit of ∼8 × 10 −4 M is derived for the dust mass, which is similar to previously published values for other dust-producing SNe.

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Section: Spectral Features and Evolutionmentioning

confidence: 88%

Section: Mir Photometry With Spitzermentioning

confidence: 99%

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Dust formation in the ejecta of the type II-P supernova 2004dj

Szalai

Vinkó

Balog

et al. 2011

A&A

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“…In Fig. 16 we compare our K-band spectrum of SN 2007gr at day +137.7 to those of SN 1987A (Meikle et al 1989) and the type IIP SN 2004dj (Kotak et al 2005). The spectra have been scaled so that the initial slopes of the CO emissions near 2.24 μm are relatively well matched.…”

Section: Carbon Monoxide Emissionmentioning

confidence: 99%

Extensive optical and near-infrared observations of the nearby, narrow-lined type Ic SN 2007gr: days 5 to 415

Hunter

Valenti

Kotak

et al. 2009

A&A

118

100

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We present photometric and spectroscopic observations at optical and near-infrared wavelengths of the nearby type Ic supernova 2007gr. These represent the most extensive data-set to date of any supernova of this sub-type, with frequent coverage from shortly after discovery to more than one year post-explosion. We deduce a rise time to B-band maximum of 11.5 ± 2.7 d. We find a peak B-band magnitude of M B = −16.8, and light curves which are remarkably similar to the so-called "hypernova" SN 2002ap. In contrast, the spectra of SNe 2007gr and 2002ap show marked differences, not least in their respective expansion velocities. We attribute these differences primarily to the density profiles of their progenitor stars at the time of explosion i.e. a more compact star for SN 2007gr compared to SN 2002ap. From the quasi-bolometric light curve of SN 2007gr, we estimate that 0.076 ± 0.010 M of 56 Ni was produced in the explosion. Our near-infrared (IR) spectra clearly show the onset and disappearance of the first overtone of carbon monoxide (CO) between ∼70 to 175 d relative to B-band maximum. The detection of the CO molecule implies that ionised He was not microscopically mixed within the carbon/oxygen layers. From the optical spectra, near-IR light curves, and colour evolution, we find no evidence for dust condensation in the ejecta out to about +400 d. Given the combination of unprecedented temporal coverage, and high signal-to-noise data, we suggest that SN 2007gr could be used as a template object for supernovae of this sub-class.

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“…Type II supernovae (SNe) are strong contenders as dust factories at high-redshift because of the short evolution time-scale of their massive stellar progenitors (∼10 6 yrs). Furthermore, dust and molecules (namely carbon monoxide, CO, and silicon monoxide, SiO) have been detected at infrared (IR) wavelengths in several local SNe, including SN1987A in the Large Magellanic Cloud, a few hundreds of days after the explosion (Lucy et al 1989;Danziger et al 1991;Kotak et al 2005Kotak et al , 2006Kotak et al , 2009Gallagher et al 2012;Mauerhan et al 2012;Szalai & Vinkó 2013). The dust mass derived is small and ranges between 10 −5 M and 10 −2 M .…”

Section: Introductionmentioning

confidence: 99%

Molecules and dust in Cassiopeia A

Biscaro

Cherchneff

2014

A&A

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Aims. We study the chemistry of the type IIb supernova ejecta, which led to the Cas A supernova remnant, to assess the chemical type and quantity of dust that forms and evolves in the remnant phase. We later model a dense oxygen-rich ejecta knot, which is crossed by the reverse shock in Cas A, to study the evolution of the clump gas phase and the possibility to reform dust clusters in the post-reverse shock gas. Methods. The chemistry is described by a chemical network that includes all possible processes that are efficient at high gas temperatures and densities. The formation of key bimolecular species (e.g., CO and SiO) and dust clusters of silicates, alumina, silica, metal carbides and sulphides, pure metals, and amorphous carbon is considered. A set of stiff, coupled ordinary differential equations is solved for the conditions pertaining to both the SN ejecta and the post-reverse shock gas. Results. We find that the ejecta of type IIb SNe are unable to form large amounts of molecules and molecular clusters that are precursors to dust grains, when compared to their type II-P counterparts, because of their diffuse ejecta. The ejecta gas density needs to be increased by several orders of magnitude to allow for the formation of dust clusters. We show that the chemical composition of the dust clusters that form changes drastically and gains in chemical complexity with increasing gas density. Hence, the ejecta of the Cas A supernova progenitor must have been in the form of dense clumps to account for the dust chemical composition and masses that have been inferred from infrared observations of Cas A. As for the impact of the reverse shock on dense ejecta clumps, we show that the ejecta molecules that are destroyed by the shock reform in the post-reverse shock gas with lower abundances than those of the initial ejecta clump, except for SiO. These molecules include CO, SiS, and O 2 . On the other hand, dust clusters are destroyed by the reverse shock and do not reform in the post-reverse shock gas, even for the highest gas density. These results indicate that the synthesis of dust grains out of the gas phase in the dense knots of Cas A and in other supernova remnants is unlikely.

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Early-Time Spitzer Observations of the Type II Plateau Supernova SN 2004dj

Cited by 62 publications

References 20 publications

Dust formation in the ejecta of the type II-P supernova 2004dj

Dust formation in the ejecta of the type II-P supernova 2004dj

Extensive optical and near-infrared observations of the nearby, narrow-lined type Ic SN 2007gr: days 5 to 415

Molecules and dust in Cassiopeia A

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