<i>Spitzer</i>
                    Measurements of Atomic and Molecular Abundances in the Type IIP SN 2005af

Kotak, R.; Meikle, P.; Pozzo, Monica; Dyk, Schuyler D. Van; Farrah, D.; Fesen, Robert A.; Filippenko, A. V.; Foley, R. J.; Fransson, Claes; Gerardy, Christopher L.; Höflich, Peter; Lundqvist, Peter; Mattila, S.; Sollerman, J.; Wheeler, J. C.

doi:10.1086/509655

Cited by 74 publications

(83 citation statements)

References 22 publications

(33 reference statements)

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“…The derived ionization fractions are shown in the last column of Table 5. These values are very close to those obtained by Wooden et al (1993) for SN 1987A, but significantly higher than the results by Kotak et al (2006). It is probable that Kotak et al overestimated the contribution of [Ni i] to the 7.51 μm feature, and therefore underestimated the ionization fraction for Ni.…”

Section: Masses Of Ni and Cosupporting

confidence: 80%

“…It is important that the 7.51 μm line in the IRS spectra is an unresolved blend of [Ni i] with Paα, Huβ and H i 7-11, which makes the direct measurement of the [Ni i] feature difficult. This was already noted by Kotak et al (2005), but in a subsequent paper Kotak et al (2006) measured the flux of this line directly and derived the ionization fraction x = Ni + /(Ni 0 + Ni + ) ∼ 0.4 for SN 2004dj at +261 days. This is roughly a factor of 2 lower than what was measured in SN 1987A at that epoch (x ∼ 0.8, Wooden et al 1993).…”

Section: Masses Of Ni and Cosupporting

confidence: 55%

“…The spectra consist of permitted emission lines of H i (Pfund-, Humphrey-and n = 7 series), and forbidden lines of Table 3 summarizes the identified lines, based on Wooden et al (1993) and Kotak et al (2005). The presence of [Ne ii], forming a blend with [Ni ii] at 12.8 μm, was suggested by Kotak et al (2006) for SN 2005af. This feature is also present in SN 2004dj for all phases covered by IRS-observations, although the two components cannot be resolved.…”

Section: Spectral Features and Evolutionmentioning

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: Masses Of Ni and Cosupporting

confidence: 80%

Section: Masses Of Ni and Cosupporting

confidence: 55%

Section: Spectral Features and Evolutionmentioning

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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“…To check the reliability of our reduction technique we also reduced these data and found a good agreement with the results of Kotak et al (2006) and Kotak (2008). We also completed this dataset with the fluxes determined from the latest measurements found in the Spitzer database.…”

Section: Mid-infrared Photometry With Spitzersupporting

confidence: 72%

Twelve type II-P supernovae seen with the eyes ofSpitzer

Szalai

Vinkó

2012

A&A

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Context. Core-collapse supernovae (CC SNe), especially those of type II-plateau (II-P), are thought to be important contributors to cosmic dust production. The most obvious indicator of newly-formed and/or pre-existing dust is the time-dependent mid-infrared (MIR) excess coming from the environment of SNe. In the past few years several CC SNe were monitored by the Spitzer Space Telescope in the nebular phase, hundreds of days after explosion. On the other hand, only a few of these objects have been analyzed and published to date. Aims. Our goal was to collect publicly available, previously unpublished measurements on type II-P (or peculiar IIP) SNe from the Spitzer database. The most important aspect was to find SNe observed with the Infrared Array Camera (IRAC) on at least two epochs. The temporal changes of the observed fluxes may be indicative of the underlying supernova, while spectral energy distribution (SED) fitting to the fluxes in different IRAC channels may reveal the physical parameters of the mid-IR radiation, which is presumably caused by warm dust. Methods. The IRS spectra were extracted and calibrated with SPICE, while photometric SEDs were assembled using IRAF and MOPEX. Calculated SEDs from observed fluxes were fit with simple dust models to obtain basic information on the dust presumed as the source of MIR radiation. Results. We found twelve SNe that satisfied the criterion above, observed at late-time epochs (typically after +300 days). In three cases we could not identify any point source at the SN position on late-time IRAC images. We found two SNe, 2005ad and 2005af, which likely have newly formed dust in their environment, while in the other seven cases the observed MIR flux may originate from pre-existing circumstellar or interstellar dust. Our results support the previous observational conclusions that warm new dust in the environment of SNe contributes only marginally to the cosmic dust content.

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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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Spitzer Measurements of Atomic and Molecular Abundances in the Type IIP SN 2005af

Cited by 74 publications

References 22 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

Twelve type II-P supernovae seen with the eyes ofSpitzer

Molecules and dust in Cassiopeia A

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