DISENTANGLING THE ORIGIN AND HEATING MECHANISM OF SUPERNOVA DUST: LATE-TIME<i>SPITZER</i>SPECTROSCOPY OF THE TYPE IIn SN 2005ip

Fox, O.; Chevalier, Roger A.; Dwek, Eli; Skrutskie, Michael F.; Sugerman, Ben; Leisenring, Jarron

doi:10.1088/0004-637x/725/2/1768

Cited by 95 publications

(204 citation statements)

References 54 publications

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“…One is an extreme red supergiant, as suggested by Smith et al (2009), because the inferred clumpy medium in the CSM is similar to small scale clumps found in the red hypergiant star VY Canis Majoris. The other suggestion is an LBV star owing to a high mass-loss rate, which is similar to what has been observed in other LBVs (Fox et al 2010;Katsuda et al 2014 There is evidence pointing to dust forming in a cool dense shell (CDS) behind the forward shock passing through the dense CSM as early as 50-100 days past explosion in some SNe, such as SN 1998S, SN 2006jd, or SN 2010jl (Pozzo et al 2004Stritzinger et al 2012;Gall et al 2014). Indeed, SN 2005ip shows signs of such early dust formation, as inferred from the attenuation of the red wing of the Hα line and the observed drop in the light curves of the optical bands (Stritzinger et al 2012).…”

Section: Introductionsupporting

confidence: 86%

Early gray dust formation in the type IIn SN 2005ip

Nielsen

Hjorth

Gall

2018

A&A

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The physical characteristics of dust formed in supernovae is poorly known. In this paper, we investigate the extinction properties of dust formed in the type IIn SN 2005ip. The observed light curves of SN 2005ip all exhibit a sudden drop around 50 days after discovery. This has been attributed to dust formation in the dense circumstellar medium. We modeled the intrinsic light curves in six optical bands, adopting a theoretical model for the luminosity evolution of supernovae interacting with their circumstellar material. From the difference between the observed and intrinsic light curves, we calculated extinction curves as a function of time. The totalto-selective extinction ratio, R V , was determined from the extinction in the B and V bands. The resulting extinction, A V , increases monotonically up to about 1 mag, 150 days after discovery. The inferred R V value also increases slightly with time, but appears constant in the range 4.5-8, beyond 100 days after discovery. The analysis confirms that dust is likely formed in SN 2005ip, starting about two months after explosion. The high value of R V , that is, gray dust, suggests dust properties different from of the Milky Way. While this result hinges on the assumed theoretical intrinsic light curve evolution, it is encouraging that the fitted light curves are as expected for standard ejecta and circumstellar medium density structures.

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Section: Introductionsupporting

confidence: 86%

Early gray dust formation in the type IIn SN 2005ip

Nielsen

Hjorth

Gall

2018

A&A

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“…Kotak et al 2009;Fox et al 2010;Otsuka et al 2010;Szalai et al 2011;Meikle et al 2011). Observations in X-ray and radio may also provide useful additional information about SN-CSM interactions.…”

Section: Discussionmentioning

confidence: 99%

“…This pre-existing matter also contains dust grains and may also permit grain condensation interacting with the forward shock (see more details e.g. in Fox et al 2010Fox et al , 2011.…”

Section: Introductionmentioning

confidence: 99%

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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“…The dust, however, may be either newly formed or pre-existing, and heating may be collisional or radiative (see Fox et al 2010 for a full discussion). To constrain the origin and heating mechanism, we first calculate the size of the dust shell.…”

Section: The Source Of the Mid-ir Emissionmentioning

confidence: 99%

AN EXCESS OF MID-INFRARED EMISSION FROM THE TYPE Iax SN 2014dt

Fox

Johansson

Kasliwal

et al. 2015

ApJL

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Supernovae Type Iax (SNe Iax) are less energetic and less luminous than typical thermonuclear explosions. A suggested explanation for the observed characteristics of this subclass is a binary progenitor system consisting of a CO white dwarf primary accreting from a helium star companion. A single-degenerate explosion channel might be expected to result in a dense circumstellar medium (CSM), although no evidence for such a CSM has yet been observed for this subclass. Here we present recent Spitzerobservations of the SN Iax 2014dt obtained by the SPIRITS program nearly one year post-explosion that reveal a strong mid-IR excess over the expected fluxes of more normal SNe Ia. This excess is consistent with 10 −5 M  of newly formed dust, which would be the first time that newly formed dust has been observed to form in a Type Ia. The excess, however, is also consistent with a dusty CSM that was likely formed in pre-explosion mass-loss, thereby suggesting a single degenerate progenitor system. Compared to other SNe Ia that show significant shock interaction (SNe Ia-CSM) and interacting corecollapse events (SNe IIn), this dust shell in SN 2014dt is less massive. We consider the implications that such a pre-existing dust shell has for the progenitor system, including a binary system with a mass donor that is a red giant, a red supergiant, or an asymptotic giant branch star.

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DISENTANGLING THE ORIGIN AND HEATING MECHANISM OF SUPERNOVA DUST: LATE-TIMESPITZERSPECTROSCOPY OF THE TYPE IIn SN 2005ip

Cited by 95 publications

References 54 publications

Early gray dust formation in the type IIn SN 2005ip

Early gray dust formation in the type IIn SN 2005ip

Twelve type II-P supernovae seen with the eyes ofSpitzer

AN EXCESS OF MID-INFRARED EMISSION FROM THE TYPE Iax SN 2014dt

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