NEAR-INFRARED PHOTOMETRY OF THE TYPE IIn SN 2005ip: THE CASE FOR DUST CONDENSATION

Fox, O.; Skrutskie, Michael F.; Chevalier, Roger A.; Kanneganti, Srikrishna; Park, Chan; Wilson, John C.; Nelson, Matthew J.; Amirhadji, Jason; Crump, Danielle; Hoeft, Alexi; Provence, Sydney; Sargeant, Benjamin; Sop, Joel; Tea, M.; Thomas, S.A.; Woolard, Kyle

doi:10.1088/0004-637x/691/1/650

Cited by 82 publications

(115 citation statements)

References 42 publications

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“…Note that dust formation in a cool dense shell has been proposed for some interacting SNe (e.g., Pozzo et al 2004;Smith et al 2008Smith et al , 2009Mattila et al 2008;Fox et al 2009;Chugai 2009). The cool dense shell may be formed at the reverse-shocked region, and thus, the dust can be heated by the UV/X-ray radiation.…”

Section: Sn Dustmentioning

confidence: 91%

A Search for Infrared Emission From Core-Collapse Supernovae at the Transitional Phase

Tanaka¹,

Nozawa²,

Sakon³

et al. 2012

ApJ

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Most of the observational studies of supernova (SN) explosions are limited to early phases (100 yr) in our Galaxy or very nearby galaxies. SNe at the epoch between these two, which we call the "transitional" phase, have not been explored in detail except for several extragalactic SNe including SN 1987A in the Large Magellanic Cloud. We present theoretical predictions for the infrared (IR) dust emissions by several mechanisms; emission from dust formed in the SN ejecta, light echo by circumstellar (CS) and interstellar (IS) dust, and emission from shocked CS dust. We search for IR emission from six core-collapse SNe at the transitional phase in the nearby galaxies NGC 1313, NGC 6946, and M101 by using the data taken with the AKARI satellite and Spitzer. Among six targets, we detect the emission from SN 1978K in NGC 1313. SN 1978K is associated with 1.3 × 10 −3 M of silicate dust. We show that, among several mechanisms, the shocked CS dust is the most probable emission source to explain the IR emission observed for SN 1978K. IR emission from the other five objects is not detected. Our current observations are sensitive to IR luminosity of >10 38 erg s −1 , and the non-detection of SN 1962M excludes the existence of the shocked CS dust for a high gas mass-loss rate of ∼10 −4 M yr −1 . Observations of SNe at the transitional phase with future IR satellites will fill the gap of IR observations of SNe with the age of 10-100 yr, and give a new opportunity to study the CS and IS environments of the progenitor, and possibly dust formation in SNe.

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Section: Sn Dustmentioning

confidence: 91%

A Search for Infrared Emission From Core-Collapse Supernovae at the Transitional Phase

Tanaka¹,

Nozawa²,

Sakon³

et al. 2012

ApJ

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“…As it was found in some CC SNe (e.g. SN 1998S, Pozzo et al 2004;SN 2005ip, Smith et al 2009and Fox et al 2009;SN 2006jc, Smith et al 2008aSN 2006tf, Smith et al 2008bSN 2007od, Andrews et al 2010, dust grains may condense in a cool dense shell (CDS) that is generated between the forward and reverse shock waves during the interaction of the SN ejecta and the preexisting circumstellar medium (CSM). The CDS may affect both the light curves and the spectral line profiles.…”

Section: Introductionmentioning

confidence: 92%

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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“…Given the maximum velocity of the ejecta of 10000 km s −1 , this constrains the distance of the inner radius of the CSM responsible for these profile peaks to Smith et al 2009, andFox et al 2009). The inner ±1500 km s −1 components may come from the forward shock created when the SN ejecta plowed into a central CSM ring, and the outer −5000 km s −1 components from the ejecta interacting with a blob of CSM out of the plane of the central ring.…”

Section: Spectral Evolutionmentioning

confidence: 99%

SN 2007od: A TYPE IIP SUPERNOVA WITH CIRCUMSTELLAR INTERACTION

Andrews

Gallagher

Clayton

et al. 2010

ApJ

136

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SN 2007od exhibits characteristics that have rarely been seen in a Type IIP supernova (SN). Optical V-band photometry reveals a very steep brightness decline between the plateau and nebular phases of ∼4.5 mag, likely due to SN 2007od containing a low mass of 56 Ni. The optical spectra show an evolution from normal Type IIP with broad Hα emission, to a complex, four-component Hα emission profile exhibiting asymmetries caused by dust extinction after day 232. This is similar to the spectral evolution of the Type IIn SN 1998S, although no early-time narrow (∼200 km s −1 ) Hα component was present in SN 2007od. In both SNe, the intermediate-width Hα emission components are thought to arise in the interaction between the ejecta and its circumstellar medium (CSM). SN 2007od also shows a mid-infrared excess due to new dust. The evolution of the Hα profile and the presence of the mid-IR excess provide strong evidence that SN 2007od formed new dust before day 232. Late-time observations reveal a flattening of the visible light curve. This flattening is a strong indication of the presence of a light echo, which likely accounts for much of the broad, underlying Hα component seen at late times. We believe that the multi-peaked Hα emission is consistent with the interaction of the ejecta with a circumstellar ring or torus (for the inner components at ±1500 km s −1 ) and a single blob or cloud of circumstellar material out of the plane of the CSM ring (for the outer component at −5000 km s −1 ). The most probable location for the formation of new dust is in the cool dense shell created by the interaction between the expanding ejecta and its CSM. Monte Carlo radiative transfer modeling of the dust emission from SN 2007od implies that up to ∼4 × 10 −4 M of new dust has formed. This is similar to the amounts of dust formed in other core-collapse supernovae such as SNe 1999em, 2004et, and 2006jc.

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NEAR-INFRARED PHOTOMETRY OF THE TYPE IIn SN 2005ip: THE CASE FOR DUST CONDENSATION

Cited by 82 publications

References 42 publications

A Search for Infrared Emission From Core-Collapse Supernovae at the Transitional Phase

A Search for Infrared Emission From Core-Collapse Supernovae at the Transitional Phase

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

SN 2007od: A TYPE IIP SUPERNOVA WITH CIRCUMSTELLAR INTERACTION

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