MULTI-WAVELENGTH OBSERVATIONS OF THE ENDURING TYPE IIn SUPERNOVAE 2005ip AND 2006jd

Stritzinger, M. D.; Taddia, F.; Fransson, Claes; Fox, O.; Morrell, N.; Phillips, M. M.; Sollerman, J.; Anderson, J. P.; Boldt, Luis; Brown, P. J.; Campillay, A.; Castellón, S.; Contreras, C.; Folatelli, G.; Habergham, S. M.; Hamuy, M.; Hjorth, J.; James, P. A.; Krzemiński, W.; Mattila, S.; Persson, S. E.; Roth, M.

doi:10.1088/0004-637x/756/2/173

Cited by 173 publications

(272 citation statements)

References 80 publications

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“…For example, the X-ray luminosities of ∼10 37 erg s −1 in 0.1-10 keV at one year after the explosion is expected in our 10 −4 M yr −1 model with the formalism of Fransson et al (1996). SN IIn 2005ip, which had a similar optical luminosity to our ecSN model at the early plateau (Stritzinger et al 2012), had an X-ray luminosity of 10 41 erg s −1 in 0.1-10 keV at one year after the explosion (Katsuda et al 2014). Thus, optically bright but X-ray-faint SNe IIn can be promising candidates for ecSNe.…”

Section: Other Supernovaesupporting

confidence: 70%

Electron-capture supernovae exploding within their progenitor wind

Moriya

Tominaga

Langer

et al. 2014

A&A

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The most massive stars on the asymptotic giant branch (AGB), or the so-called super-AGB stars, are thought to produce supernovae triggered by electron captures in their degenerate O+Ne+Mg cores. Super-AGB stars are expected to have slow winds with high mass-loss rates, so their circumstellar density is high. The explosions of super-AGB stars are therefore presumed to occur in this dense circumstellar environment. We provide the first synthetic light curves for such events by exploding realistic electron-capture supernova progenitors within their super-AGB winds. We find that the early light curve -that is, before the recombination wave reaches the bottom of the hydrogen-rich envelope of supernova ejecta (the plateau phase) -is not affected by the dense wind. However, after the luminosity drop following the plateau phase, the luminosity remains much higher when the super-AGB wind is taken into account. We compare our results to the historical light curve of SN 1054, the progenitor of the Crab Nebula, and show that the explosion of an electron-capture supernova within an ordinary super-AGB wind can explain the observed light curve features. We conclude that SN 1054 could have been a Type IIn supernova without any extra extreme mass loss, which was previously suggested to be necessary to account for its early high luminosity. We also show that our light curves match Type IIn supernovae with an early plateau phase or the so-called Type IIn-P supernovae, and suggest that they are electron-capture supernovae within super-AGB winds. Although some electron-capture supernovae can be bright in the optical spectral range due to the large progenitor radius, their X-ray luminosity from the interaction does not necessarily get as bright as other Type IIn supernovae whose optical luminosities are also powered by the interaction. Thus, we suggest that optically bright X-ray-faint Type IIn supernovae can emerge from electron-capture supernovae. Optically faint Type IIn supernovae, such as SN 2008S, can also originate from electron-capture supernovae if their hydrogen-rich envelope masses are small. We argue that some of them can be observed as Type IIn-b supernovae due to the small hydrogen-rich envelope mass.

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Section: Other Supernovaesupporting

confidence: 70%

Electron-capture supernovae exploding within their progenitor wind

Moriya

Tominaga

Langer

et al. 2014

A&A

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“…Besides 7 typical SN II and Ia, the following four SNe had more precise classifications: SN 2000ft was discovered in NGC 7469 by using radio observations and showed similar evolution properties than other compact radio sources identified as SN II (Alberdi et al 2006); SN 2000cb showed similar photometric behaviour than SN 1987A, which are thought to be SN II resulting from the explosion of blue supergiants (Pastorello et al 2005;Taddia et al 2012); SN 1993R was typed as a peculiar SN similar to the subluminous SN Ia class 1991bg-like, but with stronger Ca II NIR triplet (Filippenko & Matheson 1993). Finally, SN 2005ip spectra showed that it was interacting with the surrounding circumstellar medium and it was typed as SN IIn (Stritzinger et al 2012).The programs that proposed the observations of these 5 galaxies, observation periods, exposure times, and seeing at the time of observations are summarized in Table 1. MUSE delivers an impressive set of ∼100,000 spectra per pointing covering most of the optical domain. For NGC 6754, the observations were divided in two pointings, one for each eastern and western part of the galaxy.…”

Section: Observationsmentioning

confidence: 99%

Characterizing the environments of supernovae with MUSE

Galbany

Anderson

Rosales-Ortega

et al. 2015

Mon. Not. R. Astron. Soc.

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125

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We present a statistical analysis of the environments of 11 supernovae (SNe) which occurred in 6 nearby galaxies (z 0.016). All galaxies were observed with MUSE, the high spatial resolution integral field spectrograph mounted to the 8m VLT UT4. These data enable us to map the full spatial extent of host galaxies up to ∼3 effective radii. In this way, not only can one characterise the specific host environment of each SN, one can compare their properties with stellar populations within the full range of other environments within the host. We present a method that consists of selecting all Hii regions found within host galaxies from 2D extinction-corrected Hα emission maps. These regions are then characterised in terms of their Hα equivalent widths, star formation rates, and oxygen abundances. Identifying Hii regions spatially coincident with SN explosion sites, we are thus able to determine where within the distributions of host galaxy e.g. metallicities and ages each SN is found, thus providing new constraints on SN progenitor properties. This initial pilot study using MUSE opens the way for a revolution in SN environment studies where we are now able to study multiple environment SN progenitor dependencies using a single instrument and single pointing.

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“…For example, the shape of the light curves of type IIn SNe depend on the initial radius of the star, the ejecta mass and the explosion energy of the SNe, and the density structures of the ejecta and CSM (van Marle et al 2010;Moriya et al 2013;Taddia et al 2015). The range of potential progenitors is large and may include any star with a significant pre-SN eruption, for example, red supergiants or luminous blue variables (LBVs) (Gall et al 2011;Stritzinger et al 2012;Van Dyk 2013). Lucy et al (1991) noted a shallow optical extinction curve inferred from the light curves of SN 1987A.…”

Section: Introductionmentioning

confidence: 99%

“…While this was inferred from significant attenuation of the red wings and corresponding blueshifts of the centroids of the hydrogen emission lines, no broadband color changes were detected in the light curves. SN 2005ip was discovered on 2005 November 5.2 UT in the Scd galaxy NGC 2906 (Boles et al 2005;Stritzinger et al 2012). The measured redshift of the host galaxy is 0.00714, corresponding to a luminosity distance of about 30 Mpc (de Vaucouleurs et al 1991;Smith et al 2009).…”

Section: Introductionmentioning

confidence: 99%

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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MULTI-WAVELENGTH OBSERVATIONS OF THE ENDURING TYPE IIn SUPERNOVAE 2005ip AND 2006jd

Cited by 173 publications

References 80 publications

Electron-capture supernovae exploding within their progenitor wind

Electron-capture supernovae exploding within their progenitor wind

Characterizing the environments of supernovae with MUSE

Early gray dust formation in the type IIn SN 2005ip

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