Spectrophotometric time series of SN 2011fe from the Nearby Supernova Factory

Pereira, R.; Thomas, R. C.; Aldering, G.; Antilogus, P.; Baltay, C.; Benitez-Herrera, S.; Bongard, S.; Buton, C.; Canto, A.; Cellier-Holzem, F.; Chen, J.; Childress, M.; Chotard, N.; Copin, Y.; Fakhouri, H.; Fink, Michael; Fouchez, D.; Gangler, É.; Guy, J.; Hillebrandt, W.; Hsiao, E. Y.; Kerschhaggl, M.; Kowalski, M.; Kromer, M.; Nordin, J.; Nugent, P.; Paech, K.; Pain, R.; Pécontal, É.; Perlmutter, S.; Rabinowitz, D.; Rigault, M.; Runge, K.; Saunders, C.; Smadja, G.; Tao, C.; Taubenberger, S.; Tilquin, A.; Wu, Chenjie

doi:10.1051/0004-6361/201221008

Cited by 196 publications

(125 citation statements)

References 103 publications

(162 reference statements)

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“…Si ii λ6355 line in velocity space. For comparison, we show the spectra of SNe 2012fr (Childress et al 2013), 2002bo (Benetti et al 2004Blondin et al 2012), 2002er (Kotak et al 2005), 2002dj (Pignata et al 2008), 2004dt (Altavilla et al 2007), 2011fe (Pereira et al 2013). unlikely explained by the ejecta-companion interaction scenario . There are also two peculiar SNe Ia showing an excessive early emission that are interpreted to be an explosion initiated by the helium detonation (Jiang et al 2017;De et al 2018).…”

Section: Prep)mentioning

confidence: 99%

SN 2019ein: New Insights into the Similarities and Diversity among High-velocity Type Ia Supernovae

Kawabata

Maeda

Yamanaka

et al. 2020

ApJ

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We present optical observations of type Ia supernova (SN) 2019ein, starting at 0.3 days since the discovery. The spectra and the light curves show that SN 2019ein belongs to the High-Velocity (HV) group with relatively rapid decline in the light curves (∆m 15 (B) = 1.36 ± 0.02 mag) and the short rise time. The Si ii λ6355 velocity, associated with a photospheric component but not with a detached high-velocity feature, reached ∼ 20,000 km s −1 in our first spectrum taken at 12 days before the B-band maximum. This is among the highest velocity seen in SNe Ia. The line velocity however decreased very rapidly and smoothly toward the maximum light, where it was ∼ 13, 000 km s −1 as relatively low among HV SNe. The rapid spectral evolution and the short rise time are probably linked to the rapidly evolving light curves, suggesting that not only the (maximum) velocity but also the light curve decline rate are controlling functions of the observational properties of HV SNe. The earliest light curves did not show noticeable excess, ruling out a giant companion star. Spectral synthesis modeling shows that the outermost layer at > 17, 000 km s −1 is well described by the O-Ne-C burning layer extending to at least 25, 000 km s −1 , and there is no unburnt carbon below 30, 000 km s −1 ; these properties are largely consistent with the delayed detonation scenario, and it is shared with the prototypical HV SN 2002bo despite large difference in ∆m 15 (B). This structure is strikingly different from that derived for the well-studied NV (Normal-Velocity) SN 2011fe; we suggest that the relation between the mass of 56 Ni (or ∆m 15 ) and the extent of the O-Ne-C provides an important constraint on the explosion mechanism(s) of HV and NV SNe.

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Section: Prep)mentioning

confidence: 99%

SN 2019ein: New Insights into the Similarities and Diversity among High-velocity Type Ia Supernovae

Kawabata

Maeda

Yamanaka

et al. 2020

ApJ

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“…We correct all spectra for both Milky Way reddening (Schlegel et al 1998;Schlafly & Finkbeiner 2011) and host-galaxy reddening as derived from the SN light curves (Phillips et al 1999;Foley et al 2012bFoley et al ,c, 2014Foley & Kirshner 2013;Pereira et al 2013;Silverman et al 2013;Amanullah et al 2014;Im et al 2015;Pan et al 2015;Shappee et al 2015).…”

Section: Data and Observationsmentioning

confidence: 99%

“…We present basic parameters, including light-curve shape, velocity, and hostgalaxy morphology for the sample in Table 1. Light-curve shape measurements were taken from the literature (Phillips et al 1999;Foley et al 2012bFoley et al ,c, 2014Foley & Kirshner 2013;Pereira et al 2013;Silverman et al 2013;Amanullah et al 2014;Im et al 2015;Pan et al 2015;Shappee et al 2015). For the ejecta velocity, we measure the velocity of the Si ii absorption-line minimum in the optical spectra, and correct those data to their maximum-light values , v 0 Si II .…”

Section: Sample Demographicsmentioning

confidence: 99%

Ultraviolet diversity of Type Ia Supernovae

Foley

Pan

Brown

et al. 2016

Mon. Not. R. Astron. Soc.

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Ultraviolet (UV) observations of Type Ia supernovae (SNe Ia) probe the outermost layers of the explosion, and UV spectra of SNe Ia are expected to be extremely sensitive to differences in progenitor composition and the details of the explosion. Here we present the first study of a sample of high signal-to-noise ratio SN Ia spectra that extend blueward of 2900Å. We focus on spectra taken within 5 days of maximum brightness. Our sample of ten SNe Ia spans the majority of the parameter space of SN Ia optical diversity. We find that SNe Ia have significantly more diversity in the UV than in the optical, with the spectral variance continuing to increase with decreasing wavelengths until at least 1800Å (the limit of our data). The majority of the UV variance correlates with optical light-curve shape, while there are no obvious and unique correlations between spectral shape and either ejecta velocity or host-galaxy morphology. Using light-curve shape as the primary variable, we create a UV spectral model for SNe Ia at peak brightness. With the model, we can examine how individual SNe vary relative to expectations based on only their light-curve shape. Doing this, we confirm an excess of flux for SN 2011fe at short wavelengths, consistent with its progenitor having a subsolar metallicity. While most other SNe Ia do not show large deviations from the model, ASASSN-14lp has a deficit of flux at short wavelengths, suggesting that its progenitor was relatively metal rich.

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“…After day +20, the SN is no longer detected in the Swift bands, so the small constant fraction reflects our method of accounting for missing data (with large error bars). For comparison, in the well-observed normal SN Ia 2011fe (Pereira, Aldering & Antilogus 2013), at most 13 per cent of the luminosity is emitted blueward of 3400 Å, reaching this point 5 d before B-band maximum light; the UV fraction is 9 per cent at day −10, and only 3 per cent at day −15. UV flux contributes only 2 per cent of SN 2011fe's total luminosity by day +20, and continues to decline thereafter.…”

Section: Bolometric Light Curvementioning

confidence: 99%

Early ultraviolet emission in the Type Ia supernova LSQ12gdj: No evidence for ongoing shock interaction

Scalzo¹,

Childress²,

Tucker³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present photospheric-phase observations of LSQ12gdj, a slowly-declining, UV-bright Type Ia supernova. Classified well before maximum light, LSQ12gdj has extinction-corrected absolute magnitude M B = −19.8, and pre-maximum spectroscopic evolution similar to SN 1991T and the super-Chandrasekhar-mass SN 2007if. We use ultraviolet photometry from Swift, ground-based optical photometry, and corrections from a near-infrared photometric template to construct the bolometric (1600-23800 Å) light curve out to 45 days past B-band maximum light. We estimate that LSQ12gdj produced 0.96 ± 0.07 M ⊙ of 56 Ni, with an ejected mass near or slightly above the Chandrasekhar mass. As much as 27% of the flux at the earliest observed phases, and 17% at maximum light, is emitted bluewards of 3300 Å. The absence of excess luminosity at late times, the cutoff of the spectral energy distribution bluewards of 3000 Å, and the absence of narrow line emission and strong Na I D absorption all argue against a significant contribution from ongoing shock interaction. However, ∼ 10% of LSQ12gdj's luminosity near maximum light could be produced by the release of trapped radiation, including kinetic energy thermalized during a brief interaction with a compact, hydrogen-poor envelope (radius < 10 13 cm) shortly after explosion; such an envelope arises generically in double-degenerate merger scenarios.

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Spectrophotometric time series of SN 2011fe from the Nearby Supernova Factory

Cited by 196 publications

References 103 publications

SN 2019ein: New Insights into the Similarities and Diversity among High-velocity Type Ia Supernovae

SN 2019ein: New Insights into the Similarities and Diversity among High-velocity Type Ia Supernovae

Ultraviolet diversity of Type Ia Supernovae

Early ultraviolet emission in the Type Ia supernova LSQ12gdj: No evidence for ongoing shock interaction

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