EVIDENCE FOR TYPE Ia SUPERNOVA DIVERSITY FROM ULTRAVIOLET OBSERVATIONS WITH THE<i>HUBBLE SPACE TELESCOPE</i>

Wang, Xiaofeng; Wang, Lifan; Filippenko, A. V.; Baron, E.; Kromer, M.; Jack, D.; Zhang, Tianmeng; Aldering, G.; Antilogus, P.; Arnett, W. David; Baade, D.; Barris, B.; Benetti, S.; Bouchet, P.; Burrows, Adam; Canal, R.; Cappellaro, E.; Carlberg, R. G.; Carlo, E. Di; Challis, Peter; Crotts, Arlin; Danziger, John; Valle, M. Della; Fink, Michael; Foley, R. J.; Fransson, Claes; Gal‐Yam, A.; Garnavich, P.; Gerardy, C.; Goldhaber, G.; Hamuy, M.; Hillebrandt, W.; Höflich, Peter; Holland, S. T.; Holz, D. E.; Hughes, John P.; Jeffery, David J.; Jha, Saurabh W.; Kasen, Daniel; Khokhlov, A. M.; Kirshner, R.; Knop, R. A.; Kozma, Cecilia; Krisciunas, K.; Lee, Brian C.; Leibundgut, B.; Lentz, Eric J.; Leonard, Douglas C.; Lewin, W. H. G.; Li, Weidong; Livio, Mario; Lundqvist, Peter; Maoz, Dan; Matheson, T.; Mazzali, P. A.; Meikle, P.; Miknaitis, G.; Milne, Peter; Mochnacki, S. W.; Nomoto, Ken’ichi; Nugent, P.; Oran, Elaine S.; Panagia, N.; Perlmutter, S.; Phillips, M. M.; Pinto, Philip A.; Poznanski, D.; Pritchet, C. J.; Reinecke, M.; Riess, Adam G.; Ruiz‐Lapuente, P.; Scalzo, R.; Schlegel, Eric M.; Schmidt, B. P.; Siegrist, J.; Söderberg, A. M.; Sollerman, J.; Sonneborn, G.; Spadafora, A. L.; Spyromilio, J.; Sramek, R. A.; Starrfield, S.; Strolger, L. G.; Suntzeff, Nicholas B.; Thomas, R. C.; Tonry, J.; Tornambé, Amedeo; Truran, J. W.; Turatto, M.; Turner, Michael S.; Dyk, Schuyler D. Van; Weiler, K. W.; Wheeler, J. C.; Wood-Vasey, Michael; Woosley, S. E.; Yamaoka, H.

doi:10.1088/0004-637x/749/2/126

Cited by 52 publications

(43 citation statements)

References 97 publications

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“…SN 1998bu had a light echo (Cappellaro et al 2001;Garnavich et al 2001), but that was due to foreground material and not to a CSM. SN 2005cf was observed early in the ultraviolet (UV) with the HST (Wang et al 2012) and with Swift, starting −8.8 and −7.8 days before B maximum, respectively. A comprehensive compilation of data and an analysis were presented in Gall et al (2012), but there is no evidence of enhanced early flux indicative of the ejecta interacting with nearby material.…”

Section: Broad Lines Of Sn 2011fe and 2014jmentioning

confidence: 99%

No trace of a single-degenerate companion in late spectra of supernovae 2011fe and 2014J

Lundqvist

Nyholm

Taddia

et al. 2015

A&A

121

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Aims. This study aims at constraining the origin of the nearby Type Ia supernovae (SNe), 2011fe and 2014J. The two most favoured scenarios for triggering the explosion of the white dwarf supernova progenitor is either mass loss from a non-degenerate companion or merger with another white dwarf. In the former, there could be a significant amount of leftover material from the companion at the centre of the supernova. Detecting such material would therefore favour the single-degenerate scenario. Methods. The left-over material from a possible non-degenerate companion can reveal itself after about one year, and in this study such material was searched for in the spectra of SN 2011fe (at 294 days after the explosion) using the Large Binocular Telescope and for SN 2014J using the Nordic Optical Telescope (315 days past explosion). The observations were interpreted using numerical models simulating the expected line emission from ablated material from the companion star. λλ7291, 7324 could be traced for in any of the two supernovae. When systematic uncertainties are included, the limits on hydrogen-rich ablated gas are 0.003 M in SN 2011fe and 0.0085 M in SN 2014J, where the limit for SN 2014J is the second lowest ever, and the limit for SN 2011fe is a revision of a previous limit. Limits are also put on heliumrich ablated gas, and here limits from [O I] λ6300 provide the upper mass limits 0.002 M and 0.005 M for SNe 2011fe and 2014J, respectively. These numbers are used in conjunction with other data to argue that these supernovae can stem from double-degenerate systems or from single-degenerate systems with a spun-up/spun-down super-Chandrasekhar white dwarf. For SN 2011fe, other types of hydrogen-rich donors can very likely be ruled out, whereas a main-sequence donor system with large intrinsic separation is still possible for SN 2014J. Helium-rich donor systems cannot be ruled out for any of the two supernovae, but the expected short delay time for such progenitors makes this possibility less likely, especially for SN 2011fe. Published data for SNe 1998bu, 2000cx, 2001el, 2005am, and 2005cf are used to constrain their origin. We emphasise that the results of this study depend on the sought-after lines emerging unattenuated from the central regions of the nebula. Detailed radiative transfer calculations with longer line lists than are presently used are needed to confirm that this is, in fact, true. Finally, the broad lines of SNe 2011fe and 2014J are discussed, and it is found that the [Ni II] λ7378 emission is redshifted by ∼+1300 km s −1 , as opposed to the known blueshift of ∼−1100 km s −1 for SN 2011fe. [Fe II] λ7155 is also redshifted in SN 2014J. SN 2014J belongs to a minority of SNe Ia that both have a nebular redshift of [Fe II] λ7155 and [Ni II] λ7378, and a slow decline of the Si II λ6355 absorption trough just after B-band maximum.

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Section: Broad Lines Of Sn 2011fe and 2014jmentioning

confidence: 99%

No trace of a single-degenerate companion in late spectra of supernovae 2011fe and 2014J

Lundqvist

Nyholm

Taddia

et al. 2015

A&A

121

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“…The UV flux of SN Ia is wildly variable compared to optical counterparts, which has highlighted UV wavelength regions as a capable, albeit challenging probe for physics unseen by optical wavelengths (Kirshner et al 1993;Wang et al 2012;Milne et al 2013;Mazzali et al 2014). Compared to SN 2009dc, SN 2005cf and other normal SN Ia are typically redder at NUV wavelengths prior to maximum light (Brown et al 2009;Milne et al 2010;Brown et al 2010Brown et al , 2012, with some fraction of "carbon-positive" events being relatively bluer at NUV wavelengths (Thomas et al 2011a;Milne et al 2013).…”

Section: Colorsmentioning

confidence: 99%

Comparative analysis of SN 2012dn optical spectra: days −14 to +114

Parrent¹,

Howell²,

Fesen³

et al. 2016

Mon. Not. R. Astron. Soc.

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SN 2012dn is a super-Chandrasekhar mass candidate in a purportedly normal spiral (SAcd) galaxy, and poses a challenge for theories of type Ia supernova diversity. Here we utilize the fast and highly parameterized spectrum synthesis tool, SYNAPPS, to estimate relative expansion velocities of species inferred from optical spectra obtained with six facilities. As with previous studies of normal SN Ia, we find that both unburned carbon and intermediate mass elements are spatially coincident within the ejecta near and below 14,000 km s −1 . Although the upper limit on SN 2012dn's peak luminosity is comparable to some of the most luminous normal SN Ia, we find a progenitor mass exceeding ∼ 1.6 M is not strongly favored by leading merger models since these models do not accurately predict spectroscopic observations of SN 2012dn and more normal events. In addition, a comparison of light curves and host-galaxy masses for a sample of literature and Palomar Transient Factory SN Ia reveals a diverse distribution of SN Ia subtypes where carbon-rich material remains unburned in some instances. Such events include SN 1991T, 1997br, and 1999aa where trace signatures of C III at optical wavelengths are presumably detected.

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“…For instance, using data from 80 SNe Ia with considerable reddening (i.e., E B−V < 0.87 mag), Nobili & Goobar (2008) report an unusually low value of R V ∼ 1.75 (see also Phillips et al 2013), much lower than the typical value R V ∼ 3.1 for interstellar grains in the Milky Way. Recently, using data from UV to near-IR (λ ∼ 0.2 − 2 µm) from Hubble and Swift satellites, Amanullah et al (2015) present a diversity in extinction curves, with R V ranging from 1.4 to 3 (see also Wang et al (2012)). Unprecedented low values of R V toward numerous SNe Ia are attributed to the scattering by circumstellar (CS) dust (see, e.g.…”

Section: Introductionmentioning

confidence: 99%

Properties and Alignment of Interstellar Dust Grains toward Type Ia Supernovae with Anomalous Polarization Curves

Hoang

2017

ApJ

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Recent photometric and polarimetric observations of type Ia supernovae (SNe Ia) show unusually low total-to-selective extinction ratio (R V < 2) and wavelength of maximum polarization (λ max < 0.4 µm) for several SNe Ia, which indicates peculiar properties of interstellar (IS) dust in the SN hosted galaxies and/or the presence of circumstellar (CS) dust. In this paper, we use inversion technique to infer bestfit grain size distribution and alignment function of interstellar grains along the lines of sight toward four SNe Ia with anomalous extinction and polarization data (SNe 1986G, 2006X, 2008fp, and 2014J). We find that to reproduce low values of R V , a significant enhancement in the mass of small grains of radius a < 0.1 µm is required. For SN 2014J, a simultaneous fit to its observed extinction and polarization is unsuccessful if the entire data are attributed to IS dust (model 1), but a good fit is obtained when accounting for the contribution of CS dust (model 2). For SN 2008fp, our best-fit results for model 1 show that, to reproduce an extreme value of λ max ∼ 0.15 µm, small silicate grains must be aligned as efficiently as big grains. For this case, we suggest that strong radiation from the SN can induce efficient alignment of small grains in a nearby intervening molecular cloud via radiative torque mechanism. The resulting time dependence polarization from this RAT alignment model can be tested by observing at ultraviolet wavelengths.

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EVIDENCE FOR TYPE Ia SUPERNOVA DIVERSITY FROM ULTRAVIOLET OBSERVATIONS WITH THEHUBBLE SPACE TELESCOPE

Cited by 52 publications

References 97 publications

No trace of a single-degenerate companion in late spectra of supernovae 2011fe and 2014J

No trace of a single-degenerate companion in late spectra of supernovae 2011fe and 2014J

Comparative analysis of SN 2012dn optical spectra: days −14 to +114

Properties and Alignment of Interstellar Dust Grains toward Type Ia Supernovae with Anomalous Polarization Curves

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