NEAR-ULTRAVIOLET PROPERTIES OF A LARGE SAMPLE OF TYPE Ia SUPERNOVAE AS OBSERVED WITH THE<i>Swift</i>UVOT

Milne, Peter; Brown, P. J.; Roming, P. W. A.; Holland, S. T.; Immler, S.; Filippenko, A. V.; Ganeshalingam, M.; Li, Weidong; Stritzinger, M. D.; Phillips, M. M.; Hicken, M.; Kirshner, R.; Challis, Peter; Mazzali, P. A.; Schmidt, B.; Bufano, F.; Gehrels, N.; Berk, Daniel Vanden

doi:10.1088/0004-637x/721/2/1627

Cited by 69 publications

(82 citation statements)

References 93 publications

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“…In the process of computing definitive photometry, science images of SN 2011iv were used for host-galaxy subtraction of SN 2007on's science images, while science images of SN 2007on were used for host-galaxy subtraction of SN 2011iv's science images. photometry is provided in Table 1; we note that the photometry of SN 2007on presented here supersedes the photometry published by Milne et al (2010).…”

Section: Observationssupporting

confidence: 63%

Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv

Gall

Stritzinger

Ashall

et al. 2018

A&A

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We present an analysis of ultraviolet (UV) to near-infrared observations of the fast-declining Type Ia supernovae (SNe Ia) 2007on and 2011iv, hosted by the Fornax cluster member NGC 1404. The B-band light curves of SN 2007on and SN 2011iv are characterised by ∆m 15 (B) decline-rate values of 1.96 mag and 1.77 mag, respectively. Although they have similar decline rates, their peak B-and H-band magnitudes differ by ∼ 0.60 mag and ∼ 0.35 mag, respectively. After correcting for the luminosity vs. decline rate and the luminosity vs. colour relations, the peak B-band and H-band light curves provide distances that differ by ∼ 14% and ∼ 9%, respectively. These findings serve as a cautionary tale for the use of transitional SNe Ia located in early-type hosts in the quest to measure cosmological parameters. Interestingly, even though SN 2011iv is brighter and bluer at early times, by three weeks past maximum and extending over several months, its B − V colour is 0.12 mag redder than that of SN 2007on. To reconcile this unusual behaviour, we turn to guidance from a suite of spherical one-dimensional Chandrasekhar-mass delayed-detonation explosion models. In this context, 56 Ni production depends on both the so-called transition density and the central density of the progenitor white dwarf. To first order, the transition density drives the luminosity-width relation, while the central density is an important second-order parameter. Within this context, the differences in the B − V color evolution along the Lira regime suggests the progenitor of SN 2011iv had a higher central density than SN 2007on.

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Section: Observationssupporting

confidence: 63%

Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv

Gall

Stritzinger

Ashall

et al. 2018

A&A

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“…A comparison with observed UV light curves of SNe Ia Milne et al 2010) shows that the SN component of the model peaks brighter than most observed SNe, which show great diversity. This discrepancy is likely due to incomplete line lists for the iron-peak elements whose absorption blanket the UV (D. Kasen 2011, private communication).…”

Section: Theoretical Predictions For the Brightness Of The Shockmentioning

confidence: 86%

“…This discrepancy is likely due to incomplete line lists for the iron-peak elements whose absorption blanket the UV (D. Kasen 2011, private communication). A detailed comparison between theoretical models and the growing sample of UV photometry and spectroscopy Milne et al 2010;Bufano et al 2009;Foley et al 2012) is beyond the scope of this paper.…”

Section: Theoretical Predictions For the Brightness Of The Shockmentioning

confidence: 99%

CONSTRAINTS ON TYPE Ia SUPERNOVA PROGENITOR COMPANIONS FROM EARLY ULTRAVIOLET OBSERVATIONS WITHSWIFT

Brown

Dawson

Harris

et al. 2012

ApJ

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We compare early ultraviolet (UV) observations of Type Ia supernovae (SNe Ia) with theoretical predictions for the brightness of the shock associated with the collision between SN ejecta and a companion star. Our simple method is independent of the intrinsic flux from the SN and treats the flux observed with the Swift/Ultra-Violet Optical Telescope as conservative upper limits on the shock brightness. Comparing this limit with the predicted flux for various shock models, we constrain the geometry of the SN progenitor-companion system. We find the model of a 1 M red supergiant companion in Roche-lobe overflow to be excluded at a 95% confidence level for most individual SNe for all but the most unfavorable viewing angles. For the sample of 12 SNe taken together, the upper limits on the viewing angle are inconsistent with the expected distribution of viewing angles for red gaint stars as the majority of companions with high confidence. The separation distance constraints do allow main-sequence companions. A better understanding of the UV flux arising from the SN itself as well as continued UV observations of young SNe Ia will further constrain the possible progenitors of SNe Ia. From the first detections of the acceleration of an expanding universe (Riess et al. 1998;Perlmutter et al. 1999), Type Ia supernovae (SNe Ia) have continued to be the best probes of the distant universe for measuring cosmological parameters (see recent results in, e.g., Riess et al. 2011;Sullivan et al. 2011;Suzuki et al. 2012). They are useful as standardizable candles because of the well-established empirical relationship between the absolute brightness and other observables such as the light curve shape and colors (cf. Phillips et al. 1999;Jha et al. 2007;Guy et al. 2007). Hundreds of SNe later, SN cosmology is now limited by systematic rather than statistical errors (Wood-Vasey et al. 2007;Kessler et al. 2009;Conley et al. 2011).One systematic error for using SNe Ia at cosmological distances may arise from redshift evolution in the SN explosions due to differences in the average properties (mass, metallicity, etc.) of the progenitor systems (Mannucci et al. 2006;Howell et al. 2007). This is especially worrisome because the underlying progenitor system for an SN Ia explosion is still unknown, with two favored progenitor scenarios (Livio 2000). In the single degenerate case, a carbon-oxygen white dwarf (WD) accretes material from a main-sequence (MS) or red giant (RG) companion star and explodes when it nears the Chandrasekhar mass (Whelan & Iben 1973;Nomoto 1982). Alternatively, the double degenerate scenario involves two WDs which merge and explode (Webbink 1984; Iben & Tutukov 1984). Determining the nature of the progenitor systems of SNe Ia is critical to confidently and precisely use them as cosmological standard candles.In an effort to improve our understanding of the progenitors in the single degenerate scenario, several groups have studied various effects of an SN Ia explosion on a companion star. These include the amount...

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“…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). Brown et al (2014) report the early UV colors of SN 2012dn-like events are bluer than normal as well.…”

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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NEAR-ULTRAVIOLET PROPERTIES OF A LARGE SAMPLE OF TYPE Ia SUPERNOVAE AS OBSERVED WITH THESwiftUVOT

Cited by 69 publications

References 93 publications

Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv

Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv

CONSTRAINTS ON TYPE Ia SUPERNOVA PROGENITOR COMPANIONS FROM EARLY ULTRAVIOLET OBSERVATIONS WITHSWIFT

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

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